FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Carls, MG Holland, L Irvine, GV Mann, DH Lindeberg, M AF Carls, Mark G. Holland, Larry Irvine, Gail V. Mann, Daniel H. Lindeberg, Mandy TI PETROLEUM BIOMARKERS AS TRACERS OF EXXON VALDEZ OIL SO ENVIRONMENTAL TOXICOLOGY AND CHEMISTRY LA English DT Article DE Biomarker; Exxon Valdez oil; Forensic ID PRINCE-WILLIAM-SOUND; SUBTIDAL SEDIMENTS; NORTHERN GULF; MUSSEL BEDS; ALASKA; SPILL; PERSISTENCE; BEACHES; HYDROCARBONS; EMBAYMENTS AB Over the past quarter century, petroleum biomarkers have persisted in sequestered Exxon Valdez oil in Prince William Sound and the Gulf of Alaska (USA), and hence the oil has remained identifiable. These biomarkers are molecular fossils derived from biochemicals in previously living organisms. Novel pattern matching indicated the presence of Alaska North Slope crude oil (ANSCO) over the entire observation period at most sites (7 of 9) and distinguished this source from several other potential sources. The presence of ANSCO was confirmed with Nordtest forensics, demonstrating the veracity of the new method. The principal advantage of the new method is that it provides sample-specific identification, whereas the Nordtest approach is based on multisample statistics. Biomarkers were conserved relative to other constituents, and thus concentrations (per g oil) in initial beach samples were greater than those in fresh oil because they were lost more slowly than more labile oil constituents such as straight-chain alkanes and aromatic hydrocarbons. However, biomarker concentrations consistently declined thereafter (1989-2014), although loss varied substantially among and within sites. Isoprenoid loss was substantially greater than tricyclic triterpane, hopane, and sterane loss. (C) 2016 The Authors. Environmental Toxicology and Chemistry published by Wiley Periodicals, Inc. on behalf of SETAC. This article is aUS government work and as such, is in the public domain in the United States of America. C1 [Carls, Mark G.; Holland, Larry; Lindeberg, Mandy] Natl Marine Fisheries Serv, Auke Bay Labs, Juneau, AK 99802 USA. [Carls, Mark G.; Holland, Larry; Lindeberg, Mandy] NOAA, Juneau, AK 99802 USA. [Irvine, Gail V.] US Geol Survey, Alaska Sci Ctr, Anchorage, AK USA. [Mann, Daniel H.] Univ Alaska, Sch Nat Resources, Geog Program, Fairbanks, AK 99701 USA. RP Carls, MG (reprint author), Natl Marine Fisheries Serv, Auke Bay Labs, Juneau, AK 99802 USA.; Carls, MG (reprint author), NOAA, Juneau, AK 99802 USA. EM mark.carls@noaa.gov NR 25 TC 1 Z9 1 U1 15 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0730-7268 EI 1552-8618 J9 ENVIRON TOXICOL CHEM JI Environ. Toxicol. Chem. PD NOV PY 2016 VL 35 IS 11 BP 2683 EP 2690 DI 10.1002/etc.3454 PG 8 WC Environmental Sciences; Toxicology SC Environmental Sciences & Ecology; Toxicology GA EA2XU UT WOS:000386461000006 PM 27067268 ER PT J AU Cammarano, D Rotter, RP Asseng, S Ewert, F Wallach, D Martre, P Hatfield, JL Jones, JW Rosenzweig, C Ruane, AC Boote, KJ Thorburn, PJ Kersebaum, KC Aggarwal, PK Angulo, C Basso, B Bertuzzi, P Biernath, C Brisson, N Challinor, AJ Doltra, J Gayler, S Goldberg, R Heng, L Hooker, J Hunt, LA Ingwersen, J Izaurralde, RC Muller, C Kumar, SN Nendel, C O'Leary, GJ Olesen, JE Osborne, TM Palosuo, T Priesack, E Ripoche, D Semenov, MA Shcherbak, I Steduto, P Stockle, CO Stratonovitch, P Streck, T Supit, I Tao, F Travasso, M Waha, K White, JW Wolf, J AF Cammarano, Davide Rotter, Reimund P. Asseng, Senthold Ewert, Frank Wallach, Daniel Martre, Pierre Hatfield, Jerry L. Jones, James W. Rosenzweig, Cynthia Ruane, Alex C. Boote, Kenneth J. Thorburn, Peter J. Kersebaum, Kurt Christian Aggarwal, Pramod K. Angulo, Carlos Basso, Bruno Bertuzzi, Patrick Biernath, Christian Brisson, Nadine Challinor, Andrew J. Doltra, Jordi Gayler, Sebastian Goldberg, Richie Heng, Lee Hooker, Josh Hunt, Leslie A. Ingwersen, Joachim Izaurralde, Roberto C. Mueller, Christoph Kumar, Soora Naresh Nendel, Claas O'Leary, Garry J. Olesen, Jorgen E. Osborne, Tom M. Palosuo, Taru Priesack, Eckart Ripoche, Dominique Semenov, Mikhail A. Shcherbak, Iurii Steduto, Pasquale Stockle, Claudio O. Stratonovitch, Pierre Streck, Thilo Supit, Iwan Tao, Fulu Travasso, Maria Waha, Katharina White, Jeffrey W. Wolf, Joost TI Uncertainty of wheat water use: Simulated patterns and sensitivity to temperature and CO2 SO FIELD CROPS RESEARCH LA English DT Article DE Multi-model simulation; Transpiration efficiency; Water use; Uncertainty; Sensitivity ID CLIMATE-CHANGE; USE EFFICIENCY; CROP YIELD; POTENTIAL EVAPOTRANSPIRATION; ATMOSPHERIC CO2; FOOD SECURITY; ELEVATED CO2; IMPACTS; PRODUCTIVITY; MODELS AB Projected global warming and population growth will reduce future water availability for agriculture. Thus, it is essential to increase the efficiency in using water to ensure crop productivity. Quantifying crop water use (WU; i.e. actual evapotranspiration) is a critical step towards this goal. Here, sixteen wheat simulation models were used to quantify sources of model uncertainty and to estimate the relative changes and variability between models for simulated WU, water use efficiency (WUE, WU per unit of grain dry mass produced), transpiration efficiency (T-eff, transpiration per kg of unit of grain yield dry mass produced), grain yield, crop transpiration and soil evaporation at increased temperatures and elevated atmospheric carbon dioxide concentrations ([CO2]). The greatest uncertainty in simulating water use, potential evapotranspiration, crop transpiration and soil evaporation was due to differences in how crop transpiration was modelled and accounted for 50% of the total variability among models. The simulation results for the sensitivity to temperature indicated that crop WU will decline with increasing temperature due to reduced growing seasons. The uncertainties in simulated crop WU, and in particularly due to uncertainties in simulating crop transpiration, were greater under conditions of increased temperatures and with high temperatures in combination with elevated atmospheric [CO2] concentrations. Hence the simulation of crop WU, and in particularly crop transpiration under higher temperature, needs to be improved and evaluated with field measurements before models can be used to simulate climate change impacts on future crop water demand. (C) 2016 Elsevier B.V. All rights reserved. C1 [Cammarano, Davide; Asseng, Senthold; Jones, James W.; Boote, Kenneth J.] Univ Florida, Agr & Biol Engn Dept, Gainesville, FL 32611 USA. [Rotter, Reimund P.; Palosuo, Taru; Tao, Fulu] Nat Resources Inst Finland Luke, FI-00790 Helsinki, Finland. [Ewert, Frank; Angulo, Carlos] Univ Bonn, Inst Crop Sci & Resource Conservat INRES, D-53115 Bonn, Germany. [Wallach, Daniel] INRA, Agrosyst & Dev Terr UMR1248, F-31326 Castanet Tolosan, France. [Martre, Pierre] INRA, Genet Divers & Ecophysiol Cereals GDEC UMR1095, F-63100 Clermont Ferrand, France. [Martre, Pierre] Univ Blaise Pascal, GDEC UMR1095, F-63170 Clermont Ferrand, France. [Hatfield, Jerry L.] Natl Lab Agr & Environm, Ames, IA 50011 USA. [Rosenzweig, Cynthia; Ruane, Alex C.; Goldberg, Richie] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Thorburn, Peter J.] CSIRO, Ecosyst Sci, Dutton Pk, Qld 4102, Australia. [Kersebaum, Kurt Christian; Nendel, Claas] Leibniz Ctr Agr Landscape Res, Inst Landscape Syst Anal, D-15374 Muncheberg, Germany. [Aggarwal, Pramod K.] CIMMYT, CGIAR Res Program Climate Change Agr & Food Secur, New Delhi 110012, India. [Basso, Bruno] Michigan State Univ, Dept Geol Sci, E Lansing, MI 48824 USA. [Basso, Bruno] Michigan State Univ, Kellogg Biol Stn, E Lansing, MI 48824 USA. [Bertuzzi, Patrick; Ripoche, Dominique] INRA, AgroClim US1116, F-84914 Avignon, France. [Biernath, Christian; Priesack, Eckart] Helmholtz Zentrum Munchen, German Res Ctr Environm Hlth, Inst Soil Ecol, D-85764 Neuherberg, Germany. [Brisson, Nadine] INRA, Agron UMR0211, F-78750 Thiverval Grignon, France. [Brisson, Nadine] AgroParisTech, Agron UMR0211, F-78750 Thiverval Grignon, France. [Challinor, Andrew J.] Univ Leeds, Inst Climate & Atmospher Sci, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. [Challinor, Andrew J.] CIAT, CGIAR ESSP Program Climate Change Agr & Food Secu, Cali 6713, Colombia. [Doltra, Jordi] Cantabrian Agr Res & Training Ctr CIFA, Muriedas 39600, Spain. [Gayler, Sebastian] Univ Tubingen, Water & Earth Syst Sci Competence Cluster, D-72074 Tubingen, Germany. [Heng, Lee] IAEA, A-1400 Vienna, Austria. [Hooker, Josh] Univ Reading, Sch Agr Policy & Dev, Reading RG6 6AR, Berks, England. [Hooker, Josh] Joint Res Ctr, Via Enrico Fermi 2749, I-21027 Ispra, Italy. [Hunt, Leslie A.] Univ Guelph, Dept Plant Agr, Guelph, ON N1G 2W1, Canada. [Ingwersen, Joachim; Streck, Thilo] Univ Hohenheim, Inst Soil Sci & Land Evaluat, D-70599 Stuttgart, Germany. [Izaurralde, Roberto C.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Izaurralde, Roberto C.] Texas A&M Univ, Texas A&M AgriLife Res & Extens Ctr, Temple, TX 76502 USA. [Mueller, Christoph; Waha, Katharina] Potsdam Inst Climate Impact Res, D-14473 Potsdam, Germany. [Kumar, Soora Naresh] Indian Agr Res Inst, Ctr Environm Sci & Climate Resilient Agr, New Delhi 110012, India. [O'Leary, Garry J.] Dept Econ Dev Jobs Transport & Resources, Landscape & Water Sci, Horsham, Vic 3400, Australia. [Olesen, Jorgen E.] Aarhus Univ, Dept Agroecol, DK-8830 Tjele, Denmark. [Osborne, Tom M.] Univ Reading, Dept Meteorol, Natl Ctr Atmospher Sci, Reading RG6 6BB, Berks, England. [Semenov, Mikhail A.; Stratonovitch, Pierre] Rothamsted Res, Computat & Syst Biol Dept, Harpenden AL5 2JQ, Herts, England. [Steduto, Pasquale] Food & Agr Org United Nations FAO, Rome, Italy. [Shcherbak, Iurii; Stockle, Claudio O.] Washington State Univ, Biol Syst Engn, Pullman, WA 99164 USA. [Supit, Iwan] Wageningen Univ, Water Syt & Global Change Grp, NL-6700 AP Wageningen, Netherlands. [Tao, Fulu] Chinese Acad Sci, Inst Geog Sci & Nat Resources Res, Beijing 100101, Peoples R China. [Travasso, Maria] INTA CIRN, Inst Climate & Water, RA-1712 Castelar, Argentina. [White, Jeffrey W.] USDA ARS, ALARC, Maricopa, AZ USA. [Wolf, Joost] Wageningen Univ, Plant Prod Syst, NL-6700 AA Wageningen 37, Netherlands. [Rotter, Reimund P.] Univ Gottingen, Dept Crop Sci, Gottingen, Germany. [Ewert, Frank] Leibniz Ctr Agr Landscape Res ZALF, D-15374 Muncheberg, Germany. [Cammarano, Davide] James Hutton Inst, Dundee DD2 5DA, Scotland. [Martre, Pierre] INRA, Montpellier SupAgro, Lab Ecophysiol Plantes Stress Environm UMR759, F-34060 Montpellier, France. [Waha, Katharina] CSIRO, Agr, 306 Carmody Rd, St Lucia, Qld 4067, Australia. RP Cammarano, D (reprint author), Univ Florida, Agr & Biol Engn Dept, Gainesville, FL 32611 USA.; Cammarano, D (reprint author), James Hutton Inst, Dundee DD2 5DA, Scotland. EM Davide.Cammarano@hutton.ac.uk RI Palosuo, Taru/B-9593-2012; Thorburn, Peter/A-6884-2011; Doltra, Jordi/C-2106-2015; Challinor, Andrew/C-4992-2008 OI Palosuo, Taru/0000-0003-4322-3450; Challinor, Andrew/0000-0002-8551-6617 FU Ministry of Science, Research and Arts of Baden-Wurttemberg [AZ Zu 33-721.3-2]; Helmholtz Center for Environmental Research, Leipzig; European FACCE MACSUR project through the Finnish Ministry of Agriculture and Forestry; INRA Environment and Agronomy Division; framework of JPI FACCE MACSUR project through the INRA Metaprogram on the Adaptation of Agriculture and Forests to Climate Change; German Federal Office for Agriculture and Food; FACCE MACSUR [2812ERA147]; COST [ES1106]; KULUNDA [01LL0905L]; FACCE MACSUR through the German Federal Ministry of Education and Research (BMBF) [031A103B]; project of Regional Approaches to Climate Change for Pacific Northwest Agriculture (REACCH-PNA) from National Institute for Food and Agriculture [2011-68002-30191] FX We thank the anonymous referees for the valuable comments and suggestions that helped improve the manuscript. S.G. was supported by a grant from the Ministry of Science, Research and Arts of Baden-Wurttemberg (AZ Zu 33-721.3-2) and the Helmholtz Center for Environmental Research, Leipzig (UFZ); R.P.R., T.P. and F.T. were supported by funds from the European FACCE MACSUR project through the Finnish Ministry of Agriculture and Forestry; P.M., P.B., N.B. and D.R. were supported by INRA Environment and Agronomy Division and by the funding within the framework of JPI FACCE MACSUR project through the INRA Metaprogram on the Adaptation of Agriculture and Forests to Climate Change; K.C.K. and C.N. received support from the German Federal Office for Agriculture and Food with FACCE MACSUR (2812ERA147) and from COST ES1106; C.M. acknowledges financial support from the KULUNDA project (01LL0905L) and the FACCE MACSUR project (031A103B) funded through the German Federal Ministry of Education and Research (BMBF); C.O.S. was supported by the project of Regional Approaches to Climate Change for Pacific Northwest Agriculture (REACCH-PNA) funded through award #2011-68002-30191 from the National Institute for Food and Agriculture. This work has been carried out under the framework of the Agricultural Model Inter comparison and Improvment Project (AgMIP). NR 67 TC 2 Z9 2 U1 49 U2 49 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-4290 EI 1872-6852 J9 FIELD CROP RES JI Field Crop. Res. PD NOV PY 2016 VL 198 BP 80 EP 92 DI 10.1016/j.fcr.2016.08.015 PG 13 WC Agronomy SC Agriculture GA EA2FX UT WOS:000386409300009 ER PT J AU Hong, YL Liu, GS Li, JLF AF Hong, Yulan Liu, Guosheng Li, J. -L. F. TI Assessing the Radiative Effects of Global Ice Clouds Based on CloudSat and CALIPSO Measurements SO JOURNAL OF CLIMATE LA English DT Article ID CIRRUS CLOUDS; OPTICAL-PROPERTIES; SOFTWARE PACKAGE; WATER-CONTENT; SCATTERING; CLIMATE; RETRIEVAL; PRODUCTS; LIDAR; PARAMETERIZATION AB Although it is well established that cirrus warms Earth, the radiative effect of the entire spectrum of ice clouds is not well understood. In this study, the role of all ice clouds in Earth's radiation budget is investigated by performing radiative transfer modeling using ice cloud properties retrieved from CloudSat and CALIPSO measurements as inputs. Results show that, for the 2008 period, the warming effect (similar to 21.8 +/- 5.4 W m(-2)) induced by ice clouds trapping longwave radiation exceeds their cooling effect (similar to-16.7 +/- 1.7 W m(-2)) caused by shortwave reflection, resulting in a net warming effect (similar to 5.1 +/- 3.8 W m(-2)) globally on the earthatmosphere system. The net warming is over 15 W m(-2) in the tropical deep convective regions, whereas cooling occurs in the midlatitudes, which is less than 10 W m(-2) in magnitude. Seasonal variations of ice cloud radiative effects are evident in the midlatitudes where the net effect changes from warming during winter to cooling during summer, whereas warming occurs all year-round in the tropics. Ice cloud optical depth t is shown to be an important factor in determining the sign and magnitude of the net radiative effect. Ice clouds with tau < 4.6 display a warming effect with the largest contributions from those with tau approximate to 1.0. In addition, ice clouds cause vertically differential heating and cooling of the atmosphere, particularly with strong heating in the upper troposphere over the tropics. At Earth's surface, ice clouds produce a cooling effect no matter how small the tau value is. C1 [Hong, Yulan; Liu, Guosheng] Florida State Univ, Dept Earth Ocean & Atmospher Sci, 1017 Acad Way,319 Love Bldg, Tallahassee, FL 32306 USA. [Li, J. -L. F.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Hong, YL (reprint author), Florida State Univ, Dept Earth Ocean & Atmospher Sci, 1017 Acad Way,319 Love Bldg, Tallahassee, FL 32306 USA. EM yh12c@my.fsu.edu RI Liu, Guosheng/D-3479-2011 OI Liu, Guosheng/0000-0001-7899-6125 FU NASA [NNX13AQ39G, NNX13AG34G]; Jet Propulsion Laboratory, California Institute of Technology [NNH12ZDA001N-CCST]; NASA FX This study has been supported by NASA Grants NNX13AQ39G and NNX13AG34G. We thank three anonymous reviewers for their helpful comments. We thank members of the DARDAR project who provide the DARDAR data. We also acknowledge the members of the CloudSat Data Processing Center who provide CloudSat products, including 2C-ICE, 2B-FLXHR-LIDAR, 2B-CWC-RO, ECMWF-AUX, and 2C-RAIN-PROFILE. The CloudSat data were obtained online (http://www.cloudsat.cira.colostate.edu/). CALIPSO data were obtained online from the ASDC (https://eosweb.larc.nasa.gov/project/calipso/calipso_table). MOD43B3 data were downloaded from archives at NASA (http://modis-atmos.gsfc.nasa.gov/ALBEDO/index.html). Sea ice concentration was obtained from the National Snow and Ice Data Center (https://nsidc.org/data/seaice/index.html). CERES SSF1deg is available online (http://ceres.larc.nasa.gov/products.php?product=SSF1deg-lite). The contribution by J.-L. F. Li to this study was carried out on behalf of the Jet Propulsion Laboratory, California Institute of Technology, under contracts of ATMOS COMP 2013 (NNH12ZDA001N-CCST) with NASA. NR 58 TC 1 Z9 1 U1 14 U2 14 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD NOV PY 2016 VL 29 IS 21 BP 7651 EP 7674 DI 10.1175/JCLI-D-15-0799.1 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DZ9OH UT WOS:000386205900006 ER PT J AU Collow, ABM Miller, MA AF Collow, Allison B. Marquardt Miller, Mark A. TI The Seasonal Cycle of the Radiation Budget and Cloud Radiative Effect in the Amazon Rain Forest of Brazil SO JOURNAL OF CLIMATE LA English DT Article ID SINGLE SCATTERING ALBEDO; SOLAR-RADIATION; ENERGY; FLUX; CLIMATE; CERES; METHODOLOGY; ABSORPTION; PRODUCTS; AEROSOLS AB Changes in the climate system of the Amazon rain forest of Brazil can impact factors that influence the radiation budget such as clouds, atmospheric moisture, and the surface albedo. This study examines the relationships between clouds and radiation in this region using surface observations from the first year of the deployment of the Atmospheric Radiation Measurement (ARM) Program's Mobile Facility 1 (AMF1) in Manacapuru, Brazil, and satellite measurements from the Clouds and the Earth's Radiant Energy System (CERES). The seasonal cycles of the radiation budget and cloud radiative effects (CREs) are evaluated at the top of the atmosphere (TOA), at the surface, and within the atmospheric column using these observations and are placed into a regional context using the Modern-Era Retrospective Analysis for Research and Applications, version 2 (MERRA-2). Water vapor and clouds are abundant throughout the year, even though slight decreases are observed in the dry season. The column water vapor load is large enough that the longwave radiative flux divergence is nearly constant throughout the year. Clouds produce a significant shortwave CRE at the surface and TOA, exceeding 200 W m(-2) during the wet season. Discrepancies, especially in column shortwave radiative absorption, between the observations and MERRA-2 are demonstrated that warrant additional analysis of the microphysical and macrophysical cloud properties in MERRA-2. More trustworthy fields in the MERRA-2 product suggest that the expansive nearby river system impacts the regional radiation budget and thereby renders AMF1 observations potentially biased relative to regions farther removed from rivers within the Amazon rain forest. C1 [Collow, Allison B. Marquardt] Univ Space Res Assoc, Columbia, MD USA. [Collow, Allison B. Marquardt] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA. [Collow, Allison B. Marquardt; Miller, Mark A.] Rutgers State Univ, Inst Earth Ocean & Atmospher Sci, New Brunswick, NJ USA. RP Collow, ABM (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA. EM allison.collow@nasa.gov FU U.S. Department of Energy's Atmospheric System Research program [DE-FG02-08ER64531]; U.S. Department of Energy, Office of Science, Office of Biological and Environmental Research, Climate and Environmental Sciences Division; National Aeronautics and Space Administration FX This work is supported by the U.S. Department of Energy's Atmospheric System Research program Award DE-FG02-08ER64531. We appreciate the efforts of Mike Bosilovich for assisting with accessing data from MERRA-2 and Dr. Andrea Molod and two anonymous reviewers for their thoughtful comments. Data used in this study were obtained from the Atmospheric Radiation Measurement Program sponsored by the U.S. Department of Energy, Office of Science, Office of Biological and Environmental Research, Climate and Environmental Sciences Division (available at http://www.archive.arm.gov/armlogin/login.jsp) and the National Aeronautics and Space Administration (available at http://daac.gsfc.nasa.gov/datareleases/merra_2_data_release for MERRA-2 and https://ceres-tool.larc.nasa.gov/ord-tool/jsp/SYN1degSelection.jsp for CERES). NR 38 TC 1 Z9 1 U1 7 U2 7 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 NOV PY 2016 VL 29 IS 21 BP 7703 EP 7722 DI 10.1175/JCLI-D-16-0089.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DZ9OH UT WOS:000386205900008 ER PT J AU Schubert, S Chang, YH Wang, HL Koster, R Suarez, M AF Schubert, Siegfried Chang, Yehui Wang, Hailan Koster, Randal Suarez, Max TI A Modeling Study of the Causes and Predictability of the Spring 2011 Extreme US Weather Activity SO JOURNAL OF CLIMATE LA English DT Article ID NORTHERN-HEMISPHERE; CIRCULATION; PATTERNS; CONVECTION; COMPONENTS; DROUGHT; SYSTEM; WAVES AB This study examines the causes and predictability of the spring 2011 U.S. extreme weather using the Modern-Era Retrospective Analysis for Research and Applications (MERRA) and Goddard Earth Observing System Model, version 5, (GEOS-5) atmospheric general circulation model simulations. The focus is on assessing the impact on precipitation of sea surface temperature (SST) anomalies, land conditions, and large-scale atmospheric modes of variability. A key result is that the April record-breaking precipitation in the Ohio River valley was primarily the result of the unforced development of a positive North Atlantic Oscillation (NAO)-like mode of variability with unusually large amplitude, limiting the predictability of the precipitation in that region at 1-month leads. SST forcing (La Nina conditions) contributed to the broader continental-scale pattern of precipitation anomalies, producing drying in the southern plains and weak wet anomalies in the northeast, while the impact of realistic initial North American land conditions was to enhance precipitation in the upper Midwest and produce deficits in the Southeast. It was further found that 1) the 1 March atmospheric initial condition was the primary source of the ensemble mean precipitation response over the eastern United States in April (well beyond the limit of weather predictability), suggesting an influence on the initial state of the previous SST forcing and/or tropospheric-stratospheric coupling linked to an unusually persistent and cold polar vortex; and 2) stationary wave model experiments suggest that the SST-forced base state for April enhanced the amplitude of the NAO response compared to that of the climatological state, though the impact is modest and can be of either sign. C1 [Schubert, Siegfried; Chang, Yehui; Wang, Hailan; Koster, Randal; Suarez, Max] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD USA. [Chang, Yehui] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21239 USA. [Wang, Hailan] Sci Syst & Applicat Inc, Lanham, MD USA. RP Schubert, S (reprint author), NASA, GSFC, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM siegfried.d.schubert@nasa.gov FU NASA Modeling, Analysis, and Prediction (MAP) Program [NNH12ZDA001N] FX Support for this work was provided by the NASA Modeling, Analysis, and Prediction (MAP) Program (NASA Research Announcement NNH12ZDA001N). We wish to thank the editor and two anonymous reviewers for their valuable comments that helped to substantially improve the paper. NR 39 TC 0 Z9 0 U1 6 U2 6 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 NOV PY 2016 VL 29 IS 21 BP 7869 EP 7887 DI 10.1175/JCLI-D-15-0673.1 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DZ9OH UT WOS:000386205900017 ER PT J AU Naud, CM Booth, JF Del Genio, AD AF Naud, Catherine M. Booth, James F. Del Genio, Anthony D. TI The Relationship between Boundary Layer Stability and Cloud Cover in the Post-Cold-Frontal Region SO JOURNAL OF CLIMATE LA English DT Article ID SOUTHERN-OCEAN; CLIMATE MODEL; AIR OUTBREAKS; ERA-INTERIM; MODIS; CYCLONES; SYSTEM; HEMISPHERES; SATELLITE; WEATHER AB Using NASA Aqua MODIS and AIRS data, the relationship between low-level cloud cover (cloud top below the 700-hPa level) and boundary layer stability is explored in post-cold-frontal conditions. A linear relationship is found between seasonal cloud cover and two separate measures of inversion strength, the lower-tropospheric stability (LTS) and the estimated inversion strength (EIS), for two specific regions in the North Atlantic and Pacific in quiescent and weakly subsiding conditions. The relationship barely changes when considering dynamically active and subsiding post-cold-frontal conditions for the same regions. To explore the generality of this result and increase sample size, cold-front-centered composites of cloud cover and stability are constructed. The Northern and Southern Hemisphere seasonal cloud cover and stability distributions in the post-cold-frontal regions are then compared. A fairly good correlation between cloud cover and EIS is found in both hemispheres across all seasons, suggesting that a linear relationship between cloud cover and inversion strength proposed for quiescent conditions exists also in more dynamically active subsiding post-cold-frontal conditions. However, for a given season and hemisphere, the correlation between cloud cover and EIS degrades in post-cold-frontal regions, especially in the Northern Hemisphere. At these scales, other large-scale factors tend to correlate better with cloud cover. C1 [Naud, Catherine M.] Columbia Univ, Appl Phys & Appl Math, 2880 Broadway, New York, NY 10025 USA. [Naud, Catherine M.; Del Genio, Anthony D.] NASA GISS, New York, NY USA. [Booth, James F.] CUNY City Coll, Earth & Atmospher Sci, New York, NY 10031 USA. RP Naud, CM (reprint author), Columbia Univ, Appl Phys & Appl Math, 2880 Broadway, New York, NY 10025 USA. EM cn2140@columbia.edu FU NASA [NNX11AH22G, NNX13AQ33G]; NOAA [NA15OAR4310094]; CloudSat/CALIPSO Science Team RTOP FX The collection 5.1 MYD06 files were obtained from the level 1 Atmosphere Archive and Distribution System at the Goddard Space Flight Center. The AIRS-AMSU L2 Standard Product files and MERRA output files were obtained from the Goddard Earth Sciences Data and Information Services Center. The AMSR-E L2B ocean products were obtained from the National Snowand Ice Data Center. The Warren et al. (1988) cloud atlas climatology is available online (http://www.atmos.washington.edu/CloudMap/). ERA-Interim files are available through the European Centre for Medium-Range Weather Forecasts website. The MCMS dataset, documentation, and algorithm are available online (http://gcss-dime.giss.nasa.gov/mcms/). We thank Mike Bauer for the ERA-Interim-based dataset. CMN was funded by NASA's Science of Terra and Aqua Grant NNX11AH22G, NOAA's MAPP program Grant NA15OAR4310094, and NASA CloudSat Science Team Recompete Grant NNX13AQ33G. JFB was partially funded by NOAA's MAPP program Grant NA15OAR4310094. ADD was funded by a CloudSat/CALIPSO Science Team RTOP. We thank three anonymous reviewers and the editor who helped significantly improve this manuscript. NR 38 TC 0 Z9 0 U1 5 U2 5 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 NOV PY 2016 VL 29 IS 22 BP 8129 EP 8149 DI 10.1175/JCLI-D-15-0700.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DZ9OI UT WOS:000386206100012 ER PT J AU Mousing, EA Richardson, K Bendtsen, J Cetinic, I Perry, MJ AF Mousing, Erik Askov Richardson, Katherine Bendtsen, Jorgen Cetinic, Ivona Perry, Mary Jane TI Evidence of small-scale spatial structuring of phytoplankton alpha- and beta-diversity in the open ocean SO JOURNAL OF ECOLOGY LA English DT Article DE beta-diversity; community composition; determinants of plant community diversity and structure; dispersal; niche; phytoplankton; richness; spatiotemporal heterogeneity; submesoscale fronts ID SPECIES RICHNESS; COMMUNITY STRUCTURE; FOOD WEBS; PATTERNS; FOREST; BIODIVERSITY; BIOGEOGRAPHY; BLOOM; MICROORGANISMS; CONVECTION AB Phytoplankton assemblages in the open ocean are usually assumed to be mixed on local scales unless large semi-permanent density discontinuities separating water masses are present. Recent modelling studies have, however, suggested that ephemeral submesoscale oceanographic features leading to only subtle density discontinuities may be important for controlling phytoplankton alpha- and beta-diversity patterns. Until now, no empirical evidence has been presented to support this hypothesis. Using hydrographic and taxonomic composition data collected near Iceland during the period of the 2008 spring bloom, we show that the distribution of phytoplankton alpha- and beta-diversity was related to submesoscale heterogeneity in oceanographic conditions. Distinct phytoplankton communities as well as differences in richness were identified on either side of a front delimiting surface waters of slightly different (0.03) salinities. Alpha-diversity was significantly higher on the high salinity side of the front compared to the low salinity side. This difference was primarily driven by the presence of several large diatom species in the high salinity region, especially of the genus Chaetoceros which dominated the biomass here. By investigating beta-diversity in relation to environmental and spatiotemporal variables, we show that the regional distribution of phytoplankton taxa was influenced by both different environmental conditions on either side of the front and dispersal limitation across the front. Changes in beta-diversity were primarily driven by turnover rather than nestedness and were apparently controlled by different processes in each region.Synthesis. This study shows that small-scale and ephemeral density discontinuities created by submesoscale frontal dynamics can play a major role in structuring patterns of phytoplankton diversity. Evidence is presented that they can generate changes in environmental conditions (leading to environmental filtering) and act as physical (dispersal) barriers for phytoplankton transport. The study suggests that dispersal barriers are potentially of much greater importance for phytoplankton diversity at local scales than currently recognized and indicates that drivers of marine phytoplankton diversity are similar to those structuring diversity of land plants. C1 [Mousing, Erik Askov; Richardson, Katherine] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Macroecol Evolut & Climate, Univ Pk 15,DK, DK-2100 Copenhagen, Denmark. [Bendtsen, Jorgen] ClimateLab, Symbion Sci Pk, Copenhagen, Denmark. [Cetinic, Ivona] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Cetinic, Ivona] Univ Space Res Assoc, GESTAR, Columbia, MD USA. [Perry, Mary Jane] Univ Maine, Darling Marine Ctr, Sch Marine Sci, Walpole, ME 04573 USA. RP Mousing, EA (reprint author), Univ Copenhagen, Nat Hist Museum Denmark, Ctr Macroecol Evolut & Climate, Univ Pk 15,DK, DK-2100 Copenhagen, Denmark. EM eamousing@snm.ku.dk RI Richardson, Katherine/D-7592-2014; publicationpage, cmec/B-4405-2017; OI Richardson, Katherine/0000-0003-3785-2787; Mousing, Erik Askov/0000-0003-1663-2507 FU Danish National Research Foundation [DNRF96]; Danish Research Council for Nature and Universe; US NSF [OCE0628379, OCE0628107]; US NASA [NNX08AL92G] FX E.A.M., J.B. and K.R. acknowledge the Danish National Research Foundation for funding the Center for Macroecology, Evolution and Climate (DNRF96). This work was supported by the Danish Research Council for Nature and Universe (KR) and US NSF OCE0628379, OCE0628107 and US NASA NNX08AL92G (MJP). NR 86 TC 0 Z9 0 U1 27 U2 27 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-0477 EI 1365-2745 J9 J ECOL JI J. Ecol. PD NOV PY 2016 VL 104 IS 6 BP 1682 EP 1695 DI 10.1111/1365-2745.12634 PG 14 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA DZ5PY UT WOS:000385915200017 ER PT J AU Stanford, BK AF Stanford, Bret K. TI Static and Dynamic Aeroelastic Tailoring with Variable-Camber Control SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID FLUTTER SUPPRESSION; DESIGN OPTIMIZATION; LIFTING SURFACES; COMPOSITE WINGS; SYSTEMS; CONSTRAINTS AB This paper examines the use of a variable-camber continuous trailing-edge flap system for aeroservoelastic optimization of a transport wing box, the Common Research Model. Along with patch-level structural wing-box design variables, the quasi-steady and unsteady motions of the flap system are used as design variables, for maneuver load alleviation, cruise fuel burn reduction, and active flutter suppression. The resulting system is able to minimize structural weight and/or fuel burn while satisfying constraints upon elastic stresses, panel buckling, actuator hinge moments, flutter margins, actuator work, and control cost metrics. Limitations to this success are imposed by including load cases where the actuation system is not active (open-loop) in the optimization process. Large open-loop safety factors, for either maneuver loads or flutter, dilute the importance of the closed-loop actuation mechanism, whereas small open-loop safety factors may produce an overly flexible wing, prone to failure. Similar tradeoffs between system performance and actuator work constraints are provided. A final theme of the paper explores aeroelastic performance penalties that may arise if the shapes available to the variable-camber actuation system are limited (i.e., if certain control segments are linked together). C1 [Stanford, Bret K.] NASA, Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA. RP Stanford, BK (reprint author), NASA, Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA. EM bret.k.stanford@nasa.gov FU NASA's Advanced Air Transport Technologies program FX This work is funded by NASA's Advanced Air Transport Technologies program. Thanks to Joaquim Martins and Gaetan Kenway of the University of Michigan for providing the uCRM model. NR 44 TC 0 Z9 0 U1 4 U2 4 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD NOV PY 2016 VL 39 IS 11 BP 2522 EP 2534 DI 10.2514/1.G000413 PG 13 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA EA1DH UT WOS:000386332200005 ER PT J AU de Dilectis, F Mortari, D Zanetti, R AF de Dilectis, Francesco Mortari, Daniele Zanetti, Renato TI Bezier Description of Space Trajectories SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article C1 [de Dilectis, Francesco] Texas A&M Univ, Aerosp Engn, 301B Reed McDonald, College Stn, TX 77843 USA. [Mortari, Daniele] Texas A&M Univ, Aerosp Engn, 746C HR Bright Bldg, College Stn, TX 77843 USA. [Zanetti, Renato] NASA, Johnson Space Ctr, Aerosci & Flight Mech Div, EG6,2101 NASA Pkwy, Houston, TX 77058 USA. RP de Dilectis, F (reprint author), Texas A&M Univ, Aerosp Engn, 301B Reed McDonald, College Stn, TX 77843 USA. EM f.de.dilectis@neo.tamu.edu; mortari@tamu.edu NR 3 TC 0 Z9 0 U1 2 U2 2 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD NOV PY 2016 VL 39 IS 11 BP 2535 EP + DI 10.2514/1.G000719 PG 5 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA EA1DH UT WOS:000386332200006 ER PT J AU Suhir, E Ghaffarian, R AF Suhir, E. Ghaffarian, R. TI Column-grid-array (CGA) versus ball-grid-array (BGA): board-level drop test and the expected dynamic stress in the solder material SO JOURNAL OF MATERIALS SCIENCE-MATERIALS IN ELECTRONICS LA English DT Article ID BIMETAL THERMOSTATS AB Board level drop test is considered with an objective to develop a physically meaningful analytical predictive model for the evaluation of the expected impact-induced dynamic stresses in the solder material. Ball-grid-array (BGA) and column-grid-array (CGA) designs are addressed. Intuitively it is felt that while the application of the CGA technology to relieve thermal stresses in the solder material might be quite effective (owing to the greater interfacial compliance of the CGA in comparison with the BGA), the situation might be quite different when the PCB/package experiences dynamic loading. This is because the mass of the CGA joints exceeds considerably that of the BGA interconnections and the corresponding inertia forces might be substantially larger in the case of a CGA design. The numerical example carried out for rather arbitrary, but realistic, input data has indicated that the dynamic stresses in the solder material of the CGA design are even higher than the stresses in the BGA interconnections. This means particularly that the physically meaningful drop height in board-level tests should be thoroughly selected and that this height should be different, for BGA and CGA designs. C1 [Suhir, E.] Portland State Univ, Portland, OR 97207 USA. [Suhir, E.] ERS Co, 727 Alvina Ct, Los Altos, CA 94024 USA. [Ghaffarian, R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Suhir, E (reprint author), Portland State Univ, Portland, OR 97207 USA.; Suhir, E (reprint author), ERS Co, 727 Alvina Ct, Los Altos, CA 94024 USA. EM suhire@aol.com; reza.ghaffarian@jpl.nasa.gov NR 16 TC 0 Z9 0 U1 4 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0957-4522 EI 1573-482X J9 J MATER SCI-MATER EL JI J. Mater. Sci.-Mater. Electron. PD NOV PY 2016 VL 27 IS 11 BP 11572 EP 11582 DI 10.1007/s10854-016-5288-5 PG 11 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Engineering; Materials Science; Physics GA EA1QN UT WOS:000386367000058 ER PT J AU Fan, JW Wang, Y Rosenfeld, D Liu, XH AF Fan, Jiwen Wang, Yuan Rosenfeld, Daniel Liu, Xiaohong TI Review of Aerosol-Cloud Interactions: Mechanisms, Significance, and Challenges SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Review ID DEEP CONVECTIVE CLOUDS; MARINE BOUNDARY-LAYER; ASIAN SUMMER MONSOON; MIXED-PHASE CLOUDS; SAHARAN AIR LAYER; MESOSCALE CELLULAR CONVECTION; HETEROGENEOUS ICE FORMATION; SPECTRAL BIN MICROPHYSICS; GENERAL-CIRCULATION MODEL; SYSTEM-RESOLVING MODEL AB Over the past decade, the number of studies that investigate aerosol-cloud interactions has increased considerably. Although tremendous progress has been made to improve the understanding of basic physical mechanisms of aerosol-cloud interactions and reduce their uncertainties in climate forcing, there is still poor understanding of 1) some of the mechanisms that interact with each other over multiple spatial and temporal scales, 2) the feedbacks between microphysical and dynamical processes and between local-scale processes and large-scale circulations, and 3) the significance of cloud-aerosol interactions on weather systems as well as regional and global climate. This review focuses on recent theoretical studies and important mechanisms on aerosol-cloud interactions and discusses the significances of aerosol impacts on radiative forcing and precipitation extremes associated with different cloud systems. The authors summarize the main obstacles preventing the science from making a leap-for example, the lack of concurrent profile measurements of cloud dynamics, microphysics, and aerosols over a wide region on the observation side and the large variability of cloud microphysics parameterizations resulting in a large spread of modeling results on the modeling side. Therefore, large efforts are needed to escalate understanding. Future directions should focus on obtaining concurrent measurements of aerosol properties and cloud microphysical and dynamic properties over a range of temporal and spatial scales collected over typical climate regimes and closure studies, as well as improving understanding and parameterizations of cloud microphysics such as ice nucleation, mixed-phase properties, and hydrometeor size and fall speed. C1 [Fan, Jiwen] Pacific Northwest Natl Lab, Atmospher Sci & Global Change Div, POB 999,MSIN K9-24, Richland, WA 99352 USA. [Wang, Yuan] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Rosenfeld, Daniel] Hebrew Univ Jerusalem, Inst Earth Sci, Jerusalem, Israel. [Liu, Xiaohong] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA. RP Fan, JW (reprint author), Pacific Northwest Natl Lab, Atmospher Sci & Global Change Div, POB 999,MSIN K9-24, Richland, WA 99352 USA. EM jiwen.fan@pnnl.gov RI Liu, Xiaohong/E-9304-2011; Fan, Jiwen/E-9138-2011 OI Liu, Xiaohong/0000-0002-3994-5955; FU U.S. Department of Energy (DOE) Atmospheric System Research (ASR) Program [200180]; DOE by Battelle Memorial Institute [DE-AC06-76RLO1830]; NASA [ROSES14-ACMAP]; U.S. DOE ASR Program [DE-SC0014239] FX This study was supported by the U.S. Department of Energy (DOE) Atmospheric System Research (ASR) Program (Grant 200180). The Pacific Northwest National Laboratory (PNNL) is operated for the DOE by Battelle Memorial Institute under Contract DE-AC06-76RLO1830. Yuan Wang's contribution to this work was sponsored by NASA ROSES14-ACMAP and was carried at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. X. Liu acknowledges the funding support from the U.S. DOE ASR Program (Grant DE-SC0014239). The authors appreciate Drs. Bob Houze, Jerome Fast, and Steve Ghan at PNNL for their review and helpful comments to improve the paper prior to submission. NR 292 TC 1 Z9 1 U1 61 U2 61 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 EI 1520-0469 J9 J ATMOS SCI JI J. Atmos. Sci. PD NOV PY 2016 VL 73 IS 11 BP 4221 EP 4252 DI 10.1175/JAS-D-16-0037.1 PG 32 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DZ6YD UT WOS:000386007800001 ER PT J AU Jongeward, AR Li, ZQ He, H Xiong, XX AF Jongeward, Andrew R. Li, Zhanqing He, Hao Xiong, Xiaoxiong TI Natural and Anthropogenic Aerosol Trends from Satellite and Surface Observations and Model Simulations over the North Atlantic Ocean from 2002 to 2012 SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID LONG-TERM TREND; OPTICAL-THICKNESS; UNITED-STATES; AIR-QUALITY; DUST AEROSOLS; GOCART MODEL; GLOBAL-MODEL; PM2.5 MASS; MODIS; POLLUTION AB Aerosols contribute to Earth's radiative budget both directly and indirectly, and large uncertainties remain in quantifying aerosol effects on climate. Variability in aerosol distribution and properties, as might result from changing emissions and transport processes, must be characterized. In this study, variations in aerosol loading across the eastern seaboard of the United States and the North Atlantic Ocean during 2002 to 2012 are analyzed to examine the impacts of anthropogenic emission control measures using monthly mean data from MODIS, AERONET, and IMPROVE observations and Goddard Chemistry Aerosol Radiation and Transport (GOCART) model simulation. MODIS observes a statistically significant negative trend in aerosol optical depth (AOD) over the midlatitudes (-0.030 decade(-1)). Correlation analyses with surface AOD from AERONET sites in the upwind region combined with trend analysis from GOCART component AOD confirm that the observed decrease in the midlatitudes is chiefly associated with anthropogenic aerosols that exhibit significant negative trends from the eastern U.S. coast extending over the western North Atlantic. Additional analysis of IMPROVE surface PM2.5 observations demonstrates statistically significant negative trends in the anthropogenic components with decreasing mass concentrations over the eastern United States. Finally, a seasonal analysis of observational datasets is performed. The negative trend seen by MODIS is strongest during spring (MAM) and summer (JJA) months. This is supported by AERONET seasonal trends and is identified from IMPROVE seasonal trends as resulting from ammonium sulfate decreases during these seasons. C1 [Jongeward, Andrew R.; Li, Zhanqing; He, Hao] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Jongeward, Andrew R.; Li, Zhanqing; He, Hao] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Li, Zhanqing] Beijing Normal Univ, State Key Lab Earth Surface Proc & Resource Ecol, Beijing, Peoples R China. [Li, Zhanqing] Beijing Normal Univ, Coll Global Change & Earth Syst Sci, Beijing, Peoples R China. [Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD USA. RP Li, ZQ (reprint author), Beijing Normal Univ, GCESS, Jingshi Sci & Technol Bldg B,Coll Rd South, Beijing 100875, Peoples R China.; Li, ZQ (reprint author), Beijing Normal Univ, ESPRE, Jingshi Sci & Technol Bldg B,Coll Rd South, Beijing 100875, Peoples R China. EM zhanqingli@msn.com RI Li, Zhanqing/F-4424-2010 OI Li, Zhanqing/0000-0001-6737-382X FU U.S. EPA; National Park Service; NSF [AGS1534670]; NSFC [91544217]; MOST [2013CB955804] FX The authors would like to acknowledge Dr. Rob Levy of the MODIS Aerosol Team for valuable discussions as well as Dr. Mian Chin for providing access to the high-resolution GOCART simulation used presently. MERRA atmospheric reanalysis data were acquired from NASA's Goddard Earth Sciences (GES) Data and Information Services Center (DISC). We also thank the Principal Investigators of the AERONET network for maintaining and allowing access to their data. Finally, IMPROVE is a collaborative association of state, tribal, and federal agencies and international partners. The U.S. EPA is the primary funding source, with contracting and research support from the National Park Service. The Air Quality Group at the University of California, Davis, is the central analytical laboratory, with ion analysis provided by Research Triangle Institute, and carbon analysis provided by Desert Research Institute. The authors also thank two anonymous reviewers for their helpful comments. This research is supported by the grants of NSF (AGS1534670), NSFC (91544217), and MOST (2013CB955804). NR 52 TC 0 Z9 0 U1 10 U2 10 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 EI 1520-0469 J9 J ATMOS SCI JI J. Atmos. Sci. PD NOV PY 2016 VL 73 IS 11 BP 4469 EP 4485 DI 10.1175/JAS-D-15-0308.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DZ6YD UT WOS:000386007800012 ER PT J AU Loveland, TR Irons, JR AF Loveland, Thomas R. Irons, James R. TI Landsat 8: The plans, the reality, and the legacy SO REMOTE SENSING OF ENVIRONMENT LA English DT Article ID DATA CONTINUITY MISSION; THERMAL INFRARED-SENSOR; ON-ORBIT; RADIOMETRIC CALIBRATION; PERFORMANCE; OLI; DESIGN; TIRS AB Landsat 8, originally known as the Landsat Data Continuity Mission (LDCM), is a National Aeronautics and Space Administration (NASA)-U.S. Geological Survey (USGS) partnership that continues the legacy of continuous moderate resolution observations started in 1972. The conception of LDCM to the reality of Landsat 8 followed an arduous path extending over nearly 13 years, but the successful launch on February 11, 2013 ensures the continuity of the unparalleled Landsat record. The USGS took over mission operations on May 30, 2013 and renamed LCDM to Landsat 8. Access to Landsat 8 data was opened to users worldwide. Three years following launch we evaluate the science and applications impact of Landsat 8. With a mission objective to enable the detection and characterization of global land changes at a scale where differentiation between natural and human-induced causes of change is possible, LDCM promised incremental technical improvements in capabilities needed for Landsat scientific and applications investigations. Results show that with Landsat 8, we are acquiring more data than ever before, the radiometric and geometric quality of data are generally technically superior to data acquired by past Landsat missions, and the new measurements, e.g., the coastal aerosol and cirrus bands, are opening new opportunities. Collectively, these improvements are sparking the growth of science and applications opportunities. Equally important, with Landsat 7 still operational, we have returned to global imaging on an 8-day cycle, a capability that ended when Landsat 5 ceased operational Earth imaging in November 2011. As a result, the Landsat program is on secure footings and planning is underway to extend the record for another 20 or more years. Published by Elsevier Inc. C1 [Loveland, Thomas R.] US Geol Survey, EROS Ctr, Sioux Falls, SD 57198 USA. [Irons, James R.] NASA, Div Earth Sci, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Loveland, TR (reprint author), US Geol Survey, EROS Ctr, Sioux Falls, SD 57198 USA. EM Loveland@usgs.gov OI Loveland, Thomas/0000-0003-3114-6646 FU USGS Land Remote Sensing Program FX We thank the many Landsat data users that have contributed to the health of the Landsat program. We especially thank those that contributed abstracts and manuscripts for consideration of this special issue. The members of the USGS-NASA Landsat Science Team played a significant role in the development of this special issue and in advancing the use and impact of Landsat. Finally, we acknowledge NASA for their long commitment to continuing and improving Landsat capabilities and USGS for uncompromising stewardship of the entire Landsat record. The USGS Land Remote Sensing Program is recognized for sponsoring this Landsat 8 special issue. NR 21 TC 2 Z9 2 U1 26 U2 26 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 NOV PY 2016 VL 185 SI SI BP 1 EP 6 DI 10.1016/j.rse.2016.07.03 PG 6 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA EA1AY UT WOS:000386321900001 ER PT J AU Mishra, N Helder, D Barsi, J Markham, B AF Mishra, Nischal Helder, Dennis Barsi, Julia Markham, Brian TI Continuous calibration improvement in solar reflective bands: Landsat 5 through Landsat 8 SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Landsat; Operation land imager (OLI); Enhanced thematic mapper plus (ETM plus ); Thematic mapper (TM); Radiometric calibration ID RADIOMETRIC CALIBRATION; THEMATIC MAPPER; IMAGER; PERFORMANCE; STABILITY; DESERT; SITES AB Launched in February 2013, the Operational Land Imager (OLI) on-board Landsat 8 continues to perform exceedingly well and provides high quality science data globally. Several design enhancements have been made in the OLI instrument relative to prior Landsat instruments: pushbroom imaging which provides substantially improved Signal-to-Noise Ratio (SNR), spectral bandpasses refinement to avoid atmospheric absorption features, 12 bit data resolution to provide a larger dynamic range that limits the saturation level and increases SNR, a set of well-designed onboard calibrators to monitor the stability of the sensor. Some of these changes, such as refinements in spectral bandpasses compared to earlier Landsats and a well-designed on-board calibrator have a direct impact on the improved radiometric calibration performance of the instrument from both the stability of the response and the ability to track the changes. The on-board calibrator lamps and diffusers indicate that the instrument drift is generally <0.1% per year across the bands. The refined bandpasses of the OLI indicate that temporal uncertainty of better than 0.5% is possible when the instrument is trended over vicarious targets such as Pseudo Invariant Calibration Sites (PICS), a level of precision that was never achieved with the earlier Landsat instruments. With three years of data available, the stability measurements indicated by on-board calibrators and PICS agree to 0.5%, which is much better compared to the earlier Landsats, which is very encouraging and bodes well for the future Landsat missions too. (C) 2016 Elsevier Inc. All rights reserved. C1 [Mishra, Nischal; Helder, Dennis] SDSU, Engn Off Res, Brookings, SD 57007 USA. [Barsi, Julia] Sci Syst & Applicat Inc, NASA GSFC, Code 618, Greenbelt, MD 20771 USA. [Markham, Brian] NASA GSFC, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA. RP Mishra, N (reprint author), SDSU, Engn Off Res, Brookings, SD 57007 USA. EM Nischal.Mishra@sdstate.edu; Dennis.Helder@sdstate.edu; julia.barsi@nasa.gov; Brian.L.Markham@nasa.gov FU NASA grant [NNX15AP36A]; USGS EROS grant [G14AC00370] FX The authors would like to thank the Landsat Calibration/Validation Team at South Dakota State University, USGS EROS Data Center and NASA Goddard Space Flight Center for their advice and feedback on this journal article. We are also grateful to the reviewers and editors for their valuable comments and edits in this article. This work was supported by NASA grant NNX15AP36A, by USGS EROS grant G14AC00370. NR 18 TC 0 Z9 0 U1 12 U2 12 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 NOV PY 2016 VL 185 SI SI BP 7 EP 15 DI 10.1016/j.rse.2016.07.032 PG 9 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA EA1AY UT WOS:000386321900002 ER PT J AU Vermote, E Justice, C Claverie, M Franch, B AF Vermote, Eric Justice, Chris Claverie, Martin Franch, Belen TI Preliminary analysis of the performance of the Landsat 8/OLI land surface reflectance product SO REMOTE SENSING OF ENVIRONMENT LA English DT Article ID RADIATIVE-TRANSFER CODE; ATMOSPHERIC CORRECTION; VECTOR VERSION; SATELLITE DATA; MODIS; AEROSOL; VALIDATION; RETRIEVAL; ALBEDO; 6S AB The surface reflectance, i.e., satellite derived top of atmosphere (TOA) reflectance corrected for the temporally, spatially and spectrally varying scattering and absorbing effects of atmospheric gases and aerosols, is needed to monitor the land surface reliably. For this reason, the surface reflectance, and not TOA reflectance, is used to generate the greater majority of global land products, for example, from the Moderate Resolution Imaging Spectroradiometer (MODIS) and Visible Infrared Imaging Radiometer Suite (VIIRS) sensors. Even if atmospheric effects are minimized by sensor design, atmospheric effects are still challenging to correct. In particular, the strong impact of aerosols in the visible and near infrared spectral range can be difficult to correct, because they can be highly discrete in space and time (e.g., smoke plumes) and because of the complex scattering and absorbing properties of aerosols that vary spectrally and with aerosol size, shape, chemistry and density. This paper presents the Landsat 8 Operational Land Imager (OLI) atmospheric correction algorithm that has been developed using the Second Simulation of the Satellite Signal in the Solar Spectrum Vectorial (6SV) model, refined to take advantage of the narrow OLI spectral bands (compared to Thematic Mapper/Enhanced Thematic Mapper (TM/ETM +)), improved radiometric resolution and signal-to-noise. In addition, the algorithm uses the new OLI Coastal aerosol band (0.433-0.450 mu m), which is particularly helpful for retrieving aerosol properties, as it covers shorter wavelengths than the conventional Landsat, TM and ETM + blue bands. A cloud and cloud shadow mask has also been developed using the "cirrus" band (1.360-1.390 pm) available on OLI, and the thermal infrared bands from the Thermal Infrared Sensor (TIRS) instrument. The performance of the surface reflectance product from OLI is analyzed over the Aerosol Robotic Network (AERONET) sites using accurate atmospheric correction (based on in situ measurements of the atmospheric properties), by comparison with the MODIS Bidirectional Reflectance Distribution Function (BRDF) adjusted surface reflectance product and by comparison of OLI derived broadband albedo from United States Surface Radiation Budget Network (US SURFRAD) measurements. The results presented clearly show an improvement of Landsat 8 surface reflectance product over the ad-hoc Landsat 5/7 LEDAPS product. Published by Elsevier Inc. C1 [Vermote, Eric; Claverie, Martin; Franch, Belen] NASA GSFC, Code 619, Greenbelt, MD 20771 USA. [Justice, Chris; Claverie, Martin; Franch, Belen] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. RP Vermote, E (reprint author), NASA GSFC, Code 619, Greenbelt, MD 20771 USA. EM eric.f.vermote@nasa.gov FU NASA grant [NNX12AP82G] FX This work was supported by NASA grant NNX12AP82G. NR 37 TC 6 Z9 6 U1 20 U2 20 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 NOV PY 2016 VL 185 SI SI BP 46 EP 56 DI 10.1016/j.rse.2016.04.008 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA EA1AY UT WOS:000386321900005 ER PT J AU Roy, DP Kovalskyy, V Zhang, HK Vermote, EF Yan, L Kumar, SS Egorov, A AF Roy, D. P. Kovalskyy, V. Zhang, H. K. Vermote, E. F. Yan, L. Kumar, S. S. Egorov, A. TI Characterization of Landsat-7 to Landsat-8 reflective wavelength and normalized difference vegetation index continuity SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Landsat; Continuity; Reflectance; Ndvi; OLI; ETM ID CONTERMINOUS UNITED-STATES; ORBIT GEOMETRIC CALIBRATION; PLUS ATMOSPHERIC CORRECTION; CLOUD-COVER ASSESSMENT; GLOBAL CHANGE RESEARCH; TERM ACQUISITION PLAN; NDVI TIME-SERIES; SURFACE REFLECTANCE; RADIOMETRIC CALIBRATION; SATELLITE SENSORS AB At over 40 years, the Landsat satellites provide the longest temporal record of space-based land surface observations, and the successful. 2013 launch of the Landsat-8 is continuing this legacy. Ideally, the Landsat data record should be consistent over the Landsat sensor series. The Landsat-8 Operational Land Imager (OLI) has improved calibration, signal to noise characteristics, higher 12-bit radiometric resolution, and spectrally narrower wavebands than the previous Landsat-7 Enhanced Thematic Mapper (ETM+). Reflective wavelength differences between the two Landsat sensors depend also on the surface reflectance and atmospheric state which are difficult to model comprehensively. The orbit and sensing geometries of the Landsat-8 OLI and Landsat-7 ETM+ provide swath edge overlapping paths sensed only one day apart. The overlap regions are sensed in alternating backscatter and forward scattering orientations so Landsat bi-directional reflectance effects are evident but approximately balanced between the two sensors when large amounts of time series data are considered. Taking advantage of this configuration a total of 59 million 30 m corresponding sensor observations extracted from 6317 Landsat-7 ETM + and Landsat-8 OLI images acquired over three winter and three summer months for all the conterminous United States (CONUS) are compared. Results considering different stages of cloud and saturation filtering, and filtering to reduce one day surface state differences, demonstrate the importance of appropriate per-pixel data screening. Top of atmosphere (TOA) and atmospherically corrected surface reflectance for the spectrally corresponding visible, near infrared and shortwave infrared bands, and derived normalized difference vegetation index (NDVI), are compared and their differences quantified. On average the OLI TOA reflectance is greater than the ETM + TOA reflectance for all bands, with greatest differences in the near-infrared (NIR) and the shortwave infrared bands due to the quite different spectral response functions between the sensors. The atmospheric correction reduces the mean difference in the NIR and shortwave infrared but increases the mean difference in the visible bands. Regardless of whether TOA or surface reflectance are used to generate NDVI, on average, for vegetated soil and vegetation surfaces (0 NDVI 1), the OLI NDVI is greater than the ETM + NDVI. Statistical functions to transform between the comparable sensor bands and sensor NDVI values are presented so that the user community may apply them in their own research to improve temporal continuity between the Landsat-7 ETM + and Landsat-8 OLI sensor data. The transformation functions were developed using ordinary least squares (OLS) regression and were fit quite reliably (r(2) values > 0.7 for the reflectance data and >0.9 for the NDVI data, p-values < 0.0001). (C) 2015 The Authors. Published by Elsevier Inc. C1 [Roy, D. P.; Kovalskyy, V.; Zhang, H. K.; Yan, L.; Kumar, S. S.; Egorov, A.] South Dakota State Univ, Geospatial Sci Ctr Excellence, Brookings, SD 57007 USA. [Vermote, E. F.] NASA, Goddard Space Flight Ctr, Terr Informat Syst Branch, Greenbelt, MD 20771 USA. RP Roy, DP (reprint author), South Dakota State Univ, Geospatial Sci Ctr Excellence, Brookings, SD 57007 USA. OI Kumar, Sanath S./0000-0003-4067-4926 FU U.S. Geological Survey (USGS) [G12PC00069]; NASA Making Earth System Data Records for Use in Research Environments (MEaSUREs) program [NNX13AJ24A]; U.S. Department of Interior FX This research was funded by the U.S. Department of Interior, U.S. Geological Survey (USGS), under grant G12PC00069 and also by the NASA Making Earth System Data Records for Use in Research Environments (MEaSUREs) program under Cooperative Agreement NNX13AJ24A. The U.S. Landsat project management and staff at USGS Earth Resources Observation and Science (EROS) Center, Sioux Falls, South Dakota, are thanked for provision of the Landsat data used in this study. The anonymous reviewers are thanked for their comments which helped to improve this paper. NR 88 TC 5 Z9 5 U1 13 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 NOV PY 2016 VL 185 SI SI BP 57 EP 70 DI 10.1016/j.rse.2015.12.024 PG 14 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA EA1AY UT WOS:000386321900006 ER PT J AU Wang, ZS Erb, AM Schaaf, CB Sun, QS Liu, Y Yang, Y Shuai, YM Casey, KA Roman, MO AF Wang, Zhuosen Erb, Angela M. Schaaf, Crystal B. Sun, Qingsong Liu, Yan Yang, Yun Shuai, Yanmin Casey, Kimberly A. Roman, Miguel O. TI Early spring post-fire snow albedo dynamics in high latitude boreal forests using Landsat-8 OLI data SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Landsat-8 snow albedo; Post-fire recovery; Albedo heterogeneity and dynamics ID LAND-COVER DATABASE; BURN SEVERITY; INTERIOR ALASKA; BLACK SPRUCE; SURFACE REFLECTANCE; ENERGY-EXCHANGE; PRODUCT MCD43A; CLIMATE-CHANGE; CLOUD SHADOW; IN-SITU AB Taking advantage of the improved radiometric resolution of Landsat-8 OLI which, unlike previous Landsat sensors, does not saturate over snow, the progress of fire recovery progress at the landscape scale (<100 m) is examined. High quality Landsat-8 albedo retrievals can now capture the true reflective and layered character of snow cover over a full range of land surface conditions and vegetation densities. This new capability particularly improves the assessment of post-fire vegetation dynamics across low- to high-burn severity gradients in Arctic and boreal regions in the early spring, when the albedos during recovery show the greatest variation. We use 30 m resolution Landsat-8 surface reflectances with concurrent coarser resolution (500 m) MODIS high quality full inversion surface Bidirectional Reflectance Distribution Functions (BRDF) products to produce higher resolution values of surface albedo. The high resolution full expression shortwave blue sky albedo product performs well with an overall RMSE of 0.0267 between tower and satellite measures under both snow-free and snow-covered conditions. While the importance of post-fire albedo recovery can be discerned from the MODIS albedo product at regional and global scales, our study addresses the particular importance of early spring post-fire albedo recovery at the landscape scale by considering the significant spatial heterogeneity of burn severity, and the impact of snow on the early spring albedo of various vegetation recovery types. We found that variations in early spring albedo within a single MODIS gridded pixel can be larger than 0.6. Since the frequency and severity of wildfires in Arctic and boreal systems is expected to increase in the coming decades, the dynamics of albedo in response to these rapid surface changes will increasingly impact the energy balance and contribute to other climate processes and physical feedback mechanisms. Surface radiation products derived from Landsat-8 data will thus play an important role in characterizing the carbon cycle and ecosystem processes of high latitude systems. (C) 2016 Elsevier Inc. All rights reserved. C1 [Wang, Zhuosen; Casey, Kimberly A.; Roman, Miguel O.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wang, Zhuosen; Erb, Angela M.; Schaaf, Crystal B.; Sun, Qingsong; Liu, Yan; Shuai, Yanmin] Univ Massachusetts, Sch Environm, Boston, MA 02125 USA. [Wang, Zhuosen] Goddard Space Flight Ctr, Greenbelt, MD USA. [Yang, Yun] ARS, USDA, Beltsville, MD USA. [Casey, Kimberly A.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. RP Wang, ZS (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Erb, AM (reprint author), Univ Massachusetts, Sch Environm, Boston, MA 02125 USA. EM zhuosen.wang@nasa.gov; Angela.Erb001@umb.edu OI Sun, Qingsong/0000-0002-7710-2123 FU NASA [NNX14A173G]; USGS [G12PC00072]; Office of Science (BER), US Department of Energy through the Ameriflux Management Project FX This research was supported by NASA awards NNX14A173G and USGS award G12PC00072. The MODIS data were obtained from the NASA Distributed Active Archive Centers (DAACs). The Landsat data were obtained from the USGS Earth Resources Observation and Science (EROS) Center Science Processing Architecture (ESPA). Field albedo measurements were downloaded from NOAA SURFRAD. We gratefully acknowledge Dr. Adrian Rocha from University of Notre Dame for providing ground albedo measurements at the Imnavait site, Dr. David Y. Hollinger from USDA Forest Service Northern Research Station, Durham, NH, USA for providing ground albedo measurements at the Howland West site and Dr. Kimberly Novick and Dr. Benjamin Sulman from Indiana University for providing ground albedo measurements at the Morgan Monroe State Forest site which was supported primarily by the Office of Science (BER), US Department of Energy through the Ameriflux Management Project. NR 91 TC 0 Z9 0 U1 16 U2 16 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 NOV PY 2016 VL 185 SI SI BP 71 EP 83 DI 10.1016/j.rse.2016.02.059 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA EA1AY UT WOS:000386321900007 ER PT J AU Fahnestock, M Scambos, T Moon, T Gardner, A Haran, T Klinger, M AF Fahnestock, Mark Scambos, Ted Moon, Twila Gardner, Alex Haran, Terry Klinger, Marin TI Rapid large-area mapping of ice flow using Landsat 8 SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Landsat; Ice flow; Greenland; Antarctica; Remote sensing; Glaciers ID GREENLAND OUTLET GLACIER; SURFACE-VELOCITY; FEATURE TRACKING; NORTHWEST CANADA; SATELLITE IMAGES; WEST ANTARCTICA; ON-ORBIT; EVOLUTION; STREAM; 21ST-CENTURY AB We report on the maturation of optical satellite-image-based ice velocity mapping over the ice sheets and large glacierized areas, enabled by the high radiometric resolution and internal geometric accuracy of Landsat 8's Operational Land Imager (OLI). Detailed large-area single-season mosaics and time-series maps of ice flow were created using data spanning June 2013 to June 2015. The 12-bit radiometric quantization and 15-m pixel scale resolution of OLI band 8 enable displacement tracking of subtle snow-drift patterns on ice sheet surfaces at similar to 1 m precision. Ice sheet and snowfield snow-drift features persist for typically 16 to 64 days, and up to 432 days, depending primarily on snow accumulation rates. This results in spatially continuous mapping of ice flow, extending the mapping capability beyond crevassed areas. Our method uses image chip cross-correlation and sub-pixel peak-fitting in matching Landsat path/row pairs. High-pass filtering is applied to the imagery to enhance local surface texture. The current high image acquisition rates of Landsat 8 (725 scenes per day globally) reduces the impact of high cloudiness in polar and mountain terrain and allows rapid compilation of large areas, or dense temporal coverage of seasonal ice flow variations. The results rival the coverage and accuracy of interferometric Synthetic Aperture Radar (InSAR) mapping. (C) 2015 The Authors. Published by Elsevier Inc. C1 [Fahnestock, Mark] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. [Scambos, Ted; Moon, Twila; Haran, Terry; Klinger, Marin] Univ Colorado, Natl Snow & Ice Data Ctr, Boulder, CO 80303 USA. [Moon, Twila] Univ Oregon, Dept Geol Sci, Eugene, OR 97403 USA. [Gardner, Alex] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Fahnestock, M (reprint author), Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA.; Scambos, T (reprint author), Univ Colorado, Natl Snow & Ice Data Ctr, Boulder, CO 80303 USA. EM mark.fahnestock@mac.com; teds@nsidc.org OI Gardner, Alex/0000-0002-8394-8889 FU NASA [NNX14AR77G, NNX15AC70G, NNX10AI42G]; USGS [G12P00066]; Cooperative Institute for Research in Environmental Science (CIRES) Visiting Post-Doctoral Fellow at the University of Colorado, Boulder; NASA's Cryosphere program FX This work was supported by NASA Grants NNX14AR77G and NNX15AC70G to M. Fahnestock and NNX10Al42G (supplement) to T. Scambos, as well as USGS Contract G12P00066 to T. Scambos (supporting T. Haran and M. Klinger). T. Moon was supported as a Cooperative Institute for Research in Environmental Science (CIRES) Visiting Post-Doctoral Fellow at the University of Colorado, Boulder for July 2014 - June 2015. Funding for A. Gardner's effort was supported by NASA's Cryosphere program. We thank A. Pope for the graphic in Fig. 1, produced using Google Earth Engine. NR 46 TC 2 Z9 2 U1 21 U2 21 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD NOV PY 2016 VL 185 SI SI BP 84 EP 94 DI 10.1016/j.rse.2015.11.023 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA EA1AY UT WOS:000386321900008 ER PT J AU Wulder, MA White, JC Loveland, TR Woodcock, CE Belward, AS Cohen, WB Fosnight, EA Shaw, J Masek, JG Roy, DP AF Wulder, Michael A. White, Joanne C. Loveland, Thomas R. Woodcock, Curtis E. Belward, Alan S. Cohen, Warren B. Fosnight, Eugene A. Shaw, Jerad Masek, Jeffrey G. Roy, David P. TI The global Landsat archive: Status, consolidation, and direction SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Landsat Global Archive Consolidation; LGAC; Satellite; Monitoring; Landsat ID TERM ACQUISITION PLAN; COVER; RESOLUTION; MISSION; IMAGERY; AVAILABILITY; CONTINUITY; SATELLITE; ACCESS; RECORD AB New and previously unimaginable Landsat applications have been fostered by a policy change in 2008 that made analysis-ready Landsat data free and open access. Since 1972, Landsat has been collecting images of the Earth, with the early years of the program constrained by onboard satellite and ground systems, as well as limitations across the range of required computing, networking, and storage capabilities. Rather than robust on-satellite storage for transmission via high bandwidth downlink to a centralized storage and distribution facility as with Landsat-8, a network of receiving stations, one operated by the U.S. government, the other operated by a community of International Cooperators (ICs), were utilized. ICs paid a fee for the right to receive and distribute Landsat data and over time, more Landsat data was held outside the archive of the United State Geological Survey (USGS) than was held inside, much of it unique. Recognizing the critical value of these data, the USGS began a Landsat Global Archive Consolidation (LGAC) initiative in 2010 to bring these data into a single, universally accessible, centralized global archive, housed at the Earth Resources Observation and Science (EROS) Center in Sioux Falls, South Dakota. The primary LGAC goals are to inventory the data held by ICs, acquire the data, and ingest and apply standard ground station processing to generate an LIT analysis-ready product. As of January 1, 2015 there were 5,532,454 images in the USGS archive. LGAC has contributed approximately 3.2 million of those images, more than doubling the original USGS archive holdings. Moreover, an additional 23 million images have been identified to date through the LGAC initiative and are in the process of being added to the archive. The impact of LGAC is significant and, in terms of images in the collection, analogous to that of having had two additional Landsat-5 missions. As a result of LGAC, there are regions of the globe that now have markedly improved Landsat data coverage, resulting in an enhanced capacity for mapping, monitoring change, and capturing historic conditions. Although future missions can be planned and implemented, the past cannot be revisited, undetscoring the value and enhanced significance of historical Landsat data and the LGAC initiative. The aim of this paper is to report the current status of the global USGS Landsat archive, document the existing and anticipated contributions of LGAC to the archive, and characterize the current acquisitions of Landsat-7 and Landsat-8. Landsat-8 is adding data to the archive at an unprecedented rate as nearly all terrestrial images are now collected. We also offer key lessons learned so far from the LGAC initiative, plus insights regarding other critical elements of the Landsat program looking forward, such as acquisition, continuity, temporal revisit, and the importance of continuing to operationalize the Landsat program. Crown Copyright (C) 2015 Published by Elsevier Inc All rights reserved. C1 [Wulder, Michael A.; White, Joanne C.] Nat Resources Canada, Canadian Forest Serv, Pacific Forestry Ctr, 506 West Burnside Rd, Victoria, BC V8Z 1M5, Canada. [Loveland, Thomas R.; Fosnight, Eugene A.] US Geol Survey, Earth Resources Observat & Sci EROS Ctr, 47914 252nd St, Sioux Falls, SD 57198 USA. [Woodcock, Curtis E.] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA. [Belward, Alan S.] European Commiss, Joint Res Ctr, Inst Environm & Sustainabil, I-20133 Milan, VA, Italy. [Cohen, Warren B.] US Forest Serv, Forestry Sci Lab, USDA, Corvallis, OR 97331 USA. [Shaw, Jerad] Stinger Ghaffarian Technol, Earth Resources Observat & Sci EROS Ctr, 47914 252nd St, Sioux Falls, SD 57198 USA. [Masek, Jeffrey G.] NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Roy, David P.] South Dakota State Univ, Geospatial Sci Ctr Excellence, Brookings, SD 57007 USA. RP Wulder, MA (reprint author), Nat Resources Canada, Canadian Forest Serv, Pacific Forestry Ctr, 506 West Burnside Rd, Victoria, BC V8Z 1M5, Canada. EM mike.wulder@canada.ca OI White, Joanne/0000-0003-4674-0373; Wulder, Michael/0000-0002-6942-1896 FU Canadian Space Agency (CSA) Government Related Initiatives Program (GRIP); Canadian Forest Service (CFS) of Natural Resources Canada FX This communication has been made possible and enriched by the ongoing discussions and deliberations of the USGS/NASA Landsat Science Team (https://landsat.usgs.gov/science_Landsat_Science_Team.php). The participation of Wulder and White was supported as part of the "National Terrestrial Ecosystem Monitoring System (NTEMS): Timely and detailed national cross-sector monitoring for Canada" project jointly funded by the Canadian Space Agency (CSA) Government Related Initiatives Program (GRIP) and the Canadian Forest Service (CFS) of Natural Resources Canada. We greatly appreciate the time committed and the insightful comments made by three anonymous reviewers that helped us to improve the manuscript. NR 46 TC 11 Z9 11 U1 10 U2 10 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 NOV PY 2016 VL 185 SI SI BP 271 EP 283 DI 10.1016/j.rse.2015.11.032 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA EA1AY UT WOS:000386321900023 ER PT J AU Islam, T Srivastava, PK Dai, Q AF Islam, Tanvir Srivastava, Prashant K. Dai, Qiang TI High-resolution WRF simulation of cloud properties over the super typhoon Haiyan: physics parameterizations and comparison against MODIS SO THEORETICAL AND APPLIED CLIMATOLOGY LA English DT Article ID BULK MICROPHYSICS PARAMETERIZATION; ATMOSPHERIC BOUNDARY-LAYER; PART I; MODEL; ICE; IMPLEMENTATION; PRECIPITATION; SENSITIVITY; ALGORITHMS; TURBULENCE AB Numerical weather prediction (NWP) models can complement the satellite technology in simulating the cloud properties, especially in extreme storm events, when gathering new data becomes more than essential for accurate weather forecasting. In this study, we investigate the capability of the Weather Research and Forecasting (WRF) model to realistically simulate some important cloud properties in high-resolution grids, such as cloud phase (e.g., liquid or ice) and cloud water path. The sensitivity of different combinations of physics parameterizations to the simulated cloud fields is studied. The experiment is conducted on a super typhoon event by configuring the WRF model in two domains, with two-way nesting, allowing bidirectional information exchange between the parent and the nest. In order to do the assessment, the simulated cloud fields are compared against MODIS-derived cloud properties from one overpass scene. While the simulations have been able to capture the spatial distribution of cloud properties reasonably well, produced cloud quantities such as ice water path has been significantly overestimated when compared to the MODIS optical cloud information. The microphysics parameterizations are found to be more sensitive than the planetary boundary layer (PBL) parameterizations. C1 [Islam, Tanvir] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. [Srivastava, Prashant K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Srivastava, Prashant K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Dai, Qiang] Univ Bristol, Dept Civil Engn, Bristol, Avon, England. RP Islam, T (reprint author), CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. EM tanvir.islam@jpl.nasa.gov OI Islam, Tanvir/0000-0003-2429-3074 NR 27 TC 0 Z9 0 U1 7 U2 7 PU SPRINGER WIEN PI WIEN PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA SN 0177-798X EI 1434-4483 J9 THEOR APPL CLIMATOL JI Theor. Appl. Climatol. PD NOV PY 2016 VL 126 IS 3-4 BP 427 EP 435 DI 10.1007/s00704-015-1575-y PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DZ7UF UT WOS:000386071900002 ER PT J AU Farrell, WM Hurley, DM Poston, MJ Zimmerman, MI Orlando, TM Hibbitts, CA Killen, RM AF Farrell, W. M. Hurley, D. M. Poston, M. J. Zimmerman, M. I. Orlando, T. M. Hibbitts, C. A. Killen, R. M. TI The gas-surface interaction of a human-occupied spacecraft with a near-Earth object SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Asteroid; Water; Orion ID LUNAR; WATER AB NASA's asteroid redirect mission (ARM) will feature an encounter of the human-occupied Orion spacecraft with a portion of a near-Earth asteroid (NEA) previously placed in orbit about the Moon by a capture spacecraft. Applying a shuttle analog, we suggest that the Orion spacecraft should have a dominant local water exosphere, and that molecules from this exosphere can adsorb onto the NEA. The amount of adsorbed water is a function of the defect content of the NEA surface, with retention of shuttle-like water levels on the asteroid at 10(15) H2O's/m(2) for space weathered regolith at T similar to 300 K. Published by Elsevier Ltd on behalf of COSPAR. This is an open access article under the CC BY-NC-ND license. C1 [Farrell, W. M.; Killen, R. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hurley, D. M.; Zimmerman, M. I.; Hibbitts, C. A.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Poston, M. J.] CALTECH, Pasadena, CA 91125 USA. [Orlando, T. M.] Georgia Inst Technol, Atlanta, GA 30332 USA. RP Farrell, WM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM william.m.farrell@nasa.gov RI Farrell, William/I-4865-2013; OI Poston, Michael/0000-0001-5113-1017 FU Solar System Exploration Research Virtual Institute (SSERVI) FX We gratefully recognize the support provided by the Solar System Exploration Research Virtual Institute (SSERVI) both funding and encouraging this work. NR 13 TC 0 Z9 0 U1 4 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD NOV 1 PY 2016 VL 58 IS 9 BP 1648 EP 1653 DI 10.1016/j.asr.2016.08.031 PG 6 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA DY9RW UT WOS:000385473800005 ER PT J AU Sturrock, PA Steinitz, G Fischbach, E Parkhomov, A Scargle, JD AF Sturrock, P. A. Steinitz, G. Fischbach, E. Parkhomov, A. Scargle, J. D. TI Analysis of beta-decay data acquired at the Physikalisch-Technische Bundesanstalt: Evidence of a solar influence SO ASTROPARTICLE PHYSICS LA English DT Article DE Nuclear decays, Neutrinos; Sun ID R-MODE OSCILLATIONS; RADON SIGNALS; SPACED DATA; HALF-LIFE; SPACECRAFT; EFFICIENCY; ISRAEL; RATES AB According to an article entitled Disproof of solar influence on the decay rates of 90Sr/90Y by Kossert and Nahle of the Physikalisch-Technische Bundesanstalt (PTB) [1], the PTB measurements show no evidence of variability. We show that, on the contrary, those measurements reveal strong evidence of variability, including an oscillation at 11 year(-1) that is suggestive of an influence of internal solar rotation. An analysis of radon beta-decay data acquired at the Geological Survey of Israel (GSI) Laboratory for the same time interval yields strong confirmation of this oscillation. (C) 2016 Elsevier B.V. All rights reserved. C1 [Sturrock, P. A.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Sturrock, P. A.] Stanford Univ, Ctr Space Sci & Astrophys, Stanford, CA 94305 USA. [Steinitz, G.] Geol Survey Israel, IL-95501 Jerusalem, Israel. [Fischbach, E.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA. [Parkhomov, A.] Lomonosov Moscow State Univ, Inst Time Nat Explorat, Moscow, Russia. [Scargle, J. D.] NASA Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA. RP Sturrock, PA (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.; Sturrock, PA (reprint author), Stanford Univ, Ctr Space Sci & Astrophys, Stanford, CA 94305 USA. EM sturrock@stanford.edu NR 31 TC 2 Z9 2 U1 3 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 EI 1873-2852 J9 ASTROPART PHYS JI Astropart Phys. PD NOV PY 2016 VL 84 BP 8 EP 14 DI 10.1016/j.astropartphys.2016.07.005 PG 7 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA DZ1MG UT WOS:000385601900002 ER PT J AU Confalonieri, R Bregaglio, S Adam, M Ruget, F Li, T Hasegawa, T Yin, XY Zhu, Y Boote, K Buis, S Fumoto, T Gaydon, D Lafarge, T Marcaida, M Nakagawa, H Ruane, AC Singh, B Singh, U Tang, L Tao, FL Fugice, J Yoshida, H Zhang, Z Wilson, LT Baker, J Yang, YB Masutomi, Y Wallach, D Acutis, M Bouman, B AF Confalonieri, Roberto Bregaglio, Simone Adam, Myriam Ruget, Francoise Li, Tao Hasegawa, Toshihiro Yin, Xinyou Zhu, Yan Boote, Kenneth Buis, Samuel Fumoto, Tamon Gaydon, Donald Lafarge, Tanguy Marcaida, Manuel Nakagawa, Hiroshi Ruane, Alex C. Singh, Balwinder Singh, Upendra Tang, Liang Tao, Fulu Fugice, Job Yoshida, Hiroe Zhang, Zhao Wilson, Lloyd T. Baker, Jeff Yang, Yubin Masutomi, Yuji Wallach, Daniel Acutis, Marco Bouman, Bas TI A taxonomy-based approach to shed light on the babel of mathematical models for rice simulation SO ENVIRONMENTAL MODELLING & SOFTWARE LA English DT Article DE Model classification; Model parameterisation; Model ensemble; Model structure; Rice; Uncertainty ID CROP MODELS; SENSITIVITY-ANALYSIS; CLIMATE-CHANGE; CALIBRATION; YIELD; WHEAT; UNCERTAINTY; WATER; PLASTICITY; EVOLUTION AB For most biophysical domains, differences in model structures are seldom quantified. Here, we used a taxonomy-based approach to characterise thirteen rice models. Classification keys and binary attributes for each key were identified, and models were categorised into five clusters using a binary similarity measure and the unweighted pair-group method with arithmetic mean. Principal component analysis was performed on model outputs at four sites. Results indicated that (i) differences in structure often resulted in similar predictions and (ii) similar structures can lead to large differences in model outputs. User subjectivity during calibration may have hidden expected relationships between model structure and behaviour. This explanation, if confirmed, highlights the need for shared protocols to reduce the degrees of freedom during calibration, and to limit, in turn, the risk that user subjectivity influences model performance. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Confalonieri, Roberto; Bregaglio, Simone; Acutis, Marco] Univ Milan, Cassandra Lab, I-20122 Milan, Italy. [Adam, Myriam; Lafarge, Tanguy] CIRAD, UMR AGAP, F-34398 Montpellier, France. [Ruget, Francoise; Buis, Samuel] INRA, EMMAH UMR1114, F-84914 Avignon, France. [Li, Tao; Marcaida, Manuel; Bouman, Bas] Int Rice Res Inst, Los Banos, Philippines. [Hasegawa, Toshihiro; Fumoto, Tamon] Natl Inst Agroenvironm Sci, Tsukuba, Ibaraki, Japan. [Yin, Xinyou] Wageningen Univ, Ctr Crop Syst Anal, NL-6700 AP Wageningen, Netherlands. [Zhu, Yan; Tang, Liang] Nanjing Agr Univ, Natl Engn & Technol Ctr Informat Agr, Jiangsu Key Lab Informat Agr, Jiangsu Collaborat Innovat Ctr Modern Crop Prod, Nanjing, Jiangsu, Peoples R China. [Boote, Kenneth] Univ Florida, Gainesville, FL USA. [Gaydon, Donald] CSIRO Agr & Food, Brisbane, Qld, Australia. [Nakagawa, Hiroshi; Yoshida, Hiroe] Natl Agr & Food Res Org, Tsukuba, Ibaraki, Japan. [Ruane, Alex C.] NASA, Goddard Inst Space Studies, New York, NY USA. [Singh, Upendra; Fugice, Job] Int Fertilizer Dev Ctr, Muscle Shoals, AL 35662 USA. [Tao, Fulu] Chinese Acad Sci, Inst Geog Sci & Nat Resources Res, Beijing 100864, Peoples R China. [Zhang, Zhao] Beijing Normal Univ, State Key Lab Earth Surface Proc & Resource Ecol, Beijing 100875, Peoples R China. [Wilson, Lloyd T.; Yang, Yubin] Texas A&M AgriLife Res & Extens Ctr, Beaumont, TX USA. [Baker, Jeff] ARS, USDA, Big Spring, TX USA. [Masutomi, Yuji] Ibaraki Univ, Coll Agr, Mito, Ibaraki, Japan. [Wallach, Daniel] INRA, UMR1248, Agrosyst & Dev Terr, F-31326 Castanet Tolosan, France. [Singh, Balwinder] CIMMYT, CG Block,NASC Complex, New Delhi 110012, India. [Tao, Fulu] Nat Resources Inst Finland Luke, Vantaa 01301, Finland. [Li, Tao] AgMIP Rice Team, Tsukuba, Ibaraki, Japan. RP Confalonieri, R (reprint author), Univ Milan, Cassandra Lab, I-20122 Milan, Italy. EM roberto.confalonieri@unimi.it RI Gaydon, Donald /F-4608-2012; OI Wallach, Daniel/0000-0003-3500-8179; Hasegawa, Toshihiro/0000-0001-8501-5612; , Balwinder-Singh/0000-0002-6715-2207 FU National Science Foundation of China [31561143003]; Academy of Finland, PLUMES project [277403]; MAFF; Global Environment Research of MOE, Japan [S-10-2]; National High Tech Research and Development Program of China [2013AA100404]; EC-FP7 [613817] FX FT is supported by the National Science Foundation of China (31561143003) and the Academy of Finland, PLUMES project (277403). TH's participation was supported by MAFF and the Global Environment Research (S-10-2) of MOE, Japan. YZ's work was supported by the National High Tech Research and Development Program of China (2013AA100404). RC was partly supported by EC-FP7 under Grant Agreement No. 613817 (MODEXTREME). Nanjing Agricultural University, International Rice Research Institute, Ministry of Agriculture, Forestry and Fisheries and Ministry of the Environment of Japan, and Cassandra lab. of the University of Milan supported the annual research planning meetings of the AgMIP Rice Team. USDA is an equal opportunity provider and employer. NR 56 TC 0 Z9 0 U1 4 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1364-8152 EI 1873-6726 J9 ENVIRON MODELL SOFTW JI Environ. Modell. Softw. PD NOV PY 2016 VL 85 BP 332 EP 341 DI 10.1016/j.envsoft.2016.09.007 PG 10 WC Computer Science, Interdisciplinary Applications; Engineering, Environmental; Environmental Sciences SC Computer Science; Engineering; Environmental Sciences & Ecology GA DZ1JX UT WOS:000385595800024 ER PT J AU Blankenship, CB Case, JL Zavodsky, BT Crosson, WL AF Blankenship, Clay B. Case, Jonathan L. Zavodsky, Bradley T. Crosson, William L. TI Assimilation of SMOS Retrievals in the Land Information System SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Data assimilation; Kalman filters; land surface; microwave radiometry; passive microwave remote sensing; soil moisture ID SURFACE SOIL-MOISTURE; BRIGHTNESS TEMPERATURE; AIRBORNE CAMPAIGN; WESTERN DENMARK; TRANSFER MODEL; UNITED-STATES; NEAR-SURFACE; GLOBAL-SCALE; PRECIPITATION; VALIDATION AB The Soil Moisture and Ocean Salinity (SMOS) satellite provides retrievals of soil moisture in roughly the upper 5 cm with a 30-50-km resolution and a mission accuracy requirement of 0.04 cm(3)/cm(-3). These observations can be used to improve land surface model (LSM) soil moisture states through data assimilation (DA). In this paper, SMOS soil moisture retrievals are assimilated into the Noah LSM via an Ensemble Kalman Filter within the National Aeronautics and Space Administration Land Information System. Bias correction is implemented using cumulative distribution function (cdf) matching, with points aggregated by either land cover or soil type to reduce the sampling error in generating the cdfs. An experiment was run for the warm season of 2011 to test SMOS DA and to compare assimilation methods. Verification of soil moisture analyses in the 0-10-cm upper layer and the 0-1-m root zone was conducted using in situ measurements from several observing networks in central and southeastern United States. This experiment showed that SMOS DA significantly increased the anomaly correlation of Noah soil moisture with station measurements from 0.45 to 0.57 in the 0-10-cm layer. Time series at specific stations demonstrates the ability of SMOS DA to increase the dynamic range of soil moisture in a manner consistent with station measurements. Among the bias correction methods, the correction based on soil type performed best at bias reduction but also reduced correlations. The vegetation-based correction did not produce any significant differences compared with using a simple uniform correction curve. C1 [Blankenship, Clay B.; Crosson, William L.] Univ Space Res Assoc, Space Technol Inst, Huntsville, AL 35805 USA. [Case, Jonathan L.] ENSCO Inc, Huntsville, AL 35805 USA. [Zavodsky, Bradley T.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35805 USA. RP Blankenship, CB (reprint author), Univ Space Res Assoc, Space Technol Inst, Huntsville, AL 35805 USA. EM clay.blankenship@nasa.gov FU NASA Science Mission Directorate FX This work was supported by the NASA Science Mission Directorate. NR 86 TC 0 Z9 0 U1 12 U2 12 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD NOV PY 2016 VL 54 IS 11 BP 6320 EP 6332 DI 10.1109/TGRS.2016.2579604 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 DY6AP UT WOS:000385188200006 ER PT J AU Kholtygin, AF Mishchenko, MI AF Kholtygin, Alexander F. Mishchenko, Michael I. TI Preface: Viktor V. Sobolev and his scientific legacy SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Editorial Material C1 [Kholtygin, Alexander F.] St Petersburg State Univ, Chair Astron, 28 Univ Prospect, St Petersburg 198504, Russia. [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. RP Kholtygin, AF (reprint author), St Petersburg State Univ, Chair Astron, 28 Univ Prospect, St Petersburg 198504, Russia. EM afkholtygin@gmail.com; michael.i.mishchenko@nasa.gov NR 4 TC 0 Z9 0 U1 0 U2 0 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 NOV PY 2016 VL 183 SI SI BP 1 EP 3 DI 10.1016/j.jqsrt.2016.04.022 PG 3 WC Optics; Spectroscopy SC Optics; Spectroscopy GA DY7SL UT WOS:000385329500001 ER PT J AU Hioki, S Yang, P Kattawar, GW Hu, YX AF Hioki, Souichiro Yang, Ping Kattawar, George W. Hu, Yongxiang TI Truncation of the scattering phase matrix for vector radiative transfer simulation SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article; Proceedings Paper CT International Conference on Radiation Mechanisms of Astrophysical Objects - Classics Today CY SEP 21-25, 2015 CL Saint Petersburg, RUSSIA SP St Petersburg State Univ DE Truncation; Phase matrix; Vector radiative transfer ID TRANSFER EQUATION; DELTA-FIT; APPROXIMATION; SIMILARITY AB This short communication interprets the delta-fit technique in a context of similarity transformation and the correction to the source function, and derives the analogous form of the method to be applied for the scattering phase matrix. To adapt the delta-fit method to vector radiative transfer, the mathematically exact form of the similarity principle is used in the theoretical development. Some examples of relevant radiative transfer simulations are also presented for atmospheric ice particles. The performance of the adopted delta-fit method is comparable to the delta-M method with single scattering correction except for worse delta-fit performance for polarized radiance calculations in forward directions. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Hioki, Souichiro; Yang, Ping; Kattawar, George W.] Texas A&M Univ, College Stn, TX 77843 USA. [Hu, Yongxiang] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23665 USA. RP Hioki, S (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. EM s.hioki@tamu.edu RI Yang, Ping/B-4590-2011; Hu, Yongxiang/K-4426-2012; OI Hioki, Souichiro/0000-0001-6307-1832 NR 15 TC 1 Z9 1 U1 1 U2 1 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 NOV PY 2016 VL 183 SI SI BP 70 EP 77 DI 10.1016/j.jqsrt.2016.06.011 PG 8 WC Optics; Spectroscopy SC Optics; Spectroscopy GA DY7SL UT WOS:000385329500006 ER PT J AU Mishchenko, MI Geogdzhayev, IV Yang, P AF Mishchenko, Michael I. Geogdzhayev, Igor V. Yang, Ping TI Expansion of tabulated scattering matrices in generalized spherical functions SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article; Proceedings Paper CT International Conference on Radiation Mechanisms of Astrophysical Objects - Classics Today CY SEP 21-25, 2015 CL Saint Petersburg, RUSSIA SP St Petersburg State Univ DE Electromagnetic scattering; Polarization; Scattering matrix; Generalized spherical functions; Radiative transfer; Stokes parameters ID VECTOR RADIATIVE-TRANSFER; DISCRETE-DIPOLE APPROXIMATION; INVARIANT IMBEDDING METHOD; NONSPHERICAL ICE CRYSTALS; LIGHT-SCATTERING; T-MATRIX; POLARIZED-LIGHT; TRANSFER MODELS; MIE SCATTERING; BIDIRECTIONAL REFLECTANCE AB An efficient way to solve the vector radiative transfer equation for plane-parallel turbid media is to Fourier-decompose it in azimuth. This methodology is typically based on the analytical computation of the Fourier components of the phase matrix and is predicated on the knowledge of the coefficients appearing in the expansion of the normalized scattering matrix in generalized spherical functions. Quite often the expansion coefficients have to be determined from tabulated values of the scattering matrix obtained from measurements or calculated by solving the Maxwell equations. In such cases one needs an efficient and accurate computer procedure converting a tabulated scattering matrix into the corresponding set of expansion coefficients. This short communication summarizes the theoretical basis of this procedure and serves as the user guide to a simple public domain FORTRAN program. Published by Elsevier Ltd. C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. [Geogdzhayev, Igor V.] Columbia Univ, NASA GISS, Dept Appl Phys & Appl Math, 2880 Broadway, New York, NY 10025 USA. [Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM michael.i.mishchenko@nasa.gov RI Yang, Ping/B-4590-2011 NR 80 TC 0 Z9 0 U1 1 U2 1 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 NOV PY 2016 VL 183 SI SI BP 78 EP 84 DI 10.1016/j.jqsrt.2016.05.015 PG 7 WC Optics; Spectroscopy SC Optics; Spectroscopy GA DY7SL UT WOS:000385329500007 ER PT J AU Mishchenko, MI Dlugach, JM AF Mishchenko, Michael I. Dlugach, Janna M. TI Scattering of Gaussian beams by disordered particulate media SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article; Proceedings Paper CT International Conference on Radiation Mechanisms of Astrophysical Objects - Classics Today CY SEP 21-25, 2015 CL Saint Petersburg, RUSSIA SP St Petersburg State Univ DE Electromagnetic scattering; Multi-particle groups; Gaussian beams; Speckles; Diffuse scattering patterns; Radiative transfer theory ID MULTIPLE-SCATTERING; RADIATIVE-TRANSFER; T-MATRIX; PARTICLES; ENSEMBLES; SPHERES AB A frequently observed characteristic of electromagnetic scattering by a disordered particulate medium is the absence of pronounced speckles in angular patterns of the scattered light. It is known that such diffuse speckle-free scattering patterns can be caused by averaging over randomly changing particle positions and/or over a finite spectral range. To get further insight into the possible physical causes of the absence of speckles, we use the numerically exact superposition T-matrix solver of the Maxwell equations and analyze the scattering of plane-wave and Gaussian beams by representative multi-sphere groups. We show that phase and amplitude variations across an incident Gaussian beam do not serve to extinguish the pronounced speckle pattern typical of plane-wave illumination of a fixed multi-particle group. Averaging over random particle positions and/or over a finite spectral range is still required to generate the classical diffuse speckle-free regime. Published by Elsevier Ltd. C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. [Dlugach, Janna M.] Natl Acad Sci Ukraine, Main Astron Observ, 27 Zabolotny Str, UA-03680 Kiev, Ukraine. RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM michael.i.mishchenko@nasa.gov NR 32 TC 0 Z9 0 U1 5 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD NOV PY 2016 VL 183 SI SI BP 85 EP 89 DI 10.1016/j.jqsrt.2016.04.016 PG 5 WC Optics; Spectroscopy SC Optics; Spectroscopy GA DY7SL UT WOS:000385329500008 ER PT J AU Cui, H Grazhdankin, DV Xiao, SH Peek, S Rogov, VI Bykova, NV Sievers, NE Liu, XM Kaufman, AJ AF Cui, Huan Grazhdankin, Dmitriy V. Xiao, Shuhai Peek, Sara Rogov, Vladimir I. Bykova, Natalia V. Sievers, Natalie E. Liu, Xiao-Ming Kaufman, Alan J. TI Redox-dependent distribution of early macro-organisms: Evidence from the terminal Ediacaran Khatyspyt Formation in Arctic Siberia SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Chemostratigraphy; Redox condition; Early macro-organism distribution; Carbon and sulfur cycles; Oceanic euxinia; Superheavy pyrite ID CARBONATE-ASSOCIATED SULFATE; PRECAMBRIAN-CAMBRIAN BOUNDARY; SULFUR ISOTOPE FRACTIONATION; PROTEROZOIC OCEAN CHEMISTRY; LOW MARINE SULFATE; SULTANATE-OF-OMAN; SOUTH CHINA SEA; DOUSHANTUO FORMATION; ATMOSPHERIC OXYGEN; YANGTZE PLATFORM AB The Ediacaran Period witnessed the first appearance of macroscopic animal life in Earth's history. However, the biogeochemical context for the stratigraphic occurrence of early metazoans is largely uncertain, in part due to the dearth of integrated paleobiological and chemostratigraphic datasets. In this study, a comprehensive geochemical analysis was conducted on the fossiliferous Khatyspyt Formation in Arctic Siberia, in order to gain insights into the Ediacaran paleoenvironments. This study was designed to specifically address the relationship between paleoredox conditions and Ediacaran fossil occurrences in the Khatyspyt Formation. Our data reveal a dramatic shift in pyrite sulfur isotope compositions (delta S-34(pyrite)) from ca. -20 parts per thousand to ca. 55 parts per thousand, and this shift is intriguingly associated with the first occurrence of Ediacara-type macrofossils at the studied section, suggesting a possible link between seawater redox conditions and distribution of early macroscopic organisms. Based on multiple lines of sedimentological and geochemical evidence, we propose that the development of oceanic euxinia - which may be widespread in the continental margins due to enhanced oxidative weathering in the terminal Ediacaran Period may have locally prohibited the colonization of Ediacara-type organisms and resulted in low delta S-34(pyrite) values in the lower Khatyspyt Formation. In the middle and upper Khatyspyt Formation, progressive secular transition from euxinic to non-euxinic and more habitable conditions may have allowed for the colonization of Ediacara-type and other macro-organisms. (C) 2016 Elsevier B.V. All rights reserved. C1 [Cui, Huan] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Cui, Huan] Univ Wisconsin, NASA, Astrobiol Inst, Madison, WI 53706 USA. [Cui, Huan; Peek, Sara; Sievers, Natalie E.; Kaufman, Alan J.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Cui, Huan; Peek, Sara; Sievers, Natalie E.; Kaufman, Alan J.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Grazhdankin, Dmitriy V.; Rogov, Vladimir I.] Russian Acad Sci, Siberian Branch, Trofimuk Inst Petr Geol & Geophys, Novosibirsk 630090, Russia. [Grazhdankin, Dmitriy V.] Novosibirsk State Univ, Dept Geol & Geophys, Novosibirsk 630090, Russia. [Xiao, Shuhai; Bykova, Natalia V.] Virginia Tech, Dept Geosci, Blacksburg, VA 24061 USA. [Liu, Xiao-Ming] Univ N Carolina, Dept Geol Sci, Chapel Hill, NC 27599 USA. [Peek, Sara] US Geol Survey, 345 Middlefield Rd, Menlo Pk, CA 94025 USA. [Sievers, Natalie E.] Stanford Univ, Dept Geol Sci, Sch Earth Energy & Environm Sci, Stanford, CA 94305 USA. RP Cui, H (reprint author), Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.; Cui, H (reprint author), Univ Wisconsin, NASA, Astrobiol Inst, Madison, WI 53706 USA. EM Huan.Cui@Wisc.EDU RI Xiao, Shuhai/A-2190-2009; Grazhdankin, Dmitriy/A-4060-2008; OI Xiao, Shuhai/0000-0003-4655-2663; Grazhdankin, Dmitriy/0000-0003-0797-1347; Cui, Huan/0000-0003-0705-3423 FU NASA Exobiology grant [NNX12AR91G, NNX15AL27G]; NSF Sedimentary Geology and Paleontology grant [EAR0844270, EAR1528553]; Carnegie Institution of Washington Postdoctoral Fellowship; Russian Science Foundation [14-17-00409]; Committee of the National Geographic Society for Research and Exploration [8227-07, 8637-09, 9031-11]; NASA Astrobiology Institute FX This research is funded by the NASA Exobiology grant (NNX12AR91G to AJK and NNX15AL27G to SX), the NSF Sedimentary Geology and Paleontology grant (EAR0844270 to AJK; EAR1528553 to SX), the Carnegie Institution of Washington Postdoctoral Fellowship to XML. Part of the stratigraphic, sedimentological and paleoecological studies of the Khatyspyt Formation was supported by the Russian Science Foundation (grant 14-17-00409 to DVG) and the Committee of the National Geographic Society for Research and Exploration (grants 8227-07, 8637-09, 9031-11 to DVG). HC acknowledges the NASA Astrobiology Institute for support. NR 193 TC 1 Z9 1 U1 17 U2 17 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 EI 1872-616X J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD NOV 1 PY 2016 VL 461 BP 122 EP 139 DI 10.1016/j.palaeo.2016.08.015 PG 18 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA DZ1LM UT WOS:000385599900011 ER PT J AU Zhou, CM Guan, CG Cui, H Ouyang, Q Wang, W AF Zhou, Chuanming Guan, Chengguo Cui, Huan Ouyang, Qing Wang, Wei TI Methane-derived authigenic carbonate from the lower Doushantuo Formation of South China: Implications for seawater sulfate concentration and global carbon cycle in the early Ediacaran ocean SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Anaerobic oxidation of methane; Microbial sulfate reduction; Cold seep deposits; Carbon cycle; Sulfur cycle; Carbon isotope chemostratigraphy ID LOW MARINE SULFATE; ANAEROBIC OXIDATION; ISOTOPIC COMPOSITION; HYDROCARBON SEEPS; GEOLOGICAL RECORD; SECULAR VARIATION; JOHNNIE FORMATION; ROCK INTERACTION; ORGANIC-MATTER; DEEP BIOSPHERE AB Authigenic carbonate associated with anaerobic oxidation of methane (AOM), usually via microbial sulfate reduction (MSR) or ferric iron reduction, is generally characterized by extremely low delta C-13 values (<-30 parts per thousand, VPDB). This has been used as one of the major diagnostic features for the recognition of hydrocarbon seep carbonate in the geological past. Previous reports on Precambrian authigenic carbonates are rare, limiting our understanding of the effects of their deposition on the Earth's carbon isotopic mass balance. In this study, mainly based on petrographic features and pronounced negative delta C-13 values as low as -38.1 parts per thousand, we discovered authigenic calcite cement immediately above the cap dolostone in the basal Ediacaran Doushantuo Formation in the Jiulongwan section, Yangtze Gorges area, South China. Our observations not only provide direct evidence for the involvement of AOM during carbonate precipitation in the early Ediacaran (similar to 635 Ma), but also suggest that the seawater sulfate concentrations in the early Ediacaran may have been higher than previously thought. (C) 2016 Elsevier B.V. All rights reserved. C1 [Zhou, Chuanming; Guan, Chengguo; Ouyang, Qing; Wang, Wei] Chinese Acad Sci, Nanjing Inst Geol & Palaeontol, Key Lab Econ Stratig & Palaeogeog, Nanjing 210008, Peoples R China. [Cui, Huan] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Cui, Huan] Univ Wisconsin, NASA, Astrobiol Inst, Madison, WI 53706 USA. [Ouyang, Qing] Univ Chinese Acad Sci, Beijing 100049, Peoples R China. RP Zhou, CM (reprint author), Chinese Acad Sci, Nanjing Inst Geol & Palaeontol, Key Lab Econ Stratig & Palaeogeog, Nanjing 210008, Peoples R China. EM cmzhou@nigpas.ac.cn RI Zhou, Chuanming/E-5313-2010; OI Cui, Huan/0000-0003-0705-3423 FU Ministry of Science and Technology of China [2013CB835005]; Chinese Academy of Sciences [KZZD-EW-02] FX This work was supported by the Ministry of Science and Technology of China (2013CB835005) and Chinese Academy of Sciences (KZZD-EW-02). We thank Chen Xiaoming and Wu Yuping for assistance in carbon and sulfur isotope measurements. H.C. thanks the NASA Astrobiology Institute in UW-Madison for support. We are grateful to Thomas Algeo, Linda Kah and an anonymous reviewer for their constructive comments. NR 102 TC 2 Z9 2 U1 27 U2 27 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 EI 1872-616X J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD NOV 1 PY 2016 VL 461 BP 145 EP 155 DI 10.1016/j.palaeo.2016.08.017 PG 11 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA DZ1LM UT WOS:000385599900013 ER PT J AU Monson, RK Neice, AA Trahan, NA Shiach, I McCorkel, JT Moore, DJP AF Monson, Russell K. Neice, Amberly A. Trahan, Nicole A. Shiach, Ian McCorkel, Joel T. Moore, David J. P. TI Interactions between temperature and intercellular CO2 concentration in controlling leaf isoprene emission rates SO PLANT CELL AND ENVIRONMENT LA English DT Article DE abiotic; hot; model; ozone; photosynthesis; stress; terpene; thermotolerance ID HYBRID ASPEN; TERRESTRIAL ECOSYSTEMS; TROPOSPHERIC CHEMISTRY; CARBON-DIOXIDE; PHOTON FLUX; LEAVES; PHOTOSYNTHESIS; PLANTS; LIGHT; GROWTH AB Plant isoprene emissions have been linked to several reaction pathways involved in atmospheric photochemistry. Evidence exists from a limited set of past observations that isoprene emission rate (I-s) decreases as a function of increasing atmospheric CO2 concentration, and that increased temperature suppresses the CO2 effect. We studied interactions between intercellular CO2 concentration (C-i) and temperature as they affect I-s in field-grown hybrid poplar trees in one of the warmest climates on earth - the Sonoran Desert of the southwestern United States. We observed an unexpected midsummer downregulation of I-s despite the persistence of relatively high temperatures. High temperature suppression of the I-s:C-i relation occurred at all times during the growing season, but sensitivity of I-s to increased C-i was greatest during the midsummer period when I-s was lowest. We interpret the seasonal downregulation of I-s and increased sensitivity of I-s to C-i as being caused by weather changes associated with the onset of a regional monsoon system. Our observations on the temperature suppression of the I-s:C-i relation are best explained by the existence of a small pool of chloroplastic inorganic phosphate, balanced by several large, connected metabolic fluxes, which together, determine the C-i and temperature dependencies of phosphoenolpyruvate import into the chloroplast. Isoprene emissions from leaves are known to influence the oxidative capacity of the lower atmosphere and contribute to the formation of organic aerosol particles. Our research shows that isoprene emissions are inhibited by elevated atmospheric CO2 concentration, and that warmer leaf temperatures reduce the CO2 inhibition. The influence of warmer leaf temperatures is proposed to be because of modifications of the chloroplast inorganic phosphate balance and concomitant potential to import phosphoenolpyruvate into the chloroplast from the cytosol, which is required for isoprene biosynthesis. C1 [Monson, Russell K.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. [Monson, Russell K.] Univ Arizona, Tree Ring Res Lab, Tucson, AZ 85721 USA. [Neice, Amberly A.] Hiram Coll, Dept Biol, Hiram, OH 44234 USA. [Trahan, Nicole A.; Shiach, Ian; Moore, David J. P.] Univ Arizona, Sch Nat Resources & Environm, Tucson, AZ 85721 USA. [McCorkel, Joel T.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. RP Monson, RK (reprint author), Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA.; Monson, RK (reprint author), Univ Arizona, Tree Ring Res Lab, Tucson, AZ 85721 USA. EM russmonson@email.arizona.edu FU Arizona Technology Research Initiative Fund (TRIF); Research Experiences for Undergraduates (REU) grant FX This work was supported by a grant from the Arizona Technology Research Initiative Fund (TRIF), and the Research Experiences for Undergraduates (REU) grant to the University of Arizona, Biosphere 2 programme. The authors are grateful to Professor Tom Sharkey, Michigan State University, for comments on early draft portions of the manuscript, and two anonymous reviewers who provided valuable comments to improve the manuscript. The authors have no conflicts of interest to declare with regard to this publication. NR 52 TC 0 Z9 0 U1 18 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0140-7791 EI 1365-3040 J9 PLANT CELL ENVIRON JI Plant Cell Environ. PD NOV PY 2016 VL 39 IS 11 BP 2404 EP 2413 DI 10.1111/pce.12787 PG 10 WC Plant Sciences SC Plant Sciences GA DZ4QA UT WOS:000385842400006 PM 27352095 ER PT J AU Singh, MK Gautam, R Gatebe, CK Poudyal, R AF Singh, Manoj K. Gautam, Ritesh Gatebe, Charles K. Poudyal, Rajesh TI PolarBRDF: A general purpose Python package for visualization and quantitative analysis of multi-angular remote sensing measurements SO COMPUTERS & GEOSCIENCES LA English DT Article DE BRDF; Remote Sensing; False Color Imagery; Polar plot; Python ID AIRBORNE SPECTRAL MEASUREMENTS; SURFACE-ATMOSPHERE ANISOTROPY; RADIATIVE FLUX ESTIMATION; ENERGY SYSTEM INSTRUMENT; BIDIRECTIONAL REFLECTANCE; DISTRIBUTION MODELS; PART I; CLOUDS; METHODOLOGY; SATELLITE AB The Bidirectional Reflectance Distribution Function (BRDF) is a fundamental concept for characterizing the reflectance property of a surface, and helps in the analysis of remote sensing data from satellite, airborne and surface platforms. Multi-angular remote sensing measurements are required for the development and evaluation of BRDF models for improved characterization of surface properties. However, multi-angular data and the associated BRDF models are typically multidimensional involving multi-angular and multi-wavelength information. Effective visualization of such complex multidimensional measurements for different wavelength combinations is presently somewhat lacking in the literature, and could serve as a potentially useful research and teaching tool in aiding both interpretation and analysis of BRDF measurements. This article describes a newly developed software package in Python (PolarBRDF) to help visualize and analyze multi-angular data in polar and False Color Composite (FCC) forms. PolarBRDF also includes functionalities for computing important multi-angular reflectance/albedo parameters including spectral albedo, principal plane reflectance and spectral reflectance slope. Application of PolarBRDF is demonstrated using various case studies obtained from airborne multi-angular remote sensing measurements using NASA's Cloud Absorption Radiometer (CAR). Our visualization program also provides functionalities for untangling complex surface/atmosphere features embedded in pixel-based remote sensing measurements, such as the FCC imagery generation of BRDF measurements of grasslands in the presence of wildfire smoke and clouds. Furthermore, PolarBRDF also provides quantitative information of the angular distribution of scattered surface/atmosphere radiation, in the form of relevant BRDF variables such as sunglint, hotspot and scattering statistics. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Singh, Manoj K.; Gautam, Ritesh] Indian Inst Technol, Ctr Studies Resources Engn, Bombay 400076, Maharashtra, India. [Gautam, Ritesh] Indian Inst Technol, Interdisciplinary Program Climate Studies, Bombay 400076, Maharashtra, India. [Gatebe, Charles K.] Univ Space Res Assoc, Columbia, MD 21046 USA. [Gatebe, Charles K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Poudyal, Rajesh] Sci Syst & Applicat Inc, Lanham, MD USA. RP Singh, MK; Gautam, R (reprint author), Indian Inst Technol, Ctr Studies Resources Engn, Bombay 400076, Maharashtra, India.; Gatebe, CK (reprint author), Univ Space Res Assoc, Columbia, MD 21046 USA.; Gautam, R (reprint author), Indian Inst Technol, Ctr Studies Resources Engn, Bombay 400076, Maharashtra, India. EM manojks@iitb.ac.in; rgautam@iitb.ac.in; charles.k.gatebe@nasa.gov FU Science Mission Directorate of the National Aeronautics and Space Administration under the Radiation Sciences program (Atmospheric Composition Campaign Data Analysis and Modeling Program, ACCDAM) FX Presently, the PolarBRDF software is available at http://home pages.iitb.ac.in/similar to manojks/, after review of the manuscript is completed, the package will be publicly made available at http://car.gsfc.nasa.gov/. We greatly appreciate the comments and suggestions by the two anonymous reviewers which helped improve an earlier version of the manuscript. This research effort is supported by the Science Mission Directorate of the National Aeronautics and Space Administration under the Radiation Sciences program (Atmospheric Composition Campaign Data Analysis and Modeling Program, ACCDAM), managed by Hal Maring. NR 31 TC 1 Z9 1 U1 11 U2 11 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 NOV PY 2016 VL 96 BP 173 EP 180 DI 10.1016/j.cageo.2016.08.015 PG 8 WC Computer Science, Interdisciplinary Applications; Geosciences, Multidisciplinary SC Computer Science; Geology GA DY1LA UT WOS:000384855300016 ER PT J AU Larour, E Schlegel, N AF Larour, E. Schlegel, N. TI On ISSM and leveraging the Cloud towards faster quantification of the uncertainty in ice-sheet mass balance projections SO COMPUTERS & GEOSCIENCES LA English DT Article DE Polar; Ice sheet; Modeling; Cloud; Uncertainty quantification ID NORTHEAST GREENLAND; MODEL; FLOW; SENSITIVITY; CREEP AB With the Amazon EC2 Cloud becoming available as a viable platform for parallel computing, Earth System Models are increasingly interested in leveraging its capabilities towards improving climate projections. In particular, faced with long wait periods on high-end clusters, the elasticity of the Cloud presents a unique opportunity of potentially "infinite" availability of small-sized clusters running on high-performance instances. Among specific applications of this new paradigm, we show here how uncertainty quantification in climate projections of polar ice sheets (Antarctica and Greenland) can be significantly accelerated using the Cloud. Indeed, small-sized clusters are very efficient at delivering sensitivity and sampling analysis, core tools of uncertainty quantification. We demonstrate how this approach was used to carry out an extensive analysis of ice-flow projections on one of the largest basins in Greenland, the North-East Greenland Glacier, using the Ice Sheet System Model, the public-domain NASA-funded ice-flow modeling software. We show how errors in the projections were accurately quantified using Monte-Carlo sampling analysis on the EC2 Cloud, and how a judicious mix of high-end parallel computing and Cloud use can best leverage existing infrastructures, and significantly accelerate delivery of potentially ground-breaking climate projections, and in particular, enable uncertainty quantification that were previously impossible to achieve. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Larour, E.; Schlegel, N.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr MS 300-323, Pasadena, CA 91109 USA. [Schlegel, N.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, 607 Charles E Young Dr East,Young Hall,Room 4242, Los Angeles, CA 90095 USA. RP Larour, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr MS 300-323, Pasadena, CA 91109 USA. EM eric.larour@jpl.nasa.gov FU NASA's Cryosphere Sciences Program; Modeling, Analysis and Prediction Program; President's and Director's Fund FX This work was supported by grants from NASA's Cryosphere Sciences Program as well as funding from the Modeling, Analysis and Prediction Program and funding from the President's and Director's Fund Program. This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration, and at the University of California at Los Angeles, Joint Institute for Regional Earth System Science and Engineering. We also want to thank JPL's Office of the Chief Information Office for facilitating access to the EC2 Cloud, in particular, Tom Soderstrom (Chief Technology and Innovation Officer) and Jonathan Chiang. Finally, we want to thank Dr. Khawaja Shams (formerly at JPL at the time of this work, now VP of Engineering at Elemental Technologies) for his invaluable help and insights on the Amazon EC2 Cloud. NR 40 TC 0 Z9 0 U1 5 U2 5 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 NOV PY 2016 VL 96 BP 193 EP 201 DI 10.1016/j.cageo.2016.08.007 PG 9 WC Computer Science, Interdisciplinary Applications; Geosciences, Multidisciplinary SC Computer Science; Geology GA DY1LA UT WOS:000384855300018 ER PT J AU Hossain, K Hoglund, L Phinney, LC Golding, TD Wicks, G Khoshakhlagh, A Ting, DZY Soibel, A Gunapala, SD AF Hossain, K. Hoeglund, L. Phinney, L. C. Golding, T. D. Wicks, G. Khoshakhlagh, A. Ting, D. Z. -Y. Soibel, A. Gunapala, S. D. TI Hydrogenation Defect Passivation for Improved Minority Carrier Lifetime in Midwavelength Ga-Free InAs/InAsSb Superlattices SO JOURNAL OF ELECTRONIC MATERIALS LA English DT Article DE Hydrogenation; strain layer superlattice; type-II SLS; carrier lifetime; defect passivation; Ga-free; InAs; InAsSb AB Two hydrogenation techniques were used to passivate defects in InAs/InAsSb superlattices: UV-photon assisted hydrogenation with and without DC bias enhancement. The effects of the hydrogenation on the minority carrier lifetime were studied using photoluminescence and optical modulation response. An increase of the minority carrier lifetime from 1.8 mu s to 3.3 mu s with hydrogenation using both methods was observed; however, the processing time shortened from 24 h to 90 min when using the DC bias enhancement. The largest increase in carrier lifetime corresponded to a deuterium density of 9 x 10(14) atoms/cm(2), as measured by nuclear reaction analysis. C1 [Hossain, K.; Phinney, L. C.; Golding, T. D.; Wicks, G.] Amethyst Res Inc, 123 Case Circle, Ardmore, OK 73401 USA. [Hoeglund, L.; Khoshakhlagh, A.; Ting, D. Z. -Y.; Soibel, A.; Gunapala, S. D.] CALTECH, Jet Prop Lab, Ctr Infrared Photodetectors, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Hossain, K (reprint author), Amethyst Res Inc, 123 Case Circle, Ardmore, OK 73401 USA. EM khalid@unt.edu FU National Aeronautics and Space Administration FX The authors are grateful for the support and encouragement of Drs. Meimei Tidrow and Sumith Bandara of Night Vision and Electronic Sensors Directorate RDER-NVD. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 8 TC 0 Z9 0 U1 11 U2 11 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0361-5235 EI 1543-186X J9 J ELECTRON MATER JI J. Electron. Mater. PD NOV PY 2016 VL 45 IS 11 BP 5626 EP 5629 DI 10.1007/s11664-016-4617-z PG 4 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA DY3UT UT WOS:000385021300018 ER PT J AU Holgate, TC Bennett, R Hammel, T Caillat, T Keyser, S Sievers, B AF Holgate, Tim C. Bennett, Russell Hammel, Tom Caillat, Thierry Keyser, Steve Sievers, Bob TI Increasing the Efficiency of the Multi-mission Radioisotope Thermoelectric Generator (vol 44, pg 1814, 2015) SO JOURNAL OF ELECTRONIC MATERIALS LA English DT Correction C1 [Holgate, Tim C.; Bennett, Russell; Hammel, Tom; Keyser, Steve; Sievers, Bob] TESI, Hunt Valley, MD 21031 USA. [Caillat, Thierry] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Holgate, TC (reprint author), TESI, Hunt Valley, MD 21031 USA. EM Tim.holgate@teledyne.com NR 1 TC 0 Z9 0 U1 5 U2 5 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0361-5235 EI 1543-186X J9 J ELECTRON MATER JI J. Electron. Mater. PD NOV PY 2016 VL 45 IS 11 BP 6044 EP 6044 DI 10.1007/s11664-016-4776-y PG 1 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA DY3UT UT WOS:000385021300069 ER PT J AU Benham, K Hodyss, R Fernandez, FM Orlando, TM AF Benham, Kevin Hodyss, Robert Fernandez, Facundo M. Orlando, Thomas M. TI Laser-Induced Acoustic Desorption Atmospheric Pressure Photoionization via VUV-Generating Microplasmas SO JOURNAL OF THE AMERICAN SOCIETY FOR MASS SPECTROMETRY LA English DT Article DE Laser-induced acoustic desorption; Atmospheric pressure photoionization; Microplasma; Microhollow cathode discharge; Low-polarity analytes ID IONIZATION-MASS-SPECTROMETRY; ORGANIC-MOLECULES; DISCHARGE PLASMAS; EXCIMER EMISSION; LYMAN-ALPHA; GAS-PHASE; ENERGY; IONS; FRAGMENTATION; CHOLESTEROL AB We demonstrate the first application of laser-induced acoustic desorption (LIAD) and atmospheric pressure photoionization (APPI) as a mass spectrometric method for detecting low-polarity organics. This was accomplished using a Lyman-alpha (10.2 eV) photon generating microhollow cathode discharge (MHCD) microplasma photon source in conjunction with the addition of a gas-phase molecular dopant. This combination provided a soft desorption and a relatively soft ionization technique. Selected compounds analyzed include alpha-tocopherol, perylene, cholesterol, phenanthrene, phylloquinone, and squalene. Detectable surface concentrations as low as a few pmol per spot sampled were achievable using test molecules. The combination of LIAD and APPI provided a soft desorption and ionization technique that can allow detection of labile, low-polarity, structurally complex molecules over a wide mass range with minimal fragmentation. C1 [Benham, Kevin; Fernandez, Facundo M.; Orlando, Thomas M.] Georgia Inst Technol, Sch Chem & Biochem, 901 Atlantic Dr NW, Atlanta, GA 30332 USA. [Hodyss, Robert] CALTECH, Jet Prop Lab, Cryogen Chem Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Orlando, Thomas M.] Georgia Inst Technol, Sch Phys, 837 State St, Atlanta, GA 30332 USA. RP Orlando, TM (reprint author), Georgia Inst Technol, Sch Chem & Biochem, 901 Atlantic Dr NW, Atlanta, GA 30332 USA.; Orlando, TM (reprint author), Georgia Inst Technol, Sch Phys, 837 State St, Atlanta, GA 30332 USA. EM thomas.orlando@chemistry.gatech.edu FU NSF [CHE-1504217]; NASA Astrobiology Program under NSF Center for Chemical Evolution [CHE-1504217]; Jet Propulsion Laboratory-Georgia Institute of Technology Strategic University Research Partnership (JPL-GIT SURP) grant FX This work was jointly supported by NSF and the NASA Astrobiology Program, under the NSF Center for Chemical Evolution, CHE-1504217. Work at JPL on VUV detection was supported by a joint Jet Propulsion Laboratory-Georgia Institute of Technology Strategic University Research Partnership (JPL-GIT SURP) grant. NR 42 TC 1 Z9 1 U1 10 U2 10 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1044-0305 EI 1879-1123 J9 J AM SOC MASS SPECTR JI J. Am. Soc. Mass Spectrom. PD NOV PY 2016 VL 27 IS 11 BP 1805 EP 1812 DI 10.1007/s13361-016-1467-0 PG 8 WC Biochemical Research Methods; Chemistry, Analytical; Chemistry, Physical; Spectroscopy SC Biochemistry & Molecular Biology; Chemistry; Spectroscopy GA DY5RC UT WOS:000385158400012 PM 27624160 ER PT J AU Kourdis, PD Bellan, J AF Kourdis, Panayotis D. Bellan, Josette TI Highly Reduced Species Mechanisms for iso-Cetane Using the Local Self-Similarity Tabulation Method SO INTERNATIONAL JOURNAL OF CHEMICAL KINETICS LA English DT Article ID CHEMICAL-KINETICS; REDUCTION; MANIFOLDS; OXIDATION; CHEMISTRY; PRESSURE; STATE AB We utilize the local self-similarity tabulation method to drastically downsize the number of species involved in a detailed kinetic mechanism of iso-cetane. Reduced-species mechanisms of 20 and 15 species are constructed, out of the 1114 species involved in the detailed mechanism, with a focus on high-pressure combustion. The performance of the two reduced mechanisms are compared to the detailed one for a lean (phi = 0.5), stoichiometric (phi = 1.0), and rich (phi = 1.5) iso-cetane/air mixture at initial temperatures of 900 and 1100 K and constant pressures of 20 and 40 bar. Good to very good agreement between the detailed kinetic mechanism and the two highly reduced species mechanisms are demonstrated. C1 [Kourdis, Panayotis D.; Bellan, Josette] CALTECH, Pasadena, CA 91125 USA. [Bellan, Josette] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Kourdis, Panayotis D.] Stanford Univ, Sch Med, Stanford, CA 94305 USA. RP Bellan, J (reprint author), CALTECH, Pasadena, CA 91125 USA.; Bellan, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Josette.Bellan@jpl.nasa.gov FU U.S. Army Research Office FX This work was performed at the California Institute of Technology and the Jet Propulsion Laboratory Division of the California Institute of Technology and was sponsored by the U.S. Army Research Office, with Dr. Ralph Anthenien as contract monitor. Supercomputing time from the DoD HPCMP Open Research Systems and NASA (ARMD program) is gratefully acknowledged. NR 17 TC 1 Z9 1 U1 2 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0538-8066 EI 1097-4601 J9 INT J CHEM KINET JI Int. J. Chem. Kinet. PD NOV PY 2016 VL 48 IS 11 BP 739 EP 752 DI 10.1002/kin.21029 PG 14 WC Chemistry, Physical SC Chemistry GA DX9AP UT WOS:000384685300009 ER PT J AU Fuller, L Lopez-Rodriguez, E Packham, C Ramos-Almeida, C Alonso-Herrero, A Levenson, NA Radomski, J Ichikawa, K Garcia-Bernete, I Gonzalez-Martin, O Diaz-Santos, T Martinez-Paredes, M AF Fuller, L. Lopez-Rodriguez, E. Packham, C. Ramos-Almeida, C. Alonso-Herrero, A. Levenson, N. A. Radomski, J. Ichikawa, K. Garcia-Bernete, I. Gonzalez-Martin, O. Diaz-Santos, T. Martinez-Paredes, M. TI Investigating the dusty torus of Seyfert galaxies using SOFIA/FORCAST photometry SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: nuclei; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; INFRARED-EMISSION; MIDINFRARED EMISSION; X-RAY; NEARBY GALAXIES; LINE REGION; THICK TORI; AGN TORI; NGC 2992 AB We present 31.5 mu m imaging photometry of 11 nearby Seyfert galaxies observed from the Stratospheric Observatory For Infrared Astronomy (SOFIA) using the Faint Object infraRed CAmera for the SOFIA Telescope (FORCAST). We tentatively detect extended 31 mu m emission for the first time in our sample. In combination with this new data set, subarcsecond resolution 1-18 mu m imaging and 7.5-13 mu m spectroscopic observations were used to compute the nuclear spectral energy distribution (SED) of each galaxy. We found that the turnover of the torus emission does not occur at wavelengths <= 31.5 mu m, which we interpret as a lower-limit for the wavelength of peak emission. We used CLUMPY torus models to fit the nuclear infrared (IR) SED and infer trends in the physical parameters of the AGN torus for the galaxies in the sample. Including the 31.5 mu m nuclear flux in the SED (1) reduces the number of clumpy torus models compatible with the data, and (2) modifies the model output for the outer radial extent of the torus for 10 of the 11 objects. Specifically, six (60 per cent) objects show a decrease in radial extent while four (40 per cent) show an increase. We find torus outer radii ranging from <1 to 8.4 pc. C1 [Fuller, L.; Packham, C.; Alonso-Herrero, A.] Univ Texas San Antonio, Dept Phys & Astron, One UTSA Circle, San Antonio, TX 78249 USA. [Lopez-Rodriguez, E.] Univ Texas Austin, Dept Astron, 2515 Speedway,Stop C1402, Austin, TX 78712 USA. [Lopez-Rodriguez, E.] Univ Texas Austin, McDonald Observ, 2515 Speedway,Stop C1402, Austin, TX 78712 USA. [Packham, C.; Ichikawa, K.] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Ramos-Almeida, C.; Garcia-Bernete, I.] Inst Astrofis Canarias, Calle Via Lactea S-N, E-38205 Tenerife, Spain. [Ramos-Almeida, C.; Garcia-Bernete, I.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Alonso-Herrero, A.] CSIC INTA, Ctr Astrobil CAB, ESAC Campus, E-28692 Madrid, Spain. [Alonso-Herrero, A.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Levenson, N. A.] Gemini Observ, Casilla 603, La Serena, Chile. [Radomski, J.] NASA, SOFIA USRA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gonzalez-Martin, O.; Martinez-Paredes, M.] UNAM, Inst Radioastron & Astrofis IRyA, 3-72 Xangari,8701, Morelia, Michoacan, Mexico. [Diaz-Santos, T.] Univ Diego Portales, Nucleo Astron, Fac Ingn, Av Ejercito Libertador 441, Santiago, Chile. RP Fuller, L (reprint author), Univ Texas San Antonio, Dept Phys & Astron, One UTSA Circle, San Antonio, TX 78249 USA. EM lindsay.fuller@utsa.edu RI Alonso-Herrero, Almudena/H-1426-2015 OI Alonso-Herrero, Almudena/0000-0001-6794-2519 FU NASA [NAS2-97001, 002_35, 04_0048]; Deutsches SOFIA Institut (DSI) under DLR [50 OK 0901]; University of Texas at San Antonio; Ramon y Cajal Fellowship [RYC-2014-15779]; Spanish Plan Nacional de Astronomia y Astrofisica [AYA2012-3144]; FEDER program; JSPS [40756293]; Gemini Observatory; Instituto de Astrofisica de Canarias through Fundacion La Caixa; ALMA-CONICYT [31130005]; FONDECYT [1151239]; [NSF-0904421]; [AYA2015-64346-C2-1-P] FX This work is based on observations made with the NASA/DLR SOFIA. SOFIA is jointly operated by the Universities Space Research Association, Inc. (USRA), under NASA contract NAS2-97001, and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901 to the University of Stuttgart. Financial support for this work was provided by NASA through award 002_35 and 04_0048 issued by USRA. ELR and CP acknowledge support from the University of Texas at San Antonio. CP acknowledges support from NSF-0904421 grant. CRA is supported by a Ramon y Cajal Fellowship (RYC-2014-15779). AA-H acknowledges financial support from the Spanish Plan Nacional de Astronomia y Astrofisica under grants AYA2012-3144, which is partly funded by the FEDER program, and AYA2015-64346-C2-1-P. KI acknowledges support from JSPS Grant-in-Aid for Scientific Research (grant number 40756293). NAL is supported by the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., on behalf of the international Gemini partnership of Argentina, Australia, Brazil, Canada, Chile, and the United States of America. IGB acknowledges financial support from the Instituto de Astrofisica de Canarias through Fundacion La Caixa. TD-S acknowledges support from ALMA-CONICYT project 31130005 and FONDECYT 1151239. We would also like to acknowledge the contributions of Miguel Charcos-Llorens. NR 75 TC 2 Z9 2 U1 2 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 NOV 1 PY 2016 VL 462 IS 3 BP 2618 EP 2630 DI 10.1093/mnras/stw1780 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DX8XU UT WOS:000384676000024 ER PT J AU Matsuura, M Sargent, B Swinyard, B Yates, J Royer, P Barlow, MJ Boyer, M Decin, L Khouri, T Meixner, M van Loon, JT Woods, PM AF Matsuura, Mikako Sargent, B. Swinyard, Bruce Yates, Jeremy Royer, P. Barlow, M. J. Boyer, Martha Decin, L. Khouri, Theo Meixner, Margaret van Loon, Jacco Th. Woods, Paul M. TI The mass-loss rates of red supergiants at low metallicity: detection of rotational CO emission from two red supergiants in the Large Magellanic Cloud SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: AGB and post-AGB; circumstellar matter; stars: massive; stars: mass-loss; ISM: molecules; Magellanic Clouds ID ASYMPTOTIC GIANT BRANCH; VY-CANIS-MAJORIS; HERSCHEL-SPIRE INSTRUMENT; EVOLVED STARS; AGB STARS; CIRCUMSTELLAR DUST; RADIATIVE-TRANSFER; SUPERNOVA REMNANT; LINE-PROFILES; EFFECTIVE TEMPERATURE AB Using the PACS and SPIRE spectrometers on-board the Herschel Space Observatory, we obtained spectra of two red supergiants (RSGs) in the Large MagellanicCloud (LMC). Multiple rotational CO emission lines (J = 6-5 to 15-14) and 15 H2O lines were detected from IRAS 05280-6910, and one CO line was detected from WOH G64. This is the first time that CO rotational lines have been detected from evolved stars in the LMC. Their CO line intensities are as strong as those of the Galactic RSG, VY CMa. Modelling the CO lines and the spectral energy distribution results in an estimated mass-loss rate for IRAS 05280-6910 of 3 x 10(-4) M-circle dot yr(-1). The model assumes a gas-to-dust ratio and a CO-to-H-2 abundance ratio is estimated from the Galactic values scaled by the LMC metallicity ([Fe/H] similar to -0.3), i.e. that the CO-to-dust ratio is constant for Galactic and LMC metallicities within the uncertainties of the model. The key factor determining the CO line intensities and the mass-loss rate found to be the stellar luminosity. C1 [Matsuura, Mikako; Swinyard, Bruce; Yates, Jeremy; Barlow, M. J.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Matsuura, Mikako] Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales. [Sargent, B.] Rochester Inst Technol, Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14623 USA. [Sargent, B.] Rochester Inst Technol, Lab Multiwavelength Astrophys, 54 Lomb Mem Dr, Rochester, NY 14623 USA. [Swinyard, Bruce] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England. [Royer, P.; Decin, L.] Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-2401 Leuven, Belgium. [Boyer, Martha] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. [Decin, L.; Khouri, Theo] Univ Amsterdam, Astron Inst Anton Pannekoek, POB 94249, NL-1090 GE Amsterdam, Netherlands. [Khouri, Theo] Chalmers, Dept Radio & Space Sci, Onsala Space Observ, SE-43992 Onsala, Sweden. [Meixner, Margaret] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Meixner, Margaret] Johns Hopkins Univ, Dept Phys & Astron, 366 Bloomberg Ctr 3400 N Charles St, Baltimore, MD 21218 USA. [van Loon, Jacco Th.] Keele Univ, Lennard Jones Labs, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. [Woods, Paul M.] Queens Univ, Sch Math & Phys, Astrophys Res Ctr, Univ Rd, Belfast BT7 1NN, Antrim, North Ireland. RP Matsuura, M (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England.; Matsuura, M (reprint author), Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales.; Sargent, B (reprint author), Rochester Inst Technol, Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14623 USA.; Sargent, B (reprint author), Rochester Inst Technol, Lab Multiwavelength Astrophys, 54 Lomb Mem Dr, Rochester, NY 14623 USA. EM mikako@star.ucl.ac.uk; sargent@stsci.edu RI Barlow, Michael/A-5638-2009 OI Barlow, Michael/0000-0002-3875-1171 FU STFC Ernest Rutherford fellowship; NASA Astrophysics Data Analysis Program [NNX13AD54G]; NASA/JPL grant [NNN12AA01C]; BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain); CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA); ESO [179.B-2003] FX We would like to thank Dr S. Srinivasan for useful inputs on chi2 analysis on DUSTY fitting. MM is supported by the STFC Ernest Rutherford fellowship. M. Meixner and BS acknowledge funding from the NASA Astrophysics Data Analysis Program grant NNX13AD54G and from the NASA/JPL grant NNN12AA01C. 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 and UKSA (UK); and NASA (USA). The VISTA magnitude is based on observations collected at the European Organization for Astronomical Research in the Southern hemisphere under ESO programme(s) 179.B-2003. NR 100 TC 1 Z9 1 U1 2 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 NOV 1 PY 2016 VL 462 IS 3 BP 2995 EP 3005 DI 10.1093/mnras/stw1853 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DX8XU UT WOS:000384676000050 ER PT J AU Chiaro, G Salvetti, D La Mura, G Giroletti, M Thompson, DJ Bastieri, D AF Chiaro, G. Salvetti, D. La Mura, G. Giroletti, M. Thompson, D. J. Bastieri, D. TI Blazar flaring patterns (B-FlaP) classifying blazar candidate of uncertain type in the third Fermi-LAT catalogue by artificial neural networks SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: statistical; galaxies: active; BL Lacertae objects: general; gamma-rays: galaxies; radio continuum: galaxies ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; SKY SURVEY; CLASSIFICATION; ALGORITHMS; ASTRONOMY; RANKING AB The Fermi-Large Area Telescope (LAT) is currently the most important facility for investigating the GeV gamma-ray sky. With Fermi-LAT, more than three thousand gamma-ray sources have been discovered so far. 1144 (similar to 40 per cent) of the sources are active galaxies of the blazar class, and 573 (similar to 20 per cent) are listed as blazar candidate of uncertain type (BCU), or sources without a conclusive classification. We use the empirical cumulative distribution functions and the artificial neural networks for a fast method of screening and classification for BCUs based on data collected at gamma-ray energies only, when rigorous multiwavelength analysis is not available. Based on our method, we classify 342 BCUs as BL Lacs and 154 as flat-spectrum radio quasars, while 77 objects remain uncertain. Moreover, radio analysis and direct observations in ground-based optical observatories are used as counterparts to the statistical classifications to validate the method. This approach is of interest because of the increasing number of unclassified sources in Fermi catalogues and because blazars and in particular their subclass high synchrotron peak objects are the main targets of atmospheric Cherenkov telescopes. C1 [Chiaro, G.; La Mura, G.; Bastieri, D.] Univ Padua, Dip Fis & Astron G Galilei, I-35131 Padua, Italy. [Salvetti, D.] INAF, Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Giroletti, M.] INAF, Inst Radioastron, I-40129 Bologna, Italy. [Thompson, D. J.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. RP Chiaro, G (reprint author), Univ Padua, Dip Fis & Astron G Galilei, I-35131 Padua, Italy.; Salvetti, D (reprint author), INAF, Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. EM chiaro@pd.infn.it; salvetti@iasf-milano.inaf.it FU European Commission [607452] FX Support for science analysis during the operations phase is gratefully acknowledged from the Fermi-LAT collaboration for making the 3FGL results available in such a useful form, the Institute of Space Astrophysics and Cosmic Physics of Milano-Italy (IASF INAF), and the Radioastronomy Institute INAF in Bologna Italy. Part of this work is based on observations collected at Copernico (or/and Schmidt) telescope(s) (Asiago, Italy) of the INAF-Osservatorio Astronomico di Padova. DS acknowledges support through EXTraS, funded from the European Commission Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 607452. NR 30 TC 2 Z9 2 U1 8 U2 8 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 1 PY 2016 VL 462 IS 3 BP 3180 EP 3195 DI 10.1093/mnras/stw1830 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DX8XU UT WOS:000384676000063 ER PT J AU Gull, TR Madura, TI Teodoro, M Clementel, N Corcoran, M Damineli, A Groh, JH Hamaguchi, K Hillier, DJ Moffat, AFJ Richardson, ND Weigelt, G Lindler, D Feggans, K AF Gull, Theodore R. Madura, Thomas I. Teodoro, Mairan Clementel, Nicola Corcoran, Michael Damineli, Augusto Groh, Jose H. Hamaguchi, Kenji Hillier, D. John Moffat, Anthony F. J. Richardson, Noel D. Weigelt, Gerd Lindler, Don Feggans, Keith TI The fossil wind structures of Eta Carinae: changes across one 5.54-yr cycle SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: atmospheres; stars: individual: (Eta Carinae); stars: mass-loss; supergiants; stars: variables: general ID 3D RADIATIVE-TRANSFER; TELESCOPE IMAGING SPECTROGRAPH; 2014.6 SPECTROSCOPIC EVENT; BINARY COLLIDING WINDS; LONG-PERIOD BINARY; HE-II LAMBDA-4686; TRANSFER SIMULATIONS; IONIZATION STRUCTURE; PERIASTRON PASSAGE; ORBITAL PARAMETERS AB Eta Carinae, the closest, active, massive binary containing a highly unstable Luminous Blue Variable, exhibits expanding, compressed wind shells, seen in emission, that are spatially and spectrally resolved by Hubble Space Telescope/Space Telescope Imaging Spectrograph. Starting in 2009 June, these structures were mapped across its 5.54-yr, highly elliptical, binary orbit to follow temporal changes in the light of [Fe III] 4659 angstrom and [Fe II] 4815 angstrom. The emissions trace portions of fossil wind shells, that were formed by wind-wind interactions across each cycle. Over the high-ionization state, dense arcs, photoionized by far-ultraviolet radiation from the hot secondary, are seen in [Fe III]. Other arcs, ionized by mid-ultraviolet radiation from the primary star, are seen in [Fe II]. The [Fe III] structures tend to be interior to [Fe II] structures that trace extensive, less disturbed primary wind. During the brief periastron passage when the secondary plunges deep into the primary's extremely dense wind, on the far side of primary star, high-ionization [Fe III] structures fade and reappear in [Fe II]. Multiple fossil wind structures were traced across the 5.7-yr monitoring interval. The strong similarity of the expanding [Fe II] shells suggests that the wind and photoionization properties of the massive binary have not changed substantially from one orbit to the next over the past several orbital cycles. These observations trace structures that can be used to test 3D hydrodynamical and radiative-transfer models of massive, interacting winds. They also provide a baseline for following future changes in eta Car, especially of its winds and photoionization properties. C1 [Gull, Theodore R.; Madura, Thomas I.; Teodoro, Mairan; Corcoran, Michael; Hamaguchi, Kenji; Lindler, Don] Goddard Space Flight Ctr, Astrophys Sci Div, Code 660, Greenbelt, MD 20771 USA. [Madura, Thomas I.; Teodoro, Mairan; Corcoran, Michael] Univ Space Res Assoc, 7178 Columbia Gateway Dr, Columbia, MD 20146 USA. [Clementel, Nicola] South African Astron Observ, POB 9, ZA-7935 Observatory, South Africa. [Damineli, Augusto] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Rua Matao 1226,Cidade Univ, BR-05508900 Sao Paulo, Brazil. [Groh, Jose H.] Univ Dublin, Trinity Coll Dublin, Sch Phys, Dublin 2, Ireland. [Hamaguchi, Kenji] Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA. [Hillier, D. John] Univ Pittsburgh, Dept Phys & Astron, 3941 OHara St, Pittsburgh, PA 15260 USA. [Hillier, D. John] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr P, 3941 OHara St, Pittsburgh, PA 15260 USA. [Moffat, Anthony F. J.] Univ Montreal, Dept phys, CP 6128 Succ A, Montreal, PQ H3C 3J7, Canada. [Moffat, Anthony F. J.] Univ Montreal, Ctr Rech Astrophys Quebec, CP 6128 Succ A, Montreal, PQ H3C 3J7, Canada. [Richardson, Noel D.] Univ Toledo, Dept Phys & Astron, Ritter Observ, Toledo, OH 43606 USA. [Weigelt, Gerd] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Lindler, Don; Feggans, Keith] Sigma Space Corp, 4600 Forbes Blvd, Lanham, MD 20706 USA. [Feggans, Keith] Goddard Space Flight Ctr, Heliophys Sci Div, Code 670, Greenbelt, MD 20771 USA. RP Gull, TR; Madura, TI (reprint author), Goddard Space Flight Ctr, Astrophys Sci Div, Code 660, Greenbelt, MD 20771 USA.; Madura, TI (reprint author), Univ Space Res Assoc, 7178 Columbia Gateway Dr, Columbia, MD 20146 USA. EM Ted.Gull@nasa.gov; tmadura@udel.edu RI Damineli, Augusto/P-8829-2016; OI Damineli, Augusto/0000-0002-7978-2994; Richardson, Noel/0000-0002-2806-9339 FU Space Telescope Science Institute [12013, 12750, 12508, 13054, 13395]; NASA [NAS5-26555]; NASA; STScI [12013, 12750, 12508, 13054]; FAPESP; NSERC (Canada); FQRNT (Quebec); University of Toledo; Helen Luedtke Brooks endowed Professorship FX This paper was based on observations made with the NASA/ESA HST. Support for Program numbers 12013, 12750, 12508, 13054 and 13395 was provided through grants from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. TIM was supported by the NASA Postdoctoral Fellowship Program. TRG, TIM and MT received support from STScI grants 12013, 12750, 12508 and 13054 through 2015 June. TRG also thanks Gerd Weigelt and the Max Planck Institute for Radioastronomy for delightful stays in the fall of 2015 and spring of 2016. AD acknowledges the continuing financial support from FAPESP. AFJM is grateful for financial support from NSERC (Canada) and FQRNT (Quebec). NDR acknowledges postdoctoral support by the University of Toledo and by the Helen Luedtke Brooks endowed Professorship. We gratefully thank Ms Beth Perriello (STScI) for the extraordinary support scheduling visits at critical intervals that led to the success of this very challenging series of observing programs. We thank anonymous referee for helpful editorial comments. And most importantly, we thank the Eta Car Bunch, a truly innovative group extended across many locations but focused on one massive binary! NR 70 TC 1 Z9 1 U1 3 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 1 PY 2016 VL 462 IS 3 BP 3196 EP 3220 DI 10.1093/mnras/stw1829 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DX8XU UT WOS:000384676000064 ER PT J AU Cassady, K Koppelmans, V Reuter-Lorenz, P De Dios, Y Gadd, N Wood, S Castenada, RR Kofman, I Bloomberg, J Mulavara, A Seidler, R AF Cassady, Kaitlin Koppelmans, Vincent Reuter-Lorenz, Patricia De Dios, Yiri Gadd, Nichole Wood, Scott Castenada, Roy Riascos Kofman, Igor Bloomberg, Jacob Mulavara, Ajitkumar Seidler, Rachael TI Effects of a spaceflight analog environment on brain connectivity and behavior SO NEUROIMAGE LA English DT Article DE Bed rest; Spaceflight analog; Microgravity; Brain function ID RESTING-STATE FMRI; LONG-DURATION SPACEFLIGHT; FUNCTIONAL CONNECTIVITY; MOTOR CORTEX; SPACE-FLIGHT; BED REST; VESTIBULAR SYSTEM; HUMAN CEREBELLUM; SELF-MOTION; MULTIMODAL INTEGRATION AB Sensorimotor functioning is adaptively altered following long-duration spaceflight. The question of whether microgravity affects other central nervous system functions such as brain network organization and its relationship with behavior is largely unknown, but of importance to the health and performance of astronauts both during and post-flight. In the present study, we investigate the effects of prolonged exposure to an established spaceflight analog on resting state brain functional connectivity and its association with behavioral changes in 17 male participants. These bed rest participants remained in bed with their heads tilted down six degrees below their feet for 70 consecutive days. Resting state functional magnetic resonance imaging (rs-fMRI) and behavioral data were obtained at seven time points averaging around: 12 and 8 days prior to bed rest; 7, 50, and 70 days during bed rest; and 8 and 12 days after bed rest. To assess potential confounding effects due to scanning interval or task practice, we also acquired rs-fMRI and behavioral measurements from 14 control participants at four time points. 70 days of head-down tilt (HDT) bed rest resulted in significant changes in the functional connectivity of motor, somatosensory, and vestibular areas of the brain. Moreover, several of these network alterations were significantly associated with changes in sensorimotor and spatial working memory performance, which suggests that neuroplasticity mechanisms may facilitate adaptation to the microgravity analog environment. The findings from this study provide novel insights into the underlying neural mechanisms and operational risks of spaceflight analog-related changes in sensorimotor performance. (C) 2016 Elsevier Inc. All rights reserved. C1 [Cassady, Kaitlin; Reuter-Lorenz, Patricia; Seidler, Rachael] Univ Michigan, Dept Psychol, Ann Arbor, MI 48109 USA. [Koppelmans, Vincent; Seidler, Rachael] Univ Michigan, Sch Kinesiol, Ann Arbor, MI USA. [De Dios, Yiri; Gadd, Nichole; Kofman, Igor] Wyle Sci Technol & Engn Grp, Houston, TX USA. [Wood, Scott] Azusa Pacific Univ, Dept Psychol, Azusa, CA USA. [Castenada, Roy Riascos] Univ Texas Hlth Sci Ctr Houston, Houston, TX 77030 USA. [Bloomberg, Jacob; Mulavara, Ajitkumar] NASA, Johnson Space Ctr, Houston, TX USA. [Mulavara, Ajitkumar] Univ Space Res Assoc, Houston, TX USA. [Seidler, Rachael] Univ Michigan, Grad Program Neurosci, Ann Arbor, MI 48109 USA. RP Seidler, R (reprint author), Univ Michigan, Dept Psychol, Ann Arbor, MI 48109 USA. EM rseidler@umich.edu FU National Space Biomedical Research Institute [NASA NCC 9-58, MA02701, PF04101]; National Aeronautics and Space Administration (NASA) [NNX11AR02G]; NASA Flight Analogs Project; National Institutes of Health; National Center for Advancing Translational Sciences [1UL1RR029876-01] FX This work was supported by grants from the National Space Biomedical Research Institute (NASA NCC 9-58, MA02701, and PF04101), from the National Aeronautics and Space Administration (NASA; NNX11AR02G) and NASA Flight Analogs Project, and the National Institutes of Health, and National Center for Advancing Translational Sciences, 1UL1RR029876-01. NR 85 TC 1 Z9 1 U1 16 U2 16 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1053-8119 EI 1095-9572 J9 NEUROIMAGE JI Neuroimage PD NOV PY 2016 VL 141 BP 18 EP 30 DI 10.1016/j.neuroimage.2016.07.029 PG 13 WC Neurosciences; Neuroimaging; Radiology, Nuclear Medicine & Medical Imaging SC Neurosciences & Neurology; Radiology, Nuclear Medicine & Medical Imaging GA DX0SF UT WOS:000384074500003 PM 27423254 ER PT J AU Pavlov, DA Williams, JG Suvorkin, VV AF Pavlov, Dmitry A. Williams, James G. Suvorkin, Vladimir V. TI Determining parameters of Moon's orbital and rotational motion from LLR observations using GRAIL and IERS-recommended models SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY LA English DT Article DE Lunar laser ranging; Lunar physical libration; Tidal variations of geopotential ID LUNAR; EPM; ERA AB The aim of this work is to combine the model of orbital and rotational motion of the Moon developed for DE430 with up-to-date astronomical, geodynamical, and geo- and selenophysical models. The parameters of the orbit and physical libration are determined in this work from lunar laser ranging (LLR) observations made at different observatories in 1970-2013. Parameters of other models are taken from solutions that were obtained independently from LLR. A new implementation of the DE430 lunar model, including the liquid core equations, was done within the EPM ephemeris. The postfit residuals of LLR observations make evident that the terrestrial models and solutions recommended by the IERS Conventions are compatible with the lunar theory. That includes: EGM2008 gravitational potential with conventional corrections and variations from solid and ocean tides; displacement of stations due to solid and ocean loading tides; and precession-nutation model. Usage of these models in the solution for LLR observations has allowed us to reduce the number of parameters to be fit. The fixed model of tidal variations of the geopotential has resulted in a lesser value of Moon's extra eccentricity rate, as compared to the original DE430 model with two fit parameters. A mixed model of lunar gravitational potential was used, with some coefficients determined from LLR observations, and other taken from the GL660b solution obtained from the GRAIL spacecraft mission. Solutions obtain accurate positions for the ranging stations and the five retroreflectors. Station motion is derived for sites with long data spans. Dissipation is detected at the lunar fluid core-solid mantle boundary demonstrating that a fluid core is present. Tidal dissipation is strong at both Earth and Moon. Consequently, the lunar semimajor axis is expanding by 38.20 mm/yr, the tidal acceleration in mean longitude is , and the eccentricity is increasing by each year. C1 [Pavlov, Dmitry A.; Suvorkin, Vladimir V.] RAS, Inst Appl Astron, Kutuzov Embankment 10, St Petersburg 191187, Russia. [Williams, James G.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Pavlov, DA (reprint author), RAS, Inst Appl Astron, Kutuzov Embankment 10, St Petersburg 191187, Russia. EM dpavlov@ipa.nw.ru NR 40 TC 0 Z9 0 U1 4 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0923-2958 EI 1572-9478 J9 CELEST MECH DYN ASTR JI Celest. Mech. Dyn. Astron. PD NOV PY 2016 VL 126 IS 1-3 SI SI BP 61 EP 88 DI 10.1007/s10569-016-9712-1 PG 28 WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications SC Astronomy & Astrophysics; Mathematics GA DW2SR UT WOS:000383492600003 ER PT J AU Williams, JG Boggs, DH AF Williams, James G. Boggs, Dale H. TI Secular tidal changes in lunar orbit and Earth rotation SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY LA English DT Article DE Tides; Lunar orbit; Earth rotation; Tidal acceleration; Tidal dissipation; Moon; Lunar laser ranging (LLR) ID MOON SYSTEM; PRECESSION; DISSIPATION; EVOLUTION; EPHEMERIS; ACCELERATION; EXPRESSIONS; PARAMETERS; ELP-2000; FRICTION AB Small tidal forces in the Earth-Moon system cause detectable changes in the orbit. Tidal energy dissipation causes secular rates in the lunar mean motion n, semimajor axis a, and eccentricity e. Terrestrial dissipation causes most of the tidal change in n and a, but lunar dissipation decreases eccentricity rate. Terrestrial tidal dissipation also slows the rotation of the Earth and increases obliquity. A tidal acceleration model is used for integration of the lunar orbit. Analysis of lunar laser ranging (LLR) data provides two or three terrestrial and two lunar dissipation parameters. Additional parameters come from geophysical knowledge of terrestrial tides. When those parameters are converted to secular rates for orbit elements, one obtains dn/dt = cent, da/dt = 38.30 +/- 0.08 mm/year, and di/dt = -0.5 +/- 0.1 as/year. Solving for two terrestrial time delays and an extra de/dt from unspecified causes gives /year for the latter; solving for three LLR tidal time delays without the extra de/dt gives a larger phase lag of the N2 tide so that total de/dt = /year. For total dn/dt, there is 1 % difference between geophysical models of average tidal dissipation in oceans and solid Earth and LLR results, and most of that difference comes from diurnal tides. The geophysical model predicts that tidal deceleration of Earth rotation is /cent or 87.5 s/cent for UT1-AT, a 2.395 ms/cent increase in the length of day, and an obliquity rate of 9 as/year. For evolution during past times of slow recession, the eccentricity rate can be negative. C1 [Williams, James G.; Boggs, Dale H.] CALTECH, Jet Prop Lab, MS 238-600, Pasadena, CA 91109 USA. RP Williams, JG (reprint author), CALTECH, Jet Prop Lab, MS 238-600, Pasadena, CA 91109 USA. EM James.G.Williams@jpl.nasa.gov NR 60 TC 0 Z9 0 U1 7 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0923-2958 EI 1572-9478 J9 CELEST MECH DYN ASTR JI Celest. Mech. Dyn. Astron. PD NOV PY 2016 VL 126 IS 1-3 SI SI BP 89 EP 129 DI 10.1007/s10569-016-9702-3 PG 41 WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications SC Astronomy & Astrophysics; Mathematics GA DW2SR UT WOS:000383492600004 ER PT J AU Perez-Sierra, AM Pons, J Santamarta, R Karaman, I Noebe, RD AF Perez-Sierra, A. M. Pons, J. Santamarta, R. Karaman, I. Noebe, R. D. TI Stability of a Ni-rich Ni-Ti-Zr high temperature shape memory alloy upon low temperature aging and thermal cycling SO SCRIPTA MATERIALIA LA English DT Article DE Martensitic phase transformations; Shape memory alloys; Precipitation; Aging; Phase instability ID MICROSTRUCTURE; TRANSFORMATION; BEHAVIOR; PRECIPITATION AB The thermal stability of Ni50.3Ti29.7Zr20 with aging in austenite at 250 degrees C has been studied for three distinctive microstructures obtained after selected thermal treatments: precipitate free and containing two different sizes and densities of H-phase nanoprecipitates. The martensitic transformation is suppressed after 1-3 weeks aging, depending on the initial microstructure, due to a B2 phase instability in the form of short range atomic reordering within the Ti + Zr sublattice, considered to be precursor to the H-phase precipitation. Thermal cycling leads to notable changes in the transformation temperatures, which strongly depends on the starting microstructure. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Perez-Sierra, A. M.; Pons, J.; Santamarta, R.] Univ Illes Balears, Dept Fis, Ctra Valldemossa,Km 7-5, E-07122 Palma De Mallorca, Spain. [Karaman, I.] Texas A&M Univ, Dept Mat Sci & Engn, College Stn, TX 77843 USA. [Noebe, R. D.] NASA, Struct & Mat Div, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Pons, J (reprint author), Univ Illes Balears, Dept Fis, Ctra Valldemossa,Km 7-5, E-07122 Palma De Mallorca, Spain. EM jaume.pons@uib.es FU Spanish MINECO; FEDER [MAT2014-56116-C4-1-R]; FPI grant [BES-2012-053863]; NASA Transformative Aeronautics Concepts Program (TACP), Transformational Tools & Technologies Project; US Air Force Office of Scientific Research [FA9550-15-1-0287]; US National Science Foundation [CMMI 1534534, DMR08-44082]; International Materials Institute for Multifunctional Materials for Energy Conversion (IIMEC) at Texas AM University FX Partial financial support from the Spanish MINECO and FEDER under project MAT2014-56116-C4-1-R and FPI grant BES-2012-053863 are acknowledged. RDN gratefully acknowledges support from the NASA Transformative Aeronautics Concepts Program (TACP), Transformational Tools & Technologies Project. Partial support was also provided by the US Air Force Office of Scientific Research, under Grant no. FA9550-15-1-0287, the US National Science Foundation under Grant no. CMMI 1534534, and under Grant no. DMR08-44082, which supports the International Materials Institute for Multifunctional Materials for Energy Conversion (IIMEC) at Texas A&M University. NR 30 TC 1 Z9 1 U1 17 U2 17 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-6462 J9 SCRIPTA MATER JI Scr. Mater. PD NOV PY 2016 VL 124 BP 47 EP 50 DI 10.1016/j.scriptamat.2016.06.029 PG 4 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA DV9WZ UT WOS:000383294200011 ER PT J AU Wiesner, VL Vempati, UK Bansal, NP AF Wiesner, Valerie L. Vempati, Udaya K. Bansal, Narottam P. TI High temperature viscosity of calcium-magnesium-aluminosilicate glass from synthetic sand SO SCRIPTA MATERIALIA LA English DT Article DE CMAS; Glass; Viscosity ID THERMAL-BARRIER COATINGS; CERAMIC-MATRIX COMPOSITES; CMAS GLASS; MODEL; DELAMINATION; CALCULATE; SYSTEMS AB Viscosity of a calcium-magnesium-aluminosilicate (CMAS) glass, melted from a synthetic sand with composition replicating that of air-breathing turbine engine deposits, was experimentally measured between 1215 degrees C and 1520 degrees C using a rotating spindle viscometer. Chemical composition of the CMAS glass before and after viscosity measurements was nominally 23.3CaO-6AMg0-3.1Al(2)O(3)-62.5SiO(2)-4.1Na(2)O-0.5K(2)O-0.04Fe(2)O(3) (mol.%) as determined using inductively coupled plasma atomic emission spectroscopy. Experimental viscosity values were compared with those estimated from composition-based calculators of Giordano et al., Fluegel and FactSage software. Although none of these models exactly predicted viscosity values, those determined by Fluegel and FactSage models were found to more closely match experimental viscosity of the CMAS glass. Published by Elsevier Ltd. C1 [Wiesner, Valerie L.; Bansal, Narottam P.] NASA, Mat & Struct Div, Glenn Res Ctr, Cleveland, OH 44135 USA. [Vempati, Udaya K.] Owens Brockway Glass Container Inc, Perrysburg, OH 43551 USA. RP Wiesner, VL (reprint author), NASA, Mat & Struct Div, Glenn Res Ctr, Cleveland, OH 44135 USA. EM valerie.l.wiesner@nasa.gov FU NASA FX This research was supported by NASA's Transformative Tools and Technologies (TTT) Project within the Transformative Aeronautics Concept Program (TACP). The authors are grateful to Dr. Daniel Swiler of Owens-Brockway Glass Container Inc. for his coordination of viscosity testing, as well as to Dr. Bryan Harder, Dr. Nathan Jacobson and Dr. Arthur Pelton for helpful discussion. NR 21 TC 1 Z9 1 U1 10 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-6462 J9 SCRIPTA MATER JI Scr. Mater. PD NOV PY 2016 VL 124 BP 189 EP 192 DI 10.1016/j.scriptamat.2016.07.020 PG 4 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA DV9WZ UT WOS:000383294200043 ER PT J AU Lomeli, MJM Wakefield, WW AF Lomeli, Mark J. M. Wakefield, W. Waldo TI Evaluation of a sorting grid bycatch reduction device for the selective flatfish bottom trawl in the US West Coast fishery SO FISHERIES RESEARCH LA English DT Article DE Bycatch reduction device; Selective flatfish trawl; Recapture net; Flatfishes; Roundfishes; Pacific halibut ID SIZE SELECTION; ROCKFISH; MESH; CODENDS; DESIGN; NUMBER; MAINE; GULF AB The U.S. West Coast limited entry groundfish trawl fishery is managed under an individual fishing quota program. For many fishermen targeting flatfishes in this fishery, catches of rockfishes (Sebastes spp.), sablefish (Anoplopoma fimbria), and Pacific halibut (Hippoglossus stenolepis) can be a concern because quota is limited relative to flatfish quotas. Thus, approaches to minimize bycatch of limiting species are important to the economic viability of the fishery. In this study, we examined the size-selection characteristics of a flexible sorting grid bycatch reduction device (designed to retain flatfishes while reducing catches of rockfishes, sablefish, and Pacific halibut) using a recapture net. The mean codend retention of target flatfishes (five species evaluated) ranged from 68.1% to 92.3%. Combined, the mean flatfish retention was 85.6%. Codend catches of shelf rockfishes, slope rockfishes, sablefish, and Pacific halibut were reduced by 80.3%, 64.0%, 97.0%, and 90.3% by weight, respectively. Significant differences in selectivity parameters between flatfishes, rockfishes, sablefish, and Pacific halibut were observed. Over fishing grounds where fishermen need a more selective trawl to harvest flatfishes, the experimental gear tested could provide fishermen a technique to reduce catches of non-target species. (C) 2016 Elsevier B.V. All rights reserved. C1 [Lomeli, Mark J. M.] Pacific States Marine Fisheries Commiss, 2032 SE OSU Dr, Newport, OR 97365 USA. [Wakefield, W. Waldo] NOAA, Fishery Resource Anal & Monitoring Div, Northwest Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2032 SE OSU Dr, Newport, OR 97365 USA. RP Lomeli, MJM (reprint author), Pacific States Marine Fisheries Commiss, 2032 SE OSU Dr, Newport, OR 97365 USA. EM mlomeli@psmfc.org FU NOAA National Marine Fisheries Service Bycatch Reduction Engineering Program [NA13NMF4720276] FX We would like to thank the captain and crew of the F/V Miss Sue, and Matthew Yergey, Toby Mitchell, and Andrew Conger for their at-sea assistance with this research. We also thank the reviewers who contributed to this manuscript. Funding for this study was provided by NOAA National Marine Fisheries Service Bycatch Reduction Engineering Program (Contract No. NA13NMF4720276). NR 23 TC 0 Z9 0 U1 10 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-7836 EI 1872-6763 J9 FISH RES JI Fish Res. PD NOV PY 2016 VL 183 BP 294 EP 303 DI 10.1016/j.fishres.2016.06.011 PG 10 WC Fisheries SC Fisheries GA DV0HW UT WOS:000382599600030 ER PT J AU Dietrich, J Eder, K Thompson, D Buchanan, R Skalski, J McMichael, G Fryer, D Loge, F AF Dietrich, Joseph Eder, Kai Thompson, Donald Buchanan, Rebecca Skalski, John McMichael, Geoffrey Fryer, Derek Loge, Frank TI Survival and transit of in-river and transported yearling Chinook salmon in the lower Columbia River and estuary SO FISHERIES RESEARCH LA English DT Article DE Columbia River estuary; Salmon; Acoustic telemetry; Barge transportation; Survival ID INTEGRATED TRANSPONDER TAGS; JUVENILE SALMONIDS; SNAKE RIVER; DELAYED MORTALITY; SEAWARD MIGRATION; HYDROPOWER SYSTEM; AVIAN PREDATION; PLUME USA; STEELHEAD; RATES AB The lower Columbia River and estuary (LRE) is a critically important environment for outmigrating salmonids, yet uncertainties remain about the survival and behavior of barged and in-river migrating fish. Although studies have used telemetry to monitor Chinook salmon movement and survival through the LRE, comparisons between outmigration years are confounded by differences in tag technologies, array locations, and experimental designs. In the present study, multiple releases of barged and in-river Snake River spring/summer Chinook salmon were implanted with acoustic tags and monitored at multiple locations between Lower Granite Dam on the Snake River (695 km from the mouth of the Columbia River) to within 3 km of the Pacific Ocean. LRE survival estimates and transit rates of barged fish significantly varied throughout the outmigration season. The transit rates of in-river fish also varied, but without a corresponding seasonal difference in LRE survival estimates. Early release groups of barged salmon were slower and had lower survival in the LRE than in-river salmon. Estuary arrival timing and the magnitude of transit rates may contribute to significant differences in LRE mortality between in-river and barged juvenile salmon. Survival in the Lower River reaches was stable and exceeded 0.90 for both barged and in-river fish, while survival decreased markedly in the Estuary. Differential distributions of arrival to the LRE, transit rates, and survival suggest that the outmigration experience is not homogenous for barged and in-river yearling Snake River Chinook salmon, and that previous outmigration experience of threatened and endangered salmon should be considered in future management decisions and recovery plans. (C) 2016 Elsevier B.V. All rights reserved. C1 [Dietrich, Joseph] Natl Marine Fisheries Serv, Environm & Fisheries Sci Div, Northwest Fisheries Sci Ctr, NOAA, 2032 SE OSU Dr, Newport, OR 97365 USA. [Eder, Kai; Thompson, Donald; Loge, Frank] Univ Calif Davis, Dept Civil & Environm Engn, One Shields Ave, Davis, CA 95616 USA. [Buchanan, Rebecca; Skalski, John] Univ Washington, Sch Aquat & Fishery Sci, 1325 Fourth Ave,Suite 1820, Seattle, WA 98101 USA. [McMichael, Geoffrey] Pacific Northwest Natl Lab, Ecol Grp, POB 999,MSK6-85, Richland, WA 99352 USA. [Fryer, Derek] US Army Corps Engineers, 201 N 3rd Ave, Walla Walla, WA 99362 USA. RP Loge, F (reprint author), Univ Calif Davis, Dept Civil & Environm Engn, One Shields Ave, Davis, CA 95616 USA. EM kai.eder@csus.edu; geoff@mainstemfish.com; fjloge@ucdavis.edu OI Skalski, John/0000-0002-7070-2505 FU US Army Corps of Engineers (USACE); Walla Walla District [W912EF-08-D-0007] FX This project was funded by the US Army Corps of Engineers (USACE), Walla Walla District, Contract Number W912EF-08-D-0007, Delivery Order 1. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the supporting agency. Surgery training, tagging assistance at Lower Granite Dam, collection and analysis of JSATS data, and reporting assistance were provided by Katherine Deters, Jessica Carter, and a host of others from the Pacific Northwest National Laboratory. Programming of the PIT-tag separation-by-code functions was provided by Dave Marvin, Pacific States Marine Fisheries Commission. Assistance in fish collection and facilities were provided, in part, by Kent Blevins (USACE), Mike Halter (USACE), Doug Marsh and Neil Paasch (National Oceanic and Atmospheric Administration [NOAA]), Fred Mensik and Sean Rapp (Smolt Monitoring Program) at Lower Granite Dam. Finally, thank you to Andrew Holguin (U.C. Davis) for generating the GIS maps of our study areas. NR 57 TC 0 Z9 0 U1 34 U2 35 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-7836 EI 1872-6763 J9 FISH RES JI Fish Res. PD NOV PY 2016 VL 183 BP 435 EP 446 DI 10.1016/j.fishres.2016.07.005 PG 12 WC Fisheries SC Fisheries GA DV0HW UT WOS:000382599600045 ER PT J AU Dichmont, CM Deng, RA Punt, AE Brodziak, J Chang, YJ Cope, JM Ianelli, JN Legault, CM Methot, RD Porch, CE Prager, MH Shertzer, KW AF Dichmont, Catherine M. Deng, Roy A. Punt, Andre E. Brodziak, Jon Chang, Yi-Jay Cope, Jason M. Ianelli, James N. Legault, Christopher M. Methot, Richard D., Jr. Porch, Clay E. Prager, Michael H. Shertzer, Kyle W. TI A review of stock assessment packages in the United States SO FISHERIES RESEARCH LA English DT Review DE Fishing mortality; Reference points; Stock assessment; Population dynamics ID POPULATION-DYNAMICS MODELS; SURPLUS-PRODUCTION-MODEL; DATA-LIMITED SITUATIONS; AT-AGE DATA; STRUCTURED MODELS; FISHING MORTALITY; FISHERIES DATA; SIMULATED DATA; SOUTH-AFRICA; MULTIFAN-CL AB Stock assessments provide scientific advice in support of fisheries decision making. Ideally, assessments involve fitting population dynamics models to fishery and monitoring data to provide estimates of time trajectories of biomass and fishing mortality in absolute terms and relative to biological reference points such as B-MSY and F-MSY, along with measures of uncertainty. Some stock assessments are conducted using software developed for a specific stock or group of stocks. However, increasingly, stock assessments are being conducted using packages developed for application to several taxa and across multiple regions. We review the range of packages used to conduct assessments of fish and invertebrate stocks in the United States because these assessments tend to have common goals, and need to provide similar outputs for decision making. Sixteen packages are considered, five based on surplus production models, one based on a delay-difference model, and the remainder based on age-structured models. Most of the packages are freely available for use by analysts in the US and around the world, have been evaluated using simulations, and can form the basis for forecasts. The packages differ in their ease of use and the types of data inputs they can use. This paper highlights the benefits of stock assessment packages in terms of allowing analysts to explore many assessment configurations and facilitating the peer-review of assessments. It also highlights the disadvantages associated with the use of packages for conducting assessments. Packages with the most options and greatest flexibility are the most difficult to use, and see the greatest development of auxiliary tools to facilitate their use. Crown Copyright (C) 2016 Published by Elsevier B.V. All rights reserved. C1 [Dichmont, Catherine M.; Deng, Roy A.] CSIRO Oceans & Atmosphere Flagship, Ecosci Precinct, Dutton Park, Qld 4750, Australia. [Punt, Andre E.] CSIRO Oceans & Atmosphere Flagship, Hobart, Tas 7001, Australia. [Punt, Andre E.] Univ Washington, Sch Aquat & Fishery Sci, Box 355020, Seattle, WA 98195 USA. [Brodziak, Jon] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96818 USA. [Chang, Yi-Jay] Univ Hawaii, NOAA Fisheries, Joint Inst Marine & Atmospher Res, Honolulu, HI USA. [Cope, Jason M.; Methot, Richard D., Jr.] Natl Marine Fisheries Serv, Northwest Fisheries Sci Ctr, 2725 Montlake Blvd East, Seattle, WA 98112 USA. [Ianelli, James N.] Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, 7600 Sand Point Way NE, Seattle, WA 98115 USA. [Legault, Christopher M.] Natl Marine Fisheries Serv, Northeast Fisheries Sci Ctr, 166 Water St, Woods Hole, MA 02543 USA. [Porch, Clay E.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, 75 Virginia Beach Dr, Miami, FL 33149 USA. [Prager, Michael H.] Prager Consulting, 2124 SE Grant St, Portland, OR 97214 USA. [Shertzer, Kyle W.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, 101 Pivers Isl Rd, Beaufort, NC 28516 USA. RP Punt, AE (reprint author), CSIRO Oceans & Atmosphere, Hobart, Tas 7001, Australia. EM aepunt@uw.edu OI Chang, Yi-Jay/0000-0002-7472-4672 FU Joint Institute for the Study of the Atmosphere and Ocean (JISAO) under NOAA Cooperative agreement [NA100AR4320148, 2016-01-31]; Fisheries Research and Development Corporation; CSIRO FX The authors would like to thank Nick Davies, Beth Babcock (U. Miami), Murdoch McAllister (UBC), Paul Nitschke (NOAA, NEFSC), Erik Williams (NOAA, SEFSC), and E.J. Dick (NOAA, SWFSC) for their input to the survey undertaken to develop this paper. Melissa Haltuch (NOAA, NWFSC) and Mike Wilberg (University of Maryland) are thanked for comments on an earlier version of this paper. CMD, RAD, and AEP were funded by the Fisheries Research and Development Corporation and CSIRO. Paul Crone (SWFSC) and Richard McGarvey (SARDI) are thanked for their comments on an earlier version of the paper. AEP was partially funded by the Joint Institute for the Study of the Atmosphere and Ocean (JISAO) under NOAA Cooperative agreement No. NA100AR4320148, Contribution No. 2016-01-31. NR 134 TC 2 Z9 2 U1 17 U2 17 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-7836 EI 1872-6763 J9 FISH RES JI Fish Res. PD NOV PY 2016 VL 183 BP 447 EP 460 DI 10.1016/j.fishres.2016.07.001 PG 14 WC Fisheries SC Fisheries GA DV0HW UT WOS:000382599600046 ER PT J AU Frankland, VL James, AD Sanchez, JDC Mangan, TP Willacy, K Poppe, AR Plane, JMC AF Frankland, Victoria L. James, Alexander D. Sanchez, Juan Diego Carrillo Mangan, Thomas P. Willacy, Karen Poppe, Andrew R. Plane, John M. C. TI Uptake of acetylene on cosmic dust and production of benzene in Titan's atmosphere SO ICARUS LA English DT Article DE Titan, atmosphere; Kuiper belt; Interplanetary dust ID TRANSFORM MASS-SPECTROMETRY; PHOTOCHEMICAL MODEL; HAZE FORMATION; COUPLING PHOTOCHEMISTRY; LOW-TEMPERATURE; GRAIN SURFACES; SOLAR-SYSTEM; PD(111); KINETICS; CYCLOTRIMERIZATION AB A low-temperature flow tube and ultra-high vacuum apparatus were used to explore the uptake and heterogeneous chemistry of acetylene (C2H2) on cosmic dust analogues over the temperature range encountered in Titan's atmosphere below 600 km. The uptake coefficient, gamma, was measured at 181 K to be (1.6 +/- 0.4) x 10(-4), (1.9 +/- 0.4) x 10(-4) and (1.5 +/- 0.4) x 10(-4) for the uptake of C2H2 on Mg2SiO4, MgFeSiO4 and Fe2SiO4, respectively, indicating that gamma is independent of Mg or Fe active sites. The uptake of C2H2 was also measured on SiO2 and SiC as analogues for meteoric smoke particles in Titan's atmosphere, but was found to be below the detection limit (gamma < 6 x 10(-8) and <4 x 10(-7), respectively). The rate of cyclo-trimerization of C2H2 to C6H6 was found to be 2.6 x 10(-5) exp(-741/7) s(-1), with an uncertainty ranging from +/- 27 % at 115 K to +/- 49 % at 181 K. A chemical ablation model was used to show that the bulk of cosmic dust particles (radius 0.02-10 mu m) entering Titan's atmosphere do not ablate (< 1% mass loss through sputtering), thereby providing a significant surface for heterogeneous chemistry. A 10 model of dust sedimentation shows that the production of C6H6 via uptake of C2H2 on cosmic dust, followed by cyclo-trimerization and desorption, is probably competitive with gas-phase production of C6H6 between 80 and 120 km. (C) 2016 Elsevier Inc. All rights reserved. C1 [Frankland, Victoria L.; James, Alexander D.; Sanchez, Juan Diego Carrillo; Mangan, Thomas P.; Plane, John M. C.] Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England. [Willacy, Karen] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Poppe, Andrew R.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Plane, JMC (reprint author), Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England. EM j.m.c.plane@leeds.ac.uk RI Plane, John/C-7444-2015 OI Plane, John/0000-0003-3648-6893 FU Leverhulme Trust [F/00 122/BB - PETALS]; European Research Council [291332 - CODITA]; Science and Technology Facilities Council [ST/L000628/1]; NASA Astrobiology Institute, Titan as a Prebiotic Chemical System; NASA Planetary Atmospheres program [NNX13AG55G] FX This work was supported by funding from the Leverhulme Trust (grant F/00 122/BB - PETALS), the European Research Council (project number 291332 - CODITA) and the Science and Technology Facilities Council (grant ST/L000628/1). The authors acknowledge Rebecca Mills for her work on calibrating the C2H2 beam flux for the UHV work, and thank Dr Wuhu Feng (National Centre for Atmospheric Science and University of Leeds) for supplying output from the Caltech/JPL 1D Titan model. K.W.'s work was carried out at the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration and was supported by funding from the NASA Astrobiology Institute, Titan as a Prebiotic Chemical System. A.R.P. was supported by the NASA Planetary Atmospheres program, grant #NNX13AG55G. NR 79 TC 0 Z9 0 U1 18 U2 19 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD NOV 1 PY 2016 VL 278 BP 88 EP 99 DI 10.1016/j.icarus.2016.06.007 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DT1ML UT WOS:000381246700008 ER PT J AU Guzewich, SD Toigo, AD Waugh, DW AF Guzewich, Scott D. Toigo, A. D. Waugh, D. W. TI The effect of dust on the martian polar vortices SO ICARUS LA English DT Article DE Mars, atmosphere; Atmospheres, dynamics; Meteorology ID GENERAL-CIRCULATION MODEL; ZONAL-MEAN CIRCULATION; MIDDLE-ATMOSPHERE; POTENTIAL VORTICITY; MARS; SIMULATION; STORMS; DYNAMICS; ORIGIN; CLOUDS AB The influence of atmospheric dust on the dynamics and stability of the martian polar vortices is examined, through analysis of Mars Climate Sounder observations and MarsWRF general circulation model simulations. We show that regional and global dust storms produce "transient vortex warming" events that partially or fully disrupt the northern winter polar vortex for brief periods. Increased atmospheric dust heating alters the Hadley circulation and shifts the downwelling branch of the circulation poleward, leading to a disruption of the polar vortex for a period of days to weeks. Through our simulations, we find this effect is dependent on the atmospheric heating rate, which can be changed by increasing the amount of dust in the atmosphere or by altering the dust optical properties (e.g., single scattering albedo). Despite this, our simulations show that some level of atmospheric dust is necessary to produce a distinct northern hemisphere winter polar vortex. (C) 2016 Elsevier Inc. All rights reserved. C1 [Guzewich, Scott D.] NASA GSFC, CRESST, Greenbelt, MD 20771 USA. [Guzewich, Scott D.] NASA GSFC, Planetary Syst Lab, Greenbelt, MD 20771 USA. [Guzewich, Scott D.] Univ Space Res Assoc, 7178 Columbia Gateway Dr, Columbia, MD 21046 USA. [Toigo, A. D.] Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. [Waugh, D. W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, 301 Olin Hall,3400 N Charles St, Baltimore, MD 21218 USA. RP Guzewich, SD (reprint author), NASA GSFC, CRESST, Greenbelt, MD 20771 USA.; Guzewich, SD (reprint author), NASA GSFC, Planetary Syst Lab, Greenbelt, MD 20771 USA. EM sguzewich@gmail.com OI Guzewich, Scott/0000-0003-1149-7385 FU NASA Mars Fundamental Research Program [NNX14AG53G] FX The authors gratefully recognize funding from the NASA Mars Fundamental Research Program through Grant NNX14AG53G and thank Daniel Mitchell and Luca Montabone for sharing code for calculating Ertel's Potential Vorticity. We thank two anonymous reviewers for their helpful comments, which have improved this manuscript. NR 45 TC 2 Z9 2 U1 12 U2 12 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD NOV 1 PY 2016 VL 278 BP 100 EP 118 DI 10.1016/j.icarus.2016.06.009 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DT1ML UT WOS:000381246700009 ER PT J AU Fletcher, LN Greathouse, TK Orton, GS Sinclair, JA Giles, RS Irwin, PGJ Encrenaz, T AF Fletcher, Leigh N. Greathouse, T. K. Orton, G. S. Sinclair, J. A. Giles, R. S. Irwin, P. G. J. Encrenaz, T. TI Mid-infrared mapping of Jupiter's temperatures, aerosol opacity and chemical distributions with IRTF/TEXES SO ICARUS LA English DT Article DE Jupiter; Atmospheres; composition; Atmospheres; dynamics ID GREAT-RED-SPOT; ROTOTRANSLATIONAL ABSORPTION-SPECTRA; POTENTIAL-VORTICITY DYNAMICS; PARA-HYDROGEN FRACTION; NORTH EQUATORIAL BELT; 5-MICRON HOT-SPOTS; PROBE ENTRY SITE; CLOUD STRUCTURE; ATMOSPHERIC COMPOSITION; THERMAL STRUCTURE AB Global maps of Jupiter's atmospheric temperatures, gaseous composition and aerosol opacity are derived from a programme of 5-20 mu m mid-infrared spectroscopic observations using the Texas Echelon Cross Echelle Spectrograph (TEXES) on NASA's Infrared Telescope Facility (IRTF). Image cubes from December 2014 in eight spectral channels, with spectral resolutions of R similar to'2000-12, 000 and spatial resolutions of 2-4 degrees latitude, are inverted to generate 3D maps of tropospheric and stratospheric temperatures, 2D maps of upper tropospheric aerosols, phosphine and ammonia, and 2D maps of stratospheric ethane and acetylene. The results are compared to a re-analysis of Cassini Composite Infrared Spectrometer (CIRS) observations acquired during Cassini's closest approach to Jupiter in December 2000, demonstrating that this new archive of ground-based mapping spectroscopy can match and surpass the quality of previous investigations, and will permit future studies of Jupiter's evolving atmosphere. The visibility of cool zones and warm belts varies from channel to channel, suggesting complex vertical variations from the radiatively-controlled upper troposphere to the convective mid -troposphere. We identify mid-infrared signatures of Jupiter's 5-mu m hotspots via simultaneous M, N and Q-band observations, which are interpreted as temperature and ammonia variations in the northern Equatorial Zone and on the edge of the North Equatorial Belt (NEB). Equatorial plumes enriched in NH3 gas are located south-east of NH3-desiccated 'hotspots' on the edge of the NEB. Comparison of the hotspot locations in several channels across the 5-20 mu m range indicate that these anomalous regions tilt westward with altitude. Aerosols and PH3 are both enriched at the equator but are not co-located with the NH3 plumes. The equatorial temperature minimum and PH3/aerosol maxima have varied in amplitude over time, possibly as a result of periodic equatorial brightenings and the fresh updrafts of disequilibrium material. Temperate mid-latitudes display a correlation between mid-IR aerosol opacity and the white albedo features in visible light (i.e., zones). We find hemispheric asymmetries in the distribution of tropospheric PH3, stratospheric hydrocarbons and the 2D wind field (estimated via the thermal-wind equation) that suggest a differing efficiency of mechanical forcing (e.g., vertical mixing and wave propagation) between the two hemispheres that we argue is driven by dynamics rather than Jupiter's small seasonal cycle. Jupiter's stratosphere is notably warmer at northern mid-latitudes than in the south in both 2000 and 2014, although the latter can be largely attributed to strong thermal wave activity near 30 degrees N that dominates the 2014 stratospheric maps and may be responsible for elevated C2H2 in the northern hemisphere. A vertically-variable pattern of temperature and wind shear minima and maxima associated with Jupiter's Quasi Quadrennial Oscillation (QQO) is observed at the equator in both datasets, although the contrasts were more subdued in 2014. Large-scale equator-to pole gradients in ethane and acetylene are superimposed on top of the mid-latitude mechanically-driven maxima, with C2H2 decreasing from equator to pole and C2H6 showing a polar enhancement, consistent with a radiatively-controlled circulation from low to high latitudes. Cold polar vortices beyond 60 latitude can be identified in the upper tropospheric and lower stratospheric temperature maps, suggesting enhanced radiative cooling from polar aerosols. Finally, compositional mapping of the Great Red Spot confirms the local enhancements in PH3 and aerosols, the north-south asymmetry in NH3 gas and the presence of a warm southern periphery that have been noted by previous authors. (C) 2016 The Authors. Published by Elsevier Inc. C1 [Fletcher, Leigh N.] Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. [Greathouse, T. K.] Southwest Res Inst, Div 15,6220 Culebra Rd, San Antonio, TX 78228 USA. [Orton, G. S.; Sinclair, J. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Giles, R. S.; Irwin, P. G. J.] Univ Oxford, Dept Phys, Clarendon Lab, Atmospher Ocean & Planetary Phys, Parks Rd, Oxford OX1 3PU, England. [Encrenaz, T.] Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris, F-92195 Meudon, France. RP Fletcher, LN (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. EM leigh.fletcher@leicester.ac.uk OI Fletcher, Leigh/0000-0001-5834-9588; Giles, Rohini/0000-0002-7665-6562 FU Royal Society Research Fellowship at the University of Leicester; Science and Technology Facilities Council (STFC) FX Fletcher was supported by a Royal Society Research Fellowship at the University of Leicester. Fletcher, Greathouse, Orton and Giles were visiting astronomers at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. We recognise the significant cultural role of Mauna Kea within the indigenous Hawaiian community, and we appreciate the opportunity to conduct our Jupiter observations from this revered site. The UK authors acknowledge the support of the Science and Technology Facilities Council (STFC). A portion of this work was performed by Orton and Sinclair at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. We thank Marco Vedovato of the Italian Amateur Astronomers Union for compiling the visible light images from I. Sharp, F. Fortunato, H. Einaga and T. Horiuchi to coincide with our TEXES programme. We are extremely grateful to John Lacy and Matt Richter for their assistance in understanding the performance of the TEXES instrument and the uncertainties related to calibration. We thank S. Guerlet, J. Moses, T. Fouchet and V. Hue for helpful comments and suggestions during this work, and Gordy Bjoraker and one anonymous reviewer for their critique of this manuscript. This research used the ALICE High Performance Computing Facility at the University of Leicester. NR 133 TC 1 Z9 1 U1 11 U2 11 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD NOV 1 PY 2016 VL 278 BP 128 EP 161 DI 10.1016/j.icarus.2016.06.008 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DT1ML UT WOS:000381246700011 ER PT J AU Davies, AG Keszthelyi, LP McEwen, AS AF Davies, Ashley Gerard Keszthelyi, Laszlo P. McEwen, Alfred S. TI Determination of eruption temperature of Io's lavas using lava tube skylights SO ICARUS LA English DT Article DE Io; Volcanism; Jupiter, satellites; Satellites, composition ID JUPITERS MOON IO; THERMAL EMISSION; HEAT-FLOW; TIDAL DISSIPATION; VOLCANIC ACTIVITY; GREENSTONE-BELT; GALILEO; SPECTROMETER; MODELS; PILLAN AB Determining the eruption temperature of Io's dominant silicate lavas would constrain Io's present interior state and composition. We have examined how eruption temperature can be estimated at lava tube skylights through synthesis of thermal emission from the incandescent lava flowing within the lava tube. Lava tube skylights should be present along Io's long-lived lava flow fields, and are attractive targets because of their temporal stability and the narrow range of near -eruption temperatures revealed through them. We conclude that these skylights are suitable and desirable targets (perhaps the very best targets) for the purposes of constraining eruption temperature, with a 0.9:0.7-mu m radiant flux ratio <= 63 being diagnostic of ultramafic lava temperatures. Because the target skylights may be small - perhaps only a few m or 10 s of m across - such observations will require a future Io-dedicated mission that will obtain high spatial resolution (<100 mipixel), unsaturated observations of Io's surface at multiple wavelengths in the visible and near-infrared, ideally at night. In contrast to observations of lava fountains or roiling lava lakes, where accurate determination of surface temperature distribution requires simultaneous or near simultaneous (<0.1 s) observations at different wavelengths, skylight thermal emission data are superior for the purposes of temperature derivation, as emission is stable on much longer time scales (minutes, or longer), so long as viewing geometry does not greatly change during that time. (C) 2016 Elsevier Inc. All rights reserved. C1 [Davies, Ashley Gerard] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Keszthelyi, Laszlo P.] USGS Astrogeol Sci Ctr, Flagstaff, AZ USA. [McEwen, Alfred S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ USA. RP Davies, AG (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Ashley.Davies@jpl.nasa.gov FU NASA Outer Planets Research Program [NNN13D466T] FX This work was carried out in part at the Jet Propulsion Laboratory - California Institute of Technology, under contract to the National Aeronautics and Space Administration. We thank Alison Canning Davies and Greg Vaughan for their pre-submission reviews of the manuscript. We also thank David Williams of Arizona State University and an anonymous reviewer for their reviews of the submitted manuscript. AGD is supported by grant NNN13D466T from the NASA Outer Planets Research Program. NR 58 TC 0 Z9 0 U1 9 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD NOV 1 PY 2016 VL 278 BP 266 EP 278 DI 10.1016/j.icarus.2016.06.003 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DT1ML UT WOS:000381246700019 ER PT J AU Holdeman, JD AF Holdeman, James D. TI Re: Penetration behavior of opposed rows of staggered secondary air jets depending on jet penetration coefficient and momentum flux ratio SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER LA English DT Article DE Solid waste incinerator; Staggered jets; Momentum-flux ratio; Jet penetration coefficient; Jets in crossflow; Gas turbine combustors; Dilution jets; Empirical model; Correlations; Conserved scalar; Temperature distribution; JIC ID CROSS-FLOW; SPREADSHEET CALCULATIONS AB The purpose of this article is to explain why the extension of the previously published C = (5/H-o)sqrt(J) scaling for opposed rows of staggered jets wasn't directly successful in the study by Choi et al. (2016). It is not surprising that staggered jets from opposite sides do not pass each other at the expected C value, because H-o/D and sqrt(J) are much larger than the maximum in previous studies. These, and large x/D's, tend to suggest development of 2-dimensional flow. Although there are distinct optima for opposed rows of in-line jets, single-side injection, and opposed rows of staggered jets based on C, opposed rows of staggered jets provide as good or better mixing performance, at any C value, than opposed rows of in-line jets or jets from single-side injection. (C) 2016 The Author. Published by Elsevier Ltd. This is an open access article under the CC BY-NC-ND license (http://creativecommons.orgflicensesiby-nc-nd/4.0/). C1 [Holdeman, James D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Holdeman, James D.] 5228 Meadow Moss Ln, N Ridgeville, OH 44039 USA. RP Holdeman, JD (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.; Holdeman, JD (reprint author), 5228 Meadow Moss Ln, N Ridgeville, OH 44039 USA. EM jjdholdeman@aol.com FU Combustion Branch at the NASA Glenn Research Center FX The author would particularly like to thank Mr. Richard E. Walker (Aerojet Liquid Rocket Company, ret.) and Dr. Ram Srinivasan (then of Garrett Turbine Engine Company) for their early contributions to the NASA JIC empirical model. The author would also like to thank Professor William E. Lear, Jr. of the University of Florida for suggesting that the original computer code could be converted to an Excel (R) spreadsheet and for directing its development, and to Mr. James R. Clisset who did the initial Excel programming as an undergraduate student at UF. Also, Messrs. Timothy D. Smith and Jeffrey P. Moder of the NASA Glenn Research Center contributed significantly to development and demonstration of the spreadsheet. Finally, the author would like to thank Dr. Clarence T. Chang of the Combustion Branch at the NASA Glenn Research Center for providing funding for the Open Access publication and color printing of this paper. NR 10 TC 0 Z9 0 U1 2 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0017-9310 EI 1879-2189 J9 INT J HEAT MASS TRAN JI Int. J. Heat Mass Transf. PD NOV PY 2016 VL 102 BP 435 EP 444 DI 10.1016/j.ijheatmasstransfer.2016.06.038 PG 10 WC Thermodynamics; Engineering, Mechanical; Mechanics SC Thermodynamics; Engineering; Mechanics GA DU7QS UT WOS:000382410300043 ER PT J AU Johnson, M Gorospe, G Landry, J Schuster, A AF Johnson, Michael Gorospe, George Landry, Jonathan Schuster, Anja TI Review of mitigation technologies for terrestrial power grids against space weather effects SO INTERNATIONAL JOURNAL OF ELECTRICAL POWER & ENERGY SYSTEMS LA English DT Review DE Space weather; Gemagnetically induced currents; Power grids; Transformers; Mitigation strategies ID SYSTEMS; TRANSMISSION; SCENARIOS; EVENT AB This paper discusses the earth-based effects of solar weather and presents a review of mitigation and protection techniques for the terrestrial power grid infrastructure. Solar events such as Coronal Mass Ejections (CMEs), solar flares and associated recombination events are one of the driving factors in space weather and the solar wind intensity. Even though it is located at such a great distance from our nearest star, the Earth and its associated satellites are still directly affected by variances in these space weather phenomena. On the surface of the planet, nowhere is this more immediate and important than with the terrestrial power grid, which is responsible for delivering electrical power to much of the planets population. Large-scale variations in solar activity can result in potentially devastating effects on the terrestrial power grid and the associated infrastructure. A team project was undertaken at the International Space University (ISU) Space Studies Program (SSP) 2013 to categorize and mitigate the risks involved in such a solar event. As part of this research, which included risk assessment for satellite, spacecraft and terrestrial resources, this paper presents a review of the terrestrial power grid and its inherent susceptibility to such phenomena. Mitigation schemes, techniques and approaches ranging from adaption of the existing power grid to alternative systems are considered in this paper, which allow for continued electrical power delivery and transmission, even in the face of such detrimental space weather effects. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Johnson, Michael] Univ Limerick, Limerick, Ireland. [Gorospe, George] NASA, Ames Res Ctr, San Jose, CA USA. [Landry, Jonathan] ETS, Montreal, PQ, Canada. [Schuster, Anja] Tech Univ Darmstadt, Darmstadt, Germany. RP Johnson, M (reprint author), Univ Limerick, Limerick, Ireland. EM michael.johnson@ul.ie FU International Space University; Johns Hopkins University Applied Physics Laboratory FX The authors would like to acknowledge the work of all team members in Team Project SolarMax at the 2013 International Space University Space Studies Program 2013 for their contributions towards the team project and this work. Team SolarMAX was composed of Ang Xu, Anja Schuster, Arnaud Sternchass, Ashley Dale, Bai Baocun, Beatrice Hainaut, Caroline Smoczarski, Chandrakanta Kumar, Charles Laing, Chunhui Wang, Eric Hall, Gabriele Librandi, George Gorospe, Gongyou Wu, Hester Vermeiden, Hongbin Shi, Jaime Babb, Jonathan Landry, Julio Ceasar Salazar Ospina, Kun Li, Leo Teeney, Mark Burke, Matt Palmer, Meifang Li, Melissa Battler, Michael Johnson, Morten Salvesen, Nicolas Thiry, Paul Tarantino, Remco Timmermans, Richard Passmore, Suquan Ding, Timo Nikkanen, Xianxu Yuan, Yevgeny Tsodikovich, Yuta Nakajima. Team SolarMAX would also like to thank David Haslam, Dr. Rogan Shimmin and Dr. Pete S. Worden for their leadership and guidance, and would like to acknowledge both the International Space University and Johns Hopkins University Applied Physics Laboratory for supporting this project. NR 35 TC 0 Z9 0 U1 22 U2 22 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0142-0615 EI 1879-3517 J9 INT J ELEC POWER JI Int. J. Electr. Power Energy Syst. PD NOV PY 2016 VL 82 BP 382 EP 391 DI 10.1016/j.ijepes.2016.02.049 PG 10 WC Engineering, Electrical & Electronic SC Engineering GA DP4ET UT WOS:000378449700039 ER PT J AU Kikuchi, N Kurashima, S Ishida, M Iizuka, R Maeda, Y Hayashi, T Okajima, T Matsumoto, H Mitsuishi, I Saji, S Sato, T Tachibana, S Mori, H Christensen, F Brejnholt, N Nitta, K Uruga, T AF Kikuchi, Naomichi Kurashima, Sho Ishida, Manabu Iizuka, Ryo Maeda, Yoshitomo Hayashi, Takayuki Okajima, Takashi Matsumoto, Hironori Mitsuishi, Ikuyuki Saji, Shigetaka Sato, Toshiki Tachibana, Sasagu Mori, Hideyuki Christensen, Finn Brejnholt, Nicolai Nitta, Kiyofumi Uruga, Tomoya TI Atomic scattering factor of the ASTRO-H (Hitomi) SXT reflector around the gold's L edges SO OPTICS EXPRESS LA English DT Article AB The atomic scattering factor in the energy range of 11.2-15.4 keV for the ASTROH Soft X-ray Telescope (SXT) is reported. The large effective area of the SXT makes use of photon spectra above 10 keV viable, unlike most other X-ray satellites with total-reflection mirror optics. Presence of gold's L-edges in the energy band is a major issue, as it complicates the function of the effective area. In order to model the area, the reflectivity measurements in the 11.2-15.4 keV band with the energy pitch of 0.4-0.7 eV were made in the synchrotron beamline Spring-8 BL01B1. We obtained atomic scattering factors f1 and f2 by the curve fitting to the reflectivities of our witness sample. The edges associated with the L-I, II, and III transitions are identified, of which the depths are found to be roughly 60% shallower than those expected from the Henke's atomic scattering factor. (C) 2016 Optical Society of America C1 [Kikuchi, Naomichi; Kurashima, Sho; Ishida, Manabu; Iizuka, Ryo; Maeda, Yoshitomo; Sato, Toshiki] Tokyo Metropolitan Univ, 1-1 Minami Osawa, Hachioji, Tokyo 1920397, Japan. [Kikuchi, Naomichi; Kurashima, Sho; Ishida, Manabu; Sato, Toshiki] Japan Aerosp Explorat Agcy JAXA, Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan. [Ishida, Manabu; Maeda, Yoshitomo] Grad Univ Adv Studies, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan. [Hayashi, Takayuki; Matsumoto, Hironori; Mitsuishi, Ikuyuki; Saji, Shigetaka; Tachibana, Sasagu] Nagoya Univ, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648602, Japan. [Hayashi, Takayuki; Okajima, Takashi; Mori, Hideyuki] NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. [Christensen, Finn] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark. [Brejnholt, Nicolai] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Nitta, Kiyofumi; Uruga, Tomoya] JASRI SPring 8, Sayo Cho, Sayo, Hyogo 6795198, Japan. RP Maeda, Y (reprint author), Tokyo Metropolitan Univ, 1-1 Minami Osawa, Hachioji, Tokyo 1920397, Japan. EM ymaeda@astro.isas.jaxa.jp FU Ministry of Education, Culture, Sports, Science and Technology, Japan [25870744, 25105516, 23540280] FX The authors are grateful to all the full-time engineers and part-time workers in the GSFC/NASA laboratory for support in mass production of the Soft X-ray Telescope reflectors. R.I. and Y.M. acknowledge Support from the Grants-in-Aid for Scientific Research (numbers 25870744, 25105516 and 23540280) by the Ministry of Education, Culture, Sports, Science and Technology, Japan. We thank M. Sakano (Wise Babel Ltd.) and Chris Baluta for English correction. NR 19 TC 0 Z9 0 U1 0 U2 0 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 OCT 31 PY 2016 VL 24 IS 22 BP 25548 EP 25564 DI 10.1364/OE.24.025548 PG 17 WC Optics SC Optics GA EC8SQ UT WOS:000388413400085 PM 27828493 ER PT J AU Suazo-Davila, D Rivera-Melendez, J Koehne, J Meyyappan, M Cabrera, CR AF Suazo-Davila, D. Rivera-Melendez, J. Koehne, J. Meyyappan, M. Cabrera, C. R. TI Surface analysis and electrochemistry of a robust carbon-nanofiber-based electrode platform H2O2 sensor SO APPLIED SURFACE SCIENCE LA English DT Article DE H2O2; Cholesterol; Carbon nanofiber electrode; Cholesterol oxidase ID HYDROGEN-PEROXIDE SENSOR; BORON-DOPED DIAMOND; NANOELECTRODE ARRAYS; SILVER NANOPARTICLES; NANOTUBES; BIOSENSOR; GRAPHENE; FABRICATION; PLATINUM; GLUCOSE AB A vertically aligned carbon nanofiber-based (VACNF) electrode platform was developed for an enzyme less hydrogen peroxide sensor. Vertical nanofibers have heights on the order of 2-3 mu m, and diameters that vary from 50 to 100 nm as seen by atomic force microscopy. The VACNF was grown as individual, vertically, and freestanding structures using plasma-enhanced chemical vapor deposition. The electrochemical sensor, for the hydrogen peroxide measurement in solution, showed stability and reproducibility in five consecutive calibration curves with different hydrogen peroxide concentrations over a period of 3 days. The detection limit was 66 mu M. The sensitivity for hydrogen peroxide electrochemical detection was 0.0906 mA cm(-2) mM(-1), respectively. The sensor was also used for the measurement of hydrogen peroxide as the by-product of the reaction of cholesterol with cholesterol oxidase as a biosensor application. The sensor exhibits linear behavior in the range of 50 mu M-1 mM in cholesterol concentrations. The surface analysis and electrochemistry characterization is presented. (C) 2016 Published by Elsevier B.V. C1 [Suazo-Davila, D.; Rivera-Melendez, J.; Cabrera, C. R.] Univ Puerto Rico, Mol Sci Res Ctr, Dept Chem, NASA MIRO Ctr Adv Nanoscale Mat CANM, Rio Piedras Campus, San Juan, PR 00936 USA. [Koehne, J.; Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Cabrera, CR (reprint author), Univ Puerto Rico, Mol Sci Res Ctr, Dept Chem, NASA MIRO Ctr Adv Nanoscale Mat CANM, Rio Piedras Campus, San Juan, PR 00936 USA. EM carlos.cabrera2@upr.edu FU NASA-MIRO [NNX10AQ17A]; NSF-Chemistry [CHE-1152940]; NASA; NIH-MARC FX This work was financially supported in part by NASA-MIRO Grant No. NNX10AQ17A and NSF-Chemistry Grant No. CHE-1152940. DSD and JR acknowledge the NASA Harriet Jenkins Pre-doctoral Fellowship Program and the NIH-MARC Undergraduate Fellowship Program, respectively. NR 54 TC 2 Z9 2 U1 68 U2 173 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-4332 EI 1873-5584 J9 APPL SURF SCI JI Appl. Surf. Sci. PD OCT 30 PY 2016 VL 384 BP 251 EP 257 DI 10.1016/j.apsusc.2016.05.027 PG 7 WC Chemistry, Physical; Materials Science, Coatings & Films; Physics, Applied; Physics, Condensed Matter SC Chemistry; Materials Science; Physics GA DP5TP UT WOS:000378560900031 ER PT J AU Isakov, SV Mazzola, G Smelyanskiy, VN Jiang, Z Boixo, S Neven, H Troyer, M AF Isakov, Sergei V. Mazzola, Guglielmo Smelyanskiy, Vadim N. Jiang, Zhang Boixo, Sergio Neven, Hartmut Troyer, Matthias TI Understanding Quantum Tunneling through Quantum Monte Carlo Simulations SO PHYSICAL REVIEW LETTERS LA English DT Article ID PATH-INTEGRALS; SPIN-GLASS; OPTIMIZATION; ALGORITHM; DYNAMICS AB The tunneling between the two ground states of an Ising ferromagnet is a typical example of many-body tunneling processes between two local minima, as they occur during quantum annealing. Performing quantum Monte Carlo (QMC) simulations we find that the QMC tunneling rate displays the same scaling with system size, as the rate of incoherent tunneling. The scaling in both cases is O(Delta(2)), where Delta is the tunneling splitting (or equivalently the minimum spectral gap). An important consequence is that QMC simulations can be used to predict the performance of a quantum annealer for tunneling through a barrier. Furthermore, by using open instead of periodic boundary conditions in imaginary time, equivalent to a projector QMC algorithm, we obtain a quadratic speedup for QMC simulations, and achieve linear scaling in Delta. We provide a physical understanding of these results and their range of applicability based on an instanton picture. C1 [Isakov, Sergei V.] Google, CH-8002 Zurich, Switzerland. [Mazzola, Guglielmo; Troyer, Matthias] Swiss Fed Inst Technol, Theoret Phys, CH-8093 Zurich, Switzerland. [Smelyanskiy, Vadim N.; Boixo, Sergio; Neven, Hartmut] Google, Venice, CA 90291 USA. [Jiang, Zhang] NASA, QuAIL, Ames Res Ctr, Moffett Field, CA 94035 USA. [Jiang, Zhang] Stinger Ghaffarian Technol Inc, 7701 Greenbelt Rd,Suite 400, Greenbelt, MD 20770 USA. RP Isakov, SV (reprint author), Google, CH-8002 Zurich, Switzerland. FU Swiss National Science Foundation through the National Competence Center in Research QSIT; ODNI; IARPA via MIT Lincoln Laboratory Air Force [FA8721-05-C-0002]; NSF [PHY-1066293] FX The work of G. M. and M. T. has been supported by the Swiss National Science Foundation through the National Competence Center in Research QSIT and by ODNI, IARPA via MIT Lincoln Laboratory Air Force Contract No. FA8721-05-C-0002. M. T. acknowledges hospitality of the Aspen Center for Physics, supported by NSF Grant No. PHY-1066293. We acknowledge useful discussions with F. Becca, M. Dykman, and G. Santoro. NR 46 TC 2 Z9 2 U1 1 U2 1 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 OCT 28 PY 2016 VL 117 IS 18 AR 180402 DI 10.1103/PhysRevLett.117.180402 PG 6 WC Physics, Multidisciplinary SC Physics GA EF3MF UT WOS:000390227800001 PM 27835027 ER PT J AU Cullather, RI Lim, YK Boisvert, LN Brucker, L Lee, JN Nowicki, SMJ AF Cullather, Richard I. Lim, Young-Kwon Boisvert, Linette N. Brucker, Ludovic Lee, Jae N. Nowicki, Sophie M. J. TI Analysis of the warmest Arctic winter, 2015-2016 SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE polar amplification; winter 2015-2016; Arctic warming ID SEA-ICE; ATMOSPHERIC RESPONSE; NORTH-ATLANTIC; CLIMATE-CHANGE; AMPLIFICATION; OSCILLATION; TELECONNECTIONS; ANOMALIES; PATTERNS; ASTERISK AB December through February 2015-2016 defines the warmest winter season over the Arctic in the observational record. Positive 2m temperature anomalies were focused over regions of reduced sea ice cover in the Kara and Barents Seas and southwestern Alaska. A third region is found over the ice-covered central Arctic Ocean. The period is marked by a strong synoptic pattern which produced melting temperatures in close proximity to the North Pole in late December and anomalous high pressure near the Taymyr Peninsula. Atmospheric teleconnections from the Atlantic contributed to warming over Eurasian high-latitude land surfaces, and El Nino-related teleconnections explain warming over southwestern Alaska and British Columbia, while warm anomalies over the central Arctic are associated with physical processes including the presence of enhanced atmospheric water vapor and an increased downwelling longwave radiative flux. Preconditioning of sea ice conditions by warm temperatures affected the ensuing spring extent. C1 [Cullather, Richard I.; Boisvert, Linette N.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Cullather, Richard I.; Lim, Young-Kwon] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Lim, Young-Kwon] Goddard Earth Sci Technol & Res, IM Syst Grp, College Pk, MD USA. [Boisvert, Linette N.; Brucker, Ludovic; Nowicki, Sophie M. J.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD USA. [Brucker, Ludovic] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA. [Lee, Jae N.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. [Lee, Jae N.] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD USA. RP Cullather, RI (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.; Cullather, RI (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. EM richard.cullather@nasa.gov RI Brucker, Ludovic/A-8029-2010 OI Brucker, Ludovic/0000-0001-7102-8084 FU NASA Interdisciplinary Research in Earth Science (IDS) program FX Surface Temperature Analysis (GISTEMP) data were obtain from NASA Goddard Institute for Space Studies (http://data.giss.nasa.gov/gistemp/). Reanalysis fields [Global Modeling and Assimilation Office, 2015a, 2015b] and AIRS data products were obtained from the Goddard Earth Sciences Data and Information Services Center. Sea ice concentration data derived from passive microwave remote sensing with the NASA Team algorithm were obtained from the National Snow and Ice Data Center. Monthly indices were obtained from the NOAA Earth System Research Laboratory (http://www.esrl.noaa.gov/psd/data/climateindices/list/). The authors posthumously thank Andrew G. Slater for his helpful comments in review and thank one other anonymous reviewer. This study was funded by grants from the NASA Interdisciplinary Research in Earth Science (IDS) program to the first, fourth, and sixth authors. NR 54 TC 3 Z9 3 U1 17 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD OCT 28 PY 2016 VL 43 IS 20 BP 10808 EP 10816 DI 10.1002/2016GL071228 PG 9 WC Geosciences, Multidisciplinary SC Geology GA EC7CQ UT WOS:000388293800033 ER PT J AU Christianson, K Bushuk, M Dutrieux, P Parizek, BR Joughin, IR Alley, RB Shean, DE Abrahamsen, EP Anandakrishnan, S Heywood, KJ Kim, TW Lee, SH Nicholls, K Stanton, T Truffer, M Webber, BGM Jenkins, A Jacobs, S Bindschadler, R Holland, DM AF Christianson, Knut Bushuk, Mitchell Dutrieux, Pierre Parizek, Byron R. Joughin, Ian R. Alley, Richard B. Shean, David E. Abrahamsen, E. Povl Anandakrishnan, Sridhar Heywood, Karen J. Kim, Tae-Wan Lee, Sang Hoon Nicholls, Keith Stanton, Tim Truffer, Martin Webber, Benjamin G. M. Jenkins, Adrian Jacobs, Stan Bindschadler, Robert Holland, David M. TI Sensitivity of Pine Island Glacier to observed ocean forcing SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ANTARCTIC ICE-SHEET; AMUNDSEN SEA EMBAYMENT; GROUNDING LINE RETREAT; WEST ANTARCTICA; THWAITES GLACIER; SHELF; BENEATH; MELT; CIRCULATION; WIDESPREAD AB We present subannual observations (2009-2014) of a major West Antarctic glacier (Pine Island Glacier) and the neighboring ocean. Ongoing glacier retreat and accelerated ice flow were likely triggered a few decades ago by increased ocean-induced thinning, which may have initiated marine ice sheet instability. Following a subsequent 60% drop in ocean heat content from early 2012 to late 2013, ice flow slowed, but by<4%, with flow recovering as the ocean warmed to prior temperatures. During this cold-ocean period, the evolving glacier-bed/ice shelf system was also in a geometry favorable to stabilization. However, despite a minor, temporary decrease in ice discharge, the basin-wide thinning signal did not change. Thus, as predicted by theory, once marine ice sheet instability is underway, a single transient high-amplitude ocean cooling has only a relatively minor effect on ice flow. The long-term effects of ocean temperature variability on ice flow, however, are not yet known. C1 [Christianson, Knut; Shean, David E.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. [Bushuk, Mitchell; Holland, David M.] NYU, Courant Inst Math Sci, New York, NY USA. [Bushuk, Mitchell] Princeton Univ, Geophys Fluid Dynam Lab, Princeton, NJ 08544 USA. [Dutrieux, Pierre; Joughin, Ian R.; Shean, David E.] Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA. [Dutrieux, Pierre; Jacobs, Stan] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Parizek, Byron R.] Penn State Univ, Math & Geosci, Du Bois, PA USA. [Parizek, Byron R.; Alley, Richard B.; Anandakrishnan, Sridhar] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Parizek, Byron R.; Alley, Richard B.; Anandakrishnan, Sridhar] Penn State Univ, Earth & Environm Syst Inst, University Pk, PA 16802 USA. [Abrahamsen, E. Povl; Nicholls, Keith; Jenkins, Adrian] British Antarctic Survey, Nat Environm Res Council, Cambridge, England. [Heywood, Karen J.; Webber, Benjamin G. M.] Univ East Anglia, Sch Environm Sci, Ctr Ocean & Atmospher Sci, Norwich, Norfolk, England. [Kim, Tae-Wan; Lee, Sang Hoon] Korea Polar Res Inst, Inchon, South Korea. [Stanton, Tim] US Naval Postgrad Sch, Dept Oceanog, Monterey, CA USA. [Truffer, Martin] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. [Bindschadler, Robert] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. RP Christianson, K (reprint author), Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. EM knut@uw.edu RI Abrahamsen, Povl/B-2140-2008; OI Abrahamsen, Povl/0000-0001-5924-5350; Heywood, Karen/0000-0001-9859-0026; Dutrieux, Pierre/0000-0002-8066-934X FU National Aeronautics and Space Administration [NNX16AM01G, NNX12AB69G, NNX15AH84G]; U.S. National Science Foundation [PLR-0732869, PLR-0732730, PLR-1443190, PLR-0632282, ANT-0732926, AGS-138832, ANT-0424589]; New York University Abu Dhabi Research Institute [G1204]; U.K. Natural Environment Research Council iSTAR program [NE/J005703/1, NE/G001367/1, NE/J005746/1]; South Korean Polar Research Institute grant KOPRI [PP15020] FX The work was supported by National Aeronautics and Space Administration grants NNX16AM01G (K.C.), NNX12AB69G (K.C. and D.H.), and NNX15AH84G (B.P.); U.S. National Science Foundation grants PLR-0732869 (D.H. and M. B.), PLR-0732730 (M.T.), PLR-1443190 (B.P.), PLR-0632282 (S.J.), ANT-0732926 (T.S.), AGS-138832 (B.P. and R.A.) and ANT-0424589 (I.J., K.C., R.A., S.A., and B.P.); New York University Abu Dhabi Research Institute grant G1204 (D.H.); U.K. Natural Environment Research Council iSTAR program-grants NE/J005703/1 (K.H. and B.W.), NE/G001367/1 (A.J. and P.D.), and NE/J005746/1 (A.J., K.H., B.W., and P. D.), and South Korean Polar Research Institute grant KOPRI PP15020 (S.L. and T.K.). The U.S.-NSF POLENET project provided GPS base data. Logistical support was provided by the U.S. Air Force, 139th Expeditionary Airlift Squadron of the New York Air National Guard, Kenn Borek Air, and by many dedicated individuals working as part of the Antarctic Support Contract, managed by Raytheon Polar Services Company and Lockheed-Martin, and by the officers, scientists and crew of RV Araon, RV Nathaniel B. Palmer and RRS James Clark Ross. GPS data are archived with UNAVCO (www.unavco.org). Oceanographic data have been submitted to the NOAA National Centers for Environmental Information (https://www.nodc.noaa.gov/), British Oceanographic Data Centre (http://www.bodc.ac.uk/), and IEDA/MGDS Southern Ocean portal (http://www.marine-geo.org/index.php). SAR-derived ice velocity fields and grounding lines, and basal altimeter range data are freely available from the corresponding author. NR 55 TC 2 Z9 2 U1 7 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 OCT 28 PY 2016 VL 43 IS 20 BP 10817 EP 10825 DI 10.1002/2016GL070500 PG 9 WC Geosciences, Multidisciplinary SC Geology GA EC7CQ UT WOS:000388293800045 ER PT J AU Frederikse, T Riva, R Kleinherenbrink, M Wada, Y van den Broeke, M Marzeion, B AF Frederikse, Thomas Riva, Riccardo Kleinherenbrink, Marcel Wada, Yoshihide van den Broeke, Michiel Marzeion, Ben TI Closing the sea level budget on a regional scale: Trends and variability on the Northwestern European continental shelf SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE sea level budget ID GREENLAND ICE-SHEET; COASTAL ZONES; RISE; IMPACT; MODEL; 20TH-CENTURY; CONSISTENT; TIDE; ACCELERATION; FLUCTUATIONS AB Long-term trends and decadal variability of sea level in the North Sea and along the Norwegian coast have been studied over the period 1958-2014. We model the spatially nonuniform sea level and solid earth response to large-scale ice melt and terrestrial water storage changes. GPS observations, corrected for the solid earth deformation, are used to estimate vertical land motion. We find a clear correlation between sea level in the North Sea and along the Norwegian coast and open ocean steric variability in the Bay of Biscay and west of Portugal, which is consistent with the presence of wind-driven coastally trapped waves. The observed nodal cycle is consistent with tidal equilibrium. We are able to explain the observed sea level trend over the period 1958-2014 well within the standard error of the sum of all contributing processes, as well as the large majority of the observed decadal sea level variability. C1 [Frederikse, Thomas; Riva, Riccardo; Kleinherenbrink, Marcel] Delft Univ Technol, Dept Geosci & Remote Sensing, Delft, Netherlands. [Wada, Yoshihide] NASA Goddard Inst Space Studies, New York, NY USA. [Wada, Yoshihide] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Wada, Yoshihide] Univ Utrecht, Dept Phys Geog, Utrecht, Netherlands. [Wada, Yoshihide] Int Inst Appl Syst Anal, Laxenburg, Austria. [van den Broeke, Michiel] Univ Utrecht, Inst Marine & Atmospher Res Utrecht, Utrecht, Netherlands. [Marzeion, Ben] Univ Bremen, Inst Geog, Bremen, Germany. RP Frederikse, T (reprint author), Delft Univ Technol, Dept Geosci & Remote Sensing, Delft, Netherlands. EM t.frederikse@tudelft.nl RI Van den Broeke, Michiel/F-7867-2011 OI Van den Broeke, Michiel/0000-0003-4662-7565 FU Netherlands Organisation for Scientific Research (NWO) VIDI grant [864.12.012]; Austrian Science Fund (FWF) [P25362-N26] FX Tide gauge data have been obtained from PSMSL (www.psmsl.org), EN4.1.1 gridded profiles from Met Office Hadley Center (metoffice.gov.uk/hadobs/en4), Twentieth Century Reanalysis V2c data from NOAA/OAR/ESRL PSD (esrl.noaa.gov/psd/data/gridded/data.20thC_ReanV2c.html), ICE6G data from atmosp.physics.utoronto.ca/similar to peltier, NorESM model results were obtained from the ESGF Node at DKRZ (esgf-data.dkrz.de). Ocean Weather Station Mike data have been obtained from http://www.eurosites.info/stationm.php. All gridded plots have been made using the Generic Mapping Tools. This study was funded through the Netherlands Organisation for Scientific Research (NWO) VIDI grant 864.12.012. Ben Marzeion acknowledges support from the Austrian Science Fund (FWF): P25362-N26. We would like to thank the two anonymous reviewers for their constructive comments, which led to substantial improvements to the manuscript. NR 63 TC 0 Z9 0 U1 5 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD OCT 28 PY 2016 VL 43 IS 20 BP 10864 EP 10872 DI 10.1002/2016GL070750 PG 9 WC Geosciences, Multidisciplinary SC Geology GA EC7CQ UT WOS:000388293800009 PM 28239204 ER PT J AU Chafik, L Hakkinen, S England, MH Carton, JA Nigam, S Ruiz-Barradas, A Hannachi, A Miller, L AF Chafik, L. Hakkinen, S. England, M. H. Carton, J. A. Nigam, S. Ruiz-Barradas, A. Hannachi, A. Miller, L. TI Global linkages originating from decadal oceanic variability in the subpolar North Atlantic SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE subpolar North Atlantic; decadal variability; Atlantic climate; Walker circulation; Pacific climate; teleconnections ID MERIDIONAL OVERTURNING CIRCULATION; HEAT-CONTENT; MULTIDECADAL OSCILLATION; WARMING HIATUS; GULF-STREAM; ATMOSPHERIC CIRCULATION; SST VARIABILITY; TEMPERATURE; PACIFIC; 20TH-CENTURY AB The anomalous decadal warming of the subpolar North Atlantic Ocean (SPNA), and the northward spreading of this warm water, has been linked to rapid Arctic sea ice loss and more frequent cold European winters. Recently, variations in this heat transport have also been reported to covary with global warming slowdown/acceleration periods via a Pacific climate response. We here examine the role of SPNA temperature variability in this Atlantic-Pacific climate connectivity. We find that the evolution of ocean heat content anomalies from the subtropics to the subpolar region, likely due to ocean circulation changes, coincides with a basin-wide Atlantic warming/cooling. This induces an Atlantic-Pacific sea surface temperature seesaw, which in turn, strengthens/weakens the Walker circulation and amplifies the Pacific decadal variability that triggers pronounced global-scale atmospheric circulation anomalies. We conclude that the decadal oceanic variability in the SPNA is an essential component of the tropical interactions between the Atlantic and Pacific Oceans. C1 [Chafik, L.; Miller, L.] NOAA, NESDIS Ctr Satellite Applicat & Res, College Pk, MD 20740 USA. [Chafik, L.] Univ Maryland, Cooperat Inst Climate & Satellites, College Pk, MD 20742 USA. [Hakkinen, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [England, M. H.] Univ New South Wales, Australian Res Council Ctr Excellence Climate Sys, Sydney, NSW, Australia. [England, M. H.] Univ New South Wales, Climate Change Res Ctr, Sydney, NSW, Australia. [Carton, J. A.; Nigam, S.; Ruiz-Barradas, A.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Hannachi, A.] Stockholm Univ, Dept Meteorol, Stockholm, Sweden. RP Chafik, L (reprint author), NOAA, NESDIS Ctr Satellite Applicat & Res, College Pk, MD 20740 USA.; Chafik, L (reprint author), Univ Maryland, Cooperat Inst Climate & Satellites, College Pk, MD 20742 USA. EM leon.chafik@uib.no RI Miller, Laury/B-8305-2011; OI Miller, Laury/0000-0003-3095-5804; Carton, James/0000-0003-0598-5198 FU NASA Physical Oceanography Program; Australian Research Council; US National Science Foundation [AGS1439940] FX The authors wish to thank Thomas Rossby, Johan Nilsson, and the two anonymous reviewers for their insightful comments and helpful suggestions. L.C. is supported by the Jason Altimetry Program. S.H. is supported by the NASA Physical Oceanography Program. M.H.E. is supported by the Australian Research Council. S.N. and A.R.-B. gratefully acknowledge the support of the US National Science Foundation through grant AGS1439940. AWT data are included as a supporting information file; any additional data may be obtained from L.C. (leon.chafik@uib.no). This work was completed at the corresponding author's current affiliation (Geophysical Institute, University of Bergen, Norway). NR 78 TC 0 Z9 0 U1 7 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 OCT 28 PY 2016 VL 43 IS 20 BP 10909 EP 10919 DI 10.1002/2016GL071134 PG 11 WC Geosciences, Multidisciplinary SC Geology GA EC7CQ UT WOS:000388293800027 ER PT J AU Tan, XX Huang, Y Diao, MH Bansemer, A Zondlo, MA DiGangi, JP Volkamer, R Hu, YY AF Tan, Xiaoxiao Huang, Yi Diao, Minghui Bansemer, Aaron Zondlo, Mark A. DiGangi, Joshua P. Volkamer, Rainer Hu, Yongyun TI An assessment of the radiative effects of ice supersaturation based on in situ observations SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ATMOSPHERIC INFRARED SOUNDER; CIRRUS CLOUD SCHEME; UPPER TROPOSPHERE; LIDAR MEASUREMENTS; RELATIVE-HUMIDITY; CLIMATE MODEL; REGIONS; STRATOSPHERE; MICROPHYSICS; NUCLEATION AB We use aircraft observations combined with the reanalysis data to investigate the radiative effects of ice supersaturation (ISS). Our results show that although the excess water vapor over ice saturation itself has relatively small radiative effects, mistaking it as ice crystals in climate models would lead to considerable impacts: on average, +2.49W/m(2) change in the top of the atmosphere (TOA) radiation, -2.7W/m(2) change in surface radiation, and 1.47K/d change in heating rates. The radiative effects of ISS generally increase with the magnitudes of supersaturation. However, there is a strong dependence on the preexisting ice water path, which can even change the sign of the TOA radiative effect. It is therefore important to consider coexistence between ISS and ice clouds and to validate their relationship in the parameterizations of ISS in climate models. C1 [Tan, Xiaoxiao; Hu, Yongyun] Peking Univ, Dept Atmospher & Ocean Sci, Beijing, Peoples R China. [Tan, Xiaoxiao; Huang, Yi] McGill Univ, Dept Atmospher & Ocean Sci, Montreal, PQ, Canada. [Diao, Minghui] San Jose State Univ, Dept Meteorol & Climate Sci, San Jose, CA 95192 USA. [Bansemer, Aaron] Natl Ctr Atmospher Res, Mesoscale & Microscale Meteorol Lab, POB 3000, Boulder, CO 80307 USA. [Zondlo, Mark A.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. [DiGangi, Joshua P.] NASA Langley Res Ctr, Chem & Dynam Branch, Hampton, VA USA. [Volkamer, Rainer] Univ Colorado, Dept Chem & Biochem, Campus Box 215, Boulder, CO 80309 USA. [Volkamer, Rainer] Univ Colorado, CIRES, Boulder, CO 80309 USA. RP Huang, Y (reprint author), McGill Univ, Dept Atmospher & Ocean Sci, Montreal, PQ, Canada. EM yi.huang@mcgill.ca RI Volkamer, Rainer/B-8925-2016; Huang, Yi/E-9479-2016; OI Volkamer, Rainer/0000-0002-0899-1369; Huang, Yi/0000-0002-5065-4198; Zondlo, Mark/0000-0003-2302-9554 FU China Scholarship Council; Natural Sciences and Engineering Research Council of Canada [RGPIN 418305-13]; Fonds de recherche du Quebec-Nature et technologies [PR-190145]; National Center for Atmospheric Research Advanced Study Program; National Natural Science Foundation of China [41375072, 41530423]; National Science Foundation FX We acknowledge the ECMWF for the ERA-Interim data (http://apps.ecmwf.int/datasets/data/interim-full-moda/), the NSF for the observed ISS data, and the Atmospheric Environment Research for RRTMG model (http://rtweb.aer.com/rrtm_frame.html) used in this study. X.T. is supported by a visiting student fellowship of China Scholarship Council. Y. Huang acknowledges the grants support from the Natural Sciences and Engineering Research Council of Canada (RGPIN 418305-13) and the Fonds de recherche du Quebec-Nature et technologies (PR-190145). M.D. acknowledges the support of National Center for Atmospheric Research Advanced Study Program for her postdoctoral research in 2013-2015. Y. Hu acknowledges the grants from the National Natural Science Foundation of China (41375072 and 41530423). NCAR is sponsored by the National Science Foundation. For the observation analysis on five NSF campaigns (HIPPO Global, START08, PREDICT, DC3, and TORERO), we thank the efforts of flight, technical, and mechanical crews at the NCAR/Earth Observing Laboratory. M.A. Zondlo, M. Diao, J. DiGangi, and S.P. Beaton provided the field support and laboratory calibration of the VCSEL hygrometer. A. Bansemer, A.J. Heymsfield, D.C. Rogers, and C.J. Webster provided support on the SID-2H instrument and Fast-2 DC probes. We acknowledge the observations from the European Union INCA campaign, with recent data updates from Ulrich Schumann and Andreas Minikin. All data used in this study are free and publicly available. The aircraft observations for individual NSF campaigns were obtained at http://data.eol.ucar.edu/codiac/ NR 40 TC 0 Z9 0 U1 4 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD OCT 28 PY 2016 VL 43 IS 20 BP 11039 EP 11047 DI 10.1002/2016GL071144 PG 9 WC Geosciences, Multidisciplinary SC Geology GA EC7CQ UT WOS:000388293800053 ER PT J AU Hughes, EJ Yorks, J Krotkov, NA da Silva, AM McGill, M AF Hughes, E. J. Yorks, J. Krotkov, N. A. da Silva, A. M. McGill, M. TI Using CATS near-real-time lidar observations to monitor and constrain volcanic sulfur dioxide (SO2) forecasts SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CLOUDS; ERUPTION AB An eruption of Italian volcano Mount Etna on 3 December 2015 produced fast-moving sulfur dioxide (SO2) and sulfate aerosol clouds that traveled across Asia and the Pacific Ocean, reaching North America in just 5days. The Ozone Profiler and Mapping Suite's Nadir Mapping UV spectrometer aboard the U.S. National Polar-orbiting Partnership satellite observed the horizontal transport of the SO2 cloud. Vertical profiles of the colocated volcanic sulfate aerosols were observed between 11.5 and 13.5km by the new Cloud Aerosol Transport System (CATS) space-based lidar aboard the International Space Station. Backward trajectory analysis estimates the SO2 cloud altitude at 7-12km. Eulerian model simulations of the SO2 cloud constrained by CATS measurements produced more accurate dispersion patterns compared to those initialized with the back trajectory height estimate. The near-real-time data processing capabilities of CATS are unique, and this work demonstrates the use of these observations to monitor and model volcanic clouds. C1 [Hughes, E. J.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Yorks, J.; Krotkov, N. A.; da Silva, A. M.; McGill, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 32899 USA. RP Hughes, EJ (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. EM ehughes@umd.edu FU NASA Applied Sciences Natural Hazards Program; NASA [NNX13AG51G] FX The authors acknowledge the NASA Applied Sciences Natural Hazards Program and NASA grant NNX13AG51G, which provided funding for this research. Observations from CATS can be found at http://cats.gsfc.nasa.gov and OMPS-NM SO2 observations can be found at http://so2.gsfc.nasa.gov. Geostationary observations from Meteosat-10/SEVIRI can be found at http://www.eumetsat.int/website/home/Images/RealTimeImages/index.html. NR 33 TC 0 Z9 0 U1 5 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD OCT 28 PY 2016 VL 43 IS 20 BP 11089 EP 11097 DI 10.1002/2016GL070119 PG 9 WC Geosciences, Multidisciplinary SC Geology GA EC7CQ UT WOS:000388293800062 ER PT J AU Zuber, MT Smith, DE Neumann, GA Goossens, S Andrews-Hanna, JC Head, JW Kiefer, WS Asmar, SW Konopliv, AS Lemoine, FG Matsuyama, I Melosh, HJ McGovern, PJ Nimmo, F Phillips, RJ Solomon, SC Taylor, GJ Watkins, MM Wieczorek, MA Williams, JG Jansen, JC Johnson, BC Keane, JT Mazarico, E Miljkovic, K Park, RS Soderblom, JM Yuan, DN AF Zuber, Maria T. Smith, David E. Neumann, Gregory A. Goossens, Sander Andrews-Hanna, Jeffrey C. Head, James W. Kiefer, Walter S. Asmar, Sami W. Konopliv, Alexander S. Lemoine, Frank G. Matsuyama, Isamu Melosh, H. Jay McGovern, Patrick J. Nimmo, Francis Phillips, Roger J. Solomon, Sean C. Taylor, G. Jeffrey Watkins, Michael M. Wieczorek, Mark A. Williams, James G. Jansen, Johanna C. Johnson, Brandon C. Keane, James T. Mazarico, Erwan Miljkovic, Katarina Park, Ryan S. Soderblom, Jason M. Yuan, Dah-Ning TI Gravity field of the Orientale basin from the Gravity Recovery and Interior Laboratory Mission SO SCIENCE LA English DT Article ID MULTIRING BASINS; LUNAR CRUST; MOON; GRAIL; ORIGIN; RINGS AB The Orientale basin is the youngest and best-preserved major impact structure on the Moon. We used the Gravity Recovery and Interior Laboratory (GRAIL) spacecraft to investigate the gravitational field of Orientale at 3- to 5-kilometer (km) horizontal resolution. A volume of at least (3.4 +/- 0.2) x 10(6) km(3) of crustal material was removed and redistributed during basin formation. There is no preserved evidence of the transient crater that would reveal the basin's maximum volume, but its diameter may now be inferred to be between 320 and 460 km. The gravity field resolves distinctive structures of Orientale's three rings and suggests the presence of faults associated with the outer two that penetrate to the mantle. The crustal structure of Orientale provides constraints on the formation of multiring basins. C1 [Zuber, Maria T.; Smith, David E.; Johnson, Brandon C.; Miljkovic, Katarina; Soderblom, Jason M.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Neumann, Gregory A.; Lemoine, Frank G.; Mazarico, Erwan] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Goossens, Sander] Univ Maryland Baltimore Cty, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21250 USA. [Andrews-Hanna, Jeffrey C.; Jansen, Johanna C.] Colorado Sch Mines, Dept Geophys, Golden, CO 80401 USA. [Andrews-Hanna, Jeffrey C.; Jansen, Johanna C.] Colorado Sch Mines, Ctr Space Resources, Golden, CO 80401 USA. [Andrews-Hanna, Jeffrey C.; Phillips, Roger J.] Southwest Res Inst, Boulder, CO 80302 USA. [Head, James W.; Johnson, Brandon C.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA. [Kiefer, Walter S.; McGovern, Patrick J.] Lunar & Planetary Inst, 3303 NASA Rd 1, Houston, TX 77058 USA. [Asmar, Sami W.; Konopliv, Alexander S.; Watkins, Michael M.; Williams, James G.; Park, Ryan S.; Yuan, Dah-Ning] Jet Prop Lab, Pasadena, CA 91109 USA. [Matsuyama, Isamu; Keane, James T.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Melosh, H. Jay] Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA. [Nimmo, Francis] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Taylor, G. Jeffrey] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Watkins, Michael M.] Univ Texas Austin, Ctr Space Res, Austin, TX 78712 USA. [Wieczorek, Mark A.] Univ Paris Diderot, Sorbonne Paris Cite, Inst Phys Globe Paris, F-75205 Paris 13, France. [Miljkovic, Katarina] Curtin Univ, Dept Appl Geol, Perth, WA 6845, Australia. RP Zuber, MT (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. EM zuber@mit.edu RI Neumann, Gregory/I-5591-2013; OI Neumann, Gregory/0000-0003-0644-9944; Kiefer, Walter/0000-0001-6741-5460 FU NASA's Discovery Program FX The GRAIL mission is supported by NASA's Discovery Program and is performed under contract to the Massachusetts Institute of Technology and the Jet Propulsion Laboratory. Topography was obtained from the Lunar Orbiter Laser Altimeter on the Lunar Reconnaissance Mission, managed by NASA's Goddard Space Flight Center. The NASA Pleiades and Center for Climate Simulation supercomputers were used to compute the gravity solutions. All data used in this study are archived in the Geosciences Node of the NASA Planetary Data System at http://geo.pds.nasa.gov/missions/grail/default.htm. NR 39 TC 1 Z9 1 U1 6 U2 6 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD OCT 28 PY 2016 VL 354 IS 6311 BP 438 EP 441 DI 10.1126/science.aag0519 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EB9AT UT WOS:000387684400034 PM 27789835 ER PT J AU Ancellet, G Daskalakis, N Raut, JC Tarasick, D Hair, J Quennehen, B Ravetta, F Schlager, H Weinheimer, AJ Thompson, AM Johnson, B Thomas, JL Law, KS AF Ancellet, Gerard Daskalakis, Nikos Raut, Jean Christophe Tarasick, David Hair, Jonathan Quennehen, Boris Ravetta, Francois Schlager, Hans Weinheimer, Andrew J. Thompson, Anne M. Johnson, Bryan Thomas, Jennie L. Law, Katharine S. TI Analysis of the latitudinal variability of tropospheric ozone in the Arctic using the large number of aircraft and ozonesonde observations in early summer 2008 SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID HIGH NORTHERN LATITUDES; IN-SITU OBSERVATIONS; SATELLITE-OBSERVATIONS; LOWER STRATOSPHERE; FIELD-MEASUREMENTS; FIRE EMISSIONS; BOUNDARY-LAYER; AIRBORNE LIDAR; MIXING RATIOS; POLLUTION AB During the 2008 International Polar Year, the POLARCAT (Polar Study using Aircraft, Remote Sensing, Surface Measurements, and Models of Climate Chemistry, Aerosols, and Transport) campaign, conducted in summer over Greenland and Canada, produced a large number of measurements from three aircraft and seven ozonesonde stations. Here we present an observation-integrated analysis based on three different types of O-3 measurements: airborne lidar, airborne UV absorption or chemiluminescence measurement, and intensified electrochemical concentration cell (ECC) ozonesonde profiles. Discussion of the latitudinal and vertical variability of tropospheric ozone north of 55 degrees N during this period is performed with the aid of a regional model (WFR-Chem). The model is able to reproduce the O-3 latitudinal and vertical variability but with a negative O-3 bias of 6-15 ppbv in the free troposphere above 4 km, especially over Canada. For Canada, large average CO concentrations in the free troposphere above 4 km (> 130 ppbv) and the weak correlation (< 30 %) of O-3 and PV suggest that stratospheretroposphere exchange (STE) is not the major contributor to average tropospheric ozone at latitudes less than 70 degrees N, due to the fact that local biomass burning (BB) emissions were significant during the 2008 summer period. Conversely, significant STE is found over Greenland according to the better O-3 vs. PV correlation (> 40 %) and the higher values of the 75th PV percentile. It is related to the persistence of cyclonic activity during the summer over Baffin Bay. Using differences between average concentration above Northern and Southern Canada, a weak negative latitudinal summer ozone gradient of 6 to 8 ppbv is found in the mid-troposphere between 4 and 8 km. This is attributed to an efficient O-3 photochemical production from BB emissions at latitudes less than 65 degrees N, while the STE contribution is more homogeneous in the latitude range 55-70 degrees N. A positive ozone latitudinal gradient of 12 ppbv is observed in the same altitude range over Greenland not because of an increasing latitudinal influence of STE, but because of different long-range transport from multiple mid-latitude sources (North America, Europe, and even Asia for latitudes higher than 77 degrees N). For the Arctic latitudes (> 80 degrees N), free tropospheric O-3 concentrations during summer 2008 are related to a mixture of Asian pollution and stratospheric O-3 transport across the tropopause. C1 [Ancellet, Gerard; Daskalakis, Nikos; Raut, Jean Christophe; Quennehen, Boris; Ravetta, Francois; Thomas, Jennie L.; Law, Katharine S.] Sorbonne Univ, UPMC Univ Paris 06, LATMOS IPSL, UVSQ,CNRS, Paris, France. [Hair, Jonathan] NASA Langley Res Ctr, Hampton, VA USA. [Tarasick, David] Environm & Climate Change Canada, Downsview, ON, Canada. [Schlager, Hans] DLR, Inst Phys Atmosphare, Oberpfaffenhofen, Germany. [Weinheimer, Andrew J.] NCAR, Boulder, CO USA. [Thompson, Anne M.] NASA GSFC, Greenbelt, MD USA. [Johnson, Bryan] NOAA Earth Syst Res Lab ESRL, Boulder, CO USA. RP Ancellet, G (reprint author), Sorbonne Univ, UPMC Univ Paris 06, LATMOS IPSL, UVSQ,CNRS, Paris, France. EM gerard.ancellet@latmos.ipsl.fr RI Thompson, Anne /C-3649-2014; OI Thompson, Anne /0000-0002-7829-0920; Raut, Jean-Christophe/0000-0002-3552-2437; Daskalakis, Nikos/0000-0002-2409-0392; Tarasick, David/0000-0001-9869-0692 FU ANR; LEFE INSU/CNRS (CLIMSLIP project); ICE-ARC programme from the European Union [603887]; NASA; DLR FX We are very grateful to the support of the Meteo France/CNRS/CNES UMS SAFIRE for the ATR-42 aircraft deployment over Greenland. This work was supported by funding from ANR and LEFE INSU/CNRS (CLIMSLIP project) and from the ICE-ARC programme from the European Union 7th Framework Programme, grant number 603887. The FLEXTRA team (A. Stohl, and co-workers) is acknowledged for providing and supporting the FLEXTRA code. NASA and DLR are acknowledged for their support of the deployment of the DC-8 and Falcon-20 aircraft. WOUDC and the NASA MODIS team are acknowledged for providing the ozonesonde data and the MODIS data, respectively. NR 68 TC 0 Z9 0 U1 11 U2 11 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. PD OCT 28 PY 2016 VL 16 IS 20 BP 13341 EP 13358 DI 10.5194/acp-16-13341-2016 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EB1LP UT WOS:000387113800006 ER PT J AU Ni, X Liu, CT Zhang, QH Cecil, DJ AF Ni, Xiang Liu, Chuntao Zhang, Qinghong Cecil, Daniel J. TI Properties of hail storms over China and the United States from the Tropical Rainfall Measuring Mission SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE hail size; TRMM; microwave brightness temperature; remote sensing properties; radar reflectivity ID TRMM PRECIPITATION RADAR; PROFILING ALGORITHM; CLIMATOLOGY; SIZE; SCATTERING; THUNDERSTORMS; PERFORMANCE; VALIDATION; CONVECTION; SATELLITE AB A 16year record of hail reports over the south U.S. and from weather stations in China are collocated with precipitation features (PFs) derived from the Tropical Rainfall Measuring Mission (TRMM) radar and passive microwave observations. Differences in the way hail is reported in the two nations make it difficult to draw meaningful conclusions about storm frequency. But taking the two together yields a wide spectrum of hail sizes, suitable for comparing with remote sensing measurements. While U.S. hail reports are dominated by cases with hail size greater than 19mm, hail reports in China mostly include diameters of 1-10mm and mostly occur over the Tibetan Plateau. The fraction of PFs collocated with hail reports (hail PFs) reaches 3% in the plains of the U.S. In China, the fraction is higher in high elevation regions than low elevation regions. Hail PFs (as reported in the U.S.) show lower brightness temperatures, higher lightning flash rates, stronger maximum reflectivity, and higher echo tops than those with smaller hail, as reported in China. The average near surface maximum reflectivity of hail PFs at high elevations (2000m) in China is about 5dB smaller than those at low elevations. Larger hail is reported with PFs having stronger maximum reflectivity above 6km, though the median of maximum reflectivity values at levels below 5km is similar among the storms with large and small hail sizes. C1 [Ni, Xiang; Zhang, Qinghong] Peking Univ, Sch Phys, Dept Atmospher & Ocean Sci, Beijing, Peoples R China. [Ni, Xiang; Liu, Chuntao] Texas A&M Univ, Dept Phys & Environm Sci, Corpus Christi, TX USA. [Zhang, Qinghong] NUIST, Collaborat Innovat Ctr Forecast & Evaluat Meteoro, Nanjing, Jiangsu, Peoples R China. [Cecil, Daniel J.] NASA Marshall Space Flight Ctr, Huntsville, AL USA. RP Zhang, QH (reprint author), Peking Univ, Sch Phys, Dept Atmospher & Ocean Sci, Beijing, Peoples R China.; Zhang, QH (reprint author), NUIST, Collaborat Innovat Ctr Forecast & Evaluat Meteoro, Nanjing, Jiangsu, Peoples R China. EM qzhang@pku.edu.cn FU Chinese National Science Foundation [41330421, 41461164006]; NASA Precipitation Measurement Missions Science Team; China Scholarship Council FX This study is supported by the Chinese National Science Foundation under grants 41330421 and 41461164006 and by the NASA Precipitation Measurement Missions Science Team. The first author gratefully acknowledges the financial support from the China Scholarship Council. The TRMM Precipitation Feature Database could be obtained freely from http://atmos.tamucc.edu/trmm/. The hail reports in U. S. are updated by NCDC (http://www1.ncdc.noaa.gov/pub/data/swdi/stormevents/csvfiles/). Due to the National data management policy, the use of station hail size records in China must be authorized by the Meteorological Information Center of the China Meteorological Administration (http://www.nmic.gov.cn/web/index.htm). NR 51 TC 0 Z9 0 U1 7 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD OCT 27 PY 2016 VL 121 IS 20 BP 12031 EP 12044 DI 10.1002/2016JD025600 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EC7CJ UT WOS:000388293100017 ER PT J AU Xi, X Sokolik, IN AF Xi, Xin Sokolik, Irina N. TI Quantifying the anthropogenic dust emission from agricultural land use and desiccation of the Aral Sea in Central Asia SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE anthropogenic dust; land use; agriculture; Aral Sea; Central Asia; dust emission ID CLIMATE-CHANGE; MODEL; DESERTIFICATION; AEROSOLS AB A regional dust model system is applied to quantify the anthropogenic dust emission in the post-Soviet Central Asia from 2000 to 2014. Two physically based dust schemes suggest that a proportion of 18.3-32.8% of total dust emissions is contributed by agricultural land use and the desiccation of Aral Sea, whereas a simplified dust scheme yields higher estimates in the range of 49.7-56.5% depending on whether a static or dynamic preferential dust source function is used. The dust schemes also differ greatly in the spatial distribution of anthropogenic dust and the sensitivity to the use of land use intensity in separating natural and human-made source areas, suggesting that the model representation of erosion threshold velocity, especially the role of vegetation, is a key source of model uncertainty in quantifying anthropogenic dust. The relative importance of agriculture and dried Aral Sea bed (Aralkum) differs greatly among the dust schemes. Despite the increased dust from the expansion of Aralkum, there is a negative trend in the anthropogenic dust proportion, indicating a shift of dust emission toward natural source areas. All dust schemes show a decrease in anthropogenic dust in response to land cover changes over agricultural lands. C1 [Xi, Xin; Sokolik, Irina N.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Xi, Xin] NASA Ames Res Ctr, Div Earth Sci, Moffett Field, CA USA. RP Xi, X (reprint author), Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.; Xi, X (reprint author), NASA Ames Res Ctr, Div Earth Sci, Moffett Field, CA USA. EM xin.xi30@gmail.com OI XI, XIN/0000-0003-3804-2735 FU NASA LCLUC program FX This study was funded by the NASA LCLUC program. We thank three anonymous reviewers for improving this manuscript. Data used in this study are obtained from public domains: HYDE land use data from the PBL Netherlands Environmental Assessment Agency at http://themasites.pbl.nl/tridion/en/themasites/hyde/ and MODIS land cover product from Land Processes Distributed Active Archive Center (https://lpdaac.usgs.gov). Results are available from the corresponding author (X. Xi, xin.xi30@gmail.com) upon request. NR 34 TC 1 Z9 1 U1 5 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD OCT 27 PY 2016 VL 121 IS 20 BP 12270 EP 12281 DI 10.1002/2016JD025556 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EC7CJ UT WOS:000388293100022 ER PT J AU Duderstadt, KA Dibb, JE Jackman, CH Randall, CE Schwadron, NA Solomon, SC Spence, HE AF Duderstadt, K. A. Dibb, J. E. Jackman, C. H. Randall, C. E. Schwadron, N. A. Solomon, S. C. Spence, H. E. TI Comment on "Atmospheric ionization by high-fluence, hard spectrum solar proton events and their probable appearance in the ice core archive" by A. L. Melott et al. SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Editorial Material DE nitrate; SPE ID IMPULSIVE NITRATE EVENTS; TIME RESOLUTION ANALYSIS; MIDDLE ATMOSPHERE; ODD NITROGEN; ION SPIKES; PRECIPITATION; PROXIES; MODEL; SNOW C1 [Duderstadt, K. A.; Dibb, J. E.; Schwadron, N. A.; Spence, H. E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Jackman, C. H.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Randall, C. E.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA. [Randall, C. E.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA. [Solomon, S. C.] Natl Ctr Atmospher Res, High Altitude Observ, Pob 3000, Boulder, CO 80307 USA. RP Duderstadt, KA (reprint author), Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. EM duderstadtk@eos.sr.unh.edu RI Solomon, Stanley/J-4847-2012; Jackman, Charles/D-4699-2012; Randall, Cora/L-8760-2014 OI Solomon, Stanley/0000-0002-5291-3034; Randall, Cora/0000-0002-4313-4397 NR 26 TC 0 Z9 0 U1 0 U2 0 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 OCT 27 PY 2016 VL 121 IS 20 BP 12484 EP 12489 DI 10.1002/2016JD025220 PG 6 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EC7CJ UT WOS:000388293100013 ER PT J AU Yadav, V Michalak, AM Ray, J Shiga, YP AF Yadav, Vineet Michalak, Anna M. Ray, Jaideep Shiga, Yoichi P. TI A statistical approach for isolating fossil fuel emissions in atmospheric inverse problems SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE inverse problem; fossil fuel emissions ID CARBON-DIOXIDE EMISSIONS; FLUX ESTIMATION; UNITED-STATES; CO2 EMISSIONS; GAS EMISSIONS; MODEL; CITY; SURFACE; SYSTEM; CYCLE AB Independent verification and quantification of fossil fuel (FF) emissions constitutes a considerable scientific challenge. By coupling atmospheric observations of CO2 with models of atmospheric transport, inverse models offer the possibility of overcoming this challenge. However, disaggregating the biospheric and FF flux components of terrestrial fluxes from CO2 concentration measurements has proven to be difficult, due to observational and modeling limitations. In this study, we propose a statistical inverse modeling scheme for disaggregating winter time fluxes on the basis of their unique error covariances and covariates, where these covariances and covariates are representative of the underlying processes affecting FF and biospheric fluxes. The application of the method is demonstrated with one synthetic and two real data prototypical inversions by using in situ CO2 measurements over North America. Inversions are performed only for the month of January, as predominance of biospheric CO2 signal relative to FF CO2 signal and observational limitations preclude disaggregation of the fluxes in other months. The quality of disaggregation is assessed primarily through examination of a posteriori covariance between disaggregated FF and biospheric fluxes at regional scales. Findings indicate that the proposed method is able to robustly disaggregate fluxes regionally at monthly temporal resolution with a posteriori cross covariance lower than 0.15 mu molm(-2)s(-1) between FF and biospheric fluxes. Error covariance models and covariates based on temporally varying FF inventory data provide a more robust disaggregation over static proxies (e.g., nightlight intensity and population density). However, the synthetic data case study shows that disaggregation is possible even in absence of detailed temporally varying FF inventory data. C1 [Yadav, Vineet; Michalak, Anna M.; Shiga, Yoichi P.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Yadav, Vineet] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. [Ray, Jaideep] Sandia Natl Labs, Livermore, CA USA. [Shiga, Yoichi P.] Stanford Univ, Dept Civil & Environm Engn, Stanford, CA 94305 USA. RP Yadav, V (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.; Yadav, V (reprint author), Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. EM vineet.yadav@jpl.nasa.gov FU Sandia National Laboratories' LDRD (Laboratory Directed Research and Development) funds - Geosciences Investment Area; U.S. Department of Energy's National Nuclear Security Administration [DE-AC04-94AL85000]; National Science Foundation [1342076]; Carnegie Institution of Washington [NNN15R040T]; National Aeronautics and Space Administration [NNN15R040T]; National Science Foundation Biocomplexity in the Environment Program [ATM-0221850]; University of Virginia; DOE Office of Science-Terrestrial Carbon Processes program; NOAA [NA11OAR4310056]; U.S. Department of Energy [DE-AC09-08SR22470]; California Energy Commission's Public Interest Environmental Research Program [DE-AC02-05CH11231]; U.S. Department of Energy Office of Science TCP program [DE-FG02-06ER64315]; U.S. Department of Commerce, NOAA office of Global Programs [NA08OAR4310533]; U.S. Department of Energy through the Ameriflux Management Project; Midwestern Center of the National Institute for Global Environmental Change (NIGEC); National Institute for Climate Change Research (NICCR); Terrestrial Carbon Program (TCP) program; Terrestrial Ecosystem Sciences (TES) program; Scripps CO2 program FX This work was supported by Sandia National Laboratories' LDRD (Laboratory Directed Research and Development) funds, sponsored by the Geosciences Investment Area. Sandia National Laboratories is a multiprogram laboratory managed and operated by Sandia Corporation, a wholly owned subsidiary of Lockheed Martin Corporation, for the U.S. Department of Energy's National Nuclear Security Administration under contract DE-AC04-94AL85000. Additional funding for this research came from National Science Foundation under grant 1342076. Some of this research, was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract NNN15R040T between Carnegie Institution of Washington and National Aeronautics and Space Administration. We gratefully acknowledge the efforts of the PIs of the various towers providing continuous atmospheric CO2 observations, which were instrumental for these analyses. The sites BRW, WGC, SNP, SCT, AMT, WBI, BAO, LEF, and WKT are part of NOAA's Global Greenhouse Gas Reference Network operated by the Global Monitoring Division of NOAA's Earth System Research Laboratory with additional support from NOAA's Climate Program Office and are a contribution to the North American Carbon Program. The installation of CO2 sampling equipment was made possible at AMT, by a grant from the National Science Foundation Biocomplexity in the Environment Program (ATM-0221850), at SNP, by the University of Virginia, and at SCT by funding provided by the DOE Office of Science-Terrestrial Carbon Processes program. The Savannah River National Laboratory (SRNL) provided support during the installation at SCT and provides ongoing support via funding from NOAA. SNRL is operated by Savannah River Nuclear Solutions, LLC, under contract DE-AC09-08SR22470 with the U.S. Department of Energy. WGC measurements were supported by a combination of the California Energy Commission's Public Interest Environmental Research Program to the Lawrence Berkeley National Laboratory under contract DE-AC02-05CH11231 and NOAA. Research at CVA, OZA, KEW, CEN, MEA, ROL, and GAL was sponsored by the U.S. Department of Energy Office of Science TCP program (DE-FG02-06ER64315) and by the U.S. Department of Commerce, NOAA office of Global Programs (NA08OAR4310533). The five Oregon sites FIR, MET, YAH, MAP, and NGB were supported by NOAA (NA11OAR4310056). The research at the MMS site was sponsored by the U.S. Department of Energy through the Ameriflux Management Project, the Midwestern Center of the National Institute for Global Environmental Change (NIGEC), the National Institute for Climate Change Research (NICCR), the Terrestrial Carbon Program (TCP), and the Terrestrial Ecosystem Sciences (TES) programs. CO2 measurements at LJA were supported by the Scripps CO2 program. We thank the following individuals for collecting and providing the atmospheric CO2 data from the following sites: Arlyn Andrews (NOAA) for SNP, AMT, WBI, BAO, LEF, and WKT; Kirk Thoning (NOAA) for BRW; Mattew J.; Parker (SRNL) for SCT; Marc Fischer (LBNL) and Arlyn Andrews (NOAA) for WGC; Kenneth Davis, Scott Richardson, and Natasha Miles (Pennsylvania State University) for CVA, OZA, KEW, CEN, MEA, ROL, and GAL; Britton Stephens (NCAR) and the Regional Atmospheric Continuous CO2 Network in the Rocky Mountains (RACCOON) for NWR, SPL, and HDP; Beverly Law (Oregon State University) and the TERRA-PNW group for data from five Oregon sites, FIR, MET, YAH, MAP, and NGB; William Munger (Harvard University) and Steven Wofsy (Harvard University) for HFM; Doug Worthy (Environment Canada) for CDL, FRD, SBL, EGB, ETL, LLB, and CHM; Kimberly Novick (Indiana University) for MMS; Sebastien Biraud (LBNL) and Margaret Torn (LBNL) for SGP; and Ralph Keeling (Scripps Institution of Oceanography) and Lisa Welp (Purdue University) for LJA. Note that all the code required for evaluating, replicating, and building upon the results of this paper can be obtained without cost from Vineet Yadav by contacting him through email at vineet.yadav@jpl.nasa.gov. For obtaining the concentration data utilized in this study, researchers would have to directly (on their own) contact the principal investigators of towers listed above. NR 69 TC 1 Z9 1 U1 4 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD OCT 27 PY 2016 VL 121 IS 20 BP 12490 EP 12504 DI 10.1002/2016JD025642 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EC7CJ UT WOS:000388293100010 ER PT J AU Yeung, LY Murray, LT Ash, JL Young, ED Boering, KA Atlas, EL Schauffler, SM Lueb, RA Langenfelds, RL Krummel, PB Steele, LP Eastham, SD AF Yeung, Laurence Y. Murray, Lee T. Ash, Jeanine L. Young, Edward D. Boering, Kristie A. Atlas, Elliot L. Schauffler, Sue M. Lueb, Richard A. Langenfelds, Ray L. Krummel, Paul. B. Steele, L. Paul Eastham, Sebastian D. TI Isotopic ordering in atmospheric O-2 as a tracer of ozone photochemistry and the tropical atmosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE clumped isotopes; oxygen; ozone; stratosphere-troposphere exchange; tropical circulation; atmospheric residence times ID LAST GLACIAL MAXIMUM; STRATOSPHERE-TROPOSPHERE EXCHANGE; INTERCOMPARISON PROJECT ACCMIP; MADDEN-JULIAN OSCILLATION; CHEMISTRY-TRANSPORT MODEL; VOSTOK ICE CORE; CARBON-DIOXIDE; CLIMATE SENSITIVITY; GEOS-CHEM; MIDDLE ATMOSPHERE AB The distribution of isotopes within O-2 molecules can be rapidly altered when they react with atomic oxygen. This mechanism is globally important: while other contributions to the global budget of O-2 impart isotopic signatures, the O(P-3)+O-2 reaction resets all such signatures in the atmosphere on subdecadal timescales. Consequently, the isotopic distribution within O-2 is determined by O-3 photochemistry and the circulation patterns that control where that photochemistry occurs. The variability of isotopic ordering in O-2 has not been established, however. We present new measurements of (OO)-O-18-O-18 in air (reported as (36) values) from the surface to 33km altitude. They confirm the basic features of the clumped-isotope budget of O-2: Stratospheric air has higher (36) values than tropospheric air (i.e., more (OO)-O-18-O-18), reflecting colder temperatures and fast photochemical cycling of O-3. Lower (36) values in the troposphere arise from photochemistry at warmer temperatures balanced by the influx of high-(36) air from the stratosphere. These observations agree with predictions derived from the GEOS-Chem chemical transport model, which provides additional insight. We find a link between tropical circulation patterns and regions where (36) values are reset in the troposphere. The dynamics of these regions influences lapse rates, vertical and horizontal patterns of O-2 reordering, and thus the isotopic distribution toward which O-2 is driven in the troposphere. Temporal variations in (36) values at the surface should therefore reflect changes in tropospheric temperatures, photochemistry, and circulation. Our results suggest that the tropospheric O-3 burden has remained within a 10% range since 1978. C1 [Yeung, Laurence Y.] Rice Univ, Dept Earth Sci, Houston, TX 77005 USA. [Murray, Lee T.] NASA Goddard Inst Space Studies, New York, NY USA. [Murray, Lee T.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Murray, Lee T.] Univ Rochester, Dept Earth & Environm Sci, Rochester, NY USA. [Ash, Jeanine L.; Young, Edward D.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA. [Boering, Kristie A.] Univ Calif Berkeley, Dept Chem & Earth & Planetary Sci, Berkeley, CA USA. [Atlas, Elliot L.] Univ Miami, Div Marine & Atmospher Chem, Miami, FL USA. [Schauffler, Sue M.; Lueb, Richard A.] Natl Ctr Atmospher Res, Boulder, CO USA. [Langenfelds, Ray L.; Krummel, Paul. B.; Steele, L. Paul] CSIRO Oceans & Atmosphere, Aspendale, Vic, Australia. [Eastham, Sebastian D.] MIT, Dept Aeronaut & Astronaut, Lab Aviat & Environm, Cambridge, MA USA. RP Yeung, LY (reprint author), Rice Univ, Dept Earth Sci, Houston, TX 77005 USA. EM lyeung@rice.edu RI Steele, Paul/B-3185-2009; Krummel, Paul/A-4293-2013; Chem, GEOS/C-5595-2014; Langenfelds, Raymond/B-5381-2012; Murray, Lee/F-2296-2014; Yeung, Laurence/D-4574-2009 OI Steele, Paul/0000-0002-8234-3730; Krummel, Paul/0000-0002-4884-3678; Murray, Lee/0000-0002-3447-3952; Yeung, Laurence/0000-0001-9901-2607 FU National Science Foundation [EAR-1049655, DGE-1144087]; National Aeronautics and Space Administration Upper Atmosphere Research Program [NNX13AH10G]; Cosmochemistry Program; Deep Carbon Observatory; Rice University faculty startup funds FX We thank A.M. Fiore (Columbia University) for computational resources for simulations, S. Donnelly and R. Hendershot for engineering support, and I. Mellor-Crummey and S. Li for their efforts in construction and testing of the automated O2 sample preparation system at Rice. We also thank D.R. Blake for providing sample aliquots from the DC3 campaign, M. Bender for providing the sample of 1992 air from Niwot Ridge, CO, and M. Aydin and two anonymous reviewers for comments that improved the manuscript. Finally, we thank the staff of the Cape Grim Baseline Air Pollution Station for their diligence in collecting the air archive samples, and the Australian Bureau of Meteorology for their long-term, and ongoing support of the Cape Grim Air Archive. This work was supported in part by the National Science Foundation (EAR-1049655 and DGE-1144087), the National Aeronautics and Space Administration Upper Atmosphere Research Program (NNX13AH10G) and Cosmochemistry Program, the Deep Carbon Observatory, and Rice University faculty startup funds. The laboratory data reported in this study are freely available as supporting information (Table S1). NR 103 TC 0 Z9 0 U1 3 U2 3 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 OCT 27 PY 2016 VL 121 IS 20 BP 12541 EP 12559 DI 10.1002/2016JD025455 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EC7CJ UT WOS:000388293100030 ER PT J AU Chen, DX Huey, LG Tanner, DJ Salawitch, RJ Anderson, DC Wales, PA Pan, LL Atlas, EL Hornbrook, RS Apel, EC Blake, NJ Campos, TL Donets, V Flocke, FM Hall, SR Hanisco, TF Hills, AJ Honomichl, SB Jensen, JB Kaser, L Montzka, DD Nicely, JM Reeves, JM Riemer, DD Schauffler, SM Ullmann, K Weinheimer, AJ Wolfe, GM AF Chen, Dexian Huey, L. Gregory Tanner, David J. Salawitch, Ross J. Anderson, Daniel C. Wales, Pamela A. Pan, Laura L. Atlas, Elliot L. Hornbrook, Rebecca S. Apel, Eric C. Blake, Nicola J. Campos, Teresa L. Donets, Valeria Flocke, Frank M. Hall, Samuel R. Hanisco, Thomas F. Hills, Alan J. Honomichl, Shawn B. Jensen, Jorgen B. Kaser, Lisa Montzka, Denise D. Nicely, Julie M. Reeves, J. Michael Riemer, Daniel D. Schauffler, Sue M. Ullmann, Kirk Weinheimer, Andrew J. Wolfe, Glenn M. TI Airborne measurements of BrO and the sum of HOBr and Br-2 over the Tropical West Pacific from 1 to 15km during the CONvective TRansport of Active Species in the Tropics (CONTRAST) experiment SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE bromine oxide; hypobromous acid; CONTRAST; hydrobromic acid; product gas injection ID IONIZATION MASS-SPECTROMETRY; TROPOPAUSE LAYER; ATMOSPHERIC CHEMISTRY; LOWER STRATOSPHERE; TROPOSPHERIC BRO; DOAS MEASUREMENTS; ORGANIC BROMINE; OZONE LOSS; CHLORINE; ARCTAS AB A chemical ionization mass spectrometer was used to measure BrO and HOBr+Br-2 over the Tropical West Pacific Ocean within the altitude range of 1 to 15km, during the CONvective TRansport of Active Species in the Tropics (CONTRAST) campaign in 2014. Isolated episodes of elevated BrO (up to 6.6pptv) and/or HOBr+Br-2 (up to 7.3pptv) were observed in the tropical free troposphere (TFT) and were associated with biomass burning. However, most of the time we did not observe significant BrO or HOBr+Br-2 in the TFT and the tropical tropopause layer (TTL) above our limits of detection (LOD). The 1min average LOD for BrO ranged from 0.6 to 1.6pptv and for HOBr+Br-2 ranged from 1.3 to 3.5pptv. During one flight, BrO observations from the TTL to the extratropical lowermost stratosphere were used to infer a profile of inorganic bromine (Br-y). Based on this profile, we estimated the product gas injection of bromine species into the stratosphere to be 2pptv. Analysis of Br-y partitioning further indicates that BrO levels are likely very low in the TFT environment and that future studies should target the measurement of HBr or atomic Br. C1 [Chen, Dexian; Huey, L. Gregory; Tanner, David J.] Georgia Tech, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Salawitch, Ross J.; Anderson, Daniel C.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD USA. [Salawitch, Ross J.; Wales, Pamela A.; Nicely, Julie M.] Univ Maryland, Dept Chem & Biochem, College Pk, MD USA. [Salawitch, Ross J.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD USA. [Pan, Laura L.; Hornbrook, Rebecca S.; Apel, Eric C.; Campos, Teresa L.; Flocke, Frank M.; Hall, Samuel R.; Hills, Alan J.; Honomichl, Shawn B.; Jensen, Jorgen B.; Kaser, Lisa; Montzka, Denise D.; Reeves, J. Michael; Schauffler, Sue M.; Ullmann, Kirk; Weinheimer, Andrew J.] Natl Ctr Atmospher Res, Boulder, CO USA. [Atlas, Elliot L.; Donets, Valeria; Riemer, Daniel D.] Univ Miami, Rosenstiel Sch Marine & Atmospher Chem, Coral Gables, FL USA. [Blake, Nicola J.] Univ Calif Irvine, Dept Chem, Irvine, CA USA. [Hanisco, Thomas F.; Nicely, Julie M.; Wolfe, Glenn M.] NASA Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD USA. [Wolfe, Glenn M.] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD USA. RP Huey, LG (reprint author), Georgia Tech, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. EM greg.huey@eas.gatech.edu RI Pan, Laura/A-9296-2008; Salawitch, Ross/B-4605-2009; Wolfe, Glenn/D-5289-2011; Anderson, Daniel/I-4398-2014; OI Pan, Laura/0000-0001-7377-2114; Salawitch, Ross/0000-0001-8597-5832; Anderson, Daniel/0000-0002-9826-9811; Nicely, Julie/0000-0003-4828-0032 FU NSF [1262033, 1261657]; NASA Atmospheric Composition: Modeling and Analysis Program [NNH12ZDA001N-ACMAP]; NSF AGS grant [1261689]; NASA Upper Atmospheric Research Program [NNH12ZDA001N-UACO]; National Science Foundation FX D.C., L.G.H., and D.J.T. were supported by the NSF grant 1262033. R.J.S., P.A.W., D.C. A., and JMN received support from the NASA Atmospheric Composition: Modeling and Analysis Program under NNH12ZDA001N-ACMAP and from NSF under grant 1261657. E.A. and V.T. were supported by the NSF AGS grant 1261689. G.M.W., D.C. A., and T.F.H. received support from the NASA Upper Atmospheric Research Program under NNH12ZDA001N-UACO. The authors would like thank the CONTRAST team and the GV crew. CONTRAST data are available online at http://data.eol.ucar.edu/master_list/?project=CONTRAST. CONTRAST data are managed by the Earth Observing Laboratory of the National Center for Atmospheric Research (NCAR/EOL). NCAR is sponsored by the National Science Foundation. NR 72 TC 2 Z9 2 U1 7 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD OCT 27 PY 2016 VL 121 IS 20 BP 12560 EP 12578 DI 10.1002/2016JD025561 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EC7CJ UT WOS:000388293100039 ER PT J AU Watson, JT Haynie, AC AF Watson, Jordan T. Haynie, Alan C. TI Using Vessel Monitoring System Data to Identify and Characterize Trips Made by Fishing Vessels in the United States North Pacific SO PLoS One LA English DT Article ID POSITIONAL DATA; CLIMATE-CHANGE; FISHERY; LOCATION; PATTERNS; LANDINGS; LOGBOOK; FUTURE; RISK AB Time spent fishing is the effort metric often studied in fisheries but it may under-represent the effort actually expended by fishers. Entire fishing trips, from the time vessels leave port until they return, may prove more useful for examining trends in fleet dynamics, fisher behavior, and fishing costs. However, such trip information is often difficult to resolve. We identified similar to 30,000 trips made by vessels that targeted walleye pollock (Gadus chalcogrammus) in the Eastern Bering Sea from 2008 - 2014 by using vessel monitoring system (VMS) and landings data. We compared estimated trip durations to observer data, which were available for approximately half of trips. Total days at sea were estimated with < 1.5% error and 96.4% of trip durations were either estimated with < 5% error or they were within expected measurement error. With 99% accuracy, we classified trips as fishing for pollock, for another target species, or not fishing. This accuracy lends strong support to the use of our method with unobserved trips across North Pacific fisheries. With individual trips resolved, we examined potential errors in datasets which are often viewed as " the truth." Despite having > 5 million VMS records (timestamps and vessel locations), this study was as much about understanding and managing data errors as it was about characterizing trips. Missing VMS records were pervasive and they strongly influenced our approach. To understand implications of missing data on inference, we simulated removal of VMS records from trips. Removal of records straightened (i. e., shortened) vessel trajectories, and travel distances were underestimated, on average, by 1.5 - 13.4% per trip. Despite this bias, VMS proved robust for trip characterization and for improved quality control of human-recorded data. Our scrutiny of human-reported and VMS data advanced our understanding of the potential utility and challenges facing VMS users globally. C1 [Watson, Jordan T.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, Juneau, AK 99801 USA. [Watson, Jordan T.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Juneau, AK 99801 USA. [Haynie, Alan C.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Resource Ecol & Fisheries Management Div, Seattle, WA 98115 USA. RP Watson, JT (reprint author), NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, Juneau, AK 99801 USA.; Watson, JT (reprint author), Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Juneau, AK 99801 USA. EM jordan.watson@noaa.gov OI Watson, Jordan/0000-0002-1686-0377 FU NOM Fisheries Science and Technology through the Spatial Economics Toolbox for Fisheries (FishSET) Project; North Pacific Research Board Bering Sea Integrated Ecosystem Research Program; Alaska Sea Grant [R/112-04] FX Funding for this project came from NOM Fisheries Science and Technology through the Spatial Economics Toolbox for Fisheries (FishSET) Project, the North Pacific Research Board Bering Sea Integrated Ecosystem Research Program (www.nprb.org/bering-sea-project), and Alaska Sea Grant R/112-04 (www.seagrant.uaf.edu). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 35 TC 0 Z9 0 U1 0 U2 0 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 OCT 27 PY 2016 VL 11 IS 10 DI 10.1371/journal.pone.0165173 PG 20 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EE4VY UT WOS:000389604900050 ER PT J AU Ganeshan, M Wu, DL AF Ganeshan, Manisha Wu, Dong L. TI The open-ocean sensible heat flux and its significance for Arctic boundary layer mixing during early fall SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID COLD-AIR OUTBREAKS; SEA-ICE; CELL CONVECTION; LATE SUMMER; CLOUDS; WINDS; ROLL AB The increasing ice-free area during late summer has transformed the Arctic to a climate system with more dynamic boundary layer (BL) clouds and seasonal sea ice growth. The open-ocean sensible heat flux, a crucial mechanism of excessive ocean heat loss to the atmosphere during the fall freeze season, is speculated to play an important role in the recently observed cloud cover increase and BL instability. However, lack of observations and understanding of the resilience of the proposed mechanisms, especially in relation to meteorological and interannual variability, has left a poorly constrained BL parameterization scheme in Arctic climate models. In this study, we use multi-year Japanese cruise-ship observations from R/V Mirai over the open Arctic Ocean to characterize the surface sensible heat flux (SSHF) during early fall and investigate its contribution to BL turbulence. It is found that mixing by SSHF is favored during episodes of high surface wind speed and is also influenced by the prevailing cloud regime. The deepest BLs and maximum ocean-atmosphere temperature difference are observed during cold air advection (associated with the stratocumulus regime), yet, contrary to previous speculation, the efficiency of sensible heat exchange is low. On the other hand, the SSHF contributes significantly to BL mixing during the uplift (low pressure) followed by the highly stable (stratus) regime. Overall, it can explain similar to 10% of the open-ocean BL height variability, whereas cloud-driven (moisture and radiative) mechanisms appear to be the other dominant source of convective turbulence. Nevertheless, there is strong interannual variability in the relationship between the SSHF and the BL height which can be intensified by the changing occurrence of Arctic climate patterns, such as positive surface wind speed anomalies and more frequent conditions of uplift. This study highlights the need for comprehensive BL observations like the R/V Mirai for better understanding and predicting the dynamic nature of the Arctic climate. C1 [Ganeshan, Manisha] USRA, Goddard Earth Sci Technol & Res Studies & Invest, Greenbelt, MD 20771 USA. [Wu, Dong L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ganeshan, M (reprint author), USRA, Goddard Earth Sci Technol & Res Studies & Invest, Greenbelt, MD 20771 USA. EM mganeshan@usra.edu FU NASA Earth Science GNSS Remote Sensing and Interdisciplinary Research programs FX This work is supported by NASA Earth Science GNSS Remote Sensing and Interdisciplinary Research programs. Data used in this study were acquired during the MR02-K05 Leg 1, MR04-05, MR08-04, MR09-03 Leg 2, MR10-05 Leg 2, and MR13-06 Leg 1 cruises of R/V Mirai, Japan Agency for Marine-Earth Science and Technology. NR 48 TC 0 Z9 0 U1 5 U2 5 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. PD OCT 27 PY 2016 VL 16 IS 20 BP 13173 EP 13184 DI 10.5194/acp-16-13173-2016 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EB1LH UT WOS:000387112800002 ER PT J AU Connor, B Bosch, H McDuffie, J Taylor, T Fu, DJ Frankenberg, C O'Dell, C Payne, VH Gunson, M Pollock, R Hobbs, J Oyafuso, F Jiang, YB AF Connor, Brian Bosch, Hartmut McDuffie, James Taylor, Tommy Fu, Dejian Frankenberg, Christian O'Dell, Chris Payne, Vivienne H. Gunson, Michael Pollock, Randy Hobbs, Jonathan Oyafuso, Fabiano Jiang, Yibo TI Quantification of uncertainties in OCO-2 measurements of XCO2: simulations and linear error analysis SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID CO2 RETRIEVAL ALGORITHM; PARAMETERS; SPACE; BAND; SPECTROSCOPY; VALIDATION; SATELLITE; SHAPES AB We present an analysis of uncertainties in global measurements of the column averaged dry-air mole fraction of CO2 (XCO2) by the NASA Orbiting Carbon Observatory-2 (OCO-2). The analysis is based on our best estimates for uncertainties in the OCO-2 operational algorithm and its inputs, and uses simulated spectra calculated for the actual flight and sounding geometry, with measured atmospheric analyses. The simulations are calculated for land nadir and ocean glint observations. We include errors in measurement, smoothing, interference, and forward model parameters. All types of error are combined to estimate the uncertainty in XCO2 from single soundings, before any attempt at bias correction has been made. From these results we also estimate the "variable error" which differs between soundings, to infer the error in the difference of XCO2 between any two soundings. The most important error sources are aerosol interference, spectroscopy, and instrument calibration. Aerosol is the largest source of variable error. Spectroscopy and calibration, although they are themselves fixed error sources, also produce important variable errors in XCO2. Net variable errors are usually < 1 ppm over ocean and similar to 0.5-2.0 ppm over land. The total error due to all sources is similar to 1.5-3.5 ppm over land and similar to 1.5-2.5 ppm over ocean. C1 [Connor, Brian] BC Sci Consulting, Stony Brook, NY 11790 USA. [Bosch, Hartmut] Univ Leicester, EOS Grp, Dept Phys & Astron, Leicester, Leics, England. [McDuffie, James; Fu, Dejian; Payne, Vivienne H.; Gunson, Michael; Pollock, Randy; Hobbs, Jonathan; Oyafuso, Fabiano; Jiang, Yibo] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Taylor, Tommy; O'Dell, Chris] Cooperat Inst Res Atmosphere, Ft Collins, CO USA. [Frankenberg, Christian] CALTECH, Pasadena, CA 91125 USA. [Bosch, Hartmut] Univ Leicester, NCEO, Leicester, Leics, England. RP Connor, B (reprint author), BC Sci Consulting, Stony Brook, NY 11790 USA. EM bc.scientific.consulting@gmail.com RI Boesch, Hartmut/G-6021-2012; Frankenberg, Christian/A-2944-2013 OI Frankenberg, Christian/0000-0002-0546-5857 FU JPL [1439002, 1518224] FX We thank the following members of the OCO-2 team for support and helpful discussions: Vijay Natraj, Linda Brown, Brian Drouin, Chris Benner, Malathy Devi, and Annmarie Eldering. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The CSU contribution to this work was supported by JPL subcontract 1439002. The contribution by BC Scientific Consulting was supported by JPL subcontract 1518224. NR 28 TC 4 Z9 4 U1 13 U2 13 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. PD OCT 27 PY 2016 VL 9 IS 10 BP 5227 EP 5238 DI 10.5194/amt-9-5227-2016 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EB1LX UT WOS:000387114700001 ER PT J AU Wong, CK Pongetti, TJ Oda, T Rao, P Gurney, KR Newman, S Duren, RM Miller, CE Yung, YL Sander, SP AF Wong, Clare K. Pongetti, Thomas J. Oda, Tom Rao, Preeti Gurney, Kevin R. Newman, Sally Duren, Riley M. Miller, Charles E. Yung, Yuk L. Sander, Stanley P. TI Monthly trends of methane emissions in Los Angeles from 2011 to 2015 inferred by CLARS-FTS observations SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID INVERSE MODELING TECHNIQUE; WASTE-WATER TREATMENT; LIQUID DAIRY MANURE; TOP-DOWN ESTIMATE; SATELLITE-OBSERVATIONS; CALIFORNIA; BASIN; CO2; AGITATION; STORAGE AB This paper presents an analysis of methane emissions from the Los Angeles Basin at monthly timescales across a 4-year time period - from September 2011 to August 2015. Using observations acquired by a ground-based near-infrared remote sensing instrument on Mount Wilson, California, combined with atmospheric CH4-CO2 tracer-tracer correlations, we observed -18 to +22% monthly variability in CH4 : CO2 from the annual mean in the Los Angeles Basin. Top-down estimates of methane emissions for the basin also exhibit significant monthly variability (-19 to +31% from annual mean and a maximum month-to-month change of 47 %). During this period, methane emissions consistently peaked in the late summer/early fall and winter. The estimated annual methane emissions did not show a statistically significant trend over the 2011 to 2015 time period. C1 [Wong, Clare K.; Pongetti, Thomas J.; Rao, Preeti; Duren, Riley M.; Miller, Charles E.; Sander, Stanley P.] CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. [Wong, Clare K.; Newman, Sally; Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Oda, Tom] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA. [Oda, Tom] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD USA. [Gurney, Kevin R.] Arizona State Univ, Sch Life Sci, Tempe, AZ USA. [Wong, Clare K.] Calif State Univ Northridge, Northridge, CA 91330 USA. RP Wong, CK (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.; Wong, CK (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.; Wong, CK (reprint author), Calif State Univ Northridge, Northridge, CA 91330 USA. EM wclare@gmail.com FU California Air Resources Board; NIST GHG and Climate Science Program; W. M. Keck Institute FX The research in this study was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Clare K. Wong thanks the California Air Resources Board, NIST GHG and Climate Science Program, and the W. M. Keck Institute for Space Studies for support. The authors would like to acknowledge our colleagues at JPL and California Institute of Technology, and Risa Patarasuk at Arizona State University for helpful comments and suggestions. NR 32 TC 2 Z9 2 U1 7 U2 7 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. PD OCT 26 PY 2016 VL 16 IS 20 BP 13121 EP 13130 DI 10.5194/acp-16-13121-2016 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EB1LC UT WOS:000387112200003 ER PT J AU Tinto, M de Araujo, JCN AF Tinto, Massimo de Araujo, Jose C. N. TI Coherent observations of gravitational radiation with LISA and gLISA SO PHYSICAL REVIEW D LA English DT Article ID WAVES AB The geosynchronous Laser Interferometer Space Antenna (gLISA) is a space-based gravitational wave (GW) mission that, for the past 5 years, has been under joint study at the Jet Propulsion Laboratory; Stanford University; the National Institute for Space Research (I.N.P.E., Brazil); and Space Systems Loral. If flown at the same time as the LISA mission, the two arrays will deliver a joint sensitivity that accounts for the best performance of both missions in their respective parts of the millihertz band. This simultaneous operation will result in an optimally combined sensitivity curve that is "white" from about 3 x 10(-3) Hz to 1 Hz, making the two antennas capable of detecting, with high signal-to-noise ratios (SNRs), coalescing black-hole binaries (BHBs) with masses in the range (10 - 10(8))M-circle dot. Their ability of jointly tracking, with enhanced SNR, signals similar to that observed by the Advanced Laser Interferometer Gravitational Wave Observatory (aLIGO) on September 14, 2015 (the GW150914 event) will result in a larger number of observable small-mass binary black holes and an improved precision of the parameters characterizing these sources. Together, LISA, gLISA and aLIGO will cover, with good sensitivity, the (10(-4) - 10(3)) Hz frequency band. C1 [Tinto, Massimo] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [de Araujo, Jose C. N.] Inst Nacl Pesquisas Espaciais, Div Astrofis, Ave Astronautas 1758, BR-12227010 Sao Paulo, Brazil. RP Tinto, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.; de Araujo, JCN (reprint author), Inst Nacl Pesquisas Espaciais, Div Astrofis, Ave Astronautas 1758, BR-12227010 Sao Paulo, Brazil. EM massimo.tinto@jpl.nasa.gov; jcarlos.dearaujo@inpe.br FU FAPESP [2013/26258-4]; CNPq [308983/2013-0]; Topic Research and Technology Development program of the Jet Propulsion laboratory FX M. T. would like to thank Professor Daniel DeBra and Dr. Sasha Buchman for many stimulating conversations about the gLISA mission concept, Dr. John W. Armstrong for reading the manuscript and his valuable comments, and Dr. Anthony Freeman and Dr. Daniel McCleese for their constant encouragement. M. T. also acknowledges financial support through the Topic Research and Technology Development program of the Jet Propulsion laboratory. J. C. N. A. acknowledges partial support from FAPESP (2013/26258-4) and CNPq (308983/2013-0). This research was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 21 TC 0 Z9 0 U1 1 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD OCT 26 PY 2016 VL 94 IS 8 AR 081101 DI 10.1103/PhysRevD.94.081101 PG 5 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA EB1NT UT WOS:000387120400001 ER PT J AU Meador, MAB Agnello, M McCorkle, L Vivod, SL Wilmoth, N AF Meador, Mary Ann B. Agnello, Marika McCorkle, Linda Vivod, Stephanie L. Wilmoth, Nathan TI Moisture-Resistant Polyimide Aerogels Containing Propylene Oxide Links in the Backbone SO ACS APPLIED MATERIALS & INTERFACES LA English DT Article DE aerogel; polyimide; mesoporous; cross-linked; insulation; hydrophobic ID MECHANICALLY STRONG; ADSORPTION AB Polyimide aerogels made using anhydride capped oligomers from 4,4'-oxydianiline (ODA) and 3,3',4,4'-biphenyltetracarboxylic dianhydride (BPDA) cross-linked with 1,3,5-tri(aminophenoxy)benzene (TAB) have been reported with very good mechanical properties but poor resistance to moisture. Replacing 50 mol % of the ODA with poly(propylene glycol)bis(2-aminopropyl ether) (PPG) with an average molecular weight of 230 g/mol in the oligomer backbone gives aerogels with water contact angles of 80 degrees. The aerogels also absorb very little moisture on soaking in water. The aerogels also shrink less with increasing PPG concentration and therefore have significantly lower density and higher porosity than those made without PPG. Mechanical properties of the aerogels increased with increasing density, regardless of the polymer backbone. Brunauer-Emmett-Teller (BET) surface area of the aerogels studied ranged from 300 to 400 m(2)/g, depending mainly on PPG concentration. The high moisture resistance makes them promising materials for substrates for lightweight antennas as well as insulation for a variety of applications. C1 [Meador, Mary Ann B.; Agnello, Marika; McCorkle, Linda; Vivod, Stephanie L.; Wilmoth, Nathan] NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. RP Meador, MAB (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM maryann.meador@nasa.gov OI Meador, Mary Ann/0000-0003-2513-7372 FU National Aeronautic and Space Administration's Space Technology Mission Directorate Game Changing Development Program FX The authors are grateful for support from the National Aeronautic and Space Administration's Space Technology Mission Directorate Game Changing Development Program. We also thank Daniel Scheiman (Ohio Aerospace Institute) for thermal analysis and FT-IR and Baochau Nguyen (Ohio Aerospace Institute) for solid NMR and nitrogen sorption measurements. NR 20 TC 1 Z9 1 U1 31 U2 31 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1944-8244 J9 ACS APPL MATER INTER JI ACS Appl. Mater. Interfaces PD OCT 26 PY 2016 VL 8 IS 42 BP 29073 EP 29079 DI 10.1021/acsami.6b10248 PG 7 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Science & Technology - Other Topics; Materials Science GA EA3WP UT WOS:000386540300090 ER PT J AU Steffen, JH Coughlin, JL AF Steffen, Jason H. Coughlin, Jeffrey L. TI A Population of planetary systems characterized by short-period, Earth-sized planets SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE exoplanets; Kepler; planetary systems ID MULTIPLANET SYSTEMS; EXOPLANETARY SYSTEMS; EXTRASOLAR PLANETS; GIANT PLANETS; HOT JUPITERS; SUPER-EARTHS; KEPLER; MASS; ARCHITECTURE; EVAPORATION AB We analyze data from the Quarter 1-17 Data Release 24 (Q1-Q17 DR24) planet candidate catalog from NASA's Kepler mission, specifically comparing systems with single transiting planets to systems with multiple transiting planets, and identify a population of exoplanets with a necessarily distinct system architecture. Such an architecture likely indicates a different branch in their evolutionary past relative to the typical Kepler system. The key feature of these planetary systems is an isolated, Earth-sized planet with a roughly 1-d orbital period. We estimate that at least 24 of the 144 systems we examined (greater than or similar to 17%) are members of this population. Accounting for detection efficiency, such planetary systems occur with a frequency similar to the hot Jupiters. C1 [Steffen, Jason H.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. [Coughlin, Jeffrey L.] SETI Inst, Mountain View, CA 94043 USA. [Coughlin, Jeffrey L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Steffen, JH (reprint author), Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. EM jason.steffen@unlv.edu FU NASA [NNH12ZDA001N-KPS, NNH13ZDA001N-OSS, NNX13AD01A] FX J.H.S. thanks the Kepler multibody working group, Jason Rowe, Jason Hwang, and Chris Burke for ongoing discussions and the members of the Kepler Science Office for their work preparing the Kepler data products and catalogs. J.H.S. is supported by NASA under Grant NNH12ZDA001N-KPS issued through the Kepler Participating Scientist Program and Grant NNH13ZDA001N-OSS issued through the Origins of Solar Systems program. J.L.C. is supported by NASA Grant NNX13AD01A. This research made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with NASA under the Exoplanet Exploration Program. NR 45 TC 0 Z9 0 U1 1 U2 1 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD OCT 25 PY 2016 VL 113 IS 43 BP 12023 EP 12028 DI 10.1073/pnas.1606658113 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DZ7ZI UT WOS:000386087100035 PM 27790984 ER PT J AU Khazendar, A Rignot, E Schroeder, DM Seroussi, H Schodlok, MP Scheuchl, B Mouginot, J Sutterley, TC Velicogna, I AF Khazendar, Ala Rignot, Eric Schroeder, Dustin M. Seroussi, Helene Schodlok, Michael P. Scheuchl, Bernd Mouginot, Jeremie Sutterley, Tyler C. Velicogna, Isabella TI Rapid submarine ice melting in the grounding zones of ice shelves in West Antarctica SO NATURE COMMUNICATIONS LA English DT Article ID PINE ISLAND GLACIER; AMUNDSEN SEA EMBAYMENT; THWAITES GLACIER; LASER ALTIMETRY; DEEP-WATER; MASS-LOSS; RADAR; GREENLAND; SENSITIVITY; RETREAT AB Enhanced submarine ice-shelf melting strongly controls ice loss in the Amundsen Sea embayment (ASE) of West Antarctica, but its magnitude is not well known in the critical grounding zones of the ASE's major glaciers. Here we directly quantify bottom ice losses along tens of kilometres with airborne radar sounding of the Dotson and Crosson ice shelves, which buttress the rapidly changing Smith, Pope and Kohler glaciers. Melting in the grounding zones is found to be much higher than steady-state levels, removing 300-490m of solid ice between 2002 and 2009 beneath the retreating Smith Glacier. The vigorous, unbalanced melting supports the hypothesis that a significant increase in ocean heat influx into ASE sub-ice-shelf cavities took place in the mid-2000s. The synchronous but diverse evolutions of these glaciers illustrate how combinations of oceanography and topography modulate rapid submarine melting to hasten mass loss and glacier retreat from West Antarctica. C1 [Khazendar, Ala; Rignot, Eric; Schroeder, Dustin M.; Seroussi, Helene; Schodlok, Michael P.; Velicogna, Isabella] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Rignot, Eric; Scheuchl, Bernd; Mouginot, Jeremie; Sutterley, Tyler C.; Velicogna, Isabella] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. RP Khazendar, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ala@jpl.nasa.gov RI Sutterley, Tyler/Q-8325-2016; OI Sutterley, Tyler/0000-0002-6964-1194; Rignot, Eric/0000-0002-3366-0481 FU NASA's Cryospheric Sciences Program; NASA's Cryospheric Sciences Program at UC Irvine [NNX14AB93G, NNX13AN46G, NNX14AN03G] FX A.K. was supported by NASA's Cryospheric Sciences Program. E.R., B.S. and J.M. were funded by research grants NNX14AB93G, NNX13AN46G and NNX14AN03G from NASA's Cryospheric Sciences Program at UC Irvine. This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 50 TC 1 Z9 1 U1 22 U2 22 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD OCT 25 PY 2016 VL 7 AR 13243 DI 10.1038/ncomms13243 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DZ6VX UT WOS:000386001800001 PM 27780191 ER PT J AU Egedal, J Le, A Daughton, W Wetherton, B Cassak, PA Chen, LJ Lavraud, B Torbert, RB Dorelli, J Gershman, DJ Avanov, LA AF Egedal, J. Le, A. Daughton, W. Wetherton, B. Cassak, P. A. Chen, L. -J Lavraud, B. Torbert, R. B. Dorelli, J. Gershman, D. J. Avanov, L. A. TI Spacecraft Observations and Analytic Theory of Crescent-Shaped Electron Distributions in Asymmetric Magnetic Reconnection SO PHYSICAL REVIEW LETTERS LA English DT Article ID DIFFUSION REGION; MAGNETOPAUSE; MAGNETOTAIL AB Supported by a kinetic simulation, we derive an exclusion energy parameter EX providing a lower kinetic energy bound for an electron to cross from one inflow region to the other during magnetic reconnection. As by a Maxwell demon, only high-energy electrons are permitted to cross the inner reconnection region, setting the electron distribution function observed along the low-density side separatrix during asymmetric reconnection. The analytic model accounts for the two distinct flavors of crescent-shaped electron distributions observed by spacecraft in a thin boundary layer along the low-density separatrix. C1 [Egedal, J.; Wetherton, B.] Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA. [Le, A.; Daughton, W.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Cassak, P. A.] West Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA. [Chen, L. -J; Dorelli, J.; Gershman, D. J.; Avanov, L. A.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lavraud, B.] Univ Toulouse, Inst Rech Astrophys & Planetol, Toulouse, France. [Lavraud, B.] CNRS, UMR 5277, Toulouse, France. [Torbert, R. B.] Univ New Hampshire, Durham, NH 03824 USA. RP Egedal, J (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA. OI Wetherton, Blake/0000-0003-2723-7190 FU National Science Foundation (NSF) Geospace Environment Modeling Grant [1405166]; NASA [NNX16AF75G, NNX16AG76G, NNX14AL38G]; Centre national de la recherche scientifique (CNRS); Centre national d'etudes spatiales (CNES) FX J. E. acknowledges the support by the National Science Foundation (NSF) Geospace Environment Modeling Grant No. 1405166, P. A. C. was supported by NASA Grants No. NNX16AF75G and No. NNX16AG76G, B. L. was supported by Centre national de la recherche scientifique (CNRS) and Centre national d'etudes spatiales (CNES), while A. L. acknowledges NASA Grant No. NNX14AL38G, and simulations used NASA High End Computing program and Los Alamos National Laboratory IC resources. NR 26 TC 3 Z9 3 U1 1 U2 1 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 OCT 24 PY 2016 VL 117 IS 18 AR 185101 DI 10.1103/PhysRevLett.117.185101 PG 5 WC Physics, Multidisciplinary SC Physics GA EF3KV UT WOS:000390224200005 PM 27835028 ER PT J AU Ialongo, I Herman, J Krotkov, N Lamsal, L Boersma, KF Hovila, J Tamminen, J AF Ialongo, Iolanda Herman, Jay Krotkov, Nick Lamsal, Lok Boersma, K. Folkert Hovila, Jari Tamminen, Johanna TI Comparison of OMI NO2 observations and their seasonal and weekly cycles with ground-based measurements in Helsinki SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID OZONE MONITORING INSTRUMENT; TROPOSPHERIC NO2; SATELLITE RETRIEVALS; NITROGEN-DIOXIDE; SURFACE MEASUREMENTS; POWER-PLANTS; IN-SITU; EMISSIONS; ALGORITHM; LIFETIMES AB We present the comparison of satellite-based OMI (Ozone Monitoring Instrument) NO2 products with ground-based observations in Helsinki. OMI NO2 total columns, available from NASA's standard product (SP) and KNMI DOMINO product, are compared with the measurements performed by the Pandora spectrometer in Helsinki in 2012. The relative difference between Pandora no. 21 and OMI SP total columns is 4 and 6% for clear-sky and all-sky conditions, respectively. DOMINO NO2 retrievals showed slightly lower total columns with median differences about -5 and -14% for clear-sky and all-sky conditions, respectively. Large differences often correspond to cloudy fallwinter days with solar zenith angles above 65 degrees. Nevertheless, the differences remain within the retrieval uncertainties. The average difference values are likely the result of different factors partly canceling each other: the overestimation of the stratospheric columns causes a positive bias partly compensated by the limited spatial representativeness of the relatively coarse OMI pixel for sharp NO2 gradients. The comparison between Pandora and the new version (V3) of OMI NO2 retrievals shows a larger negative difference (about 30 %) than the current version (V2.1) because the revised spectral fitting procedure reduces the overestimation of the stratospheric column. The weekly and seasonal cycles from OMI, Pandora and NO2 surface concentrations are also compared. Both satellite-and ground-based data show a similar weekly cycle, with lower NO2 levels during the weekend compared to the weekdays as a result of reduced emissions from traffic and industrial activities. The seasonal cycle also shows a similar behavior, even though the results are affected by the fact that most of the data are available during spring-summer because of cloud cover in other seasons. This is one of few works in which OMI NO2 retrievals are evaluated in a urban site at high latitudes (60 degrees N). Despite the city of Helsinki having relatively small pollution sources, OMI retrievals have proved to be able to describe air quality features and variability similar to surface observations. This adds confidence in using satellite observations for air quality monitoring also at high latitudes. C1 [Ialongo, Iolanda; Hovila, Jari; Tamminen, Johanna] Finnish Meteorol Inst, Earth Observat Unit, Helsinki, Finland. [Herman, Jay; Krotkov, Nick; Lamsal, Lok] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD USA. [Lamsal, Lok] Univ Space Res Assoc, GESTAR, Columbia, MD USA. [Boersma, K. Folkert] Royal Netherlands Meteorol Inst, Climate Observat Dept, De Bilt, Netherlands. [Boersma, K. Folkert] Wageningen Univ, Meteorol & Air Qual Grp, Wageningen, Netherlands. RP Ialongo, I (reprint author), Finnish Meteorol Inst, Earth Observat Unit, Helsinki, Finland. EM iolanda.ialongo@fmi.fi RI Boersma, Klaas/H-4559-2012; Ialongo, Iolanda/E-1638-2014; Tamminen, Johanna/D-7959-2014 OI Boersma, Klaas/0000-0002-4591-7635; Tamminen, Johanna/0000-0003-3095-0069 FU Academy of Finland; EU-FP7 grant [QA4ECV, 607405]; NASA Earth Science Division; KNMI FX This work of Iolanda Ialongo was founded by the ILMA project (Applications of NO2 satellite observations at high latitudes for monitoring air quality) within the ESA Living Planet Programme. Johanna Tamminen was partially funded by the Academy of Finland project INQUIRE. Folkert Boersma acknowledges support by the EU-FP7 grant QA4ECV (no. 607405). The authors acknowledge the NASA Earth Science Division and KNMI for funding the OMI NO2 development and the archiving of standard and DOMINO products, respectively. The authors also thank the Atmospheric Sciences department of the University of Helsinki for providing surface concentration measurements through the SmartSMEAR download tool. NR 42 TC 0 Z9 0 U1 7 U2 7 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. PD OCT 24 PY 2016 VL 9 IS 10 BP 5203 EP 5212 DI 10.5194/amt-9-5203-2016 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EA6XF UT WOS:000386771700003 ER PT J AU Yang, CY Liu, JP Hu, YY Horton, RM Chen, LQ Cheng, X AF Yang, Chao-Yuan Liu, Jiping Hu, Yongyun Horton, Radley M. Chen, Liqi Cheng, Xiao TI Assessment of Arctic and Antarctic sea ice predictability in CMIP5 decadal hindcasts SO CRYOSPHERE LA English DT Article ID MERIDIONAL OVERTURNING CIRCULATION; NORTH-ATLANTIC; SOUTHERN-OCEAN; CLIMATE MODEL; BERING-SEA; VARIABILITY; PREDICTION; TRENDS; EXTENT; TEMPERATURE AB This paper examines the ability of coupled global climate models to predict decadal variability of Arctic and Antarctic sea ice. We analyze decadal hindcasts/predictions of 11 Coupled Model Intercomparison Project Phase 5 (CMIP5) models. Decadal hindcasts exhibit a large multimodel spread in the simulated sea ice extent, with some models deviating significantly from the observations as the predicted ice extent quickly drifts away from the initial constraint. The anomaly correlation analysis between the decadal hindcast and observed sea ice suggests that in the Arctic, for most models, the areas showing significant predictive skill become broader associated with increasing lead times. This area expansion is largely because nearly all the models are capable of predicting the observed decreasing Arctic sea ice cover. Sea ice extent in the North Pacific has better predictive skill than that in the North Atlantic (particularly at a lead time of 3-7 years), but there is a reemerging predictive skill in the North Atlantic at a lead time of 6-8 years. In contrast to the Arctic, Antarctic sea ice decadal hindcasts do not show broad predictive skill at any timescales, and there is no obvious improvement linking the areal extent of significant predictive skill to lead time increase. This might be because nearly all the models predict a retreating Antarctic sea ice cover, opposite to the observations. For the Arctic, the predictive skill of the multi-model ensemble mean outperforms most models and the persistence prediction at longer timescales, which is not the case for the Antarctic. Overall, for the Arctic, initialized decadal hindcasts show improved predictive skill compared to uninitialized simulations, although this improvement is not present in the Antarctic. C1 [Yang, Chao-Yuan; Liu, Jiping] SUNY Albany, Dept Atmospher & Environm Sci, Albany, NY 12222 USA. [Hu, Yongyun] Peking Univ, Sch Phys, Dept Atmospher & Ocean Sci, Beijing, Peoples R China. [Horton, Radley M.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Horton, Radley M.] NASA Goddard Inst Space Studies, New York, NY USA. [Chen, Liqi] SOA, Inst Oceanog 3, Key Lab Global Change & Marine Atmospher Chem, Xiamen, Peoples R China. [Cheng, Xiao] Beijing Normal Univ, Coll Global Change & Earth Syst Sci, Beijing, Peoples R China. RP Yang, CY (reprint author), SUNY Albany, Dept Atmospher & Environm Sci, Albany, NY 12222 USA. EM cyang4@albany.edu FU NOAA Climate Program Office [NA15OAR4310163, NA14OAR4310216]; NSFC [41676185] FX This research is supported by the NOAA Climate Program Office (NA15OAR4310163 and NA14OAR4310216) and the NSFC (41676185). NR 95 TC 0 Z9 0 U1 10 U2 10 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1994-0416 EI 1994-0424 J9 CRYOSPHERE JI Cryosphere PD OCT 21 PY 2016 VL 10 IS 5 BP 2429 EP 2452 DI 10.5194/tc-10-2429-2016 PG 24 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA EA6YI UT WOS:000386774700001 ER PT J AU Abbott, BP Abbott, R Abbott, TD Abernathy, MR Acernese, F Ackley, K Adams, C Adams, T Addesso, P Adhikari, RX Adya, VB Affeldt, C Agathos, M Agatsuma, K Aggarwal, N Aguiar, OD Aiello, L Ain, A Ajith, P Allen, B Allocca, A Altin, PA Anderson, SB Anderson, WG Arai, K Araya, MC Arceneaux, CC Areeda, JS Arnaud, N Arun, KG Ascenzi, S Ashton, G Ast, M Aston, SM Astone, P Aufmuth, P Aulbert, C Babak, S Bacon, P Bader, MKM Baker, PT Baldaccini, F Ballardin, G Ballmer, SW Barayoga, JC Barclay, SE Barish, BC Barker, D Barone, F Barr, B Barsotti, L Barsuglia, M Barta, D Bartlett, J Bartos, I Bassiri, R Basti, A Batch, JC Baune, C Bavigadda, V Bazzan, M Bejger, M Bell, AS Berger, BK Bergmann, G Berry, CPL Bersanetti, D Bertolini, A Betzwieser, J Bhagwat, S Bhandare, R Bilenko, IA Billingsley, G Birch, J Birney, R Birnholtz, O Biscans, S Bisht, A Bitossi, M Biwer, C Bizouard, MA Blackburn, JK Blair, CD Blair, DG Blair, RM Bloemen, S Bock, O Boer, M Bogaert, G Bogan, C Bohe, A Bond, C Bondu, F Bonnand, R Boom, BA Bork, R Boschi, V Bose, S Bouffanais, Y Bozzi, A Bradaschia, C Brady, PR Braginsky, VB Branchesi, M Brau, JE Briant, T Brillet, A Brinkmann, M Brisson, V Brockill, P Broida, JE Brooks, AF Brown, DA Brown, DD Brown, NM Brunett, S Buchanan, CC Buikema, A Bulik, T Bulten, HJ Buonanno, A Buskulic, D Buy, C Byer, RL Cabero, M Cadonati, L Cagnoli, G Cahillane, C Bustillo, JC Callister, T Calloni, E Camp, JB Cannon, KC Cao, J Capano, CD Capocasa, E Carbognani, F Caride, S Diaz, JC Casentini, C Caudill, S Cavaglia, M Cavalier, F Cella, G Cepeda, CB Baiardi, LC Cerretani, G Cesarini, E Chamberlin, SJ Chan, M Chao, S Charlton, P Chassande-Mottin, E Cheeseboro, BD Chen, HY Chen, Y Cheng, C Chincarini, A Chiummo, A Cho, HS Cho, M Chow, JH Christensen, N Chu, Q Chua, S Chung, S Ciani, G Clara, F Clark, JA Cleva, F Coccia, E Cohadon, PF Colla, A Collette, CG Cominsky, L Constancio, M Conte, A Conti, L Cook, D Corbitt, TR Cornish, N Corsi, A Cortese, S Costa, CA Coughlin, MW Coughlin, SB Coulon, JP Countryman, ST Couvares, P Cowan, EE Coward, DM Cowart, MJ Coyne, DC Coyne, R Craig, K Creighton, JDE Cripe, J Crowder, SG Cumming, A Cunningham, L Cuoco, E Dal Canton, T Danilishin, SL D'Antonio, S Danzmann, K Darman, NS Dasgupta, A Da Silva Costa, CF Dattilo, V Dave, I Davier, M Davies, GS Daw, EJ Day, R De, S DeBra, D Debreczeni, G Degallaix, J De Laurentis, M Deleglise, S Del Pozzo, W Denker, T Dent, T Dergachev, V De Rosa, R DeRosa, RT DeSalvo, R Devine, RC Dhurandhar, S Diaz, MC Di Fiore, L Di Giovanni, M Di Girolamo, T Di Lieto, A Di Pace, S Di Palma, I Di Virgilio, A Dolique, V Donovan, F Dooley, KL Doravari, S Douglas, R Downes, TP Drago, M Drever, RWP Driggers, JC Ducrot, M Dwyer, SE Edo, TB Edwards, MC Effler, A Eggenstein, HB Ehrens, P Eichholz, J Eikenberry, SS Engels, W Essick, RC Etzel, T Evans, M Evans, TM Everett, R Factourovich, M Fafone, V Fair, H Fairhurst, S Fan, X Fang, Q Farinon, S Farr, B Farr, WM Favata, M Fays, M Fehrmann, H Fejer, MM Fenyvesi, E Ferrante, I Ferreira, EC Ferrini, F Fidecaro, F Fiori, I Fiorucci, D Fisher, RP Flaminio, R Fletcher, M Fong, H Fournier, JD Frasca, S Frasconi, F Frei, Z Freise, A Frey, R Frey, V Fritschel, P Frolov, VV Fulda, P Fyffe, M Gabbard, HAG Gaebel, S Gair, JR Gammaitoni, L Gaonkar, SG Garufi, F Gaur, G Gehrels, N Gemme, G Geng, P Genin, E Gennai, A George, J Gergely, L Germain, V Ghosh, A Ghosh, A Ghosh, S Giaime, JA Giardina, KD Giazotto, A Gill, K Glaefke, A Goetz, E Goetz, R Gondan, L Gonzalez, G Castro, JMG Gopakumar, A Gordon, NA Gorodetsky, ML Gossan, SE Gosselin, M Gouaty, R Grado, A Graef, C Graff, PB Granata, M Grant, A Gras, S Gray, C Greco, G Green, AC Groot, P Grote, H Grunewald, S Guidi, GM Guo, X Gupta, A Gupta, MK Gushwa, KE Gustafson, EK Gustafson, R Hacker, JJ Hall, BR Hall, ED Hamilton, H Hammond, G Haney, M Hanke, MM Hanks, J Hanna, C Hannam, MD Hanson, J Hardwick, T Harms, J Harry, GM Harry, IW Hart, MJ Hartman, MT Haster, CJ Haughian, K Healy, J Heidmann, A Heintze, MC Heitmann, H Hello, P Hemming, G Hendry, M Heng, IS Hennig, J Henry, J Heptonstall, AW Heurs, M Hild, S Hoak, D Hofman, D Holt, K Holz, DE Hopkins, P Hough, J Houston, EA Howell, EJ Hu, YM Huang, S Huerta, EA Huet, D Hughey, B Husa, S Huttner, SH Huynh-Dinh, T Indik, N Ingram, DR Inta, R Isa, HN Isac, JM Isi, M Isogai, T Iyer, BR Izumi, K Jacqmin, T Jang, H Jani, K Jaranowski, P Jawahar, S Jian, L Jimenez-Forteza, F Johnson, WW Johnson-McDaniel, NK Jones, DI Jones, R Jonker, RJG Ju, L Haris, K Kalaghatgi, CV Kalogera, V Kandhasamy, S Kang, G Kanner, JB Kapadia, SJ Karki, S Karvinen, KS Kasprzack, M Katsavounidis, E Katzman, W Kaufer, S Kaur, T Kawabe, K Kefelian, F Kehl, MS Keitel, D Kelley, DB Kells, W Kennedy, R Key, JS Khalili, FY Khan, I Khan, S Khan, Z Khazanov, EA Kijbunchoo, N Kim, CW Kim, C Kim, J Kim, K Kim, N Kim, W Kim, YM Kimbrell, SJ King, EJ King, PJ Kissel, JS Klein, B Kleybolte, L Klimenko, S Koehlenbeck, SM Koley, S Kondrashov, V Kontos, A Korobko, M Korth, WZ Kowalska, I Kozak, DB Kringel, V Krishnan, B Krolak, A Krueger, C Kuehn, G Kumar, P Kumar, R Kuo, L Kutynia, A Lackey, BD Landry, M Lange, J Lantz, B Lasky, PD Laxen, M Lazzarini, A Lazzaro, C Leaci, P Leavey, S Lebigot, EO Lee, CH Lee, HK Lee, HM Lee, K Lenon, A Leonardi, M Leong, JR Leroy, N Letendre, N Levin, Y Lewis, JB Li, TGF Libson, A Littenberg, TB Lockerbie, NA Lombardi, AL London, LT Lord, JE Lorenzini, M Loriette, V Lormand, M Losurdo, G Lough, JD Lousto, C Luck, H Lundgren, AP Lynch, R Ma, Y Machenschalk, B MacInnis, M Macleod, DM Magana-Sandoval, F Zertuche, LM Magee, RM Majorana, E Maksimovic, I Malvezzi, V Man, N Mandel, I Mandic, V Mangano, V Mansell, GL Manske, M Mantovani, M Marchesoni, F Marion, F Marka, S Marka, Z Markosyan, AS Maros, E Martelli, F Martellini, L Martin, IW Martynov, DV Marx, JN Mason, K Masserot, A Massinger, TJ Masso-Reid, M Mastrogiovanni, S Matichard, F Matone, L Mavalvala, N Mazumder, N McCarthy, R McClelland, DE McCormick, S McGuire, SC McIntyre, G McIver, J McManus, DJ Mcrae, T McWilliams, ST Meacher, D Meadors, GD Meidam, J Melatos, A Mendell, G Mercer, RA Merilh, EL Merzougui, M Meshkov, S Messenger, C Messick, C Metzdorff, R Meyers, PM Mezzani, F Miao, H Michel, C Middleton, H Mikhailov, EE Milano, L Miller, AL Miller, A Miller, BB Miller, J Millhouse, M Minenkov, Y Ming, J Mirshekari, S Mishra, C Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Moggi, A Mohan, M Mohapatra, SRP Montani, M Moore, BC Moore, CJ Moraru, D Moreno, G Morriss, SR Mossavi, K Mours, B Mow-Lowry, CM Mueller, G Muir, AW Mukherjee, A Mukherjee, D Mukherjee, S Mukund, N Mullavey, A Munch, J Murphy, DJ Murray, PG Mytidis, A Nardecchia, I Naticchioni, L Nayak, RK Nedkova, K Nelemans, G Nelson, TJN Neri, M Neunzert, A Newton, G Nguyen, TT Nielsen, AB Nissanke, S Nitz, A Nocera, F Nolting, D Normandin, MEN Nuttall, LK Oberling, J Ochsner, E O'Dell, J Oelker, E Ogin, GH Oh, JJ Oh, SH Ohme, F Oliver, M Oppermann, P Oram, RJ O'Reilly, B O'Shaughnessy, R Ottaway, DJ Overmier, H Owen, BJ Pai, A Pai, SA Palamos, JR Palashov, O Palomba, C Pal-Singh, A Pan, H Pan, Y Pankow, C Pannarale, F Pant, BC Paoletti, F Paoli, A Papa, MA Paris, HR Parker, W Pascucci, D Pasqualetti, A Passaquieti, R Passuello, D Patricelli, B Patrick, Z Pearlstone, BL Pedraza, M Pedurand, R Pekowsky, L Pele, A Penn, S Perreca, A Perri, LM Pfeiffer, HP Phelps, M Piccinni, OJ Pichot, M Piergiovanni, F Pierro, V Pillant, G Pinard, L Pinto, IM Pitkin, M Poe, M Poggiani, R Popolizio, P Porter, E Post, A Powell, J Prasad, J Predoi, V Prestegard, T Price, LR Prijatelj, M Principe, M Privitera, S Prix, R Prodi, GA Prokhorov, L Puncken, O Punturo, M Puppo, P Purrer, M Qi, H Qin, J Qiu, S Quetschke, V Quintero, EA Quitzow-James, R Raab, FJ Rabeling, DS Radkins, H Raffai, P Raja, S Rajan, C Rakhmanov, M Rapagnani, P Raymond, V Razzano, M Re, V Read, J Reed, CM Regimbau, T Rei, L Reid, S Reitze, DH Rew, H Reyes, SD Ricci, F Riles, K Rizzo, M Robertson, NA Robie, R Robinet, F Rocchi, A Rolland, L Rollins, JG Roma, VJ Romano, JD Romano, R Romanov, G Romie, JH Rosinska, D Rowan, S Rudiger, A Ruggi, P Ryan, K Sachdev, S Sadecki, T Sadeghian, L Sakellariadou, M Salconi, L Saleem, M Salemi, F Samajdar, A Sammut, L Sanchez, EJ Sandberg, V Sandeen, B Sanders, JR Sassolas, B Sathyaprakash, BS Saulson, PR Sauter, OES Savage, RL Sawadsky, A Schale, P Schilling, R Schmidt, J Schmidt, P Schnabel, R Schofield, RMS Schoenbeck, A Schuette, D Schutz, BF Scott, J Scott, SM Sellers, D Sengupta, AS Sentenac, D Sequino, V Sergeev, A Setyawati, Y Shaddock, DA Shaffer, T Shahriar, MS Shaltev, M Shapiro, B Shawhan, P Sheperd, A Shoemaker, DH Shoemaker, DM Siellez, K Siemens, X Sieniawska, M Sigg, D Silva, AD Singer, A Singer, LP Singh, A Singh, R Singhal, A Sintes, AM Slagmolen, BJJ Smith, JR Smith, ND Smith, RJE Son, EJ Sorazu, B Sorrentino, F Souradeep, T Srivastava, AK Staley, A Steinke, M Steinlechner, J Steinlechner, S Steinmeyer, D Stephens, BC Stevenson, S Stone, R Strain, KA Straniero, N Stratta, G Strauss, NA Strigin, S Sturani, R Stuver, AL Summerscales, TZ Sun, L Sunil, S Sutton, PJ Swinkels, BL Szczepanczyk, MJ Tacca, M Talukder, D Tanner, DB Tapai, M Tarabrin, SP Taracchini, A Taylor, R Theeg, T Thirugnanasambandam, MP Thomas, EG Thomas, M Thomas, P Thorne, KA Thrane, E Tiwari, S Tiwari, V Tokmakov, KV Toland, K Tomlinson, C Tonelli, M Tornasi, Z Torres, CV Torrie, CI Toyra, D Travasso, F Traylor, G Trifiro, D Tringali, MC Trozzo, L Tse, M Turconi, M Tuyenbayev, D Ugolini, D Unnikrishnan, CS Urban, AL Usman, SA Vahlbruch, H Vajente, G Valdes, G Vallisneri, M van Bakel, N van Beuzekom, M van den Brand, JFJ van Den Broeck, C Vander-Hyde, DC van der Schaaf, L van Heijningen, JV van Veggel, AA Vardaro, M Vass, S Vasuth, M Vaulin, R Vecchio, A Vedovato, G Veitch, J Veitch, PJ Venkateswara, K Verkindt, D Vetrano, F Vicere, A Vinciguerra, S Vine, DJ Vinet, JY Vitale, S Vo, T Vocca, H Vorvick, C Voss, DV Vousden, WD Vyatchanin, SP Wade, AR Wade, LE Wade, M Walker, M Wallace, L Walsh, S Wang, G Wang, H Wang, M Wang, X Wang, Y Ward, RL Warner, J Was, M Weaver, B Wei, LW Weinert, M Weinstein, AJ Weiss, R Wen, L Wessels, P Westphal, T Wette, K Whelan, JT Whitcomb, SE Whiting, BF Williams, RD Williamson, AR Willis, JL Willke, B Wimmer, MH Winkler, W Wipf, CC Wittel, H Woan, G Woehler, J Worden, J Wright, JL Wu, DS Wu, G Yablon, J Yam, W Yamamoto, H Yancey, CC Yu, H Yvert, M Zadrozny, A Zangrando, L Zanolin, M Zendri, JP Zevin, M Zhang, L Zhang, M Zhang, Y Zhao, C Zhou, M Zhou, Z Zhu, XJ Zucker, ME Zuraw, SE Zweizig, J AF Abbott, B. 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Traylor, G. Trifiro, D. Tringali, M. C. Trozzo, L. Tse, M. Turconi, M. Tuyenbayev, D. Ugolini, D. Unnikrishnan, C. S. Urban, A. L. Usman, S. A. Vahlbruch, H. Vajente, G. Valdes, G. Vallisneri, M. van Bakel, N. van Beuzekom, M. van den Brand, J. F. J. van Den Broeck, C. Vander-Hyde, D. C. van der Schaaf, L. van Heijningen, J. V. van Veggel, A. A. Vardaro, M. Vass, S. Vasuth, M. Vaulin, R. Vecchio, A. Vedovato, G. Veitch, J. Veitch, P. J. Venkateswara, K. Verkindt, D. Vetrano, F. Vicere, A. Vinciguerra, S. Vine, D. J. Vinet, J. -Y. Vitale, S. Vo, T. Vocca, H. Vorvick, C. Voss, D. V. Vousden, W. D. Vyatchanin, S. P. Wade, A. R. Wade, L. E. Wade, M. Walker, M. Wallace, L. Walsh, S. Wang, G. Wang, H. Wang, M. Wang, X. Wang, Y. Ward, R. L. Warner, J. Was, M. Weaver, B. Wei, L. -W. Weinert, M. Weinstein, A. J. Weiss, R. Wen, L. Wessels, P. Westphal, T. Wette, K. Whelan, J. T. Whitcomb, S. E. Whiting, B. F. Williams, R. D. Williamson, A. R. Willis, J. L. Willke, B. Wimmer, M. H. Winkler, W. Wipf, C. C. Wittel, H. Woan, G. Woehler, J. Worden, J. Wright, J. L. Wu, D. S. Wu, G. Yablon, J. Yam, W. Yamamoto, H. Yancey, C. C. Yu, H. Yvert, M. Zadrozny, A. Zangrando, L. Zanolin, M. Zendri, J. -P. Zevin, M. Zhang, L. Zhang, M. Zhang, Y. Zhao, C. Zhou, M. Zhou, Z. Zhu, X. J. Zucker, M. E. Zuraw, S. E. Zweizig, J. CA LIGO Sci Collaboration Virgo Collaboration TI Binary Black Hole Mergers in the First Advanced LIGO Observing Run SO PHYSICAL REVIEW X LA English DT Article ID INSPIRALLING COMPACT BINARIES; GRAVITATIONAL-WAVE TRANSIENTS; X-RAY TRANSIENTS; NEUTRON-STAR; PARAMETER-ESTIMATION; COALESCING BINARIES; MASS MEASUREMENTS; COMMON ENVELOPE; (POST)(5/2)-NEWTONIAN ORDER; OBJECT BINARIES AB The first observational run of the Advanced LIGO detectors, from September 12, 2015 to January 19, 2016, saw the first detections of gravitational waves from binary black hole mergers. In this paper, we present full results from a search for binary black hole merger signals with total masses up to 100M. and detailed implications from our observations of these systems. Our search, based on general-relativistic models of gravitational-wave signals from binary black hole systems, unambiguously identified two signals, GW150914 and GW151226, with a significance of greater than 5 sigma over the observing period. It also identified a third possible signal, LVT151012, with substantially lower significance and with an 87% probability of being of astrophysical origin. We provide detailed estimates of the parameters of the observed systems. Both GW150914 and GW151226 provide an unprecedented opportunity to study the two-body motion of a compact-object binary in the large velocity, highly nonlinear regime. We do not observe any deviations from general relativity, and we place improved empirical bounds on several highorder post-Newtonian coefficients. From our observations, we infer stellar-mass binary black hole merger rates lying in the range 9-240 Gpc(-3) yr(-1). These observations are beginning to inform astrophysical predictions of binary black hole formation rates and indicate that future observing runs of the Advanced detector network will yield many more gravitational-wave detections. C1 [Abbott, B. P.; Abbott, R.; Adhikari, R. X.; Anderson, S. B.; Arai, K.; Araya, M. C.; Barayoga, J. C.; Barish, B. C.; Berger, B. K.; Billingsley, G.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Brunett, S.; Cahillane, C.; Callister, T.; Cepeda, C. B.; Couvares, P.; Coyne, D. C.; Dergachev, V.; Drever, R. W. P.; Ehrens, P.; Etzel, T.; Gossan, S. E.; Gushwa, K. E.; Gustafson, E. K.; Hall, E. D.; Heptonstall, A. W.; Isi, M.; Kanner, J. B.; Kells, W.; Kondrashov, V.; Korth, W. Z.; Lazzarini, A.; Lewis, J. B.; Maros, E.; Marx, J. N.; McIntyre, G.; McIver, J.; Meshkov, S.; Pedraza, M.; Perreca, A.; Price, L. R.; Quintero, E. A.; Reitze, D. H.; Rollins, J. G.; Sachdev, S.; Sanchez, E. J.; Schmidt, P.; Singer, A.; Smith, N. D.; Smith, R. J. E.; Taylor, R.; Thirugnanasambandam, M. P.; Torrie, C. I.; Vajente, G.; Vass, S.; Wallace, L.; Weinstein, A. J.; Whitcomb, S. E.; Williams, R. D.; Wipf, C. C.; Yamamoto, H.; Zhang, L.; Zucker, M. E.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Abbott, T. D.; Buchanan, C. C.; Corbitt, T. R.; Cripe, J.; Gonzalez, G.; Hardwick, T.; Johnson, W. W.; Kasprzack, M.; Macleod, D. M.; Singh, R.; Walker, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA. [Abernathy, M. R.; Harry, G. M.] Amer Univ, Washington, DC 20016 USA. [Acernese, F.; Barone, F.] Univ Salerno, I-84084 Salerno, Italy. [Acernese, F.; Calloni, E.; De laurentis, M.; De Rosa, R.; Di Fiore, L.; Di Girolamo, T.; Garufi, F.; Grado, A.; Milano, L.] Ist Nazl Fis Nucl, Sez Napoli, Complesso Univ Monte S Angelo, I-80126 Naples, Italy. [Ackley, K.; Ciani, G.; Da Silva Costa, C. F.; Eikenberry, S. S.; Fulda, P.; Goetz, R.; Hartman, M. T.; Klimenko, S.; Miller, A. L.; Mitselmakher, G.; Mueller, G.; Mytidis, A.; Reitze, D. H.; Tanner, D. B.; Voss, D. V.; Whiting, B. F.] Univ Florida, Gainesville, FL 32611 USA. [Adams, C.; Aston, S. M.; Betzwieser, J.; Birch, J.; Cowart, M. J.; DeRosa, R. T.; Effler, A.; Evans, T. M.; Frolov, V. V.; Fyffe, M.; Giardina, K. D.; Hanson, J.; Heintze, M. C.; Holt, K.; Huynh-Dinh, T.; Katzman, W.; Laxen, M.; Lormand, M.; McCormick, S.; Mullavey, A.; Nelson, T. J. N.; Nolting, D.; Oram, Richard J.; Overmier, H.; Parker, W.; Pele, A.; Romie, J. H.; Sellers, D.; Stuver, A. L.; Thomas, M.; Thorne, K. A.; Traylor, G.; Wu, G.] LIGO Livingston Observ, Livingston, LA 70754 USA. [Adams, T.; Bonnand, R.; Buskulic, D.; Ducrot, M.; Germain, V.; Gouaty, R.; Letendre, N.; Marion, F.; Masserot, A.; Mours, B.; Rolland, L.; Verkindt, D.; Was, M.; Yvert, M.] Univ Savoie Mont Blanc, CNRS, IN2P3, Lab Annecy le Vieux Phys Particules LAPP, F-74941 Annecy Le Vieux, France. [Addesso, P.; DeSalvo, R.; Pierro, V.; Pinto, I. M.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy. [Addesso, P.; DeSalvo, R.; Pierro, V.; Pinto, I. M.; Principe, M.] Ist Nazl Fis Nucl, Sez Napoli, I-80100 Naples, Italy. [Adya, V. B.; Affeldt, C.; Allen, B.; Aulbert, C.; Baune, C.; Bergmann, G.; Birnholtz, O.; Bisht, A.; Bock, O.; Bogan, C.; Brinkmann, M.; Cabero, M.; Capano, C. D.; Dal Canton, T.; Danzmann, K.; Denker, T.; Dent, T.; Doravari, S.; Drago, M.; Eggenstein, H. -B.; Fehrmann, H.; Grote, H.; Hanke, M. M.; Heurs, M.; Hu, Y. M.; Indik, N.; Kapadia, S. J.; Karvinen, K. S.; Koehlenbeck, S. M.; Kringel, V.; Krishnan, B.; Kuehn, G.; Leong, J. R.; Lueck, H.; Lundgren, A. P.; Machenschalk, B.; Meadors, G. D.; Mossavi, K.; Nielsen, A. B.; Nitz, A.; Oppermann, P.; Post, A.; Prijatelj, M.; Prix, R.; Puncken, O.; Ruediger, A.; Salemi, F.; Schilling, R.; Schmidt, J.; Schreiber, E.; Schuette, D.; Shaltev, M.; Singh, A.; Steinke, M.; Steinmeyer, D.; Tarabrin, S. P.; Theeg, T.; Walsh, S.; Weinert, M.; Wessels, P.; Westphal, T.; Wette, K.; Willke, B.; Wimmer, M. H.; Winkler, W.; Wittel, H.; Woehler, J.; Wu, D. S.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. [Agathos, M.; Agatsuma, K.; Bader, M. K. M.; Bertolini, A.; Boom, B. A.; Ghosh, S.; Jonker, R. J. G.; Koley, S.; Meidam, J.; Nelemans, G.; Nissanke, S.; Setyawati, Y.; van Bakel, N.; van Beuzekom, M.; van den Brand, J. F. J.; van Den Broeck, C.; van der Schaaf, L.; van Heijningen, J. V.] Nikhef, Sci Pk, NL-1098 XG Amsterdam, Netherlands. [Aggarwal, N.; Barsotti, L.; Biscans, S.; Brown, N. M.; Buikema, A.; Donovan, F.; Essick, R. C.; Evans, M.; Fritschel, P.; Gras, S.; Isogai, T.; Katsavounidis, E.; Kontos, A.; Libson, A.; Lynch, R.; MacInnis, M.; Martynov, D. V.; Mason, K.; Matichard, F.; Mavalvala, N.; Miller, J.; Mittleman, R.; Mohapatra, S. R. P.; Oelker, E.; Shoemaker, D. H.; Tse, M.; Vaulin, R.; Vitale, S.; Weiss, R.; Yam, W.; Yu, H.; Zucker, M. E.] MIT, LIGO, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Aguiar, O. D.; Constancio, M., Jr.; Costa, C. A.; Ferreira, E. C.; Silva, A. D.] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, SP, Brazil. [Aiello, L.; Coccia, E.; Khan, I.; Lorenzini, M.; Singhal, A.; Tiwari, S.; Wang, G.] Ist Nazl Fis Nucl, Gran Sasso Sci Inst, I-67100 Laquila, Italy. [Aiello, L.; Casentini, C.; Cesarini, E.; Fafone, V.; Lorenzini, M.; Malvezzi, V.; Minenkov, Y.; Nardecchia, I.; Rocchi, A.; Sequino, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Ain, A.; Dhurandhar, S.; Gaonkar, S. G.; Gupta, A.; Mitra, S.; Mukund, N.; Prasad, J.; Souradeep, T.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Ajith, P.; Ghosh, Abhirup; Ghosh, Archisman; Iyer, B. R.; Johnson-McDaniel, N. K.; Mishra, C.; Mukherjee, Arunava] Tata Inst Fundamental Res, Int Ctr Theoret Sci, Bangalore 560012, Karnataka, India. [Allen, B.; Anderson, W. G.; Brady, P. R.; Brockill, P.; Caudill, S.; Creighton, J. D. E.; Downes, T. P.; Manske, M.; Mercer, R. A.; Mukherjee, D.; Ochsner, E.; Papa, M. A.; Poe, M.; Qi, H.; Sadeghian, L.; Sheperd, A.; Siemens, X.; Stephens, B. C.; Urban, A. L.] Univ Wisconsin, Milwaukee, WI 53201 USA. [Allen, B.; Aufmuth, P.; Danzmann, K.; Heurs, M.; Kaufer, S.; Krueger, C.; Lough, J. D.; Lueck, H.; Sawadsky, A.; Schuette, D.; Singh, A.; Vahlbruch, H.; Willke, B.; Wimmer, M. H.; Wittel, H.] Leibniz Univ Hannover, D-30167 Hannover, Germany. [Allocca, A.; Basti, A.; Boschi, V.; Cerretani, G.; Di Lieto, A.; Ferrante, I.; Fidecaro, F.; Castro, J. M. Gonzalez; Passaquieti, R.; Patricelli, B.; Poggiani, R.; Razzano, M.; Tonelli, M.] Univ Pisa, I-56127 Pisa, Italy. [Bradaschia, C.; Cella, G.; Cerretani, G.; Di Lieto, A.; Di Virgilio, A.; Ferrante, I.; Fidecaro, F.; Frasconi, F.; Gennai, A.; Giazotto, A.; Castro, J. M. Gonzalez; Moggi, A.; Paoletti, F.; Passaquieti, R.; Passuello, D.; Patricelli, B.; Poggiani, R.; Razzano, M.; Tonelli, M.; Trozzo, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Altin, P. A.; Chow, J. H.; Mansell, G. L.; McClelland, D. E.; McManus, D. J.; McRae, T.; Nguyen, T. T.; Rabeling, D. S.; Scott, S. M.; Shaddock, D. A.; Slagmolen, B. J. J.; Wade, A. R.; Ward, R. L.] Australian Natl Univ, Canberra, ACT 0200, Australia. [Arceneaux, C. C.; Cavaglia, M.; Dooley, K. L.; Gabbard, H. A. G.; Kandhasamy, S.; Trifiro, D.] Univ Mississippi, University, MS 38677 USA. [Areeda, J. S.; Hacker, J. J.; Read, J.; Smith, J. R.] Calif State Univ Fullerton, Fullerton, CA 92831 USA. [Arnaud, N.; Bizouard, M. A.; Brisson, V.; Diaz, J. Casanueva; Cavalier, F.; Davier, M.; Frey, V.; Hello, P.; Huet, D.; Leroy, N.; Robinet, F.] Univ Paris 11, CNRS IN2P3, Univ Paris Saclay, LAL, F-91898 Orsay, France. [Arun, K. G.] Chennai Math Inst, Madras 603103, Tamil Nadu, India. [Ascenzi, S.; Casentini, C.; Cesarini, E.; Coccia, E.; Fafone, V.; Malvezzi, V.; Nardecchia, I.; Re, V.; Sequino, V.] Univ Roma Tor Vergata, I-00133 Rome, Italy. [Ashton, G.; Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [Ast, M.; Kleybolte, L.; Korobko, M.; Pal-Singh, A.; Schnabel, R.] Univ Hamburg, D-22761 Hamburg, Germany. [Astone, P.; Colla, A.; Di Pace, S.; Frasca, S.; Leaci, P.; Majorana, E.; Mastrogiovanni, S.; Mezzani, F.; Miller, A. L.; Naticchioni, L.; Palomba, C.; Papa, M. A.; Piccinni, O. J.; Puppo, P.; Rapagnani, P.; Ricci, F.] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy. [Babak, S.; Bohe, A.; Buonanno, A.; Di Palma, I.; Grunewald, S.; Harry, I. W.; Meadors, G. D.; Ming, J.; Papa, M. A.; Privitera, S.; Puerrer, M.; Raymond, V.; Schutz, B. F.; Singh, A.; Taracchini, A.; Walsh, S.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. [Bacon, P.; Barsuglia, M.; Bouffanais, Y.; Buy, C.; Capocasa, E.; Chassande-Mottin, E.; Fiorucci, D.; Lebigot, E. O.; Porter, E.; Tacca, M.] Univ Paris Diderot, CNRS IN2P3, Sorbonne Paris Cite, APC AstroParticule & Cosmol,CEA Irfu,Observ Paris, F-75205 Paris 13, France. [Baker, P. T.; Cornish, N.; Millhouse, M.] Montana State Univ, Bozeman, MT 59717 USA. [Baldaccini, F.; Gammaitoni, L.; Travasso, F.; Vocca, H.] Univ Perugia, I-06123 Perugia, Italy. [Marchesoni, F.; Punturo, M.; Travasso, F.; Vocca, H.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Ballardin, G.; Bavigadda, V.; Bitossi, M.; Bozzi, A.; Carbognani, F.; Cavalier, F.; Chiummo, A.; Cortese, S.; Cuoco, E.; Dattilo, V.; Day, R.; Ferrini, F.; Fiori, I.; Genin, E.; Gosselin, M.; Hemming, G.; Hoak, D.; Kasprzack, M.; Mantovani, M.; Mohan, M.; Nocera, F.; Paoletti, F.; Paoli, A.; Pasqualetti, A.; Pillant, G.; Popolizio, P.; Prijatelj, M.; Ruggi, P.; Salconi, L.; Sentenac, D.; Swinkels, B. L.] EGO, I-56021 Pisa, Italy. [Ballmer, S. W.; Bhagwat, S.; Biwer, C.; Brown, D. A.; De, S.; Fair, H.; Fisher, R. P.; Kelley, D. B.; Lackey, B. D.; Lenon, A.; Lord, J. E.; Magana-Sandoval, F.; Zertuche, L. Magana; Massinger, T. J.; Nuttall, L. K.; Pekowsky, L.; Reyes, S. D.; Sanders, J. R.; Saulson, P. R.; Usman, S. A.; Vander-Hyde, D. C.; Vo, T.] Syracuse Univ, Syracuse, NY 13244 USA. [Barclay, S. E.; Barr, B.; Bell, A. S.; Chan, M.; Craig, K.; Cumming, A.; Cunningham, L.; Danilishin, S. L.; Davies, G. S.; Douglas, R.; Fletcher, M.; Glaefke, A.; Gordon, N. A.; Graef, C.; Grant, A.; Hammond, G.; Hart, M. J.; Haughian, K.; Hendry, M.; Heng, I. S.; Hennig, J.; Hild, S.; Hough, J.; Houston, E. A.; Huttner, S. H.; Isa, H. N.; Jones, R.; Leavey, S.; Lee, K.; Mangano, V.; Martin, I. W.; Masso-Reid, M.; Messenger, C.; Murray, P. G.; Newton, G.; Pascucci, D.; Pearlstone, B. L.; Phelps, M.; Pitkin, M.; Powell, J.; Robie, R.; Rowan, S.; Scott, J.; Sorazu, B.; Steinlechner, J.; Steinlechner, S.; Strain, K. A.; Toland, K.; Tornasi, Z.; van Veggel, A. A.; Woan, G.; Wright, J. L.] Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland. [Barker, D.; Bartlett, J.; Batch, J. C.; Blair, R. M.; Clara, F.; Cook, D.; Driggers, J. C.; Dwyer, S. E.; Goetz, E.; Gray, C.; Hanks, J.; Ingram, D. R.; Izumi, K.; Kawabe, K.; Kijbunchoo, N.; King, P. J.; Kissel, J. S.; Landry, M.; McCarthy, R.; Mendell, G.; Merilh, E. L.; Moraru, D.; Moreno, G.; Oberling, J.; Raab, F. J.; Radkins, H.; Reed, C. M.; Ryan, K.; Sadecki, T.; Savage, R. L.; Shaffer, T.; Sigg, D.; Thomas, P.; Vorvick, C.; Warner, J.; Weaver, B.; Worden, J.] LIGO Hanford Observ, Richland, WA 99352 USA. [Barta, D.; Debreczeni, G.; Vasuth, M.] Wigner RCP, RMKI, Konkoly Thege Miklos Ut 29-33, H-1121 Budapest, Hungary. [Bartos, I.; Countryman, S. T.; Factourovich, M.; Marka, S.; Marka, Z.; Matone, L.; Murphy, D. J.; Staley, A.] Columbia Univ, New York, NY 10027 USA. [Bassiri, R.; Byer, R. L.; DeBra, D.; Fejer, M. M.; Kim, N.; Lantz, B.; Markosyan, A. S.; Paris, H. R.; Patrick, Z.; Shapiro, B.] Stanford Univ, Stanford, CA 94305 USA. [Bazzan, M.; Vardaro, M.] Univ Padua, Dipartimento Fis & Astron, I-35131 Padua, Italy. [Conti, L.; Lazzaro, C.; Vardaro, M.; Vedovato, G.; Zangrando, L.; Zendri, J. -P.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bejger, M.; Sieniawska, M.] CAMK PAN, PL-00716 Warsaw, Poland. [Berry, C. P. L.; Bond, C.; Brown, D. D.; Del Pozzo, W.; Farr, W. M.; Freise, A.; Gaebel, S.; Green, A. C.; Haster, C. -J.; Mandel, I.; Miao, H.; Middleton, H.; Mow-Lowry, C. M.; Stevenson, S.; Thomas, E. G.; Toyra, D.; Vecchio, A.; Veitch, J.; Vinciguerra, S.; Vousden, W. D.; Wang, H.; Wang, M.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England. [Bersanetti, D.; Neri, M.] Univ Genoa, I-16146 Genoa, Italy. [Chincarini, A.; Farinon, S.; Gemme, G.; Neri, M.; Rei, L.; Sorrentino, F.] Ist Nazl Fis Nucl, Sez Genova, I-16146 Genoa, Italy. [Bhandare, R.; Dave, I.; George, J.; Pai, S. A.; Pant, B. 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[Boer, M.; Bogaert, G.; Brillet, A.; Cleva, F.; Coulon, J. -P.; Fournier, J. -D.; Heitmann, H.; Kefelian, F.; Man, N.; Martellini, L.; Merzougui, M.; Pichot, M.; Regimbau, T.; Turconi, M.; Vinet, J. -Y.; Wei, L. -W.] Univ Cote dAzur, CNRS, Artemis, Observ Cote dAzur, CS 34229, F-06304 Nice 4, France. [Bondu, F.] Univ Rennes 1, CNRS, Inst Phys Rennes, F-35042 Rennes, France. [Bose, S.; Hall, B. R.; Magee, R. M.; Mazumder, N.] Washington State Univ, Pullman, WA 99164 USA. [Branchesi, M.; Baiardi, L. Cerboni; Greco, G.; Guidi, G. M.; Harms, J.; Martelli, F.; Montani, M.; Piergiovanni, F.; Stratta, G.; Vetrano, F.; Vicere, A.] Univ Urbino Carlo Bo, I-61029 Urbino, Italy. [Baiardi, L. Cerboni; Greco, G.; Guidi, G. M.; Harms, J.; Losurdo, G.; Martelli, F.; Montani, M.; Piergiovanni, F.; Stratta, G.; Vetrano, F.; Vicere, A.; Wang, G.] Ist Nazl Fis Nucl, Sez Firenze, I-50019 Florence, Italy. [Brau, J. E.; Frey, R.; Karki, S.; Palamos, J. R.; Quitzow-James, R.; Roma, V. J.; Schale, P.; Schofield, R. M. S.; Talukder, D.] Univ Oregon, Eugene, OR 97403 USA. [Briant, T.; Chua, S.; Cohadon, P. -F.; Deleglise, S.; Heidmann, A.; Isac, J. -M.; Jacqmin, T.; Metzdorff, R.] UPMC Sorbonne Univ, Coll France, ENS PSL Res Univ, Lab Kastler Brossel,CNRS, F-75005 Paris, France. [Broida, J. E.; Christensen, N.; Coughlin, M. W.; Edwards, M. C.; Strauss, N. A.] Carleton Coll, Northfield, MN 55057 USA. [Bulik, T.; Kowalska, I.] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland. [Bulten, H. J.; van den Brand, J. F. J.] Vrije Univ Amsterdam, NL-1081 HV Amsterdam, Netherlands. [Cho, M.; Graff, P. B.; Pan, Y.; Shawhan, P.; Yancey, C. C.] Univ Maryland, College Pk, MD 20742 USA. [Cadonati, L.; Bustillo, J. Calderon; Clark, J. A.; Cowan, E. E.; Jani, K.; Kimbrell, S. J.; Shoemaker, D. M.; Siellez, K.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Cadonati, L.; Bustillo, J. Calderon; Clark, J. A.; Cowan, E. E.; Jani, K.; Kimbrell, S. 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[Chao, S.; Cheng, C.; Huang, S.; Kuo, L.; Pan, H.] Natl Tsing Hua Univ, Hsinchu 30013, Taiwan. [Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia. [Cheeseboro, B. D.; Devine, R. C.; McWilliams, S. T.] West Virginia Univ, Morgantown, WV 26506 USA. [Chen, H. Y.; Farr, B.; Holz, D. E.] Univ Chicago, Chicago, IL 60637 USA. [Chen, Y.; Engels, W.; Schmidt, P.; Vallisneri, M.] Caltech CaRT, Pasadena, CA 91125 USA. [Cho, H. S.; Jang, H.; Kang, G.; Kim, Chi-Woong; Kim, Chunglee] Korea Inst Sci & Technol Informat, Daejeon 305806, South Korea. [Colla, A.; Conte, A.; Di Pace, S.; Di Palma, I.; Frasca, S.; Leaci, P.; Mastrogiovanni, S.; Mezzani, F.; Miller, A. L.; Naticchioni, L.; Piccinni, O. J.; Rapagnani, P.; Ricci, F.] Univ Roma La Sapienza, I-00185 Rome, Italy. [Collette, C. G.] Univ Brussels, B-1050 Brussels, Belgium. [Cominsky, L.] Sonoma State Univ, Rohnert Pk, CA 94928 USA. [Coughlin, S. B.; Kalogera, V.; Klein, B.; Miller, A.; Miller, B. B.; Pankow, C.; Perri, L. 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RI Sigg, Daniel/I-4308-2015; Di Virgilio, Angela Dora Vittoria/E-9078-2015; Garufi, Fabio/K-3263-2015; Sergeev, Alexander/F-3027-2017; Harms, Jan/J-4359-2012; prodi, giovanni/B-4398-2010; Leonardi, Matteo/G-9694-2015; Ferrante, Isidoro/F-1017-2012; Cesarini, Elisabetta/C-4507-2017; Costa, Cesar/G-7588-2012; Danilishin, Stefan/K-7262-2012; Hild, Stefan/A-3864-2010; Steinlechner, Sebastian/D-5781-2013; Chow, Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Prokhorov, Leonid/I-2953-2012; Gammaitoni, Luca/B-5375-2009; Ciani, Giacomo/G-1036-2011; Iyer, Bala R./E-2894-2012; Cella, Giancarlo/A-9946-2012; Sorrentino, Fiodor/M-6662-2016; Travasso, Flavio/J-9595-2016; Rocchi, Alessio/O-9499-2015; Tiwari, Shubhanshu/R-8546-2016; Strain, Kenneth/D-5236-2011; Gemme, Gianluca/C-7233-2008; Strigin, Sergey/I-8337-2012; Vecchio, Alberto/F-8310-2015; Marchesoni, Fabio/A-1920-2008; Bartos, Imre/A-2592-2017; Punturo, Michele/I-3995-2012 OI Piccinni, Ornella Juliana/0000-0001-5478-3950; Haney, Maria/0000-0001-7554-3665; Kanner, Jonah/0000-0001-8115-0577; Freise, Andreas/0000-0001-6586-9901; Nelemans, Gijs/0000-0002-0752-2974; Murphy, David/0000-0002-8538-815X; Wang, Gang/0000-0002-9668-8772; Pitkin, Matthew/0000-0003-4548-526X; Davies, Gareth/0000-0002-4289-3439; Principe, Maria/0000-0002-6327-0628; Sigg, Daniel/0000-0003-4606-6526; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Garufi, Fabio/0000-0003-1391-6168; Del Pozzo, Walter/0000-0003-3978-2030; Granata, Massimo/0000-0003-3275-1186; Berry, Christopher/0000-0003-3870-7215; prodi, giovanni/0000-0001-5256-915X; Ferrante, Isidoro/0000-0002-0083-7228; Cesarini, Elisabetta/0000-0001-9127-3167; Danilishin, Stefan/0000-0001-7758-7493; Steinlechner, Sebastian/0000-0003-4710-8548; Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Gammaitoni, Luca/0000-0002-4972-7062; Ciani, Giacomo/0000-0003-4258-9338; Iyer, Bala R./0000-0002-4141-5179; Cella, Giancarlo/0000-0002-0752-0338; Sorrentino, Fiodor/0000-0002-9605-9829; Travasso, Flavio/0000-0002-4653-6156; Rocchi, Alessio/0000-0002-1382-9016; Tiwari, Shubhanshu/0000-0003-1611-6625; Strain, Kenneth/0000-0002-2066-5355; Gemme, Gianluca/0000-0002-1127-7406; Vecchio, Alberto/0000-0002-6254-1617; Marchesoni, Fabio/0000-0001-9240-6793; Punturo, Michele/0000-0001-8722-4485 FU United States National Science Foundation (NSF); Science and Technology Facilities Council (STFC) of the United Kingdom; Max-Planck-Society (MPS); State of Niedersachsen/Germany; Australian Research Council; Netherlands Organisation for Scientific Research; Council of Scientific and Industrial Research of India; Department of Science and Technology, India; Science & Engineering Research Board (SERB), India; Ministry of Human Resource Development, India; Spanish Ministerio de Economia y Competitividad; Conselleria d'Economia i Competitivitat and Conselleria d'Educacio; Cultura i Universitats of the Govern de les Illes Balears; National Science Centre of Poland; European Commission; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; Hungarian Scientific Research Fund (OTKA); Lyon Institute of Origins (LIO); National Research Foundation of Korea; Industry Canada; Province of Ontario through the Ministry of Economic Development and Innovation; Natural Science and Engineering Research Council Canada; Canadian Institute for Advanced Research; Brazilian Ministry of Science, Technology, and Innovation; Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP); Russian Foundation for Basic Research; Leverhulme Trust; Ministry of Science and Technology (MOST), Taiwan; Kavli Foundation FX The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO, as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies, as well as by the Council of Scientific and Industrial Research of India; Department of Science and Technology, India; Science & Engineering Research Board (SERB), India; Ministry of Human Resource Development, India; the Spanish Ministerio de Economia y Competitividad; the Conselleria d'Economia i Competitivitat and Conselleria d'Educacio; Cultura i Universitats of the Govern de les Illes Balears; the National Science Centre of Poland; the European Commission; the Royal Society; the Scottish Funding Council; the Scottish Universities Physics Alliance; the Hungarian Scientific Research Fund (OTKA); the Lyon Institute of Origins (LIO); the National Research Foundation of Korea; Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation; the Natural Science and Engineering Research Council Canada; Canadian Institute for Advanced Research; the Brazilian Ministry of Science, Technology, and Innovation; Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP); Russian Foundation for Basic Research; the Leverhulme Trust, the Research Corporation; Ministry of Science and Technology (MOST), Taiwan; and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS, and the State of Niedersachsen/Germany for provision of computational resources. NR 216 TC 32 Z9 32 U1 50 U2 50 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2160-3308 J9 PHYS REV X JI Phys. Rev. X PD OCT 21 PY 2016 VL 6 IS 4 AR 041015 DI 10.1103/PhysRevX.6.041015 PG 36 WC Physics, Multidisciplinary SC Physics GA EA1YO UT WOS:000386388300002 ER PT J AU Abbott, BP Abbott, R Abbott, TD Abernathy, MR Acernese, F Ackley, K Adams, C Adams, T Addesso, P Adhikari, RX Adya, VB Affeldt, C Agathos, M Agatsuma, K Aggarwal, N Aguiar, OD Aiello, L Ain, A Ajith, P Allen, B Allocca, A Altin, PA Anderson, SB Anderson, WG Arai, K Araya, MC Arceneaux, CC Areeda, JS Arnaud, N Arun, KG Ascenzi, S Ashton, G Ast, M Aston, SM Astone, P Aufmuth, P Aulbert, C Babak, S Bacon, P Bader, MKM Baker, PT Baldaccini, F Ballardin, G Ballmer, SW Barayoga, JC Barclay, SE Barish, BC Barker, D Barone, F Barr, B Barsotti, L Barsuglia, M Barta, D Bartlett, J Bartos, I Bassiri, R Basti, A Batch, JC Baune, C Bavigadda, V Bazzan, M Bejger, M Bell, AS Berger, BK Bergmann, G Berry, CPL Bersanetti, D Bertolini, A Betzwieser, J Bhagwat, S Bhandare, R Bilenko, IA Billingsley, G Birch, J Birney, R Birnholtz, O Biscans, S 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Wipf, C. C. Wittel, H. Woan, G. Woehler, J. Worden, J. Wright, J. L. Wu, D. S. Wu, G. Yablon, J. Yam, W. Yamamoto, H. Yancey, C. C. Yu, H. Yvert, M. Zadrozny, A. Zangrando, L. Zanolin, M. Zendri, J. -P. Zevin, M. Zhang, L. Zhang, M. Zhang, Y. Zhao, C. Zhou, M. Zhou, Z. Zhu, X. J. Zucker, M. E. Zuraw, S. E. Zweizig, J. Boyle, M. Bruegmann, B. Campanelli, M. Chu, T. Clark, M. Haas, R. Hemberger, D. Hinder, I. Kidder, L. E. Kinsey, M. Laguna, P. Ossokine, S. Pan, Y. Roever, C. Scheel, M. Szilagyi, B. Teukolsky, S. Zlochower, Y. CA LIGO Sci Collaboration Virgo Collaboration TI Improved Analysis of GW150914 Using a Fully Spin-Precessing Waveform Model SO PHYSICAL REVIEW X LA English DT Article ID SCHWARZSCHILD BLACK-HOLE; GRAVITATIONAL-RADIATION; COMPACT BINARIES AB This paper presents updated estimates of source parameters for GW150914, a binary black-hole coalescence event detected by the Laser Interferometer Gravitational-wave Observatory (LIGO) in 2015 [Abbott et al. Phys. Rev. Lett. 116, 061102 (2016).]. Abbott et al. [Phys. Rev. Lett. 116, 241102 (2016).] presented parameter estimation of the source using a 13-dimensional, phenomenological precessing-spin model (precessing IMRPhenom) and an 11-dimensional nonprecessing effective-onebody (EOB) model calibrated to numerical-relativity simulations, which forces spin alignment (nonprecessing EOBNR). Here, we present new results that include a 15-dimensional precessing-spin waveform model (precessing EOBNR) developed within the EOB formalism. We find good agreement with the parameters estimated previously [Abbott et al. Phys. Rev. Lett. 116, 241102 (2016).], and we quote updated component masses of 35(-3)(+5) M-circle dot and 30(-4)(+3) M-circle dot (where errors correspond to 90% symmetric credible intervals). We also present slightly tighter constraints on the dimensionless spin magnitudes of the two black holes, with a primary spin estimate < 0.65 and a secondary spin estimate < 0.75 at 90% probability. Abbott et al. [Phys. Rev. Lett. 116, 241102 (2016).] estimated the systematic parameter-extraction errors due to waveform-model uncertainty by combining the posterior probability densities of precessing IMRPhenom and nonprecessing EOBNR. Here, we find that the two precessing-spin models are in closer agreement, suggesting that these systematic errors are smaller than previously quoted. C1 [Abbott, B. P.; Abbott, R.; Adhikari, R. X.; Anderson, S. B.; Arai, K.; Araya, M. C.; Barayoga, J. C.; Barish, B. C.; Berger, B. K.; Billingsley, G.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Brunett, S.; Cahillane, C.; Callister, T.; Cepeda, C. B.; Couvares, P.; Coyne, D. C.; Dergachev, V.; Drever, R. W. P.; Ehrens, P.; Eichholz, J.; Etzel, T.; Gossan, S. E.; Gushwa, K. E.; Gustafson, E. K.; Hall, E. D.; Heptonstall, A. W.; Isi, M.; Kanner, J. B.; Kells, W.; Kondrashov, V.; Korth, W. Z.; Kozak, D. B.; Lazzarini, A.; Lewis, J. B.; Maros, E.; Marx, J. N.; McIntyre, G.; McIver, J.; Meshkov, S.; Pedraza, M.; Perreca, A.; Price, L. R.; Quintero, E. A.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Sachdev, S.; Sanchez, E. J.; Schmidt, P.; Singer, A.; Smith, N. D.; Smith, R. J. E.; Taylor, R.; Thirugnanasambandam, M. P.; Torrie, C. I.; Vajente, G.; Vass, S.; Wallace, L.; Weinstein, A. J.; Williams, R. D.; Wipf, C. C.; Yamamoto, H.; Zhang, L.; Zucker, M. E.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Abbott, T. D.; Buchanan, C. C.; Corbitt, T. R.; Cripe, J.; Giaime, J. A.; Gonzalez, G.; Hardwick, T.; Johnson, W. W.; Kasprzack, M.; Macleod, D. M.; Singh, R.; Walker, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA. [Abernathy, M. R.; Harry, G. M.] Amer Univ, Washington, DC 20016 USA. [Acernese, F.; Barone, F.; Romano, R.] Univ Salerno, I-84084 Salerno, Italy. 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R.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales. [Favata, M.; Moore, B. C.] Montclair State Univ, Montclair, NJ 07043 USA. [Fenyvesi, E.; Frei, Z.; Gondan, L.; Raffai, P.] MTA Eotvos Univ, Lendulet Astrophys Res Grp, H-1117 Budapest, Hungary. [Flaminio, R.] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Gair, J. R.] Univ Edinburgh, Sch Math, Edinburgh EH9 3FD, Midlothian, Scotland. [Gaur, G.; Sengupta, A. S.] Indian Inst Technol, Ahmadabad 382424, Gujarat, India. [Gergely, L.; Tapai, M.] Univ Szeged, Dom Ter 9, H-6720 Szeged, Hungary. [Gill, K.; Hughey, B.; Szczepanczyk, M. J.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA. [Gopakumar, A.; Haney, M.; Unnikrishnan, C. S.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. [Grado, A.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Gustafson, R.; Neunzert, A.; Riles, K.; Sauter, O. E. S.] Univ Michigan, Ann Arbor, MI 48109 USA. [Healy, J.; Henry, J.; Lange, J.; Lousto, C. O.; O'Shaughnessy, R.; Rizzo, M.; Whelan, J. T.; Zhang, Y.] Rochester Inst Technol, Rochester, NY 14623 USA. [Huerta, E. A.] Univ Illinois, NCSA, Urbana, IL 61801 USA. [Husa, S.; Jimenez-Forteza, F.; Keitel, D.; Oliver, M.; Sintes, A. M.] Univ Illes Balears, IEEC IAC3, E-07122 Palma De Mallorca, Spain. [Jaranowski, P.] Univ Bialystok, PL-15424 Bialystok, Poland. [Jawahar, S.; Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland. [Haris, K.; Pai, A.; Saleem, M.] IISER TVM, CET Campus, Trivandrum 695016, Kerala, India. [Kehl, M. S.; Kumar, P.; Pfeiffer, H. P.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Khazanov, E. A.; Palashov, O.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia. [Kim, J.; Kim, Y. -M.; Lee, C. H.] Pusan Natl Univ, Busan 609735, South Korea. [Kim, K.; Lee, H. K.] Hanyang Univ, Seoul 133791, South Korea. [Kim, W.; King, E. J.; Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia. [Krolak, A.; Kutynia, A.; Zadrozny, A.] NCBJ, PL-05400 Otwock, Poland. [Krolak, A.] IM PAN, PL-00956 Warsaw, Poland. [Lasky, P. D.; Levin, Y.; Qiu, S.; Sammut, L.; Thrane, E.] Monash Univ, Clayton, Vic 3800, Australia. [Lee, H. M.] Seoul Natl Univ, Seoul 151742, South Korea. [Li, T. G. F.] Chinese Univ Hong Kong, Shatin, Hong Kong, Peoples R China. [Littenberg, T. B.] Univ Alabama, Huntsville, AL 35899 USA. [Lombardi, A. L.; Nedkova, K.; Zuraw, S. E.] Univ Massachusetts, Amherst, MA 01003 USA. [Loriette, V.; Maksimovic, I.] ESPCI, CNRS, F-75005 Paris, France. [Marchesoni, F.] Univ Camerino, Dipartimento Fis, I-62032 Camerino, Italy. [McGuire, S. C.] Southern Univ & A&M Coll, Baton Rouge, LA 70813 USA. [Mikhailov, E. E.; Rew, H.; Romanov, G.; Zhang, M.] Coll William & Mary, Williamsburg, VA 23187 USA. [Mirshekari, S.; Sturani, R.] Univ Estadual Paulista, ICTP, South Amer Inst Fundamental Res, Inst Fis Teor, BR-01140070 Sao Paulo, SP, Brazil. [Moore, C. J.] Univ Cambridge, Cambridge CB2 1TN, England. [Nayak, R. K.; Samajdar, A.] IISER Kolkata, Mohanpur 741252, W Bengal, India. [O'Dell, J.] Rutherford Appleton Lab, HSIC, Didcot OX11 0QX, Oxon, England. [Ogin, G. H.] Whitman Coll, 345 Boyer Ave, Walla Walla, WA 99362 USA. [Oh, J. J.; Oh, S. H.; Son, E. J.] Natl Inst Math Sci, Daejeon 305390, South Korea. [Pedurand, R.] Univ Lyon, F-69361 Lyon, France. [Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA. [Rosinska, D.] Univ Zielona Gora, Janusz Gil Inst Astron, PL-65265 Zielona Gora, Poland. [Sakellariadou, M.] Univ London, Kings Coll London, London WC2R 2LS, England. [Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA. [Trozzo, L.] Univ Siena, I-53100 Siena, Italy. [Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA. [Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA. [Wade, L. E.; Wade, M.] Kenyon Coll, Gambier, OH 43022 USA. [Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA. [Boyle, M.; Chu, T.; Kidder, L. E.; Teukolsky, S.] Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA. [Bruegmann, B.] Univ Jena, Inst Theoret Phys, D-07743 Jena, Germany. [Szilagyi, B.] Caltech JPL, Pasadena, CA 91109 USA. RP Abbott, BP (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA. RI prodi, giovanni/B-4398-2010; Leonardi, Matteo/G-9694-2015; Ferrante, Isidoro/F-1017-2012; Cesarini, Elisabetta/C-4507-2017; Costa, Cesar/G-7588-2012; Danilishin, Stefan/K-7262-2012; Hild, Stefan/A-3864-2010; Steinlechner, Sebastian/D-5781-2013; Chow, Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Prokhorov, Leonid/I-2953-2012; Gammaitoni, Luca/B-5375-2009; Ciani, Giacomo/G-1036-2011; Cella, Giancarlo/A-9946-2012; Iyer, Bala R./E-2894-2012; Sorrentino, Fiodor/M-6662-2016; Travasso, Flavio/J-9595-2016; Rocchi, Alessio/O-9499-2015; Tiwari, Shubhanshu/R-8546-2016; Strain, Kenneth/D-5236-2011; Gemme, Gianluca/C-7233-2008; Strigin, Sergey/I-8337-2012; Vecchio, Alberto/F-8310-2015; Marchesoni, Fabio/A-1920-2008; Bartos, Imre/A-2592-2017; Punturo, Michele/I-3995-2012; Sigg, Daniel/I-4308-2015; Di Virgilio, Angela Dora Vittoria/E-9078-2015; Garufi, Fabio/K-3263-2015; Sergeev, Alexander/F-3027-2017; Harms, Jan/J-4359-2012; OI prodi, giovanni/0000-0001-5256-915X; Ferrante, Isidoro/0000-0002-0083-7228; Cesarini, Elisabetta/0000-0001-9127-3167; Danilishin, Stefan/0000-0001-7758-7493; Steinlechner, Sebastian/0000-0003-4710-8548; Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Gammaitoni, Luca/0000-0002-4972-7062; Ciani, Giacomo/0000-0003-4258-9338; Cella, Giancarlo/0000-0002-0752-0338; Iyer, Bala R./0000-0002-4141-5179; Sorrentino, Fiodor/0000-0002-9605-9829; Travasso, Flavio/0000-0002-4653-6156; Rocchi, Alessio/0000-0002-1382-9016; Tiwari, Shubhanshu/0000-0003-1611-6625; Strain, Kenneth/0000-0002-2066-5355; Gemme, Gianluca/0000-0002-1127-7406; Vecchio, Alberto/0000-0002-6254-1617; Marchesoni, Fabio/0000-0001-9240-6793; Punturo, Michele/0000-0001-8722-4485; Nelemans, Gijs/0000-0002-0752-2974; Murphy, David/0000-0002-8538-815X; Wang, Gang/0000-0002-9668-8772; Pitkin, Matthew/0000-0003-4548-526X; Davies, Gareth/0000-0002-4289-3439; Principe, Maria/0000-0002-6327-0628; Sigg, Daniel/0000-0003-4606-6526; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Garufi, Fabio/0000-0003-1391-6168; Granata, Massimo/0000-0003-3275-1186; Piccinni, Ornella Juliana/0000-0001-5478-3950 FU United States National Science Foundation (NSF); Science and Technology Facilities Council (STFC) of the United Kingdom; Max-Planck Society (MPS); State of Niedersachsen/Germany; Australian Research Council; Netherlands Organisation for Scientific Research; Council of Scientific and Industrial Research of India; Department of Science and Technology, India; Science & Engineering Research Board (SERB), India; Ministry of Human Resource Development, India; Spanish Ministerio de Economia y Competitividad; Conselleria d'Economia i Competitivitat and Conselleria d'Educacio; Cultura i Universitats of the Govern de les Illes Balears; National Science Centre of Poland; European Commission; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; Hungarian Scientific Research Fund (OTKA); Lyon Institute of Origins (LIO); National Research Foundation of Korea; Industry Canada; Province of Ontario through the Ministry of Economic Development and Innovation; Natural Science and Engineering Research Council Canada; Canadian Institute for Advanced Research; Brazilian Ministry of Science, Technology, and Innovation; Russian Foundation for Basic Research; Leverhulme Trust; Ministry of Science and Technology (MOST), Taiwan; Kavli Foundation FX The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO, as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies, as well as by the Council of Scientific and Industrial Research of India; Department of Science and Technology, India; Science & Engineering Research Board (SERB), India; Ministry of Human Resource Development, India; the Spanish Ministerio de Economia y Competitividad; the Conselleria d'Economia i Competitivitat and Conselleria d'Educacio; Cultura i Universitats of the Govern de les Illes Balears; the National Science Centre of Poland; the European Commission; the Royal Society; the Scottish Funding Council; the Scottish Universities Physics Alliance; the Hungarian Scientific Research Fund (OTKA); the Lyon Institute of Origins (LIO); the National Research Foundation of Korea; Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation; the Natural Science and Engineering Research Council Canada; Canadian Institute for Advanced Research; the Brazilian Ministry of Science, Technology, and Innovation; Russian Foundation for Basic Research; the Leverhulme Trust; the Research Corporation; Ministry of Science and Technology (MOST), Taiwan; and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS, and the State of Niedersachsen/Germany for provision of computational resources. NR 57 TC 11 Z9 11 U1 37 U2 37 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2160-3308 J9 PHYS REV X JI Phys. Rev. X PD OCT 21 PY 2016 VL 6 IS 4 AR 041014 DI 10.1103/PhysRevX.6.041014 PG 19 WC Physics, Multidisciplinary SC Physics GA EA1YO UT WOS:000386388300001 ER PT J AU Haworth, TJ Ilee, JD Forgan, DH Facchini, S Price, DJ Boneberg, DM Booth, RA Clarke, CJ Gonzalez, JF Hutchison, MA Kamp, I Laibe, G Lyra, W Meru, F Mohanty, S Panic, O Rice, K Suzuki, T Teague, R Walsh, C Woitke, P AF Haworth, Thomas J. Ilee, John D. Forgan, Duncan H. Facchini, Stefano Price, Daniel J. Boneberg, Dominika M. Booth, Richard A. Clarke, Cathie J. Gonzalez, Jean-Francois Hutchison, Mark A. Kamp, Inga Laibe, Guillaume Lyra, Wladimir Meru, Farzana Mohanty, Subhanjoy Panic, Olja Rice, Ken Suzuki, Takeru Teague, Richard Walsh, Catherine Woitke, Peter TI Grand Challenges in Protoplanetary Disc Modelling SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Review DE astrochemistry; magnetohydrodynamics (MHD); hydrodynamics; planetary systems: formation; protoplanetary disks; radiative transfer ID SMOOTHED PARTICLE HYDRODYNAMICS; SHOCKED CIRCUMSTELLAR ENVELOPES; GRAVITATING ACCRETION DISCS; ADAPTIVE-MESH-REFINEMENT; LIMITED DIFFUSION-APPROXIMATION; VERTICAL SHEAR INSTABILITY; CARLO RADIATIVE-TRANSFER; D-TYPE EXPANSION; X-RAY-RADIATION; DUSTY GAS AB The Protoplanetary Discussions conference-held in Edinburgh, UK, from 2016 March 7th-11thincluded several open sessions led by participants. This paper reports on the discussions collectively concerned with the multi-physics modelling of protoplanetary discs, including the self-consistent calculation of gas and dust dynamics, radiative transfer, and chemistry. After a short introduction to each of these disciplines in isolation, we identify a series of burning questions and grand challenges associated with their continuing development and integration. We then discuss potential pathways towards solving these challenges, grouped by strategical, technical, and collaborative developments. This paper is not intended to be a review, but rather to motivate and direct future research and collaboration across typically distinct fields based on community-driven input, to encourage further progress in our understanding of circumstellar and protoplanetary discs. C1 [Haworth, Thomas J.; Ilee, John D.; Boneberg, Dominika M.; Booth, Richard A.; Clarke, Cathie J.; Meru, Farzana; Panic, Olja] Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Haworth, Thomas J.; Mohanty, Subhanjoy; Woitke, Peter] Imperial Coll London, Blackett Lab, Astrophys Grp, Prince Consort Rd, London SW7 2AZ, England. [Forgan, Duncan H.; Laibe, Guillaume] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Facchini, Stefano] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. [Price, Daniel J.] Monash Univ, Monash Ctr Astrophys, Clayton, Vic 3800, Australia. [Price, Daniel J.] Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia. [Gonzalez, Jean-Francois] Univ Lyon, Univ Lyon 1, Ens Lyon, CNRS,Ctr Rech Astrophys Lyon,UMR5574, F-69230 St Genis Laval, France. [Hutchison, Mark A.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Kamp, Inga] Univ Groningen, Kapteyn Astron Inst, Postbus 800, NL-9700 AV Groningen, Netherlands. [Lyra, Wladimir] Calif State Univ Northridge, Dept Phys & Astron, 18111 Nordhoff St, Northridge, CA 91330 USA. [Lyra, Wladimir] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Panic, Olja] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Rice, Ken] Univ Edinburgh, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. [Suzuki, Takeru] Univ Tokyo, Sch Arts & Sci, Meguro Ku, 3-8-1 Komaba, Tokyo 1538902, Japan. [Suzuki, Takeru] Nagoya Univ, Dept Phys, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648602, Japan. [Teague, Richard] Max Planck Inst Astron, Knigstuhl 17, D-69117 Heidelberg, Germany. [Walsh, Catherine] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. RP Haworth, TJ (reprint author), Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.; Haworth, TJ (reprint author), Imperial Coll London, Blackett Lab, Astrophys Grp, Prince Consort Rd, London SW7 2AZ, England. EM thaworth@ast.cam.ac.uk RI Rice, Ken/H-5084-2011; OI Rice, Ken/0000-0002-6379-9185; Facchini, Stefano/0000-0003-4689-2684; Booth, Richard/0000-0002-0364-937X; Price, Daniel/0000-0002-4716-4235 FU STFC consolidated grant [ST/K000985/1]; Imperial Junior research fellowship; DISCSIM project [341137]; European Research Council; ECOGAL project [291227]; Future Fellowship from Australian Research Council [FT130100034]; Royal Society Dorothy Hodgkin Fellowship FX Through most of this work TJH was funded by the STFC consolidated grant ST/K000985/1 and is now funded by an Imperial Junior research fellowship. JDI gratefully acknowledges support from the DISCSIM project, grant agreement 341137, funded by the European Research Council under ERC-2013-ADG. DHF acknowledges support from the ECOGAL project, grant agreement 291227, funded by the European Research Council under ERC-2011-ADG. DJP gratefully acknowledges funding via Future Fellowship FT130100034 from the Australian Research Council. OP is supported by the Royal Society Dorothy Hodgkin Fellowship. NR 294 TC 1 Z9 1 U1 4 U2 4 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. PD OCT 21 PY 2016 VL 33 AR e053 DI 10.1017/pasa.2016.45 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA8OU UT WOS:000386896700001 ER PT J AU Lange, R Moffett, AJ Driver, SP Robotham, ASG Lagos, CD Kelvin, LS Conselice, C Margalef-Bentabol, B Alpaslan, M Baldry, I Bland-Hawthorn, J Bremer, M Brough, S Cluver, M Colless, M Davies, LJM Haussler, B Holwerda, BW Hopkins, AM Kafle, PR Kennedy, R Liske, J Phillipps, S Popescu, CC Taylor, EN Tuffs, R van Kampen, E Wright, AH AF Lange, Rebecca Moffett, Amanda J. Driver, Simon P. Robotham, Aaron S. G. Lagos, Claudia del P. Kelvin, Lee S. Conselice, Christopher Margalef-Bentabol, Berta Alpaslan, Mehmet Baldry, Ivan Bland-Hawthorn, Joss Bremer, Malcolm Brough, Sarah Cluver, Michelle Colless, Matthew Davies, Luke J. M. Haussler, Boris Holwerda, Benne W. Hopkins, Andrew M. Kafle, Prajwal R. Kennedy, Rebecca Liske, Jochen Phillipps, Steven Popescu, Cristina C. Taylor, Edward N. Tuffs, Richard van Kampen, Eelco Wright, Angus H. TI Galaxy And Mass Assembly (GAMA): M-star-R-e relations of z=0 bulges, discs and spheroids SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: formation; galaxies: fundamental parameters; galaxies: spiral; galaxies: statistics ID DIGITAL SKY SURVEY; EXTRAGALACTIC LEGACY SURVEY; HUBBLE-SPACE-TELESCOPE; ULTRA-DEEP-FIELD; SIMILAR-TO 1; LESS-THAN 3; SIZE EVOLUTION; EAGLE SIMULATIONS; ELLIPTIC GALAXIES; DATA RELEASE AB We perform automated bulge + disc decomposition on a sample of similar to 7500 galaxies from the Galaxy And Mass Assembly (GAMA) survey in the redshift range of 0.002 < z < 0.06 using Structural Investigation of Galaxies via Model Analysis, a wrapper around GALFIT3. To achieve robust profile measurements, we use a novel approach of repeatedly fitting the galaxies, varying the input parameters to sample a large fraction of the input parameter space. Using this method, we reduce the catastrophic failure rate significantly and verify the confidence in the fit independently of chi(2). Additionally, using the median of the final fitting values and the 16th and 84th percentile produces more realistic error estimates than those provided by GALFIT, which are known to be underestimated. We use the results of our decompositions to analyse the stellar mass - half-light radius relations of bulges, discs and spheroids. We further investigate the association of components with a parent disc or elliptical relation to provide definite z = 0 disc and spheroid M-star-R-e relations. We conclude by comparing our local disc and spheroid M-star - R-e to simulated data from EAGLE and high-redshift data from Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey-Ultra Deep Survey. We show the potential of using the M-star-R-e relation to study galaxy evolution in both cases but caution that for a fair comparison, all data sets need to be processed and analysed in the same manner. C1 [Lange, Rebecca; Moffett, Amanda J.; Driver, Simon P.; Robotham, Aaron S. G.; Lagos, Claudia del P.; Davies, Luke J. M.; Kafle, Prajwal R.; Wright, Angus H.] Univ Western Australia, Int Ctr Radio Astron Res, M468,35 Stirling Highway, Crawley, WA 6009, Australia. [Driver, Simon P.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Lagos, Claudia del P.] Australian Res Council Ctr Excellence All Sky Ast, 44 Rosehill St, Redfern, NSW 2016, Australia. [Kelvin, Lee S.; Baldry, Ivan] Liverpool John Moores Univ, Astrophys Res Inst, IC2,Liverpool Sci Pk,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England. [Conselice, Christopher; Margalef-Bentabol, Berta; Kennedy, Rebecca] Univ Nottingham, Sch Phys & Astron, Univ Pk, Nottingham NG7 2RD, England. [Alpaslan, Mehmet] NASA, Ames Res Ctr, N232 Moffett Field, Mountain View, CA 94035 USA. [Bland-Hawthorn, Joss; Hopkins, Andrew M.] Univ Sydney, Sch Phys A28, Sydney Inst forAstron, Sydney, NSW 2006, Australia. [Bremer, Malcolm; Phillipps, Steven] Univ Bristol, Sch Phys, Astrophys Grp, Bristol BS8 1TL, Avon, England. [Brough, Sarah] Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia. [Cluver, Michelle] Univ Western Cape, Dept Phys & Astron, Robert Sobukwe Rd, ZA-7535 Bellville, South Africa. [Colless, Matthew] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Haussler, Boris] European Southern Observ, Alonso de Cordova 3107, Santiago, Chile. [Holwerda, Benne W.] Leiden Univ, Sterrenwacht Leiden, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands. [Liske, Jochen] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. [Popescu, Cristina C.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Leighton Bldg, Preston PR1 2HE, Lancs, England. [Popescu, Cristina C.] Romanian Acad, Astron Inst, Str Cutitul Argint 5, Bucharest, Romania. [Taylor, Edward N.] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia. [Tuffs, Richard] Max Planck Inst Kernphys, Saupfercheckweg 1, D-69117 Heidelberg, Germany. [van Kampen, Eelco] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. RP Lange, R; Driver, SP (reprint author), Univ Western Australia, Int Ctr Radio Astron Res, M468,35 Stirling Highway, Crawley, WA 6009, Australia.; Driver, SP (reprint author), Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. EM rebecca.lange@icrar.org; simon.driver@icrar.org FU International Centre for Radio Astronomy Research; University of Western Australia; Australian Research Council [FT140101166]; Discovery Early Career Researcher Award [DE150100618]; ESO Telescopes at the La Silla Paranal Observatory [179.A-2004]; STFC (UK); ARC (Australia); AAO FX RL would like to acknowledge funding from the International Centre for Radio Astronomy Research and the University of Western Australia. SB acknowledges the funding support from the Australian Research Council through a Future Fellowship (FT140101166). CL is funded by a Discovery Early Career Researcher Award (DE150100618).; 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 Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programs including GALEX MIS, VST KiDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT and ASKAP providing UV to radio coverage. The VISTA VIKING data used in this paper are based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 179.A-2004. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO, and the participating institutions. The GAMA website is http://www.gama-survey.org/. NR 109 TC 2 Z9 2 U1 3 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 21 PY 2016 VL 462 IS 2 BP 1470 EP 1500 DI 10.1093/mnras/stw1495 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DX8XE UT WOS:000384674100023 ER PT J AU Sbarrato, T Ghisellini, G Tagliaferri, G Perri, M Madejski, GM Stern, D Boggs, SE Christensen, FE Craig, WW Hailey, CJ Harrison, FA Zhang, WW AF Sbarrato, T. Ghisellini, G. Tagliaferri, G. Perri, M. Madejski, G. M. Stern, D. Boggs, S. E. Christensen, F. E. Craig, W. W. Hailey, C. J. Harrison, F. A. Zhang, W. W. TI Extremes of the jet-accretion power relation of blazars, as explored by NuSTAR SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; quasars: general; quasars: individual: B0222+185; quasars: individual: S5 0014+813; X-rays: general ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; HIGH-REDSHIFT QUASARS; LARGE-AREA TELESCOPE; RADIO-LOUD QUASARS; X-RAY TELESCOPE; RELATIVISTIC JETS; BLACK-HOLES; VIEW; SPECTROSCOPY AB Hard X-ray observations are crucial to study the non-thermal jet emission from high-redshift, powerful blazars. We observed two bright z > 2 flat-spectrum radio quasars (FSRQs) in hard X-rays to explore the details of their relativistic jets and their possible variability. S5 0014+81 (at z = 3.366) and B0222+185 (at z = 2.690) have been observed twice by the Nuclear Spectroscopic Telescope Array (NuSTAR) simultaneously with Swift/X-ray Telescope, showing different variability behaviours. We found that NuSTAR is instrumental to explore the variability of powerful high-redshift blazars, even when no gamma-ray emission is detected. The two sources have proven to have respectively the most luminous accretion disc and the most powerful jet among known blazars. Thanks to these properties, they are located at the extreme end of the jet-accretion disc relation previously found for gamma-ray detected blazars, to which they are consistent. C1 [Sbarrato, T.] Univ Milano Bicocca, Dipartimento Fis G Occhialini, Piazza Sci 3, I-20126 Milan, Italy. [Ghisellini, G.; Tagliaferri, G.] INAF Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy. [Perri, M.] ASI Sci Data Ctr, Via Politecn, I-00133 Rome, Italy. [Perri, M.] INAF Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy. [Madejski, G. M.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Stern, D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, Elektrovej 327, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA. [Harrison, F. A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Sbarrato, T (reprint author), Univ Milano Bicocca, Dipartimento Fis G Occhialini, Piazza Sci 3, I-20126 Milan, Italy. EM tullia.sbarrato@unimib.it OI Sbarrato, Tullia/0000-0002-3069-9399 FU ASI-INAF [I/037/12/0]; National Aeronautics and Space Administration FX We thank the referee for her/his comments, that helped us to improve the paper. We acknowledge financial support from the ASI-INAF grant I/037/12/0. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR operations, software and calibration teams for support with the execution and analysis of these observations. This research has made also use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). 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. Part of this work is based on archival data, software or online services provided by the ASDC. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASDC, Italy. NR 51 TC 0 Z9 0 U1 3 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 21 PY 2016 VL 462 IS 2 BP 1542 EP 1550 DI 10.1093/mnras/stw1730 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DX8XE UT WOS:000384674100028 ER PT J AU Evans, PA Kennea, JA Palmer, DM Bilicki, M Osborne, JP O'Brien, PT Tanvir, NR Lien, AY Barthelmy, SD Burrows, DN Campana, S Cenko, SB D'Elia, V Gehrels, N Marshall, FE Page, KL Perri, M Sbarufatti, B Siegel, MH Tagliaferri, G Troja, E AF Evans, P. A. Kennea, J. A. Palmer, D. M. Bilicki, M. Osborne, J. P. O'Brien, P. T. Tanvir, N. R. Lien, A. Y. Barthelmy, S. D. Burrows, D. N. Campana, S. Cenko, S. B. D'Elia, V. Gehrels, N. Marshall, F. E. Page, K. L. Perri, M. Sbarufatti, B. Siegel, M. H. Tagliaferri, G. Troja, E. TI Swift follow-up of gravitational wave triggers: results from the first aLIGO run and optimization for the future SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational waves; methods: data analysis; gamma-ray burst: general; X-rays: general ID GAMMA-RAY BURSTS; PHOTOMETRIC REDSHIFT CATALOG; BINARY NEUTRON-STARS; X-RAY; LUMINOSITY FUNCTION; EVENT GW150914; HOST GALAXIES; ADVANCED LIGO; JET BREAKS; TELESCOPE AB During its first observing run, in late 2015, the advanced Laser Interferometer Gravitational-wave Observatory facility announced three gravitational wave (GW) triggers to electromagnetic follow-up partners. Two of these have since been confirmed as being of astrophysical origin: both are binary black hole mergers at similar to 500 Mpc; the other trigger was later found not to be astrophysical. In this paper, we report on the Swift follow-up observations of the second and third triggers, including details of 21 X-ray sources detected; none of which can be associated with the GW event. We also consider the challenges that the next GW observing run will bring as the sensitivity and hence typical distance of GW events will increase. We discuss how to effectively use galaxy catalogues to prioritize areas for follow-up, especially in the presence of distance estimates from the GW data. We also consider two galaxy catalogues and suggest that the high completeness at larger distances of the 2MASS Photometric Redshift catalogue makes it very well suited to optimize Swift follow-up observations. C1 [Evans, P. A.; Osborne, J. P.; O'Brien, P. T.; Tanvir, N. R.; Page, K. L.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Kennea, J. A.; Burrows, D. N.; Sbarufatti, B.; Siegel, M. H.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Palmer, D. M.] Los Alamos Natl Lab, B244, Los Alamos, NM 87545 USA. [Bilicki, M.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Bilicki, M.] Univ Zielona Gora, Janusz Gil Inst Astron, Ul Lubuska 2, PL-65265 Zielona Gora, Poland. [Lien, A. Y.; Barthelmy, S. D.; Cenko, S. B.; Gehrels, N.; Marshall, F. E.; Troja, E.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. [Campana, S.; Sbarufatti, B.; Tagliaferri, G.] Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, Italy. [Cenko, S. B.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [D'Elia, V.; Perri, M.] Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, RM, Italy. [D'Elia, V.; Perri, M.] ASI Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy. [Troja, E.] Univ Maryland, Dept Phys & Astron, College Pk, MD 20742 USA. RP Evans, PA (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. EM pae9@leicester.ac.uk OI Bilicki, Maciej/0000-0002-3910-5809; Sbarufatti, Boris/0000-0001-6620-8347 FU National Aeronautics and Space Administration; National Science Foundation; UK Space Agency; ASI [I/004/11/1]; Netherlands Organisation for Scientific Research, NWO [614.001.451]; European Research Council [279396]; Polish National Science Centre [UMO-2012/07/D/ST9/02785] FX We thank Andras Kovacs for helpful discussion on galaxy catalogues. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. 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 XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. This research has also made use of the SIMBAD data base, operated at CDS, Strasbourg, France. The GW probability maps and our related galaxy maps are in HEALPIX format (Gorski et al. 2005). PAE, JPO and KLP acknowledge UK Space Agency support. SC and GT acknowledge ASI for support (contract I/004/11/1). MB is supported by the Netherlands Organisation for Scientific Research, NWO, through grant number 614.001.451; through FP7 grant number 279396 from the European Research Council; and by the Polish National Science Centre under contract #UMO-2012/07/D/ST9/02785. NR 78 TC 5 Z9 5 U1 6 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 21 PY 2016 VL 462 IS 2 BP 1591 EP 1602 DI 10.1093/mnras/stw1746 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DX8XE UT WOS:000384674100032 ER PT J AU Rappaport, S Lehmann, H Kalomeni, B Borkovits, T Latham, D Bieryla, A Ngo, H Mawet, D Howell, S Horch, E Jacobs, TL LaCourse, D Sodor, A Vanderburg, A Pavlovski, K AF Rappaport, S. Lehmann, H. Kalomeni, B. Borkovits, T. Latham, D. Bieryla, A. Ngo, H. Mawet, D. Howell, S. Horch, E. Jacobs, T. L. LaCourse, D. Sodor, A. Vanderburg, A. Pavlovski, K. TI A quintuple star system containing two eclipsing binaries SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries : close; binaries: eclipsing; binaries: general; binaries: spectroscopic; binaries: visual ID RADIAL-VELOCITIES; TIDAL FRICTION; MULTIPLE STARS; CLOSE BINARIES; DATA RELEASE; SKY SURVEY; DATA SET; KEPLER; EVOLUTION; CATALOG AB We present a quintuple star system that contains two eclipsing binaries. The unusual architecture includes two stellar images separated by 11 arcsec on the sky: EPIC 212651213 and EPIC 212651234. The more easterly image (212651213) actually hosts both eclipsing binaries which are resolved within that image at 0.09 arcsec, while the westerly image (212651234) appears to be single in adaptive optics (AO), speckle imaging, and radial velocity (RV) studies. The 'A' binary is circular with a 5.1-d period, while the 'B' binary is eccentric with a 13.1-d period. The gamma velocities of the A and B binaries are different by similar to 10 km s(-1). That, coupled with their resolved projected separation of 0.09 arcsec, indicates that the orbital period and separation of the 'C' binary (consisting of A orbiting B) are similar to 65 yr and similar or equal to 25 au, respectively, under the simplifying assumption of a circular orbit. Motion within the C orbit should be discernible via future RV, AO, and speckle imaging studies within a couple of years. The C system (i.e. 212651213) has an RV and proper motion that differ from that of 212651234 by only similar to 1.4 km s(-1) and similar to 3 mas yr(-1). This set of similar space velocities in three dimensions strongly implies that these two objects are also physically bound, making this at least a quintuple star system. C1 [Rappaport, S.; Kalomeni, B.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Rappaport, S.; Kalomeni, B.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Lehmann, H.] Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany. [Kalomeni, B.] Ege Univ, Dept Astron & Space Sci, TR-35100 Izmir, Turkey. [Borkovits, T.] Univ Szeged, Baja Astron Observ, Kt 766, H-6500 Baja, Hungary. [Latham, D.; Bieryla, A.; Vanderburg, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Ngo, H.] CALTECH, Div Geol & Planetary Sci, 1200 E Calif Blvd MC 150-21, Pasadena, CA 91125 USA. [Mawet, D.] CALTECH, Dept Astron, MC 249-17,1200 E Calif Blvd, Pasadena, CA 91125 USA. [Mawet, D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Howell, S.] NASA, Ames Res Ctr, Kepler & Missions K2, POB 1,M-S 244-30, Moffett Field, CA 94035 USA. [Horch, E.] Southern Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA. [Jacobs, T. L.] 12812 SE 69th Pl, Bellevue, WA 98006 USA. [LaCourse, D.] 7507 52nd Pl NE, Marysville, WA 98270 USA. [Sodor, A.] MTA CSFK, Konkoly Observ, Konkoly Thege M Ut 15-17, H-1121 Budapest, Hungary. [Pavlovski, K.] Univ Zagreb, Fac Sci, Dept Phys, Bijenicka Cesta 32, Zagreb 10000, Croatia. RP Rappaport, S (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA.; Rappaport, S (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM sar@mit.edu OI Ngo, Henry/0000-0001-5172-4859 FU NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G]; NSF Graduate Research Fellowship [DGE 1144152]; Turkish Scientific and Technical Research Council [TUBITAK-112T766, TUBITAK-BIDEP 2219]; Croatian HRZZ grant [2014-09-8656]; Hungarian NKFIH Grant [K-115709]; Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences; NKFIH [OTKA K-113117]; Lendulet grant of the Hungarian Academy of Sciences [LP2012-31] FX We are grateful to Mark Everett for help with the WIYN observations. We thank Alan Levine for helpful discussions about this system. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. Based, in part, on data from CMC15 Data Access Service at CAB (INTA-CSIC). This work was based on observations at the W. M. Keck Observatory granted by the California Institute of Technology. We thank the observers who contributed to the measurements reported here and acknowledge the efforts of the Keck Observatory staff. We extend special thanks to those of Hawaiian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. AV is supported by the NSF Graduate Research Fellowship, Grant No. DGE 1144152. EH is grateful for support from NASA's Ames Research Center that allowed him to participate in the speckle observations and analysis. BK gratefully acknowledges the support provided by the Turkish Scientific and Technical Research Council (TUBITAK-112T766 and TUBITAK-BIDEP 2219). KP was supported by the Croatian HRZZ grant 2014-09-8656. AS acknowledges the financial support of the Hungarian NKFIH Grant K-115709 and the Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences. TB and AS acknowledge the financial support of the NKFIH Grant OTKA K-113117. The Konkoly observations were supported by the Lendulet grant LP2012-31 of the Hungarian Academy of Sciences. NR 57 TC 1 Z9 1 U1 3 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 21 PY 2016 VL 462 IS 2 BP 1812 EP 1825 DI 10.1093/mnras/stw1745 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DX8XE UT WOS:000384674100046 ER PT J AU Srivastava, MK Banerjee, DPK Ashok, NM Venkataraman, V Sand, D Diamond, T AF Srivastava, Mudit K. Banerjee, D. P. K. Ashok, N. M. Venkataraman, V. Sand, D. Diamond, T. TI Near-infrared studies of V2944 Ophiuchi (Nova Ophiuchi 2015) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE line: identification; techniques: photometric; techniques: spectroscopic; stars: individual: V2944 Oph; novae, cataclysmic variables ID RECOMBINATION-LINE-INTENSITIES; 0.8-2.5 MICRON SPECTROSCOPY; NEUTRAL OXYGEN SPECTRUM; CLASSICAL NOVAE; T PYXIDIS; HYDROGENIC IONS; 2006 OUTBURST; EARLY DECLINE; RS-OPHIUCHI; EVOLUTION AB We present multi-epoch near-infrared observations of Nova Ophiuchi 2015 which was discovered during outburst in March 2015. This nova showed a few special properties viz. (i) it displayed an unusual prolonged flat-top light curve which does not easily fit into known classes of nova light curves, (ii) it showed evidence for possessing an evolved secondary in the outbursting binary system, and (iii) it made a rare reverse hybrid transition from the He/N class to Fe II class early during its outburst. The present studies focus on the spectroscopic evolution of the object around maximum light and early decline. We show that there was a unique, rapid strengthening and decline in the He 1.0831, 2.0581 mu m line strengths during this stage, wherein the nova combined the traits of both the He/N and Fe II classes. Possible causes for this behaviour are discussed. The relative strengths of the Ly beta fluoresced OI 0.8446, 1.1287 mu m lines are used to estimate the reddening to the nova. A recombination Case B analysis of the early spectra is used to set constraints on the electron density and emission measure, and a later time spectrum when the ejecta were optically thin is used to estimate the ejecta mass to be (0.95-1.9) x 10(-4) M-circle dot. Power-law fits made to study the evolution of the continuum, show a fairly constant slope which differs from the trend generally expected during a nova's evolution viz. beginning with a blackbody and evolving to a free-free distribution at later stages. C1 [Srivastava, Mudit K.; Banerjee, D. P. K.; Ashok, N. M.; Venkataraman, V.] Phys Res Lab, Astron & Astrophys Div, Ahmadabad 380009, Gujarat, India. [Sand, D.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Diamond, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Srivastava, MK; Banerjee, DPK; Ashok, NM (reprint author), Phys Res Lab, Astron & Astrophys Div, Ahmadabad 380009, Gujarat, India. EM mudit@prl.res.in; orion@prl.res.in; ashok@prl.res.in FU Department of Space, Government of India; National Aeronautics and Space Administration [NNH14CK55B] FX We are grateful to the anonymous referee for several helpful suggestions that have improved the content and presentation of the paper. The research work at the Physical Research Laboratory is funded by the Department of Space, Government of India. We acknowledge the use of data from the AAVSO data base. DS is a visiting astronomer at the Infrared Telescope Facility which is operated by the University of Hawaii under contract NNH14CK55B with the National Aeronautics and Space Administration. NR 62 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 21 PY 2016 VL 462 IS 2 BP 2074 EP 2084 DI 10.1093/mnras/stw1807 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DX8XE UT WOS:000384674100066 ER PT J AU Britto, RJ Bottacini, E Lott, B Razzaque, S Buson, S AF Britto, Richard J. Bottacini, Eugenio Lott, Benoit Razzaque, Soebur Buson, Sara TI FERMI-LAT OBSERVATIONS OF THE 2014 MAY-JULY OUTBURST FROM 3C 454.3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; gamma rays: galaxies; quasars: individual (3C 454.3) ID LARGE-AREA TELESCOPE; GAMMA-RAY EMISSION; EXTRAGALACTIC BACKGROUND LIGHT; BRIGHT BLAZARS; MULTIWAVELENGTH OBSERVATIONS; DETECTED BLAZARS; PAIR PRODUCTION; SOURCE CATALOG; CRAZY-DIAMOND; 2009 DECEMBER AB A prominent outburst of the flat spectrum radio quasar 3C 454.3 was observed in 2014 June with the Fermi Large Area Telescope. This outburst was characterized by a three-stage light-curve pattern-plateau, flare, and post-flare-that occurred from 2014 May to July, in a similar pattern as observed during the exceptional outburst in 2010 November. The highest flux of the outburst reported in this paper occurred during 2014 June 7-29, showing a multiple-peak structure in the light-curves. The average flux in these 22 days was found to be F[E > 100 MeV] = (7.2 +/- 0.2) x 10(-6) ph cm(-2) s(-1), with a spectral index, for a simple power law, of Gamma = 2.04 +/- 0.01. That made this outburst the first gamma-ray high state of 3C 454.3 ever to be detected by Fermi with such a hard spectrum over several days. The highest flux was recorded on 2014 June 15, in a 3 hr bin, at MJD 56823.5625, at a level of F[E > 100 MeV] = (17.6 +/- 1.9) x 10(-6) ph cm(-2) s(-1). The rise time of one of the short subflares was found to be T-r = 1200 +/- 700 s at MJD. =. 56827, when the flux increased from 4 to 12 x 10(-6) ph cm(-2) s(-1). Several photons above 20 GeV were collected during this outburst, including one at 45 GeV on MJD 56827, constraining the gamma-ray emission region to be located close to the outer boundary of the broad-line region, leading to fast flux variability. C1 [Britto, Richard J.; Razzaque, Soebur] Univ Johannesburg, Dept Phys, POB 524, ZA-2006 Auckland Pk, South Africa. [Bottacini, Eugenio] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Lott, Benoit] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, UMR 5797, CNRS,IN2P3, F-33175 Gradignan, France. [Buson, Sara] Ist Nazl Fis Nucl, Sez Padova, I-34131 Padua, Italy. [Buson, Sara] Univ Padua, Dipartimento Fis G Galilei, I-34131 Padua, Italy. [Britto, Richard J.] Univ Free State, Dept Phys, POB 339, ZA-9300 Bloemfontein, South Africa. [Buson, Sara] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Buson, Sara] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA. RP Britto, RJ (reprint author), Univ Johannesburg, Dept Phys, POB 524, ZA-2006 Auckland Pk, South Africa.; Britto, RJ (reprint author), Univ Free State, Dept Phys, POB 339, ZA-9300 Bloemfontein, South Africa. EM brittor@ufs.ac.za; eugenio.bottacini@stanford.edu; lott@cenbg.in2p3.fr; srazzaque@uj.ac.za; sara.buson@nasa.gov FU NASA [NNX13AO84G, NNX13AF13G]; National Research Foundation, South Africa; South African Gamma-ray Astronomy Programme (SA-GAMMA); Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France FX 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.; E. B. acknowledges NASA grants NNX13AO84G and NNX13AF13G.; R.J.B. and S.R. acknowledge support from the National Research Foundation, South Africa and the South African Gamma-ray Astronomy Programme (SA-GAMMA). NR 61 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 162 DI 10.3847/0004-637X/830/2/162 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA4LG UT WOS:000386583400014 ER PT J AU Brosius, JW Daw, AN Inglis, AR AF Brosius, Jeffrey W. Daw, Adrian N. Inglis, Andrew R. TI QUASI-PERIODIC FLUCTUATIONS AND CHROMOSPHERIC EVAPORATION IN A SOLAR FLARE RIBBON OBSERVED BY HINODE/EIS, IRIS, AND RHESSI SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: chromosphere; Sun: flares; Sun: oscillations; Sun: UV radiation; Sun: X-rays, gamma-rays ID HARD X-RAY; ULTRAVIOLET IMAGING SPECTROMETER; BRAGG CRYSTAL SPECTROMETER; HIGH TIME RESOLUTION; MAGNETIC RECONNECTION; EXTREME-ULTRAVIOLET; IMPULSIVE PHASE; ATOMIC DATABASE; SPECTROSCOPIC OBSERVATIONS; ELECTRON ACCELERATION AB The Hinode/Extreme-ultraviolet Imaging Spectrometer (EIS) obtained rapid cadence (11.2 s) EUV stare spectra of an M7.3 flare ribbon in AR 12036 on 2014 April 18. Quasi-periodic (P approximate to 75.6 +/- 9.2 s) intensity fluctuations occurred in emission lines of O IV, Mg VI, Mg VII, Si VII, Fe XIV, and Fe XVI during the flare's impulsive rise, and ended when the maximum intensity in Fe XXIII was reached. The profiles of the O IV-Fe XVI lines reveal that they were all redshifted during most of the interval of quasi-periodic intensity fluctuations, while the Fe XXIII profile revealed multiple components including one or two highly blueshifted ones. This indicates that the flare underwent explosive chromospheric evaporation during its impulsive rise. Fluctuations in the relative Doppler velocities were seen, but their amplitudes were too subtle to extract significant quasi-periodicities. RIIESSI detected 25-100 keV hard-X-ray sources in the ribbon near the EIS slit's pointing position during the peaks in the EIS intensity fluctuations. The observations are consistent with a series of energy injections into the chromosphere by nonthermal particle beams. Electron densities derived with Fe XIV (4.6 x 10(10) cm(-3)) and Mg VII (7.8 x 10(9) cm(-3)) average line intensity ratios during the interval of quasi-periodic intensity fluctuations, combined with the radiative loss function of an optically thin plasma, yield radiative cooling times of 32 s at 2.0 x 10(6) K, and 46 s at 6.3 x 10(5) K (about half the quasi-period); assuming Fe XIV's density for Fe XXIII yields a radiative cooling time of 10(3) s (13 times the quasi-period) at 1.4 x 10(7) K. C1 [Brosius, Jeffrey W.; Inglis, Andrew R.] Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Solar Phys Lab, Code 671, Greenbelt, MD 20771 USA. [Daw, Adrian N.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Code 671, Greenbelt, MD 20771 USA. RP Brosius, JW (reprint author), Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Solar Phys Lab, Code 671, Greenbelt, MD 20771 USA. EM Jeffrey.W.Brosius@nasa.gov FU Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract FX Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners; it is operated by these agencies in cooperation with ESA and NSC (Norway). IRIS is a NASA Small Explorer mission developed and operated by LMSAL and partner institutions with mission operations executed at NASA Ames Research Center and major contributions to downlink communications funded by the Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract. The AIA data used are provided courtesy of NASA/SDO and the AIA science team. CHIANTI is a collaborative project involving George Mason University (USA), the University of Michigan (USA), and the University of Cambridge (UK). We thank the anonymous referee for valuable comments that helped improve the manuscript. NR 83 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 101 DI 10.3847/0004-637X/830/2/101 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA3FZ UT WOS:000386488200004 ER PT J AU Faggi, S Villanueva, GL Mumma, MJ Brucato, JR Tozzi, GP Oliva, E Massi, F Sanna, N Tozzi, A AF Faggi, S. Villanueva, G. L. Mumma, M. J. Brucato, J. R. Tozzi, G. P. Oliva, E. Massi, F. Sanna, N. Tozzi, A. TI DETAILED ANALYSIS OF NEAR-IR WATER (H2O) EMISSION IN COMET C/2014 Q2 (LOVEJOY) WITH THE GIANO/TNG SPECTROGRAPH SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; comets: individual (C/2014 Q2 Lovejoy); instrumentation: spectrographs; methods: data analysis ID C/1996 B2 HYAKUTAKE; O1 HALE-BOPP; INFRARED-SPECTRUM; HALLEY; ORIGIN; FLUORESCENCE; MOLECULES; ETHANE; VAPOR AB We observed the Oort cloud comet C/2014 Q2 (Lovejoy) on 2015 January 31 and February 1 and 2 at a heliocentric distance of 1.3 au and geocentric distance of 0.8 au during its approach to the Sun. Comet Lovejoy was observed with GIANO, the near-infrared high-resolution spectrograph mounted at the Nasmyth-A focus of the TNG (Telescopio Nazionale Galileo) telescope in La Palma, Canary Islands, Spain. We detected strong emissions of radical CN and water, along with many emission features of unidentified origin, across the 1-2.5 mu m region. Spectral lines from eight ro-vibrational bands of H2O were detected, six of them for the first time. We quantified the water production rate [Q(H2O), (3.11 +/- 0.14) x 10(29) s(-1)] by comparing the calibrated line fluxes with the Goddard full non-resonance cascade fluorescence model for H2O. The production rates of ortho-water [Q(H2O)(ORTHO), (2.33 +/- 0.11) x 10(29) s(-1)] and para-water [Q(H2O)(PARA), (0.87 +/- 0.21) x 1029 s(-1)] provide a measure of the ortho-to-para ratio (2.70 +/- 0.76)). The confidence limits are not small enough to provide a critical test of the nuclear spin temperature. C1 [Faggi, S.; Brucato, J. R.; Tozzi, G. P.; Oliva, E.; Massi, F.; Sanna, N.; Tozzi, A.] Osserv Astrofis Arcetri, Largo Enrico Fermi 5, I-50125 Florence, IT, Italy. [Faggi, S.] Univ Florence, Dipartimento Fis & Astron, Via G Sansone 1, I-50019 Sesto Fiorentino, FI, Italy. [Villanueva, G. L.; Mumma, M. J.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. RP Faggi, S (reprint author), Osserv Astrofis Arcetri, Largo Enrico Fermi 5, I-50125 Florence, IT, Italy.; Faggi, S (reprint author), Univ Florence, Dipartimento Fis & Astron, Via G Sansone 1, I-50019 Sesto Fiorentino, FI, Italy. EM sfaggi@arcetri.astro.it OI Mumma, Michael/0000-0003-4627-750X NR 40 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 157 DI 10.3847/0004-637X/830/2/157 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA4LG UT WOS:000386583400009 ER PT J AU Hiranaka, K Cruz, KL Douglas, ST Marley, MS Baldassare, VF AF Hiranaka, Kay Cruz, Kelle L. Douglas, Stephanie T. Marley, Mark S. Baldassare, Vivienne F. TI EXPLORING THE ROLE OF SUB-MICRON-SIZED DUST GRAINS IN THE ATMOSPHERES OF RED L0-L6 DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; dust, extinction ID EXTRASOLAR GIANT PLANETS; PROPER-MOTION SURVEY; FIELD L-DWARFS; LOW-MASS STARS; BROWN DWARFS; ULTRACOOL DWARFS; COOL NEIGHBORS; T-DWARFS; CANDIDATE BINARIES; SPEX SPECTROSCOPY AB We examine the hypothesis that the red near-infrared colors of some L dwarfs could be explained by a "dust haze" of small particles in their upper atmospheres. This dust haze would exist in conjunction with the clouds found in dwarfs with more typical colors. We developed a model that uses Mie theory and the Hansen particle size distributions to reproduce the extinction due to the proposed dust haze. We apply our method to 23 young L dwarfs and 23 red field L dwarfs. We constrain the properties of the dust haze including particle size distribution and column density using Markov Chain Monte Carlo methods. We find that sub-micron-range silicate grains reproduce the observed reddening. Current brown dwarf atmosphere models include large-grain (1-100 mu m) dust clouds but not sub-micron dust grains. Our results provide a strong proof of concept and motivate a combination of large and small dust grains in brown dwarf atmosphere models. C1 [Hiranaka, Kay; Cruz, Kelle L.; Baldassare, Vivienne F.] CUNY, Dept Phys & Astron, Hunter Coll, 695 Pk Ave, New York, NY 10065 USA. [Hiranaka, Kay; Cruz, Kelle L.] CUNY, Grad Ctr, 365 Fifth Ave, New York, NY 10016 USA. [Hiranaka, Kay; Cruz, Kelle L.; Douglas, Stephanie T.; Baldassare, Vivienne F.] Amer Museum Nat Hist, Dept Astrophys, Cent Pk West & 79th St, New York, NY 10024 USA. [Douglas, Stephanie T.] Columbia Univ, Dept Astron, 550 West 120th St,Mail Code 5246, New York, NY 10027 USA. [Marley, Mark S.] NASA, Ames Res Ctr, MS-245-3, Moffett Field, CA 94035 USA. [Baldassare, Vivienne F.] Univ Michigan, Dept Astron, 1085 S Univ, Ann Arbor, MI 48109 USA. RP Hiranaka, K (reprint author), CUNY, Dept Phys & Astron, Hunter Coll, 695 Pk Ave, New York, NY 10065 USA.; Hiranaka, K (reprint author), CUNY, Grad Ctr, 365 Fifth Ave, New York, NY 10016 USA.; Hiranaka, K (reprint author), Amer Museum Nat Hist, Dept Astrophys, Cent Pk West & 79th St, New York, NY 10024 USA. EM khiranak@hunter.cuny.edu OI Douglas, Stephanie/0000-0001-7371-2832; Marley, Mark/0000-0002-5251-2943 FU National Science Foundation [AST-1313278]; PSC-CUNY Award; Professional Staff Congress; City University of New York FX We thank our anonymous referee for thorough and helpful comments. This material is based upon work supported by the National Science Foundation under grant No. AST-1313278. Support for this project was provided by a PSC-CUNY Award, jointly funded by The Professional Staff Congress and The City University of New York. NR 67 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 96 DI 10.3847/0004-637X/830/2/96 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA1FK UT WOS:000386337700013 ER PT J AU Kuchner, MJ Silverberg, SM Bans, AS Bhattacharjee, S Kenyon, SJ Debes, JH Currie, T Garcia, L Jung, D Lintott, C McElwain, M Padgett, DL Rebull, LM Wisniewski, JP Nesvold, E Schawinski, K Thaller, ML Grady, CA Biggs, J Bosch, M Cernohous, T Luca, HAD Hyogo, M Wah, LLW Piipuu, A Pineiro, F AF Kuchner, Marc J. Silverberg, Steven M. Bans, Alissa S. Bhattacharjee, Shambo Kenyon, Scott J. Debes, John H. Currie, Thayne Garcia, Luciano Jung, Dawoon Lintott, Chris McElwain, Michael Padgett, Deborah L. Rebull, Luisa M. Wisniewski, John P. Nesvold, Erika Schawinski, Kevin Thaller, Michelle L. Grady, Carol A. Biggs, Joseph Bosch, Milton Cernohous, Tadeas. Luca, Hugo A. Durantini Hyogo, Michiharu Wah, Lily Lau Wan Piipuu, Art Pineiro, Fernanda CA Disk Detective Collaboration TI DISK DETECTIVE: DISCOVERY OF NEW CIRCUMSTELLAR DISK CANDIDATES THROUGH CITIZEN SCIENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; infrared: planetary systems; methods: data analysis; protoplanetary disks; stars: emission line, Be; surveys ID INFRARED-SURVEY-EXPLORER; YOUNG STELLAR OBJECTS; DUSTY DEBRIS DISKS; DIGITAL-SKY-SURVEY; STAR-FORMING REGIONS; EXTRA-SOLAR PLANETS; SPECTROSCOPIC SURVEY; EXOPLANET SYSTEMS; OB ASSOCIATION; BINARY-SYSTEMS AB The Disk Detective citizen science project aims to find new stars with 22 mu m excess emission from circumstellar dust using data from NASA's Wide-field Infrared Survey Explorer (WISE) mission. Initial cuts on the AllWISE catalog provide an input catalog of 277,686 sources. Volunteers then view images of each source online in 10 different bands to identify false positives (galaxies, interstellar matter, image artifacts, etc.). Sources that survive this online vetting are followed up with spectroscopy on the FLWO Tillinghast telescope. This approach should allow us to unleash the full potential of WISE for finding new debris disks and protoplanetary disks. We announce a first list of 37 new disk candidates discovered by the project, and we describe our vetting and follow-up process. One of these systems appears to contain the first debris disk discovered around a star with a white dwarf companion: HD 74389. We also report four newly discovered classical Be stars (HD 6612, HD 7406, HD 164137, and HD 218546) and a new detection of 22 mu m excess around the previously known debris disk host star HD 22128. C1 [Kuchner, Marc J.; McElwain, Michael; Padgett, Deborah L.; Grady, Carol A.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 21230 USA. [Silverberg, Steven M.; Wisniewski, John P.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. [Bans, Alissa S.] Valparaiso Univ, Dept Phys & Astron, Neils Sci Ctr, 1610 Campus Dr East, Valparaiso, IN 46383 USA. [Bhattacharjee, Shambo] Int Space Univ, 1 Rue Jean Dominique Cassini, F-67400 Illkirch Graffenstaden, France. [Kenyon, Scott J.] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. [Debes, John H.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Currie, Thayne] Natl Astron Observ Japan, 650 N Aohokhu Pl, Hilo, HI 96720 USA. [Garcia, Luciano] Univ Nacl Cordoba, Observ Astron Cordoba, Laprida 854,X5000BGR, Cordoba, Argentina. [Jung, Dawoon] Korea Aerosp Res Inst, Lunar Explorat Program Off, 169-84 Gwahak Ro, Daejeon 34133, South Korea. [Lintott, Chris] Denys Wilkinson Bldg Keble Rd, Oxford OX1 3RH, England. [Rebull, Luisa M.] CALTECH, Infrared Proc & Anal Ctr, M-S 314-6 1200 E Calif Blvd, Pasadena, CA 91125 USA. [Nesvold, Erika] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. [Schawinski, Kevin] Swiss Fed Inst Technol, Inst Astron, Wolfgang Pauli Str 27 Bldg HIT, CH-8093 Zurich, Switzerland. [Thaller, Michelle L.] NASA, Headquarters Sci Mission Directorate, 300 E St SW, Washington, DC 20546 USA. [Biggs, Joseph; Bosch, Milton; Cernohous, Tadeas.; Luca, Hugo A. Durantini; Hyogo, Michiharu; Wah, Lily Lau Wan; Piipuu, Art; Pineiro, Fernanda; Disk Detective Collaboration] Disk Detect, Washington, DC USA. RP Kuchner, MJ (reprint author), NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 21230 USA. EM Marc.Kuchner@nasa.gov; silverberg@ou.edu; alissa.s.bans@gmail.com; shambo.bhattacharjee@community.isunet.edu; skenyon@cfa.harvard.edu; debes@stsci.edu; thayne.currie@gmail.com; lucianog@oac.uncor.edu; dwjung@kari.re.kr; cjl@astro.ox.ac.uk; michael.w.mcelwain@nasa.gov; deborah.l.padgett@nasa.gov; rebull@ipac.caltech.edu; wisniewski@ou.edu; enesvold@carnegiescience.edu; kevin.schawinski@phys.ethz.ch; michelle.thaller@nasa.gov; carol.a.grady@nasa.gov OI Kenyon, Scott/0000-0003-0214-609X FU NASA Astrophysics Data Analysis Program [14-ADAP14-0161]; NASA Astrobiology Program via the Goddard Center for Astrobiology; NASA's Science Innovation Fund; Alfred P. Sloan foundation; Google Global Impact award; NASA; NSF; Smithsonian Astrophysical Observatory; Space Telescope Science Institute under U.S. Government [NAG W-2166]; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX We acknowledge support from grant 14-ADAP14-0161 from the NASA Astrophysics Data Analysis Program. M.K. acknowledges funding from the NASA Astrobiology Program via the Goddard Center for Astrobiology and support from NASA's Science Innovation Fund.; Development of the Disk Detectives site was supported by a grant from the Alfred P. Sloan foundation, and the Zooniverse platform is supported by a Google Global Impact award.; WISE is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory (JPL)/California Institute of Technology (Caltech), funded by NASA. 2MASS is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center (IPAC) at Caltech, funded by NASA and the NSF. This paper uses data products produced by the OIR Telescope Data Center, supported by the Smithsonian Astrophysical Observatory.; The DSS was produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. This work has made use of the BeSS database, operated at LESIA, Observatoire de Meudon, France: http://basebe.obspm.fr.; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/.; The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 109 TC 0 Z9 0 U1 3 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 84 DI 10.3847/0004-637X/830/2/84 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA1FK UT WOS:000386337700001 ER PT J AU Liu, N Nittler, LR Alexander, CMO Wang, JH Pignatari, M Jose, J Nguyen, A AF Liu, Nan Nittler, Larry R. Alexander, Conel M. O'D Wang, Jianhua Pignatari, Marco Jose, Jordi Nguyen, Ann TI STELLAR ORIGINS OF EXTREMELY C-13- AND N-15-ENRICHED PRESOLAR SIC GRAINS: NOVAE OR SUPERNOVAE? (vol 820, 140, 2016) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Liu, Nan; Nittler, Larry R.; Alexander, Conel M. O'D; Wang, Jianhua] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. [Pignatari, Marco] Hungarian Acad Sci, Konkoly Observ, Res Ctr Astron & Earth Sci, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest, Hungary. [Pignatari, Marco] Univ Hull, Dept Math & Phys, EA Milne Ctr Astrophys, Kingston Upon Hull HU6 7RX, N Humberside, England. [Jose, Jordi] Univ Politecn Cataluna, EUETIB, Dept Fis, E-08036 Barcelona, Spain. [Jose, Jordi] Inst Estudis Espacials Catalunya, E-08034 Barcelona, Spain. [Nguyen, Ann] NASA, Robert M Walker Lab Space Sci, Astromat Res & Explorat Sci Directorate, Johnson Space Ctr, Houston, TX 77058 USA. [Nguyen, Ann] NASA, Jacobs, Johnson Space Ctr, Houston, TX 77058 USA. RP Liu, N (reprint author), Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. NR 1 TC 0 Z9 0 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 163 DI 10.3847/0004-637X/830/2/163 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA4LG UT WOS:000386583400015 ER PT J AU Noirot, G Vernet, J De Breuck, C Wylezalek, D Galametz, A Stern, D Mei, S Brodwin, M Cooke, EA Gonzalez, AH Hatch, NA Rettura, A Stanford, SA AF Noirot, Gael Vernet, Joel De Breuck, Carlos Wylezalek, Dominika Galametz, Audrey Stern, Daniel Mei, Simona Brodwin, Mark Cooke, Elizabeth A. Gonzalez, Anthony H. Hatch, Nina A. Rettura, Alessandro Stanford, Spencer Adam TI HST GRISM CONFIRMATION OF TWO z similar to 2 STRUCTURES FROM THE CLUSTERS AROUND RADIO-LOUD AGN (CARLA) SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (CARLA J2039-2514, CARLA J0800+4029); galaxies: high-redshift; galaxies: individual (MRC 2036-254, B3 0756+406) ID STELLAR POPULATION SYNTHESIS; MOLONGLO REFERENCE CATALOG; LUMINOUS GALAXY CLUSTER; STAR-FORMATION ACTIVITY; DIGITAL SKY SURVEY; GREATER-THAN 1.5; HIGH-REDSHIFT; X-RAY; IDCS J1426.5+3508; SPECTROSCOPIC CONFIRMATION AB Using Hubble Space Telescope slitless grism data, we report the spectroscopic confirmation of two distant structures at z similar to 2 associated with powerful high-redshift radio-loud active galactic nuclei. (AGNs). These rich structures, likely (forming) clusters, are among the most distant structures currently known, and were identified on the basis of Spitzer/IRAC [3.6]-[4.5] color. We spectroscopically confirm nine members in the field of MRC. 2036 -254, comprising eight star-forming galaxies and the targeted radio galaxy. The median redshift is z = 2.000. We spectroscopically confirm 10 members in the field of B3. 0756+ 406, comprising 8 star-forming galaxies and 2 AGNs, including the targeted radio-loud quasar. The median redshift is z = 1.986. All confirmed members are within 500 kpc (1 arcmin) of the targeted AGNs. We derive median (mean) star-formation rates of similar to 35 M-circle dot yr(-1) (similar to 50 M-circle dot yr(-1)) for the confirmed star-forming members of both structures based on their [O III]lambda 5007 luminosities, and estimate average galaxy stellar masses. <= 1 x 10(11) M-circle dot based on mid-infrared fluxes and spectral energy distribution modeling. Most of our confirmed members are located above the star-forming main. sequence toward starburst galaxies, consistent with clusters at these early epochs being the sites of significant levels of star formation. The structure around MRC. 2036-254 shows an overdensity of IRAC-selected candidate galaxy cluster members consistent with being quiescent galaxies, while the structure around B3. 0756+ 406 shows field values, albeit with many lower limits to colors that could allow an overdensity of faint red quiescent galaxies. The structure around MRC. 2036-254 shows a red sequence of passive galaxy candidates. C1 [Noirot, Gael; Mei, Simona] Univ Paris 07, Univ Paris Sorbonne Cite PSC, F-75205 Paris 13, France. [Noirot, Gael; Vernet, Joel; De Breuck, Carlos] European Southern Observ, Karl Schwarzschildstr 2, D-85748 Garching, Germany. [Noirot, Gael; Stern, Daniel] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Wylezalek, Dominika] Johns Hopkins Univ, Zanvyl Krieger Sch Arts & Sci, 3400 N Charles St, Baltimore, MD 21218 USA. [Galametz, Audrey] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. [Mei, Simona] Univ Paris Diderot, PSL Res Univ, CNRS, GEPI,Observ Paris, 61 Ave Observ, F-75014 Paris, France. [Mei, Simona] CALTECH, Pasadena, CA 91125 USA. [Brodwin, Mark] Univ Missouri, Dept Phys, 5110 Rockhill Rd, Kansas City, MO 64110 USA. [Cooke, Elizabeth A.; Hatch, Nina A.] Univ Nottingham, Sch Phys & Astron, Univ Pk, Nottingham NG7 2RD, England. [Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Rettura, Alessandro] CALTECH, Infrared Proc & Anal Ctr, KS 314-6, Pasadena, CA 91125 USA. [Stanford, Spencer Adam] Univ Calif Davis, Dept Phys, One Shields Ave, Davis, CA 95616 USA. RP Noirot, G (reprint author), Univ Paris 07, Univ Paris Sorbonne Cite PSC, F-75205 Paris 13, France.; Noirot, G (reprint author), European Southern Observ, Karl Schwarzschildstr 2, D-85748 Garching, Germany.; Noirot, G (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM gnoirot@eso.org FU NASA [NAS 5-26555]; Akbari-Mack Postdoctoral Fellowship; Institut Universitaire de France (IUF); STFC; STFC through an Ernest Rutherford Fellowship FX We thank our anonymous referee for comments and suggestions that improved the quality of this paper. This work 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. This work is also based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This work is also based in part on observations made with the 200 inch Hale Telescope, Palomar Observatory, operated by the California Institute of Technology. D.W. acknowledges support by Akbari-Mack Postdoctoral Fellowship. S.M. acknowledges financial support from the Institut Universitaire de France (IUF), of which she is senior member. E.A.C. acknowledges the support of the STFC. N.A.H. acknowledges support from STFC through an Ernest Rutherford Fellowship. NR 107 TC 2 Z9 2 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 90 DI 10.3847/0004-637X/830/2/90 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA1FK UT WOS:000386337700007 ER PT J AU Penny, MT Henderson, CB Clanton, C AF Penny, Matthew T. Henderson, Calen B. Clanton, Christian TI IS THE GALACTIC BULGE DEVOID OF PLANETS? SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: bulge; Galaxy: disk; gravitational lensing: micro; planetary systems ID SYNTHESIZING EXOPLANET DEMOGRAPHICS; MICROLENSING OPTICAL DEPTH; LEGACY SCIENCE PROPOSAL; PARALLAX SATELLITE MASS; ESA EUCLID MISSION; LATE-TYPE STAR; M DWARF; BROWN DWARF; GIANT PLANET; SNOW LINE AB We consider a sample of 31 exoplanetary systems detected by gravitational microlensing and investigate whether or not the estimated distances to these systems conform to the Galactic distribution of planets expected from models. We derive the expected distribution of distances and relative proper motions from a simulated microlensing survey, correcting for the dominant selection effects that affect the sensitivity of planet detection as a function of distance, and compare it to the observed distribution using Anderson-Darling (AD) hypothesis testing. Taking the relative abundance of planets in the bulge to that in the disk, f(bulge), as a model parameter, we find that our model is consistent with the observed distribution only for f(bulge) < 0.54 (for a p-value threshold of 0.01) implying that the bulge may be devoid of planets relative to the disk. Allowing for a dependence of planet abundance on metallicity and host mass, or an additional dependence of planet sensitivity on event timescale, does not restore consistency for f(bulge) = 1. We examine the distance estimates of some events in detail, and conclude that some parallax-based estimates could be significantly in error. Only by combining the removal of one problematic event from our sample and the inclusion of strong dependences of planet abundance or detection sensitivity on host mass, metallicity, and event timescale are we able to find consistency with the hypothesis that the bulge and disk have equal planet abundance. C1 [Penny, Matthew T.] Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA. [Henderson, Calen B.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Clanton, Christian] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Penny, MT (reprint author), Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA. EM penny@astronomy.ohio-state.edu FU NASA through the Sagan Fellowship Program FX We thank Radek Poleski, Wei Zhu, Andy Gould, Dave Bennett, and the referee for their suggestions. Work by M.T.P. was performed in part under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. Work by C.B.H. was supported 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 100 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 150 DI 10.3847/0004-637X/830/2/150 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA4LG UT WOS:000386583400002 ER PT J AU Peverati, R Bera, PP Lee, TJ Head-Gordon, M AF Peverati, Roberto Bera, Partha P. Lee, Timothy J. Head-Gordon, Martin TI INSIGHTS INTO HYDROCARBON CHAIN AND AROMATIC RING FORMATION IN THE INTERSTELLAR MEDIUM: COMPUTATIONAL STUDY OF THE ISOMERS OF C4H3+ C6H3+ AND C6H5+ AND THEIR FORMATION PATHWAYS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; evolution; ISM: clouds ID EXTRAORDINARY SOURCES ANALYSIS; CROSSED-BEAM REACTION; PHENYL CATION; HERSCHEL OBSERVATIONS; CHEMICAL-DYNAMICS; MOLECULAR CLOUDS; EXCITED-STATES; ROAMING ATOMS; ACETYLENE; CHEMISTRY AB Small hydrocarbons such as acetylene is present in circumstellar envelopes of carbon-rich stars, but the processes that yield larger molecules, and eventually polycyclic aromatic hydrocarbons (PAHs), remain poorly understood. To gain additional insight into the early steps of such processes, electronic structure calculations were performed on the potential energy surfaces of C4H3+, C6H3+ and C6H5+. The results establish reactive pathways from acetylene and its ion to formation of the first aromatic ring. We characterize the stable isomers, their spectroscopic properties, and many of the transition structures that represent barriers to isomerization. The pathways to stabilized C4H3+ and C6H3+ are most likely to arise from unimolecular decomposition of hot C4H4+ and C6H4+ by H atom elimination. By contrast, we found an ion-molecule pathway to C6H5+ to be very stable to fragmentation and elimination reactions even without collisional stabilization. This aromatic species is a good nucleation center for the growth of larger PAHs in interstellar conditions. C1 [Peverati, Roberto; Head-Gordon, Martin] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA. [Peverati, Roberto; Head-Gordon, Martin] Lawrence Berkeley Natl Lab, Div Chem Sci, Berkeley, CA 94720 USA. [Bera, Partha P.] NASA, BAERI, Space Sci & Astrobiol Div, Ames Res Ctr, Mountain View, CA 94035 USA. [Bera, Partha P.; Lee, Timothy J.] NASA, Ames Res Ctr, MS 245-1, Mountain View, CA 94035 USA. RP Head-Gordon, M (reprint author), Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA.; Head-Gordon, M (reprint author), Lawrence Berkeley Natl Lab, Div Chem Sci, Berkeley, CA 94720 USA. EM mhg@cchem.berkeley.edu RI Lee, Timothy/K-2838-2012 FU NASA Carbon in the Galaxy consortium grant [NNH10ZDA001N]; National Aeronautics and Space Administration through the NASA Astrobiology Institute [NNH13ZDA017C] FX The authors gratefully acknowledge financial support from the NASA Carbon in the Galaxy consortium grant NNH10ZDA001N. Some of this material is based upon work supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement Notice NNH13ZDA017C issued through the Science Mission Directorate. NR 68 TC 0 Z9 0 U1 10 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 128 DI 10.3847/0004-637X/830/2/128 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA3FZ UT WOS:000386488200031 ER PT J AU Tombesi, F Reeves, JN Kallman, T Reynolds, CS Mushotzky, RF Braito, V Behar, E Leutenegger, MA Cappi, M AF Tombesi, F. Reeves, J. N. Kallman, T. Reynolds, C. S. Mushotzky, R. F. Braito, V. Behar, E. Leutenegger, M. A. Cappi, M. TI THE COMPLEX CIRCUMNUCLEAR ENVIRONMENT OF THE BROAD-LINE RADIO GALAXY 3C 390.3 REVEALED BY CHANDRA HETG SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: active; line: identification; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; ULTRA-FAST OUTFLOWS; ACCRETION-DISK WINDS; X-RAY-ABSORPTION; REFLECTION GRATING SPECTROMETER; SUPERMASSIVE BLACK-HOLE; HIGHLY IONIZED OUTFLOWS; XMM-NEWTON; WARM ABSORBERS; SUZAKU VIEW AB We present the first high spectral resolution X-ray observation of the broad-line radio galaxy 3C 390.3 obtained with the high-energy transmission grating spectrometer on board the Chandra X-ray Observatory. The spectrum shows complex emission and absorption features in both the soft X-rays and Fe K band. We detect emission and absorption lines in the energy range E = 700-1000 eV associated with ionized Fe L transitions (Fe XVII-XX). An emission line at the energy of E similar or equal to 6.4 keV consistent with the Fe K alpha is also observed. Our best-fit model requires at least three different components: (i) a hot emission component likely associated with the hot interstellar medium in this elliptical galaxy with temperature kT = 0.5 +/- 0.1 keV; (ii) a warm absorber with ionization parameter log xi = 2.3 +/- 0.5 erg s(-1) cm, column density logN(H) = 20.7 +/- 0.1 cm(-2), and outflow velocity nu(out) < 150 km s(-1); and (iii) a lowly ionized reflection component in the Fe K band likely associated with the optical broad-line region or the outer accretion disk. These evidences suggest the possibility that we are looking directly down the ionization cone of this active galaxy and that the central X-ray source only photoionizes along the unobscured cone. This is overall consistent with the angle-dependent unified picture of active galactic nuclei. C1 [Tombesi, F.; Kallman, T.; Leutenegger, M. A.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Tombesi, F.; Reynolds, C. S.; Mushotzky, R. F.; Behar, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Reeves, J. N.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, 1000 Hilltop Circle, Baltimore, MD 21250 USA. [Reeves, J. N.] Keele Univ, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Braito, V.] Osservatorio Astronomico Brera, INAF, Via Bianchi 46, I-23807 Merate, LC, Italy. [Behar, E.; Cappi, M.] Technion 32000, Dept Phys, IL-32000 Haifa, Israel. INAF IASF Bologna, Via Gobetti 101, I-40129 Bologna, Italy. RP Tombesi, F (reprint author), NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.; Tombesi, F (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM francesco.tombesi@nasa.gov OI Reynolds, Christopher/0000-0002-1510-4860 FU National Aeronautics and Space Administration (NASA) [GO4-15103A]; NASA [NAS8-03060]; EU Horizon research and innovation program under the Marie Sklodowska Curie grant [655324] FX F.T. thanks K. Fukumura, D. Kazanas, and F. Paerels for the useful discussions. F.T. acknowledges support for this work by the National Aeronautics and Space Administration (NASA) through Chandra Award Number GO4-15103A issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. E.B. received funding from the EU Horizon 2020 research and innovation program under the Marie Sklodowska Curie grant agreement No. 655324. NR 75 TC 1 Z9 1 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 98 DI 10.3847/0004-637X/830/2/98 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA3FZ UT WOS:000386488200001 ER PT J AU Umurhan, OM Shariff, K Cuzzi, JN AF Umurhan, Orkan M. Shariff, Karim Cuzzi, Jeffrey N. TI CRITICAL LAYERS AND PROTOPLANETARY DISK TURBULENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; instabilities; protoplanetary disks; turbulence; waves ID VERTICAL-SHEAR INSTABILITY; ROSSBY-WAVE INSTABILITY; BAROCLINIC VORTICITY PRODUCTION; THIN ACCRETION DISKS; SHALLOW-WATER THEORY; VORTEX FORMATION; CONVECTIVE OVERSTABILITY; THERMAL RELAXATION; ANGULAR-MOMENTUM; LINEAR-ANALYSIS AB A linear analysis of the zombie vortex instability (ZVI) is performed in a stratified shearing sheet setting for three model barotropic shear flows. The linear analysis is done by utilizing a Green's function formulation to resolve the critical layers of the associated normal-mode problem. The instability is the result of a resonant interaction between a Rossby wave and a gravity wave that we refer to as Z-modes. The associated critical layer is the location where the Doppler-shifted frequency of a distant Rossby wave equals the local Brunt-Vaisala frequency. The minimum required Rossby number for instability, Ro = 0.2, is confirmed for parameter values reported in the literature. It is also found that the shear layer supports the instability in the limit where stratification vanishes. The ZVI is examined in a jet model, finding that the instability can occur for Ro = 0.05. Nonlinear vorticity forcing due to unstable Z-modes is shown to result in the creation of a jet flow at the critical layer emerging as the result of the competition between the vertical lifting of perturbation radial vorticity and the radial transport of perturbation vertical vorticity. We find that the picture of this instability leading to a form of nonlinearly driven self-replicating pattern of creation and destruction is warranted: a parent jet spawns a growing child jet at associated critical layers. A mature child jet creates a next generation of child jets at associated critical layers of the former while simultaneously contributing to its own destruction via the Rossby wave instability. C1 [Umurhan, Orkan M.; Shariff, Karim; Cuzzi, Jeffrey N.] NASA, Ames Res Ctr, Moffett Field, CA 94053 USA. [Umurhan, Orkan M.] SETI Inst, 189 Bernardo Way, Mountain View, CA 94043 USA. RP Umurhan, OM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94053 USA. EM orkan.m.umurhan@nasa.gov OI Shariff, Karim/0000-0002-7256-2497 NR 48 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 95 DI 10.3847/0004-637X/830/2/95 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA1FK UT WOS:000386337700012 ER PT J AU Wirstrom, ES Charnley, SB Cordiner, MA Ceccarelli, C AF Wirstrom, Eva S. Charnley, Steven B. Cordiner, Martin A. Ceccarelli, Cecilia TI A SEARCH FOR O-2 IN CO-DEPLETED MOLECULAR CLOUD CORES WITH HERSCHEL SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: abundances; ISM: clouds; ISM: molecules; molecular processes ID DENSE INTERSTELLAR CLOUDS; GRAIN CHEMICAL-MODELS; RHO-OPHIUCHI CLOUD; LOW-MASS PROTOSTAR; STAR-FORMATION; DARK CLOUDS; DESORPTION PROCESSES; TENTATIVE DETECTION; HIFI OBSERVATIONS; WATER FORMATION AB The general lack of molecular oxygen in molecular clouds is an outstanding problem in astrochemistry. Extensive searches with the Submillimeter Astronomical Satellite, Odin,. and Herschel have only produced two detections; upper limits to the O-2 abundance in the remaining sources observed are about 1000 times lower than predicted by chemical models. Previous atomic oxygen observations and inferences from observations of other molecules indicated that high abundances of O atoms might be present in dense cores exhibiting large amounts of CO depletion. Theoretical arguments concerning the oxygen gas-grain interaction in cold dense cores suggested that, if O atoms could survive in the gas after most of the rest of the heavy molecular material has frozen out onto dust, then O-2 could be formed efficiently in the gas. Using Herschel HIFI, we searched a small sample of four depletion cores-L1544, L694-2, L429, and. Oph D-for emission in the low excitation O-2 N-J = 3(3)-1(2) line at 487.249 GHz. Molecular oxygen was not detected and we derive upper limits to its abundance in the range of N(O-2)/N(H-2) approximate to (0.6-1.6) x 10(-7). We discuss the absence of O-2 in the light of recent laboratory and observational studies. C1 [Wirstrom, Eva S.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden. [Charnley, Steven B.; Cordiner, Martin A.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Mailstop 691,8800 Greenbelt Rd, Greenbelt, MD 20770 USA. [Cordiner, Martin A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Ceccarelli, Cecilia] Observ Grenoble, Astrophys Lab, BP 53, F-38041 Grenoble 09, France. RP Wirstrom, ES (reprint author), Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden. EM eva.wirstrom@chalmers.se OI Wirstrom, Eva/0000-0002-0656-876X FU Swedish National Space Board; NASA's Origins of Solar Systems Program FX E.S.W. acknowledges generous financial support from the Swedish National Space Board. The work of S.B.C. and M.A.C. was supported by NASA's Origins of Solar Systems Program. NR 72 TC 1 Z9 1 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 102 DI 10.3847/0004-637X/830/2/102 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA3FZ UT WOS:000386488200005 ER PT J AU Silverberg, SM Kuchner, MJ Wisniewski, JP Gagne, J Bans, AS Bhattacharjee, S Currie, TR Debes, JR Biggs, JR Bosch, M Doll, K Durantini-Luca, HA Enachioaie, A Griffith, P Hyogo, M Piniero, F AF Silverberg, Steven M. Kuchner, Marc J. Wisniewski, John P. Gagne, Jonathan Bans, Alissa S. Bhattacharjee, Shambo Currie, Thayne R. Debes, John R. Biggs, Joseph R. Bosch, Milton Doll, Katharina Durantini-Luca, Hugo A. Enachioaie, Alexandru Griffith, Philip, Sr. Hyogo, Michiharu Piniero, Fernanda CA Disk Detective Collaboration TI A NEW M DWARF DEBRIS DISK CANDIDATE IN A YOUNG MOVING GROUP DISCOVERED WITH DISK DETECTIVE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; open clusters and associations: individual (Carina); stars: low-mass ID LOW-MASS STARS; CIRCUMSTELLAR DISKS; KINEMATIC GROUPS; BURNING LIMIT; HR 8799; ASSOCIATION; EVOLUTION; PLANETS; SEARCH; NEARBY AB We used the Disk Detective citizen science project and the BANYAN II Bayesian analysis tool to identify a new candidate member of a nearby young association with infrared excess. WISE J080822.18-644357.3, an M5.5-type debris disk system with significant excess at both 12 and 22 mu m, is a likely member (similar to 90% BANYAN II probability) of the similar to 45 Myr old Carina association. Since this would be the oldest M dwarf debris disk detected in a moving group, this discovery could be an important constraint on our understanding of M dwarf debris disk evolution. C1 [Silverberg, Steven M.; Wisniewski, John P.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. [Kuchner, Marc J.] NASA, Goddard Space Flight Ctr, Code 667, Greenbelt, MD 20771 USA. [Gagne, Jonathan] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. [Bans, Alissa S.] Adler Planetarium, 1300 S Lake Shore Dr, Chicago, IL 60605 USA. [Bhattacharjee, Shambo] Univ Leeds, Sch Stat, Leeds LS2 9JT, W Yorkshire, England. [Currie, Thayne R.] Natl Astron Observ Japan, Subaru Telescope, Tokyo, Japan. [Debes, John R.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. RP Silverberg, SM (reprint author), Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. EM silverberg@ou.edu OI Doll, Katharina/0000-0002-2993-9869; Gagne, Jonathan/0000-0002-2592-9612; Bhattacharjee, Shambo/0000-0002-0862-9108 NR 45 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 20 PY 2016 VL 830 IS 2 AR L28 DI 10.3847/2041-8205/830/2/L28 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA2XE UT WOS:000386459000001 ER PT J AU Cyburt, RH Amthor, AM Heger, A Johnson, E Keek, L Meisel, Z Schatz, H Smith, K AF Cyburt, R. H. Amthor, A. M. Heger, A. Johnson, E. Keek, L. Meisel, Z. Schatz, H. Smith, K. TI DEPENDENCE OF X-RAY BURST MODELS ON NUCLEAR REACTION RATES SO ASTROPHYSICAL JOURNAL LA English DT Article DE nuclear reactions, nucleosynthesis, abundances; X-rays: bursts ID ACCRETING NEUTRON-STARS; THERMONUCLEAR REACTION-RATES; WEAK INTERACTION RATES; RP-PROCESS; RADIUS EXPANSION; RATE TABLES; HYDROGEN; MASS; NUCLEOSYNTHESIS; FLASHES AB X-ray bursts are thermonuclear flashes on the surface of accreting neutron stars, and reliable burst models are needed to interpret observations in terms of properties of the neutron star and the binary system. We investigate the dependence of X-ray burst models on uncertainties in (p,gamma),(alpha,gamma), and (alpha, p) nuclear reaction rates using fully self-consistent burst models that account for the feedbacks between changes in nuclear energy generation and changes in astrophysical conditions. A two-step approach first identified sensitive nuclear reaction rates in a singlezone model with ignition conditions chosen to match calculations with a state-of-the-art 1D multi-zone model based on the Kepler stellar evolution code. All relevant reaction rates on neutron-deficient isotopes up to mass 106 were individually varied by a factor of 100 up and down. Calculations of the 84 changes in reaction rate with the highest impact were then repeated in the 1D multi-zone model. We find a number of uncertain reaction rates that affect predictions of light curves and burst ashes significantly. The results provide insights into the nuclear processes that shape observables from X-ray bursts, and guidance for future nuclear physics work to reduce nuclear uncertainties in X-ray burst models. C1 [Cyburt, R. H.; Keek, L.; Schatz, H.] Michigan State Univ, Natl Superconducting Cyclotron Lab, E Lansing, MI 48824 USA. [Cyburt, R. H.; Heger, A.; Keek, L.; Meisel, Z.; Schatz, H.; Smith, K.] Michigan State Univ, Joint Inst Nucl Astrophys, E Lansing, MI 48824 USA. [Amthor, A. M.] Bucknell Univ, Dept Phys & Astron, Lewisburg, PA 17837 USA. [Heger, A.] Monash Univ, Sch Phys & Astron, Monash Ctr Astrophys, Clayton, Vic 3800, Australia. [Heger, A.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Heger, A.] Shanghai Jiao Tong Univ, Dept Phys & Astron, Ctr Nucl Astrophys, Shanghai 200240, Peoples R China. [Johnson, E.; Keek, L.; Schatz, H.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Meisel, Z.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Keek, L.] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA. [Keek, L.] NASA, Xray Astrophys Lab, GSFC, Greenbelt, MD 20771 USA. [Smith, K.] Oak Ridge Natl Lab, Oak Ridge, TN 37831 USA. RP Cyburt, RH (reprint author), Michigan State Univ, Natl Superconducting Cyclotron Lab, E Lansing, MI 48824 USA.; Cyburt, RH (reprint author), Michigan State Univ, Joint Inst Nucl Astrophys, E Lansing, MI 48824 USA. FU National Science Foundation [PHY-02-016783, PHY-08-22648, PHY-1430152]; ARC Future Fellowship [FT120100363]; US Department of Energy [SC0005012]; NASA [NNG06EO90A] FX We thank R. Ferguson, M. Klein, and S. Warren for help with the data analysis, F.-K. Thielemann for providing the network solver, and L. Bildsten for contributions to the one-zone model. This material is based upon work supported by the National Science Foundation under Grant Numbers PHY-02-016783, PHY-08-22648, and PHY-1430152 (JINA Center for the Evolution of the Elements). A.H. was supported by an ARC Future Fellowship (FT120100363) and the US Department of Energy (SC0005012). L.K. is supported by NASA under award number NNG06EO90A. NR 65 TC 1 Z9 1 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 55 DI 10.3847/0004-637X/830/2/55 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ8MN UT WOS:000386124600001 ER PT J AU McIntyre, ABR Rizzardi, L Yu, AM Alexander, N Rosen, GL Botkin, DJ Stahl, SE John, KK Castro-Wallace, SL McGrath, K Burton, AS Feinberg, AP Mason, CE AF McIntyre, Alexa B. R. Rizzardi, Lindsay Yu, Angela M. Alexander, Noah Rosen, Gail L. Botkin, Douglas J. Stahl, Sarah E. John, Kristen K. Castro-Wallace, Sarah L. McGrath, Ken Burton, Aaron S. Feinberg, Andrew P. Mason, Christopher E. TI Nanopore sequencing in microgravity SO NPJ MICROGRAVITY LA English DT Article ID SPACE-FLIGHT; RNA MODIFICATIONS; QUERY; TIME; VIRULENCE AB Rapid DNA sequencing and analysis has been a long-sought goal in remote research and point-of-care medicine. In microgravity, DNA sequencing can facilitate novel astrobiological research and close monitoring of crew health, but spaceflight places stringent restrictions on the mass and volume of instruments, crew operation time, and instrument functionality. The recent emergence of portable, nanopore-based tools with streamlined sample preparation protocols finally enables DNA sequencing on missions in microgravity. As a first step toward sequencing in space and aboard the International Space Station (ISS), we tested the Oxford Nanopore Technologies MinION during a parabolic flight to understand the effects of variable gravity on the instrument and data. In a successful proof-of-principle experiment, we found that the instrument generated DNA reads over the course of the flight, including the first ever sequenced in microgravity, and additional reads measured after the flight concluded its parabolas. Here we detail modifications to the sample-loading procedures to facilitate nanopore sequencing aboard the ISS and in other microgravity environments. We also evaluate existing analysis methods and outline two new approaches, the first based on a wave-fingerprint method and the second on entropy signal mapping. Computationally light analysis methods offer the potential for in situ species identification, but are limited by the error profiles (stays, skips, and mismatches) of older nanopore data. Higher accuracies attainable with modified sample processing methods and the latest version of flow cells will further enable the use of nanopore sequencers for diagnostics and research in space. C1 [McIntyre, Alexa B. R.; Yu, Angela M.] Triinst Training Program Computat Biol & Med, New York, NY USA. [McIntyre, Alexa B. R.; Alexander, Noah; Mason, Christopher E.] Weill Cornell Med Coll, Dept Physiol & Biophys, New York, NY 10065 USA. [Rizzardi, Lindsay; Feinberg, Andrew P.] Johns Hopkins Univ, Sch Med, Ctr Epigenet, Baltimore, MD 21205 USA. [Rosen, Gail L.] Drexel Univ, Dept Elect & Comp Engn, Philadelphia, PA 19104 USA. [Botkin, Douglas J.; Stahl, Sarah E.] JES Tech, Houston, TX USA. [John, Kristen K.; Burton, Aaron S.] NASA, Johnson Space Ctr, Astromat Res & Explorat Sci Div, Explorat Integrat & Sci Directorate, Houston, TX 77058 USA. [John, Kristen K.] NASA, Johnson Space Ctr, Postdoctoral Program, Houston, TX USA. [Castro-Wallace, Sarah L.] NASA, Johnson Space Ctr, Biomed Res & Environm Sci Div, Houston, TX USA. [McGrath, Ken] Univ Queensland, Australian Genome Res Facil, Gehrmann Labs, St Lucia, Qld, Australia. [Mason, Christopher E.] HRH Prince Alwaleed Bin Talal Bin Abdulaziz Alsau, New York, NY 10021 USA. [Mason, Christopher E.] Feil Family Brain & Mind Res Inst BMRI, New York, NY 10065 USA. RP Mason, CE (reprint author), Weill Cornell Med Coll, Dept Physiol & Biophys, New York, NY 10065 USA.; Feinberg, AP (reprint author), Johns Hopkins Univ, Sch Med, Ctr Epigenet, Baltimore, MD 21205 USA.; Burton, AS (reprint author), NASA, Johnson Space Ctr, Astromat Res & Explorat Sci Div, Explorat Integrat & Sci Directorate, Houston, TX 77058 USA.; Mason, CE (reprint author), HRH Prince Alwaleed Bin Talal Bin Abdulaziz Alsau, New York, NY 10021 USA.; Mason, CE (reprint author), Feil Family Brain & Mind Res Inst BMRI, New York, NY 10065 USA. EM afeinberg@jhu.edu; chm2042@med.cornell.edu OI Rizzardi, Lindsay/0000-0002-2866-9625 NR 28 TC 0 Z9 0 U1 13 U2 13 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 2373-8065 J9 NPJ MICROGRAVITY JI NPJ Microgravity PD OCT 20 PY 2016 VL 2 AR 16035 DI 10.1038/npjmgrav.2016.35 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DZ6KV UT WOS:000385972200001 ER PT J AU Mallick, K Trebs, I Boegh, E Giustarini, L Schlerf, M Drewry, DT Hoffmann, L von Randow, C Kruijt, B Araujo, A Saleska, S Ehleringer, JR Domingues, TF Ometto, JPHB Nobre, AD de Moraes, OLL Hayek, M Munger, JW Wofsy, SC AF Mallick, Kaniska Trebs, Ivonne Boegh, Eva Giustarini, Laura Schlerf, Martin Drewry, Darren T. Hoffmann, Lucien von Randow, Celso Kruijt, Bart Araujo, Alessandro Saleska, Scott Ehleringer, James R. Domingues, Tomas F. Ometto, Jean Pierre H. B. Nobre, Antonio D. Leal de Moraes, Osvaldo Luiz Hayek, Matthew Munger, J. William Wofsy, Steven C. TI Canopy-scale biophysical controls of transpiration and evaporation in the Amazon Basin SO HYDROLOGY AND EARTH SYSTEM SCIENCES LA English DT Article ID MODELING STOMATAL CONDUCTANCE; TROPICAL FOREST; SURFACE-TEMPERATURE; ENERGY-BALANCE; BOUNDARY-LAYER; LAND-SURFACE; EVAPOTRANSPIRATION RATES; DECIDUOUS FOREST; CARBON-CYCLE; RAIN-FOREST AB Canopy and aerodynamic conductances (g(C) and g(A)) are two of the key land surface biophysical variables that control the land surface response of land surface schemes in climate models. Their representation is crucial for predicting transpiration (lambda E-T) and evaporation (lambda E-E) flux components of the terrestrial latent heat flux (lambda E), which has important implications for global climate change and water resource management. By physical integration of radiometric surface temperature (T-R) into an integrated framework of the Penman-Monteith and Shuttleworth-Wallace models, we present a novel approach to directly quantify the canopy-scale biophysical controls on lambda E-T and lambda E-E over multiple plant functional types (PFTs) in the Amazon Basin. Combining data from six LBA (Large-scale Biosphere-Atmosphere Experiment in Amazonia) eddy covariance tower sites and a T-R-driven physically based modeling approach, we identified the canopy-scale feedback-response mechanism between g(C), lambda E-T, and atmospheric vapor pressure deficit (D-A), without using any leaf-scale empirical parameterizations for the modeling. The T-R-based model shows minor biophysical control on lambda E-T during the wet (rainy) seasons where lambda E-T becomes predominantly radiation driven and net radiation (RN) determines 75 to 80% of the variances of lambda E-T. However, biophysical control on lambda E-T is dramatically increased during the dry seasons, and particularly the 2005 drought year, explaining 50 to 65% of the variances of lambda E-T, and indicates lambda E-T to be substantially soil moisture driven during the rainfall deficit phase. Despite substantial differences in g(A) between forests and pastures, very similar canopy-atmosphere "coupling" was found in these two biomes due to soil moistureinduced decrease in g(C) in the pasture. This revealed the pragmatic aspect of the T-R-driven model behavior that exhibits a high sensitivity of g(C) to per unit change in wetness as opposed to g(A) that is marginally sensitive to surface wetness variability. Our results reveal the occurrence of a significant hysteresis between lambda E-T and g(C) during the dry season for the pasture sites, which is attributed to relatively low soil water availability as compared to the rainforests, likely due to differences in rooting depth between the two systems. Evaporation was significantly influenced by g(A) for all the PFTs and across all wetness conditions. Our analytical framework logically captures the responses of g(C) and g(A) to changes in atmospheric radiation, D-A, and surface radiometric temperature, and thus appears to be promising for the improvement of existing land-surface-atmosphere exchange parameterizations across a range of spatial scales. C1 [Mallick, Kaniska; Trebs, Ivonne; Giustarini, Laura; Schlerf, Martin; Hoffmann, Lucien] Luxembourg Inst Sci & Technol, Dept Environm Res & Innovat, L-4422 Belvaux, Luxembourg. [Boegh, Eva] Roskilde Univ, Dept Sci & Environm, Roskilde, Denmark. [Drewry, Darren T.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [von Randow, Celso; Ometto, Jean Pierre H. B.; Nobre, Antonio D.] Ctr Ciencia Sistema Terr, INPE, Sao Jose Dos Campos, SP, Brazil. [Kruijt, Bart] Wageningen Environm Res ALTERRA, Wageningen, Netherlands. [Araujo, Alessandro] Empresa Brasileira Pesquisa Agr EMBRAPA, Belem, Para, Brazil. [Saleska, Scott] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ USA. [Ehleringer, James R.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Domingues, Tomas F.] Univ Sao Paulo, Fac Filosofia Ciencias & Letras Ribeirao Preto, Sao Paulo, SP, Brazil. [Leal de Moraes, Osvaldo Luiz] Ctr Nacl Monitoramento & Alertas Desastres Nat, Sao Paulo, SP, Brazil. [Hayek, Matthew; Munger, J. William; Wofsy, Steven C.] Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. [Drewry, Darren T.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. RP Mallick, K; Trebs, I (reprint author), Luxembourg Inst Sci & Technol, Dept Environm Res & Innovat, L-4422 Belvaux, Luxembourg. EM kaniska.mallick@gmail.com; ivonne.trebs@list.lu RI Munger, J/H-4502-2013; Trebs, Ivonne/L-9125-2013; OI Munger, J/0000-0002-1042-8452; Von Randow, Celso/0000-0003-1045-4316 FU Luxembourg Institute of Science and Technology (LIST); German Science Foundation (DFG) [FOR 1598]; BELSPO; FNR; Jet Propulsion Laboratory, California Institute of Technology; National Aeronautics and Space Administration FX This study was funded by the Luxembourg Institute of Science and Technology (LIST). The developed modeling framework contributes to the Catchments As Organized Systems (CAOS) Phase-2 research group (FOR 1598) funded by the German Science Foundation (DFG) and to the HiWET (High-resolution modelling and monitoring of Water and Energy Transfers in wetland ecosystems) consortium funded by BELSPO and FNR. We sincerely thank Andrew Jarvis (Lancaster University, UK), Monica Garcia (Technical University of Denmark, Denmark), and Georg Wohlfahrt (University of Innsbruck, Austria) for very helpful discussions and edits of the manuscript. We are grateful to all Brazilian and international collaborators and all the funding agencies that have contributed to the Large-scale Biosphere Atmosphere Experiment in Amazonia (LBA). The authors are indebted to Pavel Kabat, Antonio Ocimar Manzi, David R. Fitzjarrald, Julio Tota, Humberto Ribeiro da Rocha, Michael Goulden, Maarten J. Waterloo, and Luiz Martinelli for planning, coordinating, conducting, and evaluating the eddy covariance, meteorological, and leaf-gas exchange measurements at the LBA sites. We are particularly grateful to all field technicians whose hard work was the key ingredient to establishing the quality of the datasets used in this paper. The authors declare no conflict of interest. Darren T. Drewry acknowledges the support of the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 102 TC 1 Z9 1 U1 17 U2 17 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. PD OCT 19 PY 2016 VL 20 IS 10 BP 4237 EP 4264 DI 10.5194/hess-20-4237-2016 PG 28 WC Geosciences, Multidisciplinary; Water Resources SC Geology; Water Resources GA EA4OR UT WOS:000386592900001 ER PT J AU Thakkar, H Eastman, S Hajari, A Rownaghi, AA Knox, JC Rezaei, F AF Thakkar, Harshul Eastman, Stephen Hajari, Amit Rownaghi, Ali A. Knox, James C. Rezaei, Fateme TI 3D-Printed Zeolite Monoliths for CO2 Removal from Enclosed Environments SO ACS APPLIED MATERIALS & INTERFACES LA English DT Article DE 3D-printed monolith; enclosed-environments; CO2 removal from air; adsorption; zeolite 5A; zeolite 13X ID CARBON HONEYCOMB MONOLITH; CAPTURE; PERFORMANCE; ADSORBENTS; AIR; ADSORPTION AB Structured adsorbents, especially in the form of monolithic contactors, offer an excellent gassolid contacting strategy for the development of practical and scalable CO2 capture technologies. In this study, the fabrication of three-dimensional (3D)-printed 13X and 5A zeolite monoliths with novel structures and their use in CO2 removal from air are reported. The physical and structural properties of these printed monoliths are evaluated and compared with their powder counterparts. Our results indicate that 3D-printed monoliths with zeolite loadings as high as 90 wt % exhibit adsorption uptake that is comparable to that of powder sorbents. The adsorption capacities of 5A and 13X monoliths were found to be 1.59 and 1.60 mmol/g, respectively, using 5000 ppm (0.5%) CO2 in nitrogen at room temperature. The dynamic CO2/N-2 breakthrough experiments show relatively fast dynamics for monolithic structures. In addition, the printed zeolite monoliths show reasonably good mechanical stability that can eventually prevent attrition and dusting issues commonly encountered in traditional pellets and beads packing systems. The 3D printing technique offers an alternative, cost-effective, and facile approach to fabricate structured adsorbents with tunable structural, chemical, and mechanical properties for use in gas separation processes. C1 [Thakkar, Harshul; Eastman, Stephen; Hajari, Amit; Rownaghi, Ali A.; Rezaei, Fateme] Missouri Univ Sci & Technol, Dept Chem & Biochem Engn, Rolla, MO 65409 USA. [Knox, James C.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Rezaei, F (reprint author), Missouri Univ Sci & Technol, Dept Chem & Biochem Engn, Rolla, MO 65409 USA. EM rezaeif@mst.edu FU NASA-EPSCoR [NNX15AK38A] FX This work was financially supported by NASA-EPSCoR (No. NNX15AK38A). The authors thank Dr. Rahaman's laboratory for using their 3D printer and Materials Research Center (MRC) of Missouri S&T for SEM and XRD. The authors also thank Dr. Karren More at ORNL for helping with the SEM images, through CNMS User Proposal No. CNMS2015-339. NR 43 TC 2 Z9 2 U1 30 U2 30 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1944-8244 J9 ACS APPL MATER INTER JI ACS Appl. Mater. Interfaces PD OCT 19 PY 2016 VL 8 IS 41 BP 27753 EP 27761 DI 10.1021/acsami.6b09647 PG 9 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Science & Technology - Other Topics; Materials Science GA DZ6SO UT WOS:000385992400038 ER PT J AU Wilcox, EM Thomas, RM Praveen, PS Pistone, K Bender, FAM Ramanathan, V AF Wilcox, Eric M. Thomas, Rick M. Praveen, Puppala S. Pistone, Kristina Bender, Frida A. -M. Ramanathan, Veerabhadran TI Black carbon solar absorption suppresses turbulence in the atmospheric boundary layer SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE atmospheric turbulence; cloud cover; aerosols; radiative forcing; autonomous unmanned aerial vehicles ID UNMANNED AERIAL VEHICLES; NORTHERN INDIAN-OCEAN; CLOUD COVER; VERTICAL PROFILES; AEROSOL; SMOKE; POLLUTION; STRATOCUMULUS; MICROPHYSICS; PERFORMANCE AB The introduction of cloud condensation nuclei and radiative heating by sunlight-absorbing aerosols can modify the thickness and coverage of low clouds, yielding significant radiative forcing of climate. The magnitude and sign of changes in cloud coverage and depth in response to changing aerosols are impacted by turbulent dynamics of the cloudy atmosphere, but integrated measurements of aerosol solar absorption and turbulent fluxes have not been reported thus far. Here we report such integrated measurements made from unmanned aerial vehicles (UAVs) during the CARDEX (Cloud Aerosol Radiative Forcing and Dynamics Experiment) investigation conducted over the northern Indian Ocean. The UAV and surface data reveal a reduction in turbulent kinetic energy in the surface mixed layer at the base of the atmosphere concurrent with an increase in absorbing black carbon aerosols. Polluted conditions coincide with a warmer and shallower surface mixed layer because of aerosol radiative heating and reduced turbulence. The polluted surface mixed layer was also observed to be more humid with higher relative humidity. Greater humidity enhances cloud development, as evidenced by polluted clouds that penetrate higher above the top of the surface mixed layer. Reduced entrainment of dry air into the surface layer from above the inversion capping the surface mixed layer, due to weaker turbulence, may contribute to higher relative humidity in the surface layer during polluted conditions. Measurements of turbulence are important for studies of aerosol effects on clouds. Moreover, reduced turbulence can exacerbate both the human health impacts of high concentrations of fine particles and conditions favorable for low-visibility fog events. C1 [Wilcox, Eric M.] Desert Res Inst, Div Atmospher Sci, Reno, NV 89512 USA. [Thomas, Rick M.; Praveen, Puppala S.; Pistone, Kristina; Ramanathan, Veerabhadran] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Clouds Chem & Climate, La Jolla, CA 92093 USA. [Thomas, Rick M.] Univ Birmingham, Sch Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England. [Praveen, Puppala S.] Int Ctr Integrated Mt Dev, Kathmandu, Nepal. [Pistone, Kristina] NASA, Ames Res Ctr, Univ Space Res Assoc, Moffett Field, CA 94035 USA. [Bender, Frida A. -M.] Stockholm Univ, Dept Meteorol, S-10691 Stockholm, Sweden. [Bender, Frida A. -M.] Stockholm Univ, Bolin Ctr Climate Res, S-10691 Stockholm, Sweden. RP Wilcox, EM (reprint author), Desert Res Inst, Div Atmospher Sci, Reno, NV 89512 USA.; Thomas, RM; Ramanathan, V (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Ctr Clouds Chem & Climate, La Jolla, CA 92093 USA.; Thomas, RM (reprint author), Univ Birmingham, Sch Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England. EM Eric.Wilcox@dri.edu; r.thomas@bham.ac.uk; vramanathan@ucsd.edu FU National Science Foundation [NSF-0721142]; Desert Research Institute; National Aeronautics and Space Administration [NNX11AG89G] FX We thank Hung Nguyen for the expert project and flight management for CARDEX. The CARDEX campaign is supported by National Science Foundation Grant NSF-0721142 and was conducted by Scripps Institution of Oceanography with V. Ramanathan as the principal investigator. E.M.W. acknowledges support from the Desert Research Institute to participate in CARDEX, as well as from National Aeronautics and Space Administration Grant NNX11AG89G. NR 38 TC 0 Z9 0 U1 16 U2 16 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD OCT 18 PY 2016 VL 113 IS 42 BP 11794 EP 11799 DI 10.1073/pnas.1525746113 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DZ1PN UT WOS:000385610400059 PM 27702889 ER PT J AU Tompson, SR AF Tompson, Sara R. TI The Pope of Physics: Enrico Fermi and the Birth of the Atomic Age. SO LIBRARY JOURNAL LA English DT Book Review C1 [Tompson, Sara R.] Jet Prop Lab Lib, Arch & Records Sect, Pasadena, CA 91109 USA. RP Tompson, SR (reprint author), Jet Prop Lab Lib, Arch & Records Sect, Pasadena, CA 91109 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD OCT 15 PY 2016 VL 141 IS 17 BP 107 EP 107 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA EJ6SJ UT WOS:000393348800262 ER PT J AU Yayathi, S Walker, W Doughty, D Ardebili, H AF Yayathi, Sandeep Walker, William Doughty, Daniel Ardebili, Haleh TI Energy distributions exhibited during thermal runaway of commercial lithium ion batteries used for human spaceflight applications SO JOURNAL OF POWER SOURCES LA English DT Article DE Lithium ion battery; Thermal runaway; Battery safety; Accelerating rate calorimetry; Total energy release ID ACCELERATING RATE CALORIMETRY; MICROGRAVITY CONDITIONS; INTERCALATED GRAPHITE; HIGH-POWER; CELLS; MODEL; OVERCHARGE; STABILITY; PROPAGATION; PERFORMANCE AB Lithium ion (Li-ion) batteries provide low mass and energy dense solutions necessary for space exploration, but thermal related safety concerns impede the utilization of Li-ion technology for human applications. Experimental characterization of thermal runaway energy release with accelerated rate calorimetry supports safer thermal management systems. 'Standard' accelerated rate calorimetry setup provides means to measure the addition of energy exhibited through the body of a Li-ion cell. This study considers the total energy generated during thermal runaway as distributions between cell body and hot gases via inclusion of a unique secondary enclosure inside the calorimeter; this closed system not only contains the cell body and gaseous species, but also captures energy release associated with rapid heat transfer to the system unobserved by measurements taken on the cell body. Experiments include Boston Power Swing 5300, Samsung 18650-26F and MoliCel 18650-J Li-ion cells at varied states-of-charge. An inverse relationship between state-of-charge and onset temperature is observed. Energy contained in the cell body and gaseous species are successfully characterized; gaseous energy is minimal. Significant additional energy is measured with the heating of the secondary enclosure. Improved calorimeter apparatus including a secondary enclosure provides essential capability to measuring total energy release distributions during thermal runaway. Published by Elsevier B.V. C1 [Yayathi, Sandeep; Walker, William] NASA Johnson Space Ctr, 2101 NASA Rd 1, Houston, TX 77058 USA. [Walker, William; Ardebili, Haleh] Univ Houston, 4800 Calhoun Rd, Houston, TX 77004 USA. [Doughty, Daniel] Battery Safety Consulting Inc, 139 Big Horn Ridge Dr NE, Albuquerque, NM 87122 USA. RP Walker, W (reprint author), NASA Johnson Space Ctr, Engn Directorate, Struct Engn Div, 2101 NASA Rd 1, Houston, TX 77058 USA. EM william.walker@nasa.gov FU NASA JSC Energy Systems Test Area (ESTA); NASA Engineering and Safety Center (NESC) FX The authors would like to express deepest gratitude for the support of Dr. Christopher Iannello, the NASA Engineering and Safety Center (NESC) and the NASA JSC Energy Systems Test Area (ESTA) team members. Special thanks to the Thermal Hazard Technology (THT) test team. NR 52 TC 1 Z9 1 U1 24 U2 24 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-7753 EI 1873-2755 J9 J POWER SOURCES JI J. Power Sources PD OCT 15 PY 2016 VL 329 BP 197 EP 206 DI 10.1016/j.jpowsour.2016.08.078 PG 10 WC Chemistry, Physical; Electrochemistry; Energy & Fuels; Materials Science, Multidisciplinary SC Chemistry; Electrochemistry; Energy & Fuels; Materials Science GA DY1KB UT WOS:000384852800021 ER PT J AU Mahjoub, A Schwell, M Carrasco, N Benilan, Y Cernogora, G Szopa, C Gazeau, MC AF Mahjoub, Ahmed Schwell, Martin Carrasco, Nathalie Benilan, Yves Cernogora, Guy Szopa, Cyril Gazeau, Marie-Claire TI Characterization of aromaticity in analogues of titan's atmospheric aerosols with two-step laser desorption ionization mass spectrometry SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Aromatics; Titan's atmosphere; Aerosols; L2DI-MS ID ULTRAVIOLET-ABSORPTION-SPECTRA; OPTICAL INDEXES; ORGANIC-MATTER; GAS-PHASE; RF PLASMA; THOLINS; SPECTROSCOPY; CHEMISTRY; HAZE; HYDROCARBONS AB The role of polycyclic aromatic hydrocarbons (PAH) and Nitrogen containing PAH (PANH) as intermediates of aerosol production in the atmosphere of Titan has been a subject of controversy for a long time. An analysis of the atmospheric emission band observed by the Visible and Infrared Mapping Spectrometer (VIMS) at 3.28 mu m suggests the presence of neutral polycyclic aromatic species in the upper atmosphere of Titan. These molecules are seen as the counter part of negative and positive aromatics ions suspected by the Plasma Spectrometer onboard the Cassini spacecraft, but the low resolution of the instrument hinders any molecular speciation. In this work we investigate the specific aromatic content of Titan's atmospheric aerosols through laboratory simulations. We report here the selective detection of aromatic compounds in tholins, Titan's aerosol analogs, produced with a capacitively coupled plasma in a N-2:CH4 95:5 gas mixture. For this purpose, Two-Step Laser Desorption Ionization Time-of-Flight Mass Spectrometry (L2DI-TOF-MS) technique is used to analyze the so produced analogs. This analytical technique is based on the ionization of molecules by Resonance Enhanced Multi-Photon Ionization (REMPI) using a lambda=248 nm wavelength laser which is selective for aromatic species. This allows for the selective identification of compounds having at least one aromatic ring. Our experiments show that tholins contain a trace amount of small PAHs with one to three aromatic rings. Nitrogen containing PAHs (PANHs) are also detected as constituents of tholins. Molecules relevant to astrobiology are detected as is the case of the substituted DNA base adenine. (C) 2016 Published by Elsevier Ltd. C1 [Mahjoub, Ahmed; Schwell, Martin; Benilan, Yves; Gazeau, Marie-Claire] Univ Paris Est Creteil, LISA UMR CNRS 7583, 61 Ave Gen Gaulle, F-94010 Creteil, France. [Mahjoub, Ahmed; Schwell, Martin; Benilan, Yves; Gazeau, Marie-Claire] Univ Paris Diderot, Inst Pierre Simon Laplace, 61 Ave Gen Gaulle, F-94010 Creteil, France. [Carrasco, Nathalie; Cernogora, Guy; Szopa, Cyril] Univ Paris 06, Univ Versailles St Quentin, CNRS INSU, LATMOS IPSL, 11 Bd Alembert, F-78280 Guyancourt, France. [Carrasco, Nathalie; Szopa, Cyril] Inst Univ France, Paris, France. [Mahjoub, Ahmed] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mahjoub, A (reprint author), Univ Paris Est Creteil, LISA UMR CNRS 7583, 61 Ave Gen Gaulle, F-94010 Creteil, France.; Mahjoub, A (reprint author), Univ Paris Diderot, Inst Pierre Simon Laplace, 61 Ave Gen Gaulle, F-94010 Creteil, France.; Mahjoub, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM ahmed.mahjoub@lisa.u-pec.fr RI Carrasco, Nathalie/D-2365-2012 OI Carrasco, Nathalie/0000-0002-0596-6336 FU Universite Creteil Paris 12; European Research Council (ERC Starting Grant PRIMCHEM) [636829] FX Dr. Mahjoub would like to thank Universite Creteil Paris 12 for financial support. NC acknowledges the European Research Council for their financial support (ERC Starting Grant PRIMCHEM, Grant agreement no. 636829). NR 74 TC 0 Z9 0 U1 17 U2 17 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 OCT 15 PY 2016 VL 131 BP 1 EP 13 DI 10.1016/j.pss.2016.05.003 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY1LT UT WOS:000384857200001 ER PT J AU Managadze, GG Engel, MH Getty, S Wurz, P Brinckerhoff, WB Shokolov, AG Sholin, GV Terent'ev, SA Chumikov, AE Skalkin, AS Blank, VD Prokhorov, VM Managadze, NG Luchnikov, KA AF Managadze, George G. Engel, Michael H. Getty, Stephanie Wurz, Peter Brinckerhoff, William B. Shokolov, Anatoly G. Sholin, Gennady V. Terent'ev, Sergey A. Chumikov, Alexander E. Skalkin, Alexander S. Blank, Vladimir D. Prokhorov, Vyacheslav M. Managadze, Nina G. Luchnikov, Konstantin A. TI Excess of L-alanine in amino acids synthesized in a plasma torch generated by a hypervelocity meteorite impact reproduced in the laboratory SO PLANETARY AND SPACE SCIENCE LA English DT Article ID BIOMOLECULAR CHIRALITY; MURCHISON METEORITE; SHOCK SYNTHESIS; ORIGIN; SELECTION; COMETARY; FIELDS; VAPOR AB We present a laboratory reproduction of hypervelocity impacts of a carbon containing meteorite on a mineral substance representative of planetary surfaces. The physical conditions of the resulting impact plasma torch provide favorable conditions for abiogenic synthesis of protein amino acids: We identified glycine and alanine, and in smaller quantities serine, in the produced material. Moreover, we observe breaking of alanine mirror symmetry with L excess, which coincides with the bioorganic world. Therefore the selection of L-amino acids for the formation of proteins for living matter could have been the result from plasma processes occurring during the impact meteorites on the surface. This indicates that the plasma torch from meteorite impacts could play an important role in the formation of biomolecular homochirality. Thus, meteorite impacts possibly were the initial stage of this process and promoted conditions for the emergence of a living matter. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Managadze, George G.; Chumikov, Alexander E.; Managadze, Nina G.; Luchnikov, Konstantin A.] Space Res Inst, Profsoyuznaya St 84-32, Moscow 117997, Russia. [Engel, Michael H.] Univ Oklahoma, Sch Geol & Geophys, Norman, OK 73019 USA. [Getty, Stephanie; Brinckerhoff, William B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wurz, Peter] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Shokolov, Anatoly G.; Skalkin, Alexander S.] Cent Res Inst Machine Bldg, Moscow, Russia. [Sholin, Gennady V.] NRC Kurchatov Inst, Moscow, Russia. [Blank, Vladimir D.; Prokhorov, Vyacheslav M.] Technol Inst Super Hard & Novel Carbon Mat, Moscow, Russia. RP Wurz, P (reprint author), Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. EM peter.wurz@space.unibe.ch FU Presidium of the Russian Academy of Sciences [22]; Swiss National Science Foundation [200020_153047] FX We thank Dr. A.A. Ignatov, Dr. A.I. Rukhadze, Dr. V.A. Avetisov, Dr. A.S. Brodskii, Dr. A. Riedo, Dr. M. Tulej, Dr. L.M. Zelenyi, Dr. R. R. Nazirov, Dr. A.V. Zakharov, Dr. L. Kelner, and Dr. Yu. M. Lipnitskii for useful discussions and support, Dr. V.A. Davankov for valuable remarks, A.I. Kuznetsov and D.A. Moiseenko for their assistance. Supported by the Presidium of the Russian Academy of Sciences (Grant no. 22) and the Swiss National Science Foundation (Grant no. 200020_153047). NR 45 TC 0 Z9 0 U1 11 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 OCT 15 PY 2016 VL 131 BP 70 EP 78 DI 10.1016/j.pss.2016.07.005 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY1LT UT WOS:000384857200007 ER PT J AU Rapin, W Meslin, PY Maurice, S Vaniman, D Nachon, M Mangold, N Schroder, S Gasnault, O Forni, O Wiens, RC Martinez, GM Cousin, A Sautter, V Lasue, J Rampe, EB Archer, D AF Rapin, W. Meslin, P. -Y. Maurice, S. Vaniman, D. Nachon, M. Mangold, N. Schroder, S. Gasnault, O. Forni, O. Wiens, R. C. Martinez, G. M. Cousin, A. Sautter, V. Lasue, J. Rampe, E. B. Archer, D. TI Hydration state of calcium sulfates in Gale crater, Mars: Identification of bassanite veins SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Mars; calcium sulfate; bassanite; LIBS; hydrogen; ChemCam ID CHEMCAM INSTRUMENT SUITE; OMEGA/MARS EXPRESS; GYPSUM; ANHYDRITE; STABILITY; SEDIMENTS; PHASE; BASIN; UNIT AB In-situ analyses reveal the presence of hydrogen within calcium sulfate veins crosscutting the sediments found in Gale crater. Laboratory experiments were performed to calibrate the hydrogen signal measured by laser induced breakdown spectroscopy (LIBS) in a range applicable to martian data. The analyses indicate that all veins targeted so far at Gale consist predominantly of bassanite which most likely formed by dehydration of gypsum. This scenario suggests that the percolating water produced gypsum, possibly by hydration of anhydrite in aqueous solution, and remained at temperatures below 60 degrees C at that time. Desiccating conditions followed, consistent with a hyperarid climate and favored by burial or impacts. Additionally, anhydrite with lesser bassanite has been found by XRD in samples of sediments hosting the veins. Our result suggests bassanite is likely found in the veins and anhydrite may be more common as a fine-grained component within the sediments. (C) 2016 Elsevier B.V. All rights reserved. C1 [Rapin, W.; Meslin, P. -Y.; Maurice, S.; Gasnault, O.; Forni, O.; Cousin, A.; Lasue, J.] Univ Toulouse, UPS OMP, Toulouse, France. [Rapin, W.; Meslin, P. -Y.; Maurice, S.; Schroder, S.; Gasnault, O.; Forni, O.; Cousin, A.; Lasue, J.] CNRS, Inst Rech Astrophys & Planetol, UMR 5277, Toulouse, France. [Vaniman, D.] Planetary Sci Inst, Tucson, AZ USA. [Nachon, M.; Mangold, N.] Univ Nantes, CNRS, Lab Planetol & Geodynam Nantes, UMR6112, Nantes, France. [Wiens, R. C.] Los Alamos Natl Lab, Los Alamos, NM USA. [Martinez, G. M.] Univ Michigan, Ann Arbor, MI 48109 USA. [Sautter, V.] Museum Natl Hist Nat, Lab Mineral & Cosmochim Museum, Paris, France. [Rampe, E. B.] NASA Johnson Space Ctr, Aerodyne Ind, Houston, TX USA. [Archer, D.] NASA Johnson Space Ctr, Houston, TX USA. RP Rapin, W (reprint author), IRAP CNRS, 9 Ave Colonel Roche, F-31028 Toulouse, France. EM william.rapin@irap.omp.eu FU Universite Paul Sabatier, Institut de Recherche en Astrophysique et Planetologie (IRAP); CNES; NASA Mars Exploration Program FX This research was funded by Universite Paul Sabatier as part of a PhD thesis, and experiments were conducted at Institut de Recherche en Astrophysique et Planetologie (IRAP) with support from CNES. Funding for MSL and ChemCam operations and science in the US were provided by the NASA Mars Exploration Program. Funding for ChemCam operations in France was provided by CNES. The authors gratefully acknowledge the support of all of the people at JPL involved in making MSL a successful mission. The Raman spectroscopy analysis to assess the purity of the calcium sulfate pellets was performed by Olivier Beyssac and Sylvain Bernard from the Institut de Mineralogie, de Physique des Materiaux et de Cosmochimie (IMPMC). The authors thankfully recognize their valuable help. The authors also thank Mikhail Zolotov and one anonymous reviewer for their helpful comments. NR 53 TC 2 Z9 2 U1 32 U2 32 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 OCT 15 PY 2016 VL 452 BP 197 EP 205 DI 10.1016/j.epsl.2016.07.045 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DV5YE UT WOS:000383005800019 ER PT J AU Richter, A Ivins, E Lange, H Mendoza, L Schroder, L Hormaechea, JL Casassa, G Marderwald, E Fritsche, M Perdomo, R Horwath, M Dietrich, R AF Richter, A. Ivins, E. Lange, H. Mendoza, L. Schroeder, L. Hormaechea, J. L. Casassa, G. Marderwald, E. Fritsche, M. Perdomo, R. Horwath, M. Dietrich, R. TI Crustal deformation across the Southern Patagonian Icefield observed by GNSS SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE crustal deformation; glacial-isostatic adjustment; GNSS; Patagonia ID RIDGE SUBDUCTION REGION; ANTARCTIC PENINSULA; ARGENTINA; CHILE; GPS; HOLOCENE; EVOLUTION; HISTORY; MODELS; MOTION AB Geodetic GNSS observations at 43 sites well distributed over the Southern Patagonian Icefield region yield site velocities with a mean accuracy of 1 mm/a and 6 mm/a for the horizontal and vertical components, respectively. These velocities are analyzed to reveal the magnitudes and patterns of vertical and horizontal present-day crustal deformation as well as their primary driving processes. The observed vertical velocities confirm a rapid uplift, with rates peaking at 41 mmia, causally related to glacial-isostatic adjustment (GIA). They yield now an unambiguous preference between two competing GIA models. Remaining discrepancies between the preferred model and our observations point toward an effective upper mantle viscosity even lower than 1.6 . 10(18) Pa s and effects of lateral rheological heterogeneities. An analysis of the horizontal strain and strain-rate fields reveals some complex superposition, with compression dominating in the west and extension in the east. This deformation field suggests significant contributions from three processes: GIA, a western interseismic tectonic deformation field related to plate subduction, and an extensional strain-rate field related to active Patagonian slab window tectonics. (C) 2016 Elsevier B.V. All rights reserved. C1 [Richter, A.; Lange, H.; Schroeder, L.; Fritsche, M.; Horwath, M.; Dietrich, R.] Tech Univ Dresden, Inst Planetare Geodasie, Dresden, Germany. [Richter, A.; Mendoza, L.; Hormaechea, J. L.; Marderwald, E.; Perdomo, R.] Univ Nacl La Plata, Fac Ciencias Astron & Geofis, La Plata, Buenos Aires, Argentina. [Richter, A.; Mendoza, L.; Hormaechea, J. L.; Marderwald, E.] Consejo Nacl Invest Cient & Tecn, RA-1033 Buenos Aires, DF, Argentina. [Ivins, E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Hormaechea, J. L.] Estn Astron Rio Grande, Rio Grande, Argentina. [Casassa, G.] Geoestudios, Santiago, Chile. [Casassa, G.] Univ Magallanes, Punta Arenas, Chile. [Fritsche, M.] GFZ German Res Ctr Geosci, Potsdam, Germany. RP Richter, A (reprint author), Tech Univ Dresden, Inst Planetare Geodasie, Dresden, Germany. EM andreas.richter@tu-dresden.de RI Ivins, Erik/C-2416-2011; OI Hormaechea, Jose Luis/0000-0003-4533-3282 FU German Research Foundation DFG [RI 2340/1-1, DI 473/40-1]; Jet Propulsion Laboratory, California Institute of Technology, by the Cryosphere Program; Earth Surface and Interior Focus Area as part of GRACE Science; Earth Surface and Interior Focus Area as part of NASA Sea-level Change Teams; administrations of Parque Nacional Los Glaciares; administrations of Parque Nacional Torres del Paine; administrations of DIFROL; administrations of GRACE Science FX The German part of the project was funded by the German Research Foundation DFG (grants RI 2340/1-1, DI 473/40-1). E. Ivins was funded at the Jet Propulsion Laboratory, California Institute of Technology, by the Cryosphere Program, the Earth Surface and Interior Focus Area and as part of both the GRACE Science and NASA Sea-level Change Teams. We thank Gerardo Connon, Luis Barbero, Anja Wendt, Andres Rivera, Rodrigo Traub, Marcelo Arevalo and Hans Silva for their valuable help in the field. We thank the administrations of Parque Nacional Los Glaciares, Parque Nacional Torres del Paine, CONAF and DIFROL for support, advice and permission of our field activities. Logistic support was provided by Prefectura Naval Lago Argentine, Estancia Cristina, Patagonia Expeditions El Chalten, Hosteria Grey and the crews of motor boat Soberania and ferry boat Integracion. We thank two anonymous reviewers and the editor Dr. An Yin for their valuable suggestions, which helped to improve this paper. NR 54 TC 0 Z9 0 U1 9 U2 9 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 OCT 15 PY 2016 VL 452 BP 206 EP 215 DI 10.1016/j.epsl.2016.07.042 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DV5YE UT WOS:000383005800020 ER PT J AU Ma, WP Jacobs, G Sparks, DE Klettlinger, JLS Yen, CH Davis, BH AF Ma, Wenping Jacobs, Gary Sparks, Dennis E. Klettlinger, Jennifer L. S. Yen, Chia H. Davis, Burtron H. TI Fischer-Tropsch synthesis and water gas shift kinetics for a precipitated iron catalyst SO CATALYSIS TODAY LA English DT Article; Proceedings Paper CT Syngas Convention on Fuels and Chemicals from Synthesis Gas - State of the Art 2 CY MAR 29-APR 01, 2015 CL Cape Town, SOUTH AFRICA SP Univ Cape Town, Natl DST NRF Ctr Excellence Catalysis, Catalysis Soc S Africa DE Fischer-Tropsch synthesis; Water gas shift reaction; Fe catalyst; Kinetics; CO2 inhibition; Water inhibition ID INTRINSIC KINETICS; OXIDE CATALYSTS; CARBON-MONOXIDE; HYDROGENATION AB A large number of kinetic data points (83 sets) was obtained over a wide range of CO conversion (7-90%), pressure (1.3-2.5 MPa) and H-2/CO ratio (0.67-1.5) with an iron catalyst (100 Fe/5.1 Si/1.25 K). The kinetics of the catalyst in the low (X-co <70%) and high conversion (X-co >70%) regions were studied separately. Twenty six Fischer-Tropsch synthesis (FTS) and water gas shift (WGS) kinetic models were tested and discriminated. Water and CO2 inhibition was evaluated. While all thirteen FTS models gave a satisfactory fit, the new FTS models that included CO2 inhibition surpassed the others. Water inhibition of the FTS rate was insignificant over both low and high conversion ranges. For the WGS kinetics of the iron catalyst, a newly constructed empirical model and one from the literature provided the best fits of the WGS rates, while nine mechanistic models and one power law WGS model were unable to satisfactorily fit the WGS kinetic data. Water did not significantly limit the WGS rate and CO2 only inhibited the rate at high CO conversions. The equations obtained for the low and high CO conversion ranges varied greatly. The errors for the models for 85% of the FTS and WGS data points were less than 10%, and the errors of the remaining points fell in the range of 10-15%. (C) 2016 Elsevier B.V. All rights reserved. C1 [Ma, Wenping; Jacobs, Gary; Sparks, Dennis E.; Davis, Burtron H.] Univ Kentucky, Ctr Appl Energy Res, 2540 Res Pk Dr, Lexington, KY 40511 USA. [Klettlinger, Jennifer L. S.; Yen, Chia H.] NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. RP Davis, BH (reprint author), Univ Kentucky, Ctr Appl Energy Res, 2540 Res Pk Dr, Lexington, KY 40511 USA. EM burtron.davis@uky.edu NR 37 TC 0 Z9 0 U1 18 U2 20 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0920-5861 EI 1873-4308 J9 CATAL TODAY JI Catal. Today PD OCT 15 PY 2016 VL 275 BP 49 EP 58 DI 10.1016/j.cattod.2016.01.006 PG 10 WC Chemistry, Applied; Chemistry, Physical; Engineering, Chemical SC Chemistry; Engineering GA DU7UO UT WOS:000382420300009 ER PT J AU Mannucci, AJ Hagan, ME Vourlidas, A Huang, CY Verkhoglyadova, OP Deng, Y AF Mannucci, Anthony J. Hagan, Maura E. Vourlidas, Angelos Huang, Cheryl Y. Verkhoglyadova, Olga P. Deng, Yue TI Scientific challenges in thermosphere-ionosphere forecasting - conclusions from the October 2014 NASA JPL community workshop SO JOURNAL OF SPACE WEATHER AND SPACE CLIMATE LA English DT Editorial Material DE Ionosphere (general); Thermosphere; Storm; Interplanetary Coronal Mass Ejection (CME); Heliosphere ID CORONAL MASS EJECTIONS; TOTAL ELECTRON-CONTENT; HEIGHT-INTEGRATED PEDERSEN; SOLAR-WIND STREAMS; MAGNETIC-FLUX ROPE; INTERPLANETARY ORIGIN; NUMERICAL SIMULATIONS; TIME-GCM; SPACE; STORMS AB Interest in forecasting space weather in the thermosphere and ionosphere (T-I) led to a community workshop held at NASA's Jet Propulsion Laboratory in October, 2014. The workshop focus was "Scientific Challenges in Thermosphere-Ionosphere Forecasting'' to emphasize that forecasting presumes a sufficiently advanced state of scientific knowledge, yet one that is still evolving. The purpose of the workshop, and this topical issue that arose from the workshop, was to discuss research frontiers that will lead to improved space weather forecasts. Three areas are discussed in some detail in this paper: (1) the role of lower atmosphere forcing in the response of the T-I to geomagnetic disturbances; (2) the significant deposition of energy at polar latitudes during geomagnetic disturbances; and (3) recent developments in understanding the propagation of coronal mass ejections through the heliosphere and prospects for forecasting the north-south component of the interplanetary magnetic field (IMF) using observations at the Lagrangian L-5 point. We describe other research presented at the workshop that appears in the topical issue. The possibility of establishing a "positive feedback loop'' where improved scientific knowledge leads to improved forecasts is described C1 [Mannucci, Anthony J.; Verkhoglyadova, Olga P.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Hagan, Maura E.] Utah State Univ, Logan, UT 84322 USA. [Vourlidas, Angelos] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Huang, Cheryl Y.] US Air Force, Res Lab, Kirtland AFB, NM 87117 USA. [Deng, Yue] Univ Texas Arlington, Arlington, TX 76029 USA. RP Mannucci, AJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM anthony.j.mannucci@jpl.nasa.gov RI Vourlidas, Angelos/C-8231-2009 OI Vourlidas, Angelos/0000-0002-8164-5948 FU NASA/NSF; National Center for Atmospheric Research (NCAR) under National Science Foundation (NSF); U.S. Participating Investigator (USPI) Program under NASA [NNX12AD26G]; internal APL funds; Air Force Office of Scientific Research [LRIR 14 RV11COR] FX Portions of this research were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Sponsorship of the NASA/NSF Partnership for Collaborative Space Weather Modeling is gratefully acknowledged. MH thanks K. Hausler for the TIME-GCM figures. MH was supported by the National Center for Atmospheric Research (NCAR) under the sponsorship of the National Science Foundation (NSF) and by the U.S. Participating Investigator (USPI) Program under NASA Grant NNX12AD26G. AV was supported by internal APL funds. CH acknowledges the support of the Air Force Office of Scientific Research under Grant LRIR 14 RV11COR. NR 88 TC 0 Z9 0 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 2115-7251 J9 J SPACE WEATHER SPAC JI J. Space Weather Space Clim. PD OCT 14 PY 2016 VL 6 AR E01 DI 10.1051/swsc/2016030 PG 10 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA EI9BS UT WOS:000392802900001 ER PT J AU Jethva, H Torres, O Remer, L Redemann, J Livingston, J Dunagan, S Shinozuka, Y Kacenelenbogen, M Rosenheimer, MS Spurr, R AF Jethva, Hiren Torres, Omar Remer, Lorraine Redemann, Jens Livingston, John Dunagan, Stephen Shinozuka, Yohei Kacenelenbogen, Meloe Rosenheimer, Michal Segal Spurr, Rob TI Validating MODIS above-cloud aerosol optical depth retrieved from "color ratio" algorithm using direct measurements made by NASA's airborne AATS and 4STAR sensors SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID SENSITIVITY-ANALYSIS; ABSORBING AEROSOLS; LIDAR MEASUREMENTS; COLUMN CLOSURE; WATER-VAPOR; SAFARI 2000; ACE-ASIA; LAYERS; SPECTROMETER; C-130 AB We present the validation analysis of above-cloud aerosol optical depth (ACAOD) retrieved from the "color ratio" method applied to MODIS cloudy-sky reflectance measurements using the limited direct measurements made by NASA's airborne Ames Airborne Tracking Sunphotometer (AATS) and Spectrometer for Sky-Scanning, Sun-Tracking Atmospheric Research (4STAR) sensors. A thorough search of the airborne database collection revealed a total of five significant events in which an airborne sun photometer, coincident with the MODIS overpass, observed partially absorbing aerosols emitted from agricultural biomass burning, dust, and wildfires over a low-level cloud deck during SAFARI-2000, ACE-ASIA 2001, and SEAC4RS 2013 campaigns, respectively. The co-located satellite-airborne matchups revealed a good agreement (root-mean-square difference < 0.1), with most matchups falling within the estimated uncertainties associated the MODIS retrievals (about -10 to +50 %). The co-retrieved cloud optical depth was comparable to that of the MODIS operational cloud product for ACE-ASIA and SEAC4RS, however, higher by 30-50% for the SAFARI-2000 case study. The reason for this discrepancy could be attributed to the distinct aerosol optical properties encountered during respective campaigns. A brief discussion on the sources of uncertainty in the satellite-based ACAOD retrieval and co-location procedure is presented. Field experiments dedicated to making direct measurements of aerosols above cloud are needed for the extensive validation of satellite-based retrievals. C1 [Jethva, Hiren] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21044 USA. [Jethva, Hiren; Torres, Omar] NASA, Goddard Space Flight Ctr, Earth Sci Div, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA. [Remer, Lorraine] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. [Redemann, Jens; Dunagan, Stephen] NASA, Ames Res Ctr, Earth Sci Div, Moffett Field, CA 94035 USA. [Livingston, John] SRI Int, 333 Ravenswood Ave, Menlo Pk, CA 94025 USA. [Shinozuka, Yohei; Kacenelenbogen, Meloe; Rosenheimer, Michal Segal] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Spurr, Rob] RT Solut, Cambridge, MA 02138 USA. RP Jethva, H (reprint author), Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21044 USA.; Jethva, H (reprint author), NASA, Goddard Space Flight Ctr, Earth Sci Div, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA. EM hiren.t.jethva@nasa.gov NR 30 TC 0 Z9 0 U1 4 U2 4 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. PD OCT 14 PY 2016 VL 9 IS 10 BP 5053 EP 5062 DI 10.5194/amt-9-5053-2016 PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DY8VJ UT WOS:000385409400001 ER PT J AU Darr, S Dong, J Glikin, N Hartwig, J Majumdar, A Leclair, A Chung, J AF Darr, Samuel Dong, Jun Glikin, Neil Hartwig, Jason Majumdar, Alok Leclair, Andre Chung, Jacob TI The effect of reduced gravity on cryogenic nitrogen boiling and pipe chilldown SO NPJ MICROGRAVITY LA English DT Article ID CRITICAL HEAT-FLUX; QUENCHING EXPERIMENTS; FLOW; TUBE; MICROGRAVITY AB Manned deep space exploration will require cryogenic in-space propulsion. Yet, accurate prediction of cryogenic pipe flow boiling heat transfer is lacking, due to the absence of a cohesive reduced gravity data set covering the expected flow and thermodynamic parameter ranges needed to validate cryogenic two-phase heat transfer models. This work provides a wide range of cryogenic chilldown data aboard an aircraft flying parabolic trajectories to simulate reduced gravity. Liquid nitrogen is used to quench a 1.27 cm diameter tube from room temperature. The pressure, temperature, flow rate, and inlet conditions are reported from 10 tests covering liquid Reynolds number from 2,000 to 80,000 and pressures from 80 to 810 kPa. Corresponding terrestrial gravity tests were performed in upward, downward, and horizontal flow configurations to identify gravity and flow direction effects on chilldown. Film boiling heat transfer was lessened by up to 25% in reduced gravity, resulting in longer time and more liquid to quench the pipe to liquid temperatures. Heat transfer was enhanced by increasing the flow rate, and differences between reduced and terrestrial gravity diminished at high flow rates. The new data set will enable the development of accurate and robust heat transfer models of cryogenic pipe chilldown in reduced gravity. C1 [Darr, Samuel; Dong, Jun; Glikin, Neil; Chung, Jacob] Univ Florida, Dept Mech & Aerosp Engineer, Gainesville, FL 32611 USA. [Hartwig, Jason] NASA, Power & In Space Prop Branch, Glenn Res Ctr, Cleveland, OH USA. [Majumdar, Alok; Leclair, Andre] NASA, Marshall Spaceflight Ctr, Huntsville, AL USA. RP Chung, J (reprint author), Univ Florida, Dept Mech & Aerosp Engineer, Gainesville, FL 32611 USA. EM jnchung@ufl.edu OI Darr, Samuel/0000-0002-1891-405X NR 31 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 2373-8065 J9 NPJ MICROGRAVITY JI NPJ Microgravity PD OCT 13 PY 2016 VL 2 AR 16033 DI 10.1038/npjmgrav.2016.33 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DY6EB UT WOS:000385198100001 ER PT J AU Vernikos, J Walter, N Worms, JC Blanc, S AF Vernikos, Joan Walter, Nicolas Worms, Jean Claude Blanc, Stephane TI THESEUS: The European research priorities for human exploration of space SO NPJ MICROGRAVITY LA English DT Editorial Material ID PHYSICAL INACTIVITY C1 [Vernikos, Joan] NASA HQ, Life Sci, Washington, DC USA. [Walter, Nicolas; Worms, Jean Claude] European Sci Fdn, Strasbourg, France. [Blanc, Stephane] Univ Strasbourg, IPHC, Strasbourg, France. [Blanc, Stephane] CNRS, UMR7178, Strasbourg, France. RP Blanc, S (reprint author), Univ Strasbourg, IPHC, Strasbourg, France.; Blanc, S (reprint author), CNRS, UMR7178, Strasbourg, France. EM stephane.blanc@iphc.cnrs.fr NR 7 TC 0 Z9 0 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 2373-8065 J9 NPJ MICROGRAVITY JI NPJ Microgravity PD OCT 13 PY 2016 VL 2 AR 16034 DI 10.1038/npjmgrav.2016.34 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DY6EB UT WOS:000385198100002 ER PT J AU Thorson, JT Rindorf, A Gao, J Hanselman, DH Winker, H AF Thorson, James T. Rindorf, Anna Gao, Jin Hanselman, Dana H. Winker, Henning TI Density-dependent changes in effective area occupied for sea-bottom-associated marine fishes SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE density-dependent habitat selection; ideal-free distribution; basin model; spatio-temporal; meta-analysis ID COD GADUS-MORHUA; IDEAL FREE DISTRIBUTION; HABITAT SELECTION; GEOGRAPHIC-DISTRIBUTION; POPULATION-DYNAMICS; STOCK ASSESSMENT; CLIMATE-CHANGE; SOUTHERN GULF; ST-LAWRENCE; ABUNDANCE AB The spatial distribution of marine fishes can change for many reasons, including density-dependent distributional shifts. Previous studies show mixed support for either the proportional-density model (PDM; no relationship between abundance and area occupied, supported by ideal-free distribution theory) or the basin model (BM; positive abundance-area relationship, supported by density-dependent habitat selection theory). The BM implies that fishes move towards preferred habitat as the population declines. We estimate the average relationship using bottom trawl data for 92 fish species from six marine regions, to determine whether the BM or PDM provides a better description for sea-bottom-associated fishes. We fit a spatio-temporal model and estimate changes in effective area occupied and abundance, and combine results to estimate the average abundance-area relationship as well as variability among taxa and regions. The average relationship is weak but significant (0.6% increase in area for a 10% increase in abundance), whereas only a small proportion of species-region combinations show a negative relationship (i.e. shrinking area when abundance increases). Approximately one-third of combinations (34.6%) are predicted to increase in area more than 1% for every 10% increase in abundance. We therefore infer that population density generally changes faster than effective area occupied during abundance changes. Gadiformes have the strongest estimated relationship (average 1.0% area increase for every 10% abundance increase) followed by Pleuronectiformes and Scorpaeniformes, and the Eastern Bering Sea shows a strong relationship between abundance and area occupied relative to other regions. We conclude that the BM explains a small but important portion of spatial dynamics for sea-bottom-associated fishes, and that many individual populations merit cautious management during population declines, because a compressed range may increase the efficiency of harvest. C1 [Thorson, James T.; Gao, Jin] NOAA, Fisheries Resource Assessment & Monitoring Div, Northwest Fisheries Sci Ctr, Natl Marine Fisheries Serv, Seattle, WA 98115 USA. [Rindorf, Anna] Tech Univ Denmark DTU, DTU Aqua Natl Inst Aquat Resources, Jaegersborg 1, DK-2920 Charlottenlund, Denmark. [Gao, Jin] Univ Washington, Sch Aquat & Fishery Sci, Box 355020, Seattle, WA 98195 USA. [Hanselman, Dana H.] NOAA, Auke Bay Lab, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK USA. [Winker, Henning] Kirstenbosch Res Ctr, SANBI, ZA-7735 Claremont, South Africa. [Winker, Henning] Univ Cape Town, Dept Stat Sci, Ctr Stat Ecol Environm & Conservat SEEC, Private Bag X3, ZA-7701 Rondebosch, South Africa. RP Thorson, JT (reprint author), NOAA, Fisheries Resource Assessment & Monitoring Div, Northwest Fisheries Sci Ctr, Natl Marine Fisheries Serv, Seattle, WA 98115 USA. EM james.thorson@noaa.gov OI Thorson, James/0000-0001-7415-1010 FU NOAA Habitat Assessment Improvement Project [15-027] FX J.G. was supported by NOAA Habitat Assessment Improvement Project no. 15-027. NR 40 TC 1 Z9 1 U1 4 U2 4 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD OCT 12 PY 2016 VL 283 IS 1840 AR 20161853 DI 10.1098/rspb.2016.1853 PG 10 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA EA3GN UT WOS:000386490000017 ER PT J AU Hanasaki, N Yoshikawa, S Kakinuma, K Kanae, S AF Hanasaki, Naota Yoshikawa, Sayaka Kakinuma, Kaoru Kanae, Shinjiro TI A seawater desalination scheme for global hydrological models SO HYDROLOGY AND EARTH SYSTEM SCIENCES LA English DT Article ID WATER-RESOURCES; FUTURE CHALLENGES; INTEGRATED MODEL; AVAILABILITY; PATHWAYS; SCARCITY; DEMAND; GROWTH; SCALE AB Seawater desalination is a practical technology for providing fresh water to coastal arid regions. Indeed, the use of desalination is rapidly increasing due to growing water demand in these areas and decreases in production costs due to technological advances. In this study, we developed a model to estimate the areas where seawater desalination is likely to be used as a major water source and the likely volume of production. The model was designed to be incorporated into global hydrological models (GHMs) that explicitly include human water usage. The model requires spatially detailed information on climate, income levels, and industrial and municipal water use, which represent standard input/output data in GHMs. The model was applied to a specific historical year (2005) and showed fairly good reproduction of the present geographical distribution and national production of desalinated water in the world. The model was applied globally to two periods in the future (2011-2040 and 2041-2070) under three distinct socioeconomic conditions, i.e., SSP (shared socioeconomic pathway) 1, SSP2, and SSP3. The results indicate that the usage of seawater desalination will have expanded considerably in geographical extent, and that production will have increased by 1.4-2.1-fold in 2011-2040 compared to the present (from 2.8 x 10(9) m(3) yr(-1) in 2005 to 4.0-6.0 x 10(9) m(3) yr(-1)), and 6.7-17.3-fold in 2041-2070 (from 18.7 to 48.6 x 10(9) m(3) yr(-1)). The estimated global costs for production for each period are USD 1.1-10.6 x 10(9) (0.002-0.019% of the total global GDP), USD 1.6-22.8 x 10(9) (0.001-0.020 %), and USD 7.5-183.9 x 10(9) (0.002-0.100 %), respectively. The large spreads in these projections are primarily attributable to variations within the socioeconomic scenarios. C1 [Hanasaki, Naota] Natl Inst Environm Studies, 16-2 Onogawa, Tsukuba, Ibaraki, Japan. [Hanasaki, Naota] Int Inst Appl Syst Anal, Schlosspl 1, Laxenburg, Austria. [Yoshikawa, Sayaka; Kakinuma, Kaoru; Kanae, Shinjiro] Tokyo Inst Technol, Dept Civil & Environm Engn, Meguro Ku, 2-12-1-M1-6 Ookayama, Tokyo, Japan. [Kakinuma, Kaoru] Columbia Univ, Earth Inst, Ctr Climate Syst Res, 2880 Broadway, New York, NY USA. [Kakinuma, Kaoru] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. RP Hanasaki, N (reprint author), Natl Inst Environm Studies, 16-2 Onogawa, Tsukuba, Ibaraki, Japan.; Hanasaki, N (reprint author), Int Inst Appl Syst Anal, Schlosspl 1, Laxenburg, Austria. EM hanasaki@nies.go.jp RI Hanasaki, Naota/C-2932-2009; Kanae, Shinjiro/E-5606-2010 OI Hanasaki, Naota/0000-0002-5092-7563; Kanae, Shinjiro/0000-0002-3176-4957 FU CREST, Japan Science and Technology Agency; JSPS KAKENHI [25820230, 15H04047, 16H06291]; Ministry of the Environment, Japan FX This work was mainly supported by CREST, Japan Science and Technology Agency. N. Hanasaki acknowledges the support of JSPS KAKENHI grant number 25820230 and the Environment Research and Technology Development Fund (S-14) of the Ministry of the Environment, Japan. S. Yoshikawa, K. Kakinuma, and S. Kanae acknowledge the support of JSPS KAKENHI Grant number 15H04047 and 16H06291. The authors are grateful to three anonymous reviewers, Yoshie Maeda, and Yaling Liu for helpful suggestions. The present work was partially developed within the framework of theWater Futures and Solutions initiative at IIASA and the Panta Rhei Research Initiative of the International Association of Hydrological Sciences (IAHS) by the Water Scarcity Assessment: Methodology and Application working group. Map colors are based on www.colorbrewer.org, by Cynthia A. Brewer of Pennsylvania State University. NR 30 TC 0 Z9 0 U1 5 U2 5 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. PD OCT 12 PY 2016 VL 20 IS 10 BP 4143 EP 4157 DI 10.5194/hess-20-4143-2016 PG 15 WC Geosciences, Multidisciplinary; Water Resources SC Geology; Water Resources GA EA3EB UT WOS:000386481400001 ER PT J AU Tan, ZL Zhuang, QL Henze, DK Frankenberg, C Dlugokencky, E Sweeney, C Turner, AJ Sasakawa, M Machida, T AF Tan, Zeli Zhuang, Qianlai Henze, Daven K. Frankenberg, Christian Dlugokencky, Ed Sweeney, Colm Turner, Alexander J. Sasakawa, Motoki Machida, Toshinobu TI Inverse modeling of pan-Arctic methane emissions at high spatial resolution: what can we learn from assimilating satellite retrievals and using different process-based wetland and lake biogeochemical models? SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID COMPARISON PROJECT WETCHIMP; ATMOSPHERIC METHANE; GROWTH-RATE; ANTHROPOGENIC EMISSIONS; SIBERIAN SHELF; CH4 EMISSIONS; PRESENT STATE; CO2; NORTH; SCIAMACHY AB Understanding methane emissions from the Arctic, a fast-warming carbon reservoir, is important for projecting future changes in the global methane cycle. Here we optimized methane emissions from north of 60 degrees N (pan-Arctic) regions using a nested-grid high-resolution inverse model that assimilates both high-precision surface measurements and column-average SCanning Imaging Absorption spectroMeter for Atmospheric CHartogrphY (SCIAMACHY) satellite retrievals of methane mole fraction. For the first time, methane emissions from lakes were integrated into an atmospheric transport and inversion estimate, together with prior wetland emissions estimated with six biogeochemical models. In our estimates, in 2005, global methane emissions were in the range of 496.4-511.5 Tg yr(-1), and pan-Arctic methane emissions were in the range of 11.9-28.5 Tg yr(-1). Methane emissions from pan-Arctic wetlands and lakes were 5.5-14.2 and 2.4-14.2 Tg yr(-1), respectively. Methane emissions from Siberian wetlands and lakes are the largest and also have the largest uncertainty. Our results indicate that the uncertainty introduced by different wetland models could be much larger than the uncertainty of each inversion. We also show that assimilating satellite retrievals can reduce the un-certainty of the nested-grid inversions. The significance of lake emissions cannot be identified across the pan-Arctic by high-resolution inversions, but it is possible to identify high lake emissions from some specific regions. In contrast to global inversions, high-resolution nested-grid inversions perform better in estimating near-surface methane concentrations. C1 [Tan, Zeli; Zhuang, Qianlai] Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA. [Tan, Zeli; Zhuang, Qianlai] Purdue Univ, Purdue Climate Change Res Ctr, W Lafayette, IN 47907 USA. [Zhuang, Qianlai] Purdue Univ, Dept Agron, W Lafayette, IN 47907 USA. [Henze, Daven K.] Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA. [Frankenberg, Christian] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Dlugokencky, Ed; Sweeney, Colm] NOAA, Global Monitoring Div, Earth Syst Res Lab, Boulder, CO USA. [Turner, Alexander J.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Sasakawa, Motoki; Machida, Toshinobu] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan. RP Zhuang, QL (reprint author), Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA.; Zhuang, QL (reprint author), Purdue Univ, Purdue Climate Change Res Ctr, W Lafayette, IN 47907 USA.; Zhuang, QL (reprint author), Purdue Univ, Dept Agron, W Lafayette, IN 47907 USA. EM qzhuang@purdue.edu RI Chem, GEOS/C-5595-2014; Frankenberg, Christian/A-2944-2013 OI Frankenberg, Christian/0000-0002-0546-5857 FU NASA [NASA-NNX09AI26G]; Department of Energy (DOE) [DE-FG02-08ER64599]; NSF Division of Information and Intelligent Systems [NSF-1028291]; NSF [NSF-0630319]; Office of Science, Office of Biological and Environmental Research of the US Department of Energy [DE-AC02-05CH11231]; NOAA [NA14OAR4310136]; DOE Computational Science Graduate Fellowship (CSGF) FX We would like to thank the two anonymous reviewers for their thorough and constructive reviews. Many thanks are given to the WETCHIMP investigators for making their simulations of wetland methane emissions available. We appreciate the help from Guang-Dih Lei and Bhagirath M. Trivedi at NASA and Robert Yantosca at Harvard for processing nested-grid GOES-5 met data, and the help from Christoph A. Keller at Harvard for processing nested-grid emission data by HEMCO. This study is supported through projects funded to Qianlai Zhuang by the NASA Land Use and Land Cover Change Program (NASA-NNX09AI26G), the Department of Energy (DOE) (DE-FG02-08ER64599), the NSF Division of Information and Intelligent Systems (NSF-1028291), and the NSF Carbon and Water in the Earth Program (NSF-0630319). This research is also in part supported by the Director, Office of Science, Office of Biological and Environmental Research of the US Department of Energy under contract no. DE-AC02-05CH11231 as part of their Earth System Modeling Program. Daven K. Henze acknowledges NOAA grant no. NA14OAR4310136. Alexander J. Turner was supported by a DOE Computational Science Graduate Fellowship (CSGF). The supercomputing resource is provided by the Rosen Center for Advanced Computing at Purdue University. NR 100 TC 0 Z9 0 U1 11 U2 11 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. PD OCT 12 PY 2016 VL 16 IS 19 BP 12649 EP 12666 DI 10.5194/acp-16-12649-2016 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DY8TG UT WOS:000385403300001 ER PT J AU Muller, D Bockmann, C Kolgotin, A Schneidenbach, L Chemyakin, E Rosemann, J Znak, P Romanov, A AF Mueller, Detlef Boeckmann, Christine Kolgotin, Alexei Schneidenbach, Lars Chemyakin, Eduard Rosemann, Julia Znak, Pavel Romanov, Anton TI Microphysical particle properties derived from inversion algorithms developed in the framework of EARLINET SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID AEROSOL-SIZE DISTRIBUTION; BACKSCATTER LIDAR DATA; MULTIWAVELENGTH LIDAR; RAMAN-LIDAR; TROPOSPHERIC AEROSOL; REGULARIZATION METHOD; INTEGRAL EQUATIONS; OPTICAL-DATA; PARAMETERS; RETRIEVAL AB We present a summary on the current status of two inversion algorithms that are used in EARLINET (European Aerosol Research Lidar Network) for the inversion of data collected with EARLINET multiwavelength Raman lidars. These instruments measure backscatter coefficients at 355, 532, and 1064 nm, and extinction coefficients at 355 and 532 nm. Development of these two algorithms started in 2000 when EARLINET was founded. The algorithms are based on a manually controlled inversion of optical data which allows for detailed sensitivity studies. The algorithms allow us to derive particle effective radius as well as volume and surface area concentration with comparably high confidence. The retrieval of the real and imaginary parts of the complex refractive index still is a challenge in view of the accuracy required for these parameters in climate change studies in which light absorption needs to be known with high accuracy. It is an extreme challenge to retrieve the real part with an accuracy better than 0.05 and the imaginary part with accuracy better than 0.005-0.1 or +/- 50 %. Single-scattering albedo can be computed from the retrieved microphysical parameters and allows us to categorize aerosols into high-and low-absorbing aerosols. On the basis of a few exemplary simulations with synthetic optical data we discuss the current status of these manually operated algorithms, the potentially achievable accuracy of data products, and the goals for future work. One algorithm was used with the purpose of testing how well microphysical parameters can be derived if the real part of the complex refractive index is known to at least 0.05 or 0.1. The other algorithm was used to find out how well microphysical parameters can be derived if this constraint for the real part is not applied. The optical data used in our study cover a range of Angstrom exponents and extinction-to-backscatter (lidar) ratios that are found from lidar measurements of various aerosol types. We also tested aerosol scenarios that are considered highly unlikely, e.g. the lidar ratios fall outside the commonly accepted range of values measured with Raman lidar, even though the underlying microphysical particle properties are not uncommon. The goal of this part of the study is to test the robustness of the algorithms towards their ability to identify aerosol types that have not been measured so far, but cannot be ruled out based on our current knowledge of aerosol physics. We computed the optical data from monomodal logarithmic particle size distributions, i.e. we explicitly excluded the more complicated case of bimodal particle size distributions which is a topic of ongoing research work. Another constraint is that we only considered particles of spherical shape in our simulations. We considered particle radii as large as 7-10 mu m in our simulations where the Potsdam algorithm is limited to the lower value. We considered optical-data errors of 15% in the simulation studies. We target 50% uncertainty as a reasonable threshold for our data products, though we attempt to obtain data products with less uncertainty in future work. C1 [Mueller, Detlef] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield, Herts, England. [Boeckmann, Christine; Rosemann, Julia] Univ Potsdam, Inst Math, Neuen Palais 10, D-14469 Potsdam, Germany. [Kolgotin, Alexei] Phys Instrumentat Ctr, Troitsk, Russia. [Chemyakin, Eduard] NASA, Langley Res Ctr, Sci Syst & Applicat Inc, Hampton, VA 23665 USA. [Znak, Pavel] St Petersburg Univ, VA Fock Inst Phys, Ulyanovskaya 1, St Petersburg 198504, Russia. [Romanov, Anton] Natl Univ Sci & Technol, Moscow, Russia. [Schneidenbach, Lars] Univ Potsdam, Inst Comp Sci, Neuen Palais 10, D-14469 Potsdam, Germany. RP Muller, D (reprint author), Univ Hertfordshire, Sch Phys Astron & Math, Hatfield, Herts, England. EM d.mueller@herts.ac.uk RI Znak, Pavel/Q-6700-2016 OI Znak, Pavel/0000-0002-3555-1414 FU European Union [EVR1-CT-1999-40003, 289923 - ITaRS, 654109]; EU [RICA-025991]; DAAD project "Ostpartnerschaften" of Potsdam University FX This work has been supported since 2000 under Grant No. EVR1-CT-1999-40003 (EARLINET project) of the Environment Program of the European Union and Grant No. RICA-025991 (EARLINET-ASOS project) of the 6th Framework EU program. The work has been supported partially by the European Union Seventh Framework Program for research, technological development, and demonstration under grant agreement No. 289923 - ITaRS and by DAAD project "Ostpartnerschaften" of Potsdam University. Finally, this work received partial funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No. 654109 (Actris). NR 49 TC 1 Z9 1 U1 3 U2 3 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. PD OCT 12 PY 2016 VL 9 IS 10 BP 5007 EP 5035 DI 10.5194/amt-9-5007-2016 PG 29 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DY8UW UT WOS:000385408000001 ER PT J AU Johlander, A Schwartz, SJ Vaivads, A Khotyaintsev, YV Gingell, I Peng, IB Markidis, S Lindqvist, PA Ergun, RE Marklund, GT Plaschke, F Magnes, W Strangeway, RJ Russell, CT Wei, H Torbert, RB Paterson, WR Gershman, DJ Dorelli, JC Avanov, LA Lavraud, B Saito, Y Giles, BL Pollock, CJ Burch, JL AF Johlander, A. Schwartz, S. J. Vaivads, A. Khotyaintsev, Yu. V. Gingell, I. Peng, I. B. Markidis, S. Lindqvist, P. -A. Ergun, R. E. Marklund, G. T. Plaschke, F. Magnes, W. Strangeway, R. J. Russell, C. T. Wei, H. Torbert, R. B. Paterson, W. R. Gershman, D. J. Dorelli, J. C. Avanov, L. A. Lavraud, B. Saito, Y. Giles, B. L. Pollock, C. J. Burch, J. L. TI Rippled Quasiperpendicular Shock Observed by the Magnetospheric Multiscale Spacecraft SO PHYSICAL REVIEW LETTERS LA English DT Article ID COLLISIONLESS SHOCK; BOW SHOCK; MACH NUMBER; PLASMA; SIMULATIONS; NORMALS AB Collisionless shock nonstationarity arising from microscale physics influences shock structure and particle acceleration mechanisms. Nonstationarity has been difficult to quantify due to the small spatial and temporal scales. We use the closely spaced (subgyroscale), high-time-resolution measurements from one rapid crossing of Earth's quasiperpendicular bow shock by the Magnetospheric Multiscale (MMS) spacecraft to compare competing nonstationarity processes. Using MMS's high-cadence kinetic plasma measurements, we show that the shock exhibits nonstationarity in the form of ripples. C1 [Johlander, A.; Vaivads, A.; Khotyaintsev, Yu. V.] Swedish Inst Space Phys, S-75121 Uppsala, Sweden. [Johlander, A.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. [Schwartz, S. J.] Imperial Coll London, Blackett Lab, London SW7 2AZ, England. [Schwartz, S. J.; Ergun, R. E.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA. [Peng, I. B.; Markidis, S.; Lindqvist, P. -A.; Marklund, G. T.] KTH Royal Inst Technol, S-11428 Stockholm, Sweden. [Plaschke, F.; Magnes, W.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria. [Strangeway, R. J.; Russell, C. T.; Wei, H.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. [Torbert, R. B.] Univ New Hampshire, Durham, NH 03824 USA. [Paterson, W. R.; Gershman, D. J.; Dorelli, J. C.; Avanov, L. A.; Giles, B. L.; Pollock, C. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gershman, D. J.] Univ Maryland, College Pk, MD 20742 USA. [Lavraud, B.] Univ Toulouse, Inst Rech Astrophys & Planetol, F-31028 Toulouse, France. [Lavraud, B.] CNRS, UMR 5277, F-31400 Toulouse, France. [Saito, Y.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan. [Burch, J. L.] Inst Space & Astronaut Sci, San Antonio, TX 78238 USA. RP Johlander, A (reprint author), Swedish Inst Space Phys, S-75121 Uppsala, Sweden.; Johlander, A (reprint author), Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. RI NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 FU CNES; CNRS; Leverhulme Trust Research Fellowship; Swedish National Space Board [139/12, 97/13] FX We thank the entire MMS team and instrument PIs for data access and support. The IRAP contribution to MMS was funded by CNES and CNRS. S. J. S. gratefully acknowledges the receipt of a Leverhulme Trust Research Fellowship. This study was supported by Swedish National Space Board Contracts No. 139/12 and No. 97/13. NR 28 TC 1 Z9 1 U1 6 U2 6 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 OCT 12 PY 2016 VL 117 IS 16 AR 165101 DI 10.1103/PhysRevLett.117.165101 PG 5 WC Physics, Multidisciplinary SC Physics GA DZ1ZQ UT WOS:000385641500003 PM 27792387 ER PT J AU Merlin, G Riedi, J Labonnote, LC Cornet, C Davis, AB Dubuisson, P Desmons, M Ferlay, N Parol, F AF Merlin, Guillaume Riedi, Jerome Labonnote, Laurent C. Cornet, Celine Davis, Anthony B. Dubuisson, Phillipe Desmons, Marine Ferlay, Nicolas Parol, Frederic TI Cloud information content analysis of multi-angular measurements in the oxygen A-band: application to 3MI and MSPI SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID MOLECULAR LINE ABSORPTION; SCATTERING ATMOSPHERE; GEOMETRICAL THICKNESS; POLARIZED-LIGHT; TOP PRESSURE; PART II; MODIS; RETRIEVAL; SATELLITE; POLDER AB Information content analyses on cloud top altitude (CTOP) and geometrical thickness (CGT) from multi-angular A-band measurements in the case of monolayer homogeneous clouds are conducted. In the framework of future multi-angular radiometer development, we compared the potential performances of the 3MI (Multiviewing, Multi-channel and Multi-polarization Imaging) instrument developed by EUMETSAT, which is an extension of POLDER/PARASOL instrument and MSPI (Multiangle SpectroPolarimetric Imager) developed by NASA's Jet Propulsion Laboratory. Quantitative information content estimates were realized for thin, moderately opaque and opaque clouds for different surface albedo and viewing geometry configurations. Analyses show that retrieval of CTOP is possible with a high accuracy in most of the cases investigated. Retrieval of CGT is also possible for optically thick clouds above a black surface, at least when CGT >1-2 km and for thin clouds for CGT > 2-3 km. However, for intermediate optical thicknesses (COT similar or equal to 4), we show that the retrieval of CGT is not simultaneously possible with CTOP. A comparison between 3MI and MSPI shows a higher information content for MSPI's measurements, traceable to a thinner filter inside the oxygen A-band, yielding higher signal-to-noise ratio for absorption estimation. Cases of cloud scenes above bright surfaces are more complex but it is shown that the retrieval of CTOP remains possible in almost all situations while the information content on CGT appears to be insufficient in many cases, particularly for COT <4 and CGT <2-3 km. C1 [Merlin, Guillaume; Riedi, Jerome; Labonnote, Laurent C.; Cornet, Celine; Dubuisson, Phillipe; Desmons, Marine; Ferlay, Nicolas; Parol, Frederic] Univ Lille 1, Lab Opt Atmospher, Sci & Technol, Villeneuve Dascq, France. [Davis, Anthony B.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Riedi, J (reprint author), Univ Lille 1, Lab Opt Atmospher, Sci & Technol, Villeneuve Dascq, France. EM jerome.riedi@univ-lille1.fr FU CNES; NASA's SMD/ESD; Region Nord-Pas de Calais FX The authors are grateful for financial support from CNES as well as NASA's SMD/ESD (several programmes managed by H. Maring, K. Jucks and R. Eckman). They also thank Dave Diner, Jay Herman and Yuequi Yang for fruitful discussions. Guillaume Merlin is supported by a PhD grad from CNES and Region Nord-Pas de Calais. NR 53 TC 0 Z9 0 U1 3 U2 3 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. PD OCT 11 PY 2016 VL 9 IS 10 BP 4977 EP 4995 DI 10.5194/amt-9-4977-2016 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DY8UT UT WOS:000385407600001 ER PT J AU Alonzo, M Van Den Hoek, J Ahmed, N AF Alonzo, Michael Van Den Hoek, Jamon Ahmed, Nabil TI Capturing coupled riparian and coastal disturbance from industrial mining using cloud-resilient satellite time series analysis SO SCIENTIFIC REPORTS LA English DT Article ID FOREST COVER LOSS; EXTRACTIVE INDUSTRIES; SUSPENDED-SOLIDS; DETECTING TRENDS; LANDSAT IMAGERY; VEGETATION; SEGMENTATION; ALGORITHMS; INDONESIA; QUALITY AB The socio-ecological impacts of large scale resource extraction are frequently underreported in underdeveloped regions. The open-pit Grasberg mine in Papua, Indonesia, is one of the world's largest copper and gold extraction operations. Grasberg mine tailings are discharged into the lowland Ajkwa River deposition area (ADA) leading to forest inundation and degradation of water bodies critical to indigenous peoples. The extent of the changes and temporal linkages with mining activities are difficult to establish given restricted access to the region and persistent cloud cover. Here, we introduce remote sensing methods to "peer through" atmospheric contamination using a dense Landsat time series to simultaneously quantify forest loss and increases in estuarial suspended particulate matter (SPM) concentration. We identified 138 km(2) of forest loss between 1987 and 2014, an area >42 times larger than the mine itself. Between 1987 and 1998, the rate of disturbance was highly correlated (Pearson's r = 0.96) with mining activity. Following mine expansion and levee construction along the ADA in the mid-1990s, we recorded significantly (p < 0.05) higher SPM in the Ajkwa Estuary compared to neighboring estuaries. This research provides a means to quantify multiple modes of ecological damage from mine waste disposal or other disturbance events. C1 [Alonzo, Michael] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Alonzo, Michael] Amer Univ, Dept Environm Sci, Washington, DC 20016 USA. [Van Den Hoek, Jamon] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Geog & Geospatial Sci, Corvallis, OR 97331 USA. [Ahmed, Nabil] London Metropolitan Univ, Cass Sch Architecture, London, England. RP Alonzo, M (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.; Alonzo, M (reprint author), Amer Univ, Dept Environm Sci, Washington, DC 20016 USA. EM michael.g.alonzo@nasa.gov NR 58 TC 1 Z9 1 U1 4 U2 4 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2045-2322 J9 SCI REP-UK JI Sci Rep PD OCT 11 PY 2016 VL 6 AR 35129 DI 10.1038/srep35129 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DY2MT UT WOS:000384927400001 PM 27725748 ER PT J AU Gheller, C Vazza, F Bruggen, M Alpaslan, M Holwerda, BW Hopkins, AM Liske, J AF Gheller, C. Vazza, F. Brueggen, M. Alpaslan, M. Holwerda, B. W. Hopkins, A. M. Liske, J. TI Evolution of cosmic filaments and of their galaxy population from MHD cosmological simulations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; intergalactic medium; large-scale structure of Universe ID MASS ASSEMBLY GAMA; HOT INTERGALACTIC MEDIUM; LARGE-SCALE STRUCTURE; MAGNETIC-FIELDS; STAR-FORMATION; DARK-MATTER; HYDRODYNAMICAL SIMULATIONS; ELLIPTIC GALAXIES; RAM PRESSURE; SHOCK-WAVES AB Despite containing about a half of the total matter in the Universe, at most wavelengths the filamentary structure of the cosmic web is difficult to observe. In this work, we use large unigrid cosmological simulations to investigate how the geometrical, thermodynamical and magnetic properties of cosmological filaments vary with mass and redshift (z <= 1). We find that the average temperature, length, volume and magnetic field of filaments scales well with their total mass. This reflects the role of self-gravity in shaping their properties and enables statistical predictions of their observational properties based on their mass. We also focus on the properties of the simulated population of galaxy-sized haloes within filaments, and compare their properties to the results obtained from the spectroscopic GAMA survey. Simulated and observed filaments with the same length are found to contain an equal number of galaxies, with very similar distribution of masses. The total number of galaxies within each filament and the total/average stellar mass in galaxies can now be used to predict also the large-scale properties of the gas in the host filaments across tens or hundreds of Mpc in scale. These results are the first steps towards the future use of galaxy catalogues in order to select the best targets for observations of the warm-hot intergalactic medium. C1 [Gheller, C.] ETHZ CSCS, Via Trevano 131, CH-6900 Lugano, Switzerland. [Vazza, F.; Brueggen, M.; Liske, J.] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. [Vazza, F.] INAF Ist Radio Astron, Via Gobetti 101, I-40129 Bologna, Italy. [Alpaslan, M.] NASA, Ames Res Ctr, N232, Moffett Field, CA 94035 USA. [Holwerda, B. W.] Leiden Univ, Sterrenwacht Leiden, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands. [Hopkins, A. M.] Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia. RP Gheller, C (reprint author), ETHZ CSCS, Via Trevano 131, CH-6900 Lugano, Switzerland. EM cgheller@cscs.ch; franco.vazza@hs.uni-hamburg.de OI Holwerda, Benne/0000-0002-4884-6756 FU Chronos project [ch2, s585]; Deutsche Forschungsgemeinschaft (DFG) [VA 876/3-1]; DFG [FOR1254]; NASA; STFC (UK); ARC (Australia); AAO; ESO Telescopes at the La Silla Paranal Observatory [179.A-2004] FX Computations accomplished in this work were performed using the ENZO code (http://enzo-project.org), which is the product of a collaborative effort of scientists at many universities and national laboratories. We gratefully acknowledge the ENZO development group for providing helpful and well-maintained online documentation and tutorials. We also acknowledge ETHZ-CSCS1 for the use of the Piz Daint systems in the Chronos project ID ch2 and s585, and of the Piz Dora system for data processing and visualization. We would like to thank Jean Favre for the support on VISIT and Maria Grazia Giuffreda for her valuable technical assistance at CSCS. FV acknowledges personal support from the grant VA 876/3-1 from the Deutsche Forschungsgemeinschaft (DFG). FV and MB acknowledge partial support from the grant FOR1254 from DFG. We also acknowledge the use of computing resources under allocations no. 7006 and 9016 (FV) and 9059 (MB) on supercomputers at the NIC of the Forschungszentrum Julich. MA is funded by an appointment to the NASA Postdoctoral Program at Ames Research Centre, administered by Universities Space Research Association through a contract with NASA. 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 Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programs 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 VISTA VIKING data used in this paper is based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 179.A-2004. NR 61 TC 0 Z9 0 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 11 PY 2016 VL 462 IS 1 BP 448 EP 463 DI 10.1093/mnras/stw1595 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW3BI UT WOS:000383516700059 ER PT J AU Contopoulos, I Kazanas, D Papadopoulos, DB AF Contopoulos, I. Kazanas, D. Papadopoulos, D. B. TI The magnetic Rayleigh-Taylor instability in astrophysical discs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitation; MHD ID BLACK-HOLE; ACCRETION DISKS; COSMIC BATTERY; JETS; ELECTRODYNAMICS; FIELD AB This is our first study of the magnetic Rayleigh Taylor instability at the inner edge of an astrophysical disc around a central back hole. We derive the equations governing small-amplitude oscillations in general relativistic ideal magnetodydrodynamics and obtain a criterion for the onset of the instability. We suggest that static disc configurations where magnetic field is held by the disc material are unstable around a Schwarzschild black hole. On the other hand, we find that such configurations are stabilized by the space-time rotation around a Kerr black hole. We obtain a crude estimate of the maximum amount of poloidal magnetic flux that can be accumulated around the centre, and suggest that it is proportional to the black hole spin. Finally, we discuss the astrophysical implications of our result for the theoretical and observational estimations of the black hole jet power. C1 [Contopoulos, I.] Acad Athens, Res Ctr Astron & Appl Math, Athens 11527, Greece. [Contopoulos, I.] Natl Res Nucl Univ, Moscow 115409, Russia. [Kazanas, D.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Code 661, Greenbelt, MD 20771 USA. [Papadopoulos, D. B.] Aristotle Univ Thessaloniki, Dept Phys, Thessaloniki 54124, Greece. RP Contopoulos, I (reprint author), Acad Athens, Res Ctr Astron & Appl Math, Athens 11527, Greece.; Contopoulos, I (reprint author), Natl Res Nucl Univ, Moscow 115409, Russia. EM icontop@academyofathens.gr FU General Secretariat for Research and Technology of Greece; European Social Fund FX This work was supported by the General Secretariat for Research and Technology of Greece and the European Social Fund in the framework of Action 'Excellence'. NR 22 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 11 PY 2016 VL 462 IS 1 BP 565 EP 575 DI 10.1093/mnras/stw1565 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW3BI UT WOS:000383516700069 ER PT J AU Garcia, JA Fabian, AC Kallman, TR Dauser, T Parker, ML McClintock, JE Steiner, JF Wilms, J AF Garcia, Javier A. Fabian, Andrew C. Kallman, Timothy R. Dauser, Thomas Parker, Michael L. McClintock, Jeffrey E. Steiner, James F. Wilms, Joern TI The effects of high density on the X-ray spectrum reflected from accretion discs around black holes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; atomic processes; line: formation; radiative transfer; relativistic processes; X-rays: general ID ACTIVE GALACTIC NUCLEI; K-SHELL PHOTOABSORPTION; ENERGY-DISTRIBUTIONS; SUZAKU OBSERVATIONS; XMM-NEWTON; GX 339-4; SOFT EXCESS; HARD STATE; CYGNUS X-1; IRON LINES AB Current models of the spectrum of X-rays reflected from accretion discs around black holes and other compact objects are commonly calculated assuming that the density of the disc atmosphere is constant within several Thomson depths from the irradiated surface. An important simplifying assumption of these models is that the ionization structure of the gas is completely specified by a single, fixed value of the ionization parameter xi, which is the ratio of the incident flux to the gas density. The density is typically fixed at n(e) = 10(15) cm(-3). Motivated by observations, we consider higher densities in the calculation of the reflected spectrum. We show by computing model spectra for n(e) greater than or similar to 10(17) cm(-3) that high-density effects significantly modify reflection spectra. The main effect is to boost the thermal continuum at energies less than or similar to 2 keV. We discuss the implications of these results for interpreting observations of both active galactic nuclei and black hole binaries. We also discuss the limitations of our models imposed by the quality of the atomic data currently available. C1 [Garcia, Javier A.; McClintock, Jeffrey E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Fabian, Andrew C.; Parker, Michael L.] Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Kallman, Timothy R.] NASA Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. [Dauser, Thomas; Wilms, Joern] Univ Erlangen Nurnberg, Remeis Observ, Sternwartstr 7, D-96049 Bamberg, Germany. [Dauser, Thomas; Wilms, Joern] Univ Erlangen Nurnberg, ECAP, Sternwartstr 7, D-96049 Bamberg, Germany. [Steiner, James F.] MIT, Kavli Inst Astrophys & Space Res, 70 Vassar St, Cambridge, MA 02139 USA. RP Garcia, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM javier@head.cfa.harvard.edu; acf@ast.cam.ac.uk RI Wilms, Joern/C-8116-2013 OI Wilms, Joern/0000-0003-2065-5410 FU CGPS grant from the Smithsonian Institution; ERC [340442]; Einstein Fellowship [PF5-160144] FX We thank the anonymous referee for their positive and useful comments, and Laura Brenneman for insightful discussions. JG and JEM acknowledge the support of a CGPS grant from the Smithsonian Institution. ACF acknowledges ERC Advanced Grant 340442 Feedback. JFS has been supported by the Einstein Fellowship grant PF5-160144. NR 73 TC 3 Z9 3 U1 3 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 11 PY 2016 VL 462 IS 1 BP 751 EP 760 DI 10.1093/mnras/stw1696 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW3BI UT WOS:000383516700083 ER PT J AU De Pasquale, M Page, MJ Kann, DA Oates, SR Schulze, S Zhang, B Cano, Z Gendre, B Malesani, D Rossi, A Troja, E Piro, L Boer, M Stratta, G Gehrels, N AF De Pasquale, M. Page, M. J. Kann, D. A. Oates, S. R. Schulze, S. Zhang, B. Cano, Z. Gendre, B. Malesani, D. Rossi, A. Troja, E. Piro, L. Boer, M. Stratta, G. Gehrels, N. TI The 80 Ms follow-up of the X-ray afterglow of GRB 130427A challenges the standard forward shock model SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gamma-ray burst: general; gamma-ray burst: individual: GRB 130427A ID LIGHT CURVES; BURST AFTERGLOWS; TELESCOPE OBSERVATIONS; STAR-FORMATION; CENTRAL ENGINE; VIEWING ANGLE; GEV EMISSION; JET BREAKS; BROAD-BAND; SWIFT-ERA AB GRB 130427A was the brightest gamma-ray burst detected in the last 30 yr. With an equivalent isotropic energy output of 8.5 x 10(53) erg and redshift z = 0.34, it uniquely combined very high energetics with a relative proximity to Earth. As a consequence, its X-ray afterglow has been detected by sensitive X-ray observatories such as XMM-Newton and Chandra for a record-breaking baseline longer than 80 million seconds. We present the X-ray light curve of this event over such an interval. The light curve shows a simple power-law decay with a slope alpha = 1.309 +/- 0.007 over more than three decades in time (47 ks-83 Ms). We discuss the consequences of this result for a few models proposed so far to interpret GRB 130427A, and more in general the significance of this outcome in the context of the standard forward shock model. We find that this model has difficulty in explaining our data, in both cases of constant density and stellar-wind circumburst media, and requires far-fetched values for the physical parameters involved. C1 [De Pasquale, M.; Page, M. J.; Oates, S. R.] Univ Coll London, Mullard Space Sci Lab, Holmbury Rd, Dorking RH5 6NT, Surrey, England. [De Pasquale, M.] Ist Astrofis Spaziale & Fis Cosm Palermo INAF, Via U Malfa 153, I-90146 Palermo, Italy. [De Pasquale, M.] Ist Euro Mediterraneo Sci & Tecnol, Via Michele Miraglia 20, I-90139 Palermo, Italy. [Kann, D. A.] Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany. [Oates, S. R.] CSIC, Inst Astrofis Andalucia, Glorieta Astron, E-18008 Granada, Spain. [Schulze, S.] Millennium Inst Astrophys, Vicuna Mackenna 4860, Santiago 7820436, Chile. [Schulze, S.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Vicuna Mackenna 4860, Santiago 7820436, Chile. [Zhang, B.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. [Cano, Z.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland. [Gendre, B.] Univ Virgin Isl, 2 John Brewers Bay, St Thomas, VI 00802 USA. [Gendre, B.] Etelman Observ, St Thomas, VI 00802 USA. [Malesani, D.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. [Rossi, A.] Ist Astrofis Spaziale & Fis Cosm Bologna INAF, Via P Gobetti 101, I-40129 Bologna, Italy. [Troja, E.; Gehrels, N.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Piro, L.] Inst Space Astrophys & Planetol, Via F Del Cavaliere 100, I-00133 Rome, Italy. [Gendre, B.; Boer, M.] CNRS, ARTEMIS, Blvd Observ,CS 34229, F-06304 Nice 4, France. [Stratta, G.] Univ Urbino, Dept Phys, VS Chiara 27, I-61029 Urbino, Italy. RP De Pasquale, M (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury Rd, Dorking RH5 6NT, Surrey, England.; De Pasquale, M (reprint author), Ist Astrofis Spaziale & Fis Cosm Palermo INAF, Via U Malfa 153, I-90146 Palermo, Italy.; De Pasquale, M (reprint author), Ist Euro Mediterraneo Sci & Tecnol, Via Michele Miraglia 20, I-90139 Palermo, Italy. EM m.depasquale@ucl.ac.uk; s.oates@warwick.ac.uk OI Gendre, Bruce/0000-0002-9077-2025 FU PRIN-INAF [2012/13]; Premiale LBT; NASA [NNX13AD28A, NNX15AP95A]; FIGARONet collaborative network; Agence Nationale de la Recherche [ANR-14-CE33]; TLS Tautenburg; Ida; Instrument Center for Danish Astrophysics (IDA); Italian Ministry of Education, University and Research (MIUR) [FIRB 2012 RBFR12PM1F]; UK Space Agency; Spanish Ministry [AYA2012-39727-C03-01]; Icelandic Research Fund (IRF) FX MDP thanks Lara Nava and Daisuke Kawata for helpful discussions and references, Alice Breeveld for her helping hand, and his friends Marco D'Alessandro, John Moore, Ernesto Amato, Peter Rockhill, Peter Veasny, Alexander J. Zech, and Pierluigi Cox for their encouragement. AR acknowledge support from PRIN-INAF 2012/13 and from Premiale LBT 2013. BG acknowledges financial support of the NASA through the NASA Award NNX13AD28A and the NASA Award NNX15AP95A. Part of this work is under the auspice of the FIGARONet collaborative network, supported by the Agence Nationale de la Recherche, programme ANR-14-CE33. DAK acknowledges support by TLS Tautenburg in form of a research stipend. DM acknowledges support from Ida as well as financial support from Instrument Center for Danish Astrophysics (IDA). GS acknowledge the financial support of the Italian Ministry of Education, University and Research (MIUR) through grant FIRB 2012 RBFR12PM1F. MDP and MJP acknowledge support from the UK Space Agency. SRO acknowledges the support of the Spanish Ministry, Project Number AYA2012-39727-C03-01. ZC gratefully acknowledges financial support from the Icelandic Research Fund (IRF). NR 98 TC 0 Z9 0 U1 3 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 11 PY 2016 VL 462 IS 1 BP 1111 EP 1122 DI 10.1093/mnras/stw1704 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW3BI UT WOS:000383516700112 ER PT J AU Szypryt, P Mazin, BA Ulbricht, G Bumble, B Meeker, SR Bockstiegel, C Walter, AB AF Szypryt, P. Mazin, B. A. Ulbricht, G. Bumble, B. Meeker, S. R. Bockstiegel, C. Walter, A. B. TI High quality factor platinum silicide microwave kinetic inductance detectors SO APPLIED PHYSICS LETTERS LA English DT Article ID ARRAYS; INSTRUMENT; ARCONS; NIKA2 AB We report on the development of microwave kinetic inductance detectors (MKIDs) using platinum silicide as the sensor material. MKIDs are an emerging superconducting detector technology, capable of measuring the arrival times of single photons to better than two microseconds and their energies to around ten percent. Previously, MKIDs have been fabricated using either substoichiometric titanium nitride or aluminum, but TiN suffers from the spatial inhomogeneities in the superconducting critical temperature and Al has a low kinetic inductance fraction, causing low detector sensitivity. To address these issues, we have instead fabricated the PtSi microresonators with the superconducting critical temperatures of 944 +/- 12 mK and high internal quality factors (Qi greater than or similar to 106). These devices show typical quasiparticle lifetimes of tau(qp) approximate to 30-40 mu s and spectral resolution, R = lambda/Delta lambda, of 8 at 406.6 nm. We compare PtSi MKIDs to those fabricated with TiN and detail the substantial advantages that PtSi MKIDs have to offer. Published by AIP Publishing. C1 [Szypryt, P.; Mazin, B. A.; Ulbricht, G.; Meeker, S. R.; Bockstiegel, C.; Walter, A. B.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Bumble, B.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP Szypryt, P (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. EM pszypryt@physics.ucsb.edu OI Ulbricht, Gerhard/0000-0002-6497-3763 FU NASA Space Technology Research Fellowship (NSTRF) FX This work was supported by a NASA Space Technology Research Fellowship (NSTRF). Fabrication was done in the UCSB Nanofabrication Facility. The authors would like to thank the Las Cumbres Observatory Global Telescope (LCOGT) network for assisting in broadband quantum efficiency measurements and Omid Noroozian for providing archival noise data. NR 20 TC 0 Z9 0 U1 3 U2 3 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD OCT 10 PY 2016 VL 109 IS 15 AR 151102 DI 10.1063/1.4964665 PG 4 WC Physics, Applied SC Physics GA EA3VI UT WOS:000386534800002 ER PT J AU Burleigh, MR Richey, CR Rinehart, SA Quijada, MA Wollack, EJ AF Burleigh, M. R. Richey, C. R. Rinehart, S. A. Quijada, M. A. Wollack, E. J. TI Spectrometer baseline control via spatial filtering SO APPLIED OPTICS LA English DT Article ID FOURIER-TRANSFORM SPECTROSCOPY; FIELD DIFFRACTION PATTERNS; TERTIARY INTERFEROGRAMS; FRAUNHOFER DIFFRACTION; SEMICIRCULAR APERTURES; MULTIPLE REFLECTIONS; SPECTRA; REDUCTION; SILICON AB An absorptive half-moon aperture mask is experimentally explored as a broad-bandwidth means of eliminating spurious spectral features arising from reprocessed radiation in an infrared Fourier transform spectrometer. In the presence of the spatial filter, an order of magnitude improvement in the fidelity of the spectrometer baseline is observed. The method is readily accommodated within the context of commonly employed instrument configurations and leads to a factor of two reduction in optical throughput. A detailed discussion of the underlying mechanism and limitations of the method are provided. C1 [Burleigh, M. R.; Richey, C. R.; Rinehart, S. A.; Quijada, M. A.; Wollack, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Burleigh, M. R.] Embry Riddle Aeronaut Univ, Daytona Beach, FL 32114 USA. RP Wollack, EJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM edward.j.wollack@nasa.gov RI Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 FU National Aeronautics and Space Administration (NASA) Astronomy Physics Research and Analysis (APRA) [NNH09ZDA001N]; Goddard Space Flight Center (GSFC) Internal Research and Development (IRAD) FX National Aeronautics and Space Administration (NASA) Astronomy Physics Research and Analysis (APRA) (NNH09ZDA001N); Goddard Space Flight Center (GSFC) Internal Research and Development (IRAD). NR 33 TC 0 Z9 0 U1 3 U2 3 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD OCT 10 PY 2016 VL 55 IS 29 BP 8201 EP 8206 DI 10.1364/AO.55.008201 PG 6 WC Optics SC Optics GA DZ3AQ UT WOS:000385715900010 PM 27828063 ER PT J AU Liu, X Yang, QG Li, H Jin, ZH Wu, W Kizer, S Zhou, DK Yang, P AF Liu, Xu Yang, Qiguang Li, Hui Jin, Zhonghai Wu, Wan Kizer, Susan Zhou, Daniel K. Yang, Ping TI Development of a fast and accurate PCRTM radiative transfer model in the solar spectral region SO APPLIED OPTICS LA English DT Article ID MONTE-CARLO CALCULATIONS; DISCRETE-ORDINATE-METHOD; ATMOSPHERE-OCEAN SYSTEM; MULTIPLE-SCATTERING; INHOMOGENEOUS ATMOSPHERES; PLANETARY-ATMOSPHERES; POLARIZED-LIGHT; ABSORBING GAS; CIRRUS CLOUDS; BIDIRECTIONAL REFLECTANCE AB A fast and accurate principal component-based radiative transfer model in the solar spectral region (PCRTM-SOLAR) has been developed. The algorithm is capable of simulating reflected solar spectra in both clear sky and cloudy atmospheric conditions. Multiple scattering of the solar beam by the multilayer clouds and aerosols are calculated using a discrete ordinate radiative transfer scheme. The PCRTM-SOLAR model can be trained to simulate top-of-atmosphere radiance or reflectance spectra with spectral resolution ranging from 1 cm(-1) resolution to a few nanometers. Broadband radiances or reflectance can also be calculated if desired. The current version of the PCRTM-SOLAR covers a spectral range from 300 to 2500 nm. The model is valid for solar zenith angles ranging from 0 to 80 deg, the instrument view zenith angles ranging from 0 to 70 deg, and the relative azimuthal angles ranging from 0 to 360 deg. Depending on the number of spectral channels, the speed of the current version of PCRTM-SOLAR is a few hundred to over one thousand times faster than the medium speed correlated-k option MODTRAN5. The absolute RMS error in channel radiance is smaller than 10(-3) mW/cm(2)/sr/cm(-1) and the relative error is typically less than 0.2%. (C) 2016 Optical Society of America C1 [Liu, Xu; Zhou, Daniel K.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Yang, Qiguang; Li, Hui; Jin, Zhonghai; Wu, Wan; Kizer, Susan] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. RP Liu, X (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM xu.liu-1@nasa.gov RI Yang, Ping/B-4590-2011 FU National Aeronautics and Space Administration (NASA) FX National Aeronautics and Space Administration (NASA). NR 120 TC 1 Z9 1 U1 3 U2 3 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD OCT 10 PY 2016 VL 55 IS 29 BP 8236 EP 8247 DI 10.1364/AO.55.008236 PG 12 WC Optics SC Optics GA DZ3AQ UT WOS:000385715900015 PM 27828068 ER PT J AU Hell, N Brown, GV Wilms, J Grinberg, V Clementson, J Liedahl, D Porter, FS Kelley, RL Kilbourne, CA Beiersdorfer, P AF Hell, N. Brown, G. V. Wilms, J. Grinberg, V. Clementson, J. Liedahl, D. Porter, F. S. Kelley, R. L. Kilbourne, C. A. Beiersdorfer, P. TI LABORATORY MEASUREMENTS OF THE K-SHELL TRANSITION ENERGIES IN L-SHELL IONS OF SI AND S SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; methods: laboratory: atomic; X-rays: binaries; X-rays: general ID X-RAY SPECTROSCOPY; CHANDRA GRATING SPECTROSCOPY; FLEXIBLE ATOMIC CODE; HIGHLY-CHARGED IONS; ELECTRON-BEAM; VELA X-1; ABSORPTION-LINES; CALORIMETER SPECTROMETER; ISOELECTRONIC SEQUENCE; XRS MICROCALORIMETER AB We have measured the energies of the strongest 1s-2l (l = s, p) transitions in He-through Ne-like silicon and sulfur ions to an accuracy of < 1 eV using the Lawrence Livermore National Laboratory's electron beam ion traps, EBIT-I and SuperEBIT, and the NASA/GSFC EBIT Calorimeter Spectrometer (ECS). We identify and measure the energies of 18 and 21 X-ray features from silicon and sulfur, respectively. The results are compared to new Flexible Atomic Code calculations and to semi-relativistic Hartree-Fock calculations by Palmeri et al. (2008). These results will be especially useful for wind diagnostics in high-mass X-ray binaries, such as Vela X-1 and Cygnus X-1, where high-resolution spectral measurements using Chandra's high-energy transmission grating has made it possible to measure Doppler shifts of 100 km s(-1). The accuracy of our measurements is consistent with that needed to analyze Chandra observations, exceeding Chandra's 100 km s(-1) limit. Hence, the results presented here not only provide benchmarks for theory, but also accurate rest energies that can be used to determine the bulk motion of material in astrophysical sources. We show the usefulness of our results by applying them to redetermine Doppler shifts from Chandra observations of Vela X-1. C1 [Hell, N.; Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, Sternwartstr 7, D-96049 Bamberg, Germany. [Hell, N.; Brown, G. V.; Clementson, J.; Liedahl, D.; Beiersdorfer, P.] Lawrence Livermore Natl Lab, 7000 East Ave, Livermore, CA 94550 USA. [Grinberg, V.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Porter, F. S.; Kelley, R. L.; Kilbourne, C. A.] NASA GSFC, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. RP Hell, N (reprint author), Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, Sternwartstr 7, D-96049 Bamberg, Germany.; Hell, N (reprint author), Lawrence Livermore Natl Lab, 7000 East Ave, Livermore, CA 94550 USA. EM natalie.hell@sternwarte.uni-erlangen.de RI Wilms, Joern/C-8116-2013; Porter, Frederick/D-3501-2012 OI Wilms, Joern/0000-0003-2065-5410; Porter, Frederick/0000-0002-6374-1119 FU US DOE [DE-AC52-07NA27344]; NASA [NNX/2AH84G, NAS8-03060]; Bundesministerium fur Wirtschaft und Technologie [DLR 50 OR 1113]; European Space Agency [4000114313/15/NL/CB]; NASA through the Smithsonian Astrophysical Observatory (SAO) [SV3-73016] FX This work was performed by LLNL under the auspices of the US DOE under Contract DE-AC52-07NA27344. It was supported by NASA work orders NNX/2AH84G; by the Bundesministerium fur Wirtschaft und Technologie under grant number DLR 50 OR 1113; by the European Space Agency under contract No. 4000114313/15/NL/CB; and by NASA through the Smithsonian Astrophysical Observatory (SAO) contract SV3-73016 to MIT for support of the Chandra X-ray Center (CXC) and Science Instruments. CXC is operated by SAO for and on the behalf of NASA under contract NAS8-03060. This research has made use of ISIS functions provided by ECAP/Remeis observatory and MIT (http://www.sternwarte.uni-erlangen.de/isis/). We thank John E. Davis for providing the s1xfig module used for creating the presented plots. CHIANTI is a collaborative project involving George Mason University, the University of Michigan (USA) and the University of Cambridge (UK). NR 81 TC 0 Z9 0 U1 4 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 OCT 10 PY 2016 VL 830 IS 1 AR 26 DI 10.3847/0004-637X/830/1/26 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ1XA UT WOS:000385633900009 ER PT J AU Kane, SR Hill, ML Kasting, JF Kopparapu, RK Quintana, EV Barclay, T Batalha, NM Borucki, WJ Ciardi, DR Haghighipour, N Hinkel, NR Kaltenegger, L Selsis, F Torres, G AF Kane, Stephen R. Hill, Michelle L. Kasting, James F. Kopparapu, Ravi Kumar Quintana, Elisa V. Barclay, Thomas Batalha, Natalie M. Borucki, William J. Ciardi, David R. Haghighipour, Nader Hinkel, Natalie R. Kaltenegger, Lisa Selsis, Franck Torres, Guillermo TI A CATALOG OF KEPLER HABITABLE ZONE EXOPLANET CANDIDATES SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; astronomical databases: miscellaneous; planetary systems; techniques: photometric ID MAIN-SEQUENCE STARS; FALSE-POSITIVE PROBABILITIES; CARBON-DIOXIDE CLOUDS; EARTH-LIKE PLANETS; INNER EDGE; STELLAR MULTIPLICITY; TERRESTRIAL PLANETS; EXTRASOLAR PLANETS; SYSTEMS. I.; MASS STARS AB The NASA Kepler mission has discovered thousands of new planetary candidates, many of which have been confirmed through follow-up observations. A primary goal of the mission is to determine the occurrence rate of terrestrial-size planets within the Habitable Zone (HZ) of their host stars. Here we provide a list of HZ exoplanet candidates from the Kepler Q1-Q17 Data Release 24 data-vetting process. This work was undertaken as part of the Kepler HZ Working Group. We use a variety of criteria regarding HZ boundaries and planetary sizes to produce complete lists of HZ candidates, including a catalog of 104 candidates within the optimistic HZ and 20 candidates with radii less than two Earth radii within the conservative HZ. We cross-match our HZ candidates with the stellar properties and confirmed planet properties from Data Release 25 to provide robust stellar parameters and candidate dispositions. We also include false-positive probabilities recently calculated by Morton et al. for each of the candidates within our catalogs to aid in their validation. Finally, we performed dynamical analysis simulations for multi-planet systems that contain candidates with radii less than two Earth radii as a step toward validation of those systems. C1 [Kane, Stephen R.; Hill, Michelle L.; Hinkel, Natalie R.] San Francisco State Univ, Dept Phys & Astron, 1600 Holloway Ave, San Francisco, CA 94132 USA. [Kasting, James F.] Penn State Univ, Dept Geosci, 443 Deike Bldg, University Pk, PA 16802 USA. [Kopparapu, Ravi Kumar] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Mail Stop 699-0 Bldg 34, Greenbelt, MD 20771 USA. [Quintana, Elisa V.; Barclay, Thomas; Batalha, Natalie M.; Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ciardi, David R.] NASA, Exoplanet Sci Inst, CALTECH, MS 100-22,770 South Wilson Ave, Pasadena, CA 91125 USA. [Haghighipour, Nader] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Hinkel, Natalie R.] Arizona State Univ, Sch Earth Space Explorat, Tempe, AZ 85287 USA. [Kaltenegger, Lisa] Cornell Univ, Carl Sagan Inst, Ithaca, NY 14853 USA. [Selsis, Franck] Univ Bordeaux, Lab Astrophys Bordeaux, CNRS, B18N, Allee Geoffroy St Hilaire, F-33615 Pessac, France. [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Kane, SR (reprint author), San Francisco State Univ, Dept Phys & Astron, 1600 Holloway Ave, San Francisco, CA 94132 USA. EM skane@sfsu.edu OI Ciardi, David/0000-0002-5741-3047; Kasting, James/0000-0003-4042-2067 FU NASA ADAP grant [NNX13AF20G]; NASA Astrobiology Institute; NASA [NNH05ZDA001C]; NASA Habitable Worlds grant [NNH14ZDA001N-HW]; agency's Science Mission Directorate FX The authors would like to thank the anonymous referee, whose comments greatly improved the quality of the paper. The authors also thank Douglas Caldwell and Timothy Morton for enlightening discussions regarding Kepler candidate validation. Nader Haghighipour acknowledges support from NASA ADAP grant NNX13AF20G. James Kasting and Ravi Kopparapu gratefully acknowledge funding from the NASA Astrobiology Institute's lead team, supported by NASA under cooperative agreement NNH05ZDA001C. Ravi Kopparapu also acknowledges support from NASA Habitable Worlds grant NNH14ZDA001N-HW. Kepler is NASA's 10th Discovery Mission and was funded by the agency's Science Mission Directorate. This research has made use of the NASA Exoplanet Archive and the ExoFOP site, which are operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This work has also made use of the Habitable Zone Gallery at hzgallery.org. The results reported herein benefited from collaborations and/or information exchange within NASA's Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA's Science Mission Directorate. NR 88 TC 1 Z9 1 U1 15 U2 15 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 OCT 10 PY 2016 VL 830 IS 1 AR 1 DI 10.3847/0004-637X/830/1/1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ2EP UT WOS:000385655400001 ER PT J AU Mason, JP Woods, TN Webb, DF Thompson, BJ Colaninno, RC Vourlidas, A AF Mason, James Paul Woods, Thomas N. Webb, David F. Thompson, Barbara J. Colaninno, Robin C. Vourlidas, Angelos TI RELATIONSHIP OF EUV IRRADIANCE CORONAL DIMMING SLOPE AND DEPTH TO CORONAL MASS EJECTION SPEED AND MASS SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; Sun: activity; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: UV radiation ID SOLAR-FLARE; CMES; STEREO/EUVI; ENERGETICS AB Extreme ultraviolet (EUV) coronal dimmings are often observed in response to solar eruptive events. These phenomena can be generated via several different physical processes. For space weather, the most important of these is the temporary void left behind by a coronal mass ejection (CME). Massive, fast CMEs tend to leave behind a darker void that also usually corresponds to minimum irradiance for the cooler coronal emissions. If the dimming is associated with a solar flare, as is often the case, the flare component of the irradiance light curve in the cooler coronal emission can be isolated and removed using simultaneous measurements of warmer coronal lines. We apply this technique to 37 dimming events identified during two separate two-week periods in 2011. plus an event on 2010 August 7, analyzed in a previous paper. to parameterize dimming in terms of depth and slope. We provide statistics on which combination of wavelengths worked best for the flare-removal method, describe the fitting methods applied to the dimming light curves, and compare the dimming parameters with corresponding CME parameters of mass and speed. The best linear relationships found are nu(CME) [km/s] approximate to 2.36 x 10(6) [km/%] x s(dim) [%/s] m(CME) [g] approximate to 2.59 x 10(15) [g/%] x root d(dim) [%]. These relationships could be used for space weather operations of estimating CME mass and speed using near-real-time irradiance dimming measurements. C1 [Mason, James Paul; Woods, Thomas N.] Univ Colorado, Lab Atmospher & Space Phys, 3665 Discovery Dr, Boulder, CO 80303 USA. [Webb, David F.] Boston Coll, Inst Sci Res, Newton, MA 02458 USA. [Thompson, Barbara J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Colaninno, Robin C.] Naval Res Lab, Div Space Sci, Washington, DC 20009 USA. [Vourlidas, Angelos] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20732 USA. RP Mason, JP (reprint author), Univ Colorado, Lab Atmospher & Space Phys, 3665 Discovery Dr, Boulder, CO 80303 USA. EM james.mason@lasp.colorado.edu RI Vourlidas, Angelos/C-8231-2009; OI Vourlidas, Angelos/0000-0002-8164-5948; WOODS, THOMAS/0000-0002-2308-6797; Colaninno, Robin/0000-0002-3253-4205 FU NASA SDO project; NASA [NAS5-02140, S-136361-Y]; Navy grant [N00173-14-1-G014]; CNR funds FX The authors thank Jim Klimchuk for discussions about the physical motivation for mass-loss dimming, and Amir Caspi for identifying the need for a new mathematical derivation to establish the expected relationships between dimming and CME parameters. The CDAW CME catalog is generated and maintained at the CDAW Data Center by NASA and The Catholic University of America in cooperation with the Naval Research Laboratory. SOHO is a project of international cooperation between ESA and NASA. This research is supported by the NASA SDO project and NASA grant NAS5-02140. Author D.F. Webb was supported by Navy grant N00173-14-1-G014. Authors R.C. Colaninno and A. Vourlidas were supported by NASA contract S-136361-Y to the Naval Research Laboratory, and CNR funds. NR 35 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2016 VL 830 IS 1 AR 20 DI 10.3847/0004-637X/830/1/20 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ1XA UT WOS:000385633900003 ER PT J AU Duan, L Choudhari, MM Zhang, C AF Duan, Lian Choudhari, Meelan M. Zhang, Chao TI Pressure fluctuations induced by a hypersonic turbulent boundary layer SO JOURNAL OF FLUID MECHANICS LA English DT Article DE high-speed flow; turbulence simulation; turbulent boundary layers ID DIRECT NUMERICAL-SIMULATION; REYNOLDS-NUMBER; TUNNEL NOISE; CHANNEL FLOW; RADIATION; MOTION; TRANSITION; GENERATION; SCHEMES; FIELD AB Direct numerical simulations (DNS) are used to examine the pressure fluctuations generated by a spatially developed Mach 5.86 turbulent boundary layer. The unsteady pressure field is analysed at multiple wall-normal locations, including those at the wall, within the boundary layer (including inner layer, the log layer, and the outer layer), and in the free stream. The statistical and structural variations of pressure fluctuations as a function of wall-normal distance are highlighted. Computational predictions for mean-velocity profiles and surface pressure spectrum are in good agreement with experimental measurements, providing a first ever comparison of this type at hypersonic Mach numbers. The simulation shows that the dominant frequency of boundary-layer-induced pressure fluctuations shifts to lower frequencies as the location of interest moves away from the wall. The pressure wave propagates with a speed nearly equal to the local mean velocity within the boundary layer (except in the immediate vicinity of the wall) while the propagation speed deviates from Taylor's hypothesis in the free stream. Compared with the surface pressure fluctuations, which are primarily vortical, the acoustic pressure fluctuations in the free stream exhibit a significantly lower dominant frequency, a greater spatial extent, and a smaller bulk propagation speed. The free-stream pressure structures are found to have similar Lagrangian time and spatial scales as the acoustic sources near the wall. As the Mach number increases, the free-stream acoustic fluctuations exhibit increased radiation intensity, enhanced energy content at high frequencies, shallower orientation of wave fronts with respect to the flow direction, and larger propagation velocity. C1 [Duan, Lian; Zhang, Chao] Missouri Univ Sci & Technol, Rolla, MO 65409 USA. [Choudhari, Meelan M.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Duan, L (reprint author), Missouri Univ Sci & Technol, Rolla, MO 65409 USA. EM duanl@mst.edu RI Choudhari, Meelan/F-6080-2017 OI Choudhari, Meelan/0000-0001-9120-7362 FU Air Force Office of Scientific Research [FA9550-14-1-0170]; NASA Langley Research Center through the National Institute of Aerospace [NNLO9AA00A] FX This material is based on the work supported by the Air Force Office of Scientific Research with Award no. FA9550-14-1-0170, managed by Dr I. Leyva. The work was initiated under the support of NASA Langley Research Center under the Research Cooperative Agreement no. NNLO9AA00A (through the National Institute of Aerospace). The authors would like to thank Professor S. Schneider of Purdue University and Dr K. Casper of Sandia National Laboratory for providing their wind-tunnel measurements for comparison with DNS. Computational resources are provided by the NASA Advanced Supercomputing Division and the DoD High Performance Computing Modernization Program. NR 68 TC 0 Z9 0 U1 8 U2 8 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-1120 EI 1469-7645 J9 J FLUID MECH JI J. Fluid Mech. PD OCT 10 PY 2016 VL 804 BP 578 EP 607 DI 10.1017/jfm.2016.548 PG 30 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA DX0WU UT WOS:000384087900031 ER PT J AU Fortenberry, RC Lee, TJ Francisco, JS AF Fortenberry, Ryan C. Lee, Timothy J. Francisco, Joseph S. TI Quantum Chemical Analysis of the CO-HNN+ Proton-Bound Complex SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID QUARTIC FORCE-FIELDS; VIBRATIONAL FREQUENCIES; SPECTROSCOPIC CONSTANTS; PROTOPLANETARY DISKS; CATION; HCO+; N2H+; ISOTOPOLOGUES; ACETYLENE AB Proton-bound complexes produce exceptionally bright vibrational modes for stretches involving the hydrogen atom. Binding a proton between various arrangements of N-2 and carbon monoxide molecules is known to produce such behavior, and there are four distinct structures involving N-2, CO, and a proton. The problem arises in that all four have the same mass and are, consequently, extremely difficult, if not impossible, to resolve experimentally. Fortunately, quantum chemical predictions have produced accurate descriptions of this bright mode and other spectral features for OCHCO+, NNHNN+, and NN-HCO+. The last of this family to be analyzed is CO-HNN+, which is done here. Utilizing high-level coupled cluster computations and quartic force fields, the bright vibrational mode of CO-HNN+ is shown to shift to the red, and the C-O bond is destabilized in this arrangement as opposed to the lower-energy NN-HCO+ isomer studied previously. Furthermore, the 1.87 D center-of-mass dipole moment, spectroscopic constants, and other anharmonic fundamental frequencies and intensities are produced for CO-HNN+ to assist in definitive experimental and even astrochemical classification of this and the other three related mass-57 proton-bound complexes. C1 [Fortenberry, Ryan C.] Georgia Southern Univ, Dept Chem & Biochem, Statesboro, GA 30460 USA. [Lee, Timothy J.] NASA, Ames Res Ctr, MS 245-1, Moffett Field, CA 94035 USA. [Francisco, Joseph S.] Univ Nebraska, Dept Chem, Lincoln, NE 68588 USA. RP Fortenberry, RC (reprint author), Georgia Southern Univ, Dept Chem & Biochem, Statesboro, GA 30460 USA. EM rfortenberry@georgiasouthem.edu RI Lee, Timothy/K-2838-2012 FU Georgia Southern University; National Aeronautics and Space Administration through NASA Astrobiology Institute under Science Mission Directorate [NNH13ZDA017C] FX R.C.F. acknowledges the start-up funds provided by Georgia Southern University that were utilized in this work. This work is also supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement Notice NNH13ZDA017C issued through the Science Mission Directorate. NR 50 TC 2 Z9 2 U1 3 U2 3 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD OCT 6 PY 2016 VL 120 IS 39 BP 7745 EP 7752 DI 10.1021/acs.jpca.6b07515 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA DY2YZ UT WOS:000384959300018 PM 27643412 ER PT J AU Sainio, S Nordlund, D Gandhiraman, R Jiang, H Koehne, J Koskinen, J Meyyappan, M Laurila, T AF Sainio, S. Nordlund, D. Gandhiraman, R. Jiang, H. Koehne, J. Koskinen, J. Meyyappan, M. Laurila, T. TI What Does Nitric Acid Really Do to Carbon Nanofibers? SO JOURNAL OF PHYSICAL CHEMISTRY C LA English DT Article ID ABSORPTION FINE-STRUCTURE; DIAMOND SURFACES; NANOTUBE GROWTH; GRAPHENE OXIDE; OXIDATION; FUNCTIONALIZATION; SPECTROSCOPY; ELECTRODES; EXCITATION; DOPAMINE AB Understanding the chemical nature of the surface of carbon nanofibers (CNF) is critical in assessing their fundamental properties and tailoring them for the right application. To gain such knowledge, we present here a detailed X-ray adsorption spectroscopy (XAS) study accompanied by high resolution transmission electron microscopy (TEM) micrographs of two morphologically different CNF pairs (tetrahedral amorphous carbon (ta-C) grown "open structured" fibers and traditional bamboo-like "closed structured" fibers), where the surface chemical properties and structural features of the fibers are investigated in depth and the effects of nitric acid treatment on the fibers are revealed. The morphology of the fiber and/or the original seed- and adhesion layers markedly affect the response of the fibers to the acid treatment. Results also show that the nitric acid treatment increases the observed se intensity and modifies the two types of fibers to become more-alike both structurally and with respect to their oxygen functionalities. The XAS and HRTEM results confirm that a short nitric acid treatment does not remove the Ni catalyst particle but, instead, oxidizes their surfaces, especially in the case of ta-C grown fibers. C1 [Sainio, S.; Laurila, T.] Aalto Univ, Sch Elect Engn, Dept Elect Engn & Automat, Espoo 02150, Finland. [Nordlund, D.] SLAC Natl Accelerator Lab, Stanford Synchrotron Radiat Lightsource, Menlo Pk, CA 94025 USA. [Gandhiraman, R.; Koehne, J.; Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. [Jiang, H.] Aalto Univ, Sch Sci, Dept Appl Phys, Espoo 02150, Finland. [Koskinen, J.] Aalto Univ, Sch Chem Technol, Dept Mat Sci, Espoo 02150, Finland. RP Laurila, T (reprint author), Aalto Univ, Sch Elect Engn, Dept Elect Engn & Automat, Espoo 02150, Finland. EM tomi.laurila@aalto.fi RI Koskinen, Jari/J-3886-2014; Laurila, Tomi/B-2076-2013 FU Academy of Finland [285015, 285526] FX The authors T.L. and S.S. acknowledge funding from Academy of Finland (Grant Numbers 285015 and 285526). NR 39 TC 1 Z9 1 U1 8 U2 8 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1932-7447 J9 J PHYS CHEM C JI J. Phys. Chem. C PD OCT 6 PY 2016 VL 120 IS 39 BP 22655 EP 22662 DI 10.1021/acs.jpcc.6b06353 PG 8 WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Chemistry; Science & Technology - Other Topics; Materials Science GA DY2YX UT WOS:000384959100060 ER PT J AU Marrero, JE Townsend-Small, A Lyon, DR Tsai, TR Meinardi, S Blake, DR AF Marrero, Josette E. Townsend-Small, Amy Lyon, David R. Tsai, Tracy R. Meinardi, Simone Blake, Donald R. TI Estimating Emissions of Toxic Hydrocarbons from Natural Gas Production Sites in the Barnett Shale Region of Northern Texas SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID VOLATILE ORGANIC-COMPOUNDS; INTERCOMPARISON EXPERIMENT NOMHICE; METHANE EMISSIONS; UNITED-STATES; HUMAN HEALTH; AIR; OPERATIONS; OIL; COLORADO; BENZENE AB Oil and natural gas operations have continued to expand and move closer to densely populated areas, contributing to growing public concerns regarding exposure to hazardous air pollutants. During the Barnett Shale Coordinated Campaign in October, 2013, ground-based whole air samples collected downwind of oil and gas sites revealed enhancements in several potentially toxic volatile organic compounds (VOCs) when compared to background values. Molar emissions ratios relative to methane were determined for hexane, benzene, toluene, ethylbenzene, and xylene (BTEX compounds). Using methane leak rates measured from the Picarro mobile flux plane (MFP) system and a Barnett Shale regional methane emissions inventory, the rates of emission of these toxic gases were calculated. Benzene emissions ranged between 51 +/- 4 and 60 +/- 4 kg h(-1). Hexane, the most abundantly emitted pollutant, ranged from 642 +/- 45 to 1070 +/- 340 kg h(-1). While observed hydrocarbon enhancements fall below federal workplace standards, results may indicate a link between emissions from oil and natural gas operations and concerns about exposure to hazardous air pollutants. The larger public health risks associated with the production and distribution of natural gas are of particular importance and warrant further investigation, particularly as the use of natural gas increases in the United States and internationally. C1 [Marrero, Josette E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Townsend-Small, Amy] Univ Cincinnati, Dept Geol, Cincinnati, OH 45221 USA. [Townsend-Small, Amy] Univ Cincinnati, Dept Geog, Cincinnati, OH 45221 USA. [Lyon, David R.] Environm Def Fund, Austin, TX 78701 USA. [Tsai, Tracy R.] Picarro Inc, Santa Clara, CA 95054 USA. [Meinardi, Simone; Blake, Donald R.] Univ Calif Irvine, Dept Chem, Irvine, CA 92697 USA. RP Marrero, JE (reprint author), NASA, Ames Res Ctr, Atmospher Sci Branch, Mail Stop 245-5, Moffett Field, CA 94035 USA. EM josette.e.marrero@nasa.gov FU Environmental Defense Fund FX The authors would like to thank the following people for assistance with field work: Ramon Alvarez and Bob Harriss, Environmental Defense Fund; April Covington and Nigel Clark, University of West Virginia; Brian Lamb, Washington State University; Tom Ferrara and Touche Howard, GHD, Inc.; Rob Jackson and Morgan Gallagher, Duke University; Bob Talbot, University of Houston; Chris Rella, Connor Botkin, and David Steele, Picarro Inc.; and Brent Love and Gloria Liu, University of California, Irvine. Data collection was partially funded by Environmental Defense Fund. NR 54 TC 1 Z9 1 U1 17 U2 17 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X EI 1520-5851 J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD OCT 4 PY 2016 VL 50 IS 19 BP 10756 EP 10764 DI 10.1021/acs.est.6b02827 PG 9 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA DY1GC UT WOS:000384841900052 PM 27580823 ER PT J AU Sennett, N Marsat, S Buonanno, A AF Sennett, Noah Marsat, Sylvain Buonanno, Alessandra TI Gravitational waveforms in scalar-tensor gravity at 2PN relative order SO PHYSICAL REVIEW D LA English DT Article ID INSPIRALLING COMPACT BINARIES; POST-NEWTONIAN ORDER; GENERAL-RELATIVITY; BRANS-DICKE; RADIATION; SYSTEMS; PULSAR; ENERGY; FIELD AB We compute the gravitational waveform from a binary system in scalar-tensor gravity at 2PN relative order. We restrict our calculation to nonspinning binary systems on quasicircular orbits and compute the spin-weighted spherical modes of the radiation. The evolution of the phase of the waveform is computed in the time and frequency domains. The emission of dipolar radiation is the lowest-order dissipative process in scalar-tensor gravity. However, stringent constraints set by current astrophysical observations indicate that this effect is subdominant to quadrupolar radiation for most prospective gravitational-wave sources. We compute the waveform for systems whose inspiral is driven by: (a) dipolar radiation (e.g., binary pulsars or spontaneously scalarized systems) and (b) quadrupolar radiation (e.g., typical sources for space-based and ground-based detectors). For case (a), we provide complete results at 2PN, whereas for case (b), we must introduce unknown terms in the 2PN flux; these unknown terms are suppressed by constraints on scalar-tensor gravity. C1 [Sennett, Noah; Marsat, Sylvain; Buonanno, Alessandra] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Sennett, Noah; Marsat, Sylvain; Buonanno, Alessandra] Albert Einstein Inst, Max Planck Inst Gravitat Phys, Muhlenberg 1, D-14476 Potsdam, Germany. [Marsat, Sylvain] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA. RP Sennett, N (reprint author), Univ Maryland, Dept Phys, College Pk, MD 20742 USA.; Sennett, N (reprint author), Albert Einstein Inst, Max Planck Inst Gravitat Phys, Muhlenberg 1, D-14476 Potsdam, Germany. EM nsennett@umd.edu FU NSF [PHY-1208881]; NASA [11-ATP-046]; NASA at the University of Maryland, College Park [NNX12AN10G] FX We are grateful to Ryan Lang for providing a Mathematica notebook containing the results of Ref. [21] and to Lijing Shao for useful discussions concerning current binary pulsar constraints. N. S. acknowledges support from NSF Grant No. PHY-1208881. S. M. acknowledges support from NASA Grant No. 11-ATP-046 and NASA Grant No. NNX12AN10G at the University of Maryland, College Park. N. S. thanks the Max Planck Institute for Gravitational Physics for its hospitality during the completion of this work. NR 62 TC 0 Z9 0 U1 2 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 OCT 4 PY 2016 VL 94 IS 8 AR 084003 DI 10.1103/PhysRevD.94.084003 PG 24 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA DX8AD UT WOS:000384609600010 ER PT J AU Briscoe, DK Parker, DM Bograd, S Hazen, E Scales, K Balazs, GH Kurita, M Saito, T Okamoto, H Rice, M Polovina, JJ Crowder, LB AF Briscoe, D. K. Parker, D. M. Bograd, S. Hazen, E. Scales, K. Balazs, G. H. Kurita, M. Saito, T. Okamoto, H. Rice, M. Polovina, J. J. Crowder, L. B. TI Multi-year tracking reveals extensive pelagic phase of juvenile loggerhead sea turtles in the North Pacific SO MOVEMENT ECOLOGY LA English DT Article DE Loggerhead sea turtle; Migration; Foraging; Movement; Distribution; Pelagic ID REGIONAL MAGNETIC-FIELDS; LONG-DISTANCE MIGRATION; CARETTA-CARETTA; LEATHERBACK TURTLES; OCEAN; BEHAVIOR; HABITAT; ORIENTATION; DISPERSAL; MOVEMENT AB Background: The juvenile stage of loggerhead sea turtles (Caretta caretta) can last for decades. In the North Pacific Ocean, much is known about their seasonal movements in relation to pelagic habitat, yet understanding their multi-year, basin-scale movements has proven more difficult. Here, we categorize the large-scale movements of 231 turtles satellite tracked from 1997 to 2013 and explore the influence of biological and environmental drivers on basin-scale movement. Results: Results show high residency of juvenile loggerheads within the Central North Pacific and a moderate influence of the Earth's magnetic field, but no real-time environmental driver to explain migratory behavior. Conclusions: We suggest the Central North Pacific acts as important developmental foraging grounds for young juvenile loggerhead sea turtles, rather than just a migratory corridor. We propose several hypotheses that may influence the connectivity between western and eastern juvenile loggerhead foraging grounds in the North Pacific Ocean. C1 [Briscoe, D. K.] Stanford Univ, Hopkins Marine Stn, Pacific Grove, CA 93950 USA. [Parker, D. M.] NOAA, Joint Inst Marine & Atmospher Res, Newport, OR USA. [Bograd, S.; Hazen, E.; Scales, K.] NOAA, Environm Res Div, Natl Marine Fisheries Serv, Southwest Fisheries Sci Ctr, Monterey, CA USA. [Balazs, G. H.; Polovina, J. J.] NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI USA. [Kurita, M.; Okamoto, H.] Port Nagoya Publ Aquarium, Minato Ku, Nagoya, Aichi 4550033, Japan. [Saito, T.] Kochi Univ, Usa Marine Biol Inst, Usa Tosa, Kochi 7811164, Japan. [Rice, M.] Hawaii Preparatory Acad, 65-1692 Kohala Mt Rd, Kamuela, HI 96743 USA. [Crowder, L. B.] Stanford Univ, Ctr Ocean Solut, Monterey, CA USA. RP Briscoe, DK (reprint author), Stanford Univ, Hopkins Marine Stn, Pacific Grove, CA 93950 USA. EM dbriscoe@stanford.edu OI Scales, Kylie/0000-0003-0843-0956 FU Crowder Lab at Hopkins Marine Station, Stanford University FX Funding for DKB was provided by the Crowder Lab at Hopkins Marine Station, Stanford University. NR 63 TC 0 Z9 0 U1 1 U2 1 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 2051-3933 J9 MOV ECOL JI Mov. Ecol. PD OCT 3 PY 2016 VL 4 AR 23 DI 10.1186/s40462-016-0087-4 PG 12 WC Ecology SC Environmental Sciences & Ecology GA EM4VG UT WOS:000395310400001 PM 27729983 ER PT J AU Flanigan, D Johnson, BR Abitbol, MH Bryan, S Cantor, R Day, P Jones, G Mauskopf, P McCarrick, H Miller, A Zmuidzinas, J AF Flanigan, D. Johnson, B. R. Abitbol, M. H. Bryan, S. Cantor, R. Day, P. Jones, G. Mauskopf, P. McCarrick, H. Miller, A. Zmuidzinas, J. TI Magnetic field dependence of the internal quality factor and noise performance of lumped-element kinetic inductance detectors SO APPLIED PHYSICS LETTERS LA English DT Article ID FILMS; SN AB We present a technique for increasing the internal quality factor of kinetic inductance detectors (KIDs) by nulling ambient magnetic fields with a properly applied magnetic field. The KIDs used in this study are made from thin-film aluminum, they are mounted inside a light-tight package made from bulk aluminum, and they are operated near 150 mK. Since the thin-film aluminum has a slightly elevated critical temperature (T-c = 1.4 K), it therefore transitions before the package (T-c = 1.2 K), which also serves as a magnetic shield. On cooldown, ambient magnetic fields as small as approximately 30 mu T can produce vortices in the thin-film aluminum as it transitions because the bulk aluminum package has not yet transitioned and therefore is not yet shielding. These vortices become trapped inside the aluminum package below 1.2K and ultimately produce low internal quality factors in the thin-film superconducting resonators. We show that by controlling the strength of the magnetic field present when the thin film transitions, we can control the internal quality factor of the resonators. We also compare the noise performance with and without vortices present, and find no evidence for excess noise beyond the increase in amplifier noise, which is expected with increasing loss. (C) 2016 Author(s). C1 [Flanigan, D.; Johnson, B. R.; Abitbol, M. H.; Jones, G.; McCarrick, H.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Bryan, S.; Mauskopf, P.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Cantor, R.] STAR Cryoelect, Santa Fe, NM 87508 USA. [Day, P.; Zmuidzinas, J.] Jet Prop Lab, Pasadena, CA 91109 USA. [Mauskopf, P.] Arizona State Univ, Dept Phys, Tempe, AZ 85287 USA. [Mauskopf, P.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Miller, A.] Univ Southern Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA. [Zmuidzinas, J.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Flanigan, D (reprint author), Columbia Univ, Dept Phys, New York, NY 10027 USA. EM daniel.flanigan@columbia.edu FU NASA; Research Initiatives for Science and Engineering program at Columbia University FX R.C. was both an author and the owner of STAR Cryoelectronics, where the devices used in this study were fabricated. H.M. was supported by a NASA Earth and Space Sciences Fellowship. This research was supported, in part, by a grant from the Research Initiatives for Science and Engineering program at Columbia University to B.R.J. We thank the Xilinx University Program for their donation of FPGA hardware and software tools used in the readout system. NR 20 TC 0 Z9 0 U1 6 U2 6 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD OCT 3 PY 2016 VL 109 IS 14 AR 143503 DI 10.1063/1.4964119 PG 4 WC Physics, Applied SC Physics GA DZ8WJ UT WOS:000386152800061 ER PT J AU Dolci, M Romero-Wolf, A Wissel, S AF Dolci, Marco Romero-Wolf, Andrew Wissel, Stephanie TI A lower bound on the number of cosmic ray events required to measure source catalogue correlations SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE ultra high energy cosmic rays; cosmic ray experiments; active galactic nuclei ID GALACTIC MAGNETIC-FIELD; TELESCOPE ARRAY EXPERIMENT; EXTRAGALACTIC OBJECTS; ARRIVAL DIRECTIONS; ROTATION MEASURES; NUCLEI; PHOTODISINTEGRATION; ANISOTROPY; EVOLUTION; SPECTRUM AB Recent analyses of cosmic ray arrival directions have resulted in evidence for a positive correlation with active galactic nuclei positions that has weak significance against an isotropic source distribution. In this paper, we explore the sample size needed to measure a highly statistically significant correlation to a parent source catalogue. We compare several scenarios for the directional scattering of ultra-high energy cosmic rays given our current knowledge of the galactic and intergalactic magnetic fields. We find significant correlations are possible for a sample of >1000 cosmic ray protons with energies above 60 EeV. C1 [Dolci, Marco; Romero-Wolf, Andrew] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Dolci, Marco] Politecn Torino, Dept Mech & Aerosp Engn, Corso Duca Abruzzi 24, I-10129 Turin, Italy. [Wissel, Stephanie] Univ Calif Los Angeles, Dept Phys & Astron, 475 Portola Plaza, Los Angeles, CA 90095 USA. [Wissel, Stephanie] Calif Polytech State Univ San Luis Obispo, Dept Phys, 1 Grand Ave, San Luis Obispo, CA 93407 USA. RP Dolci, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.; Dolci, M (reprint author), Politecn Torino, Dept Mech & Aerosp Engn, Corso Duca Abruzzi 24, I-10129 Turin, Italy. EM marco.dolci@polito.it; Andrew.Romero-Wolf@jpl.nasa.gov; swissel@calpoly.edu NR 55 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD OCT PY 2016 IS 10 AR 028 DI 10.1088/1475-7516/2016/10/028 PG 23 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA EL4FZ UT WOS:000394578400012 ER PT J AU Ade, PAR Aghanim, N Akrami, Y Aluri, PK Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartolo, N Basak, S Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bock, JJ Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Boulanger, F Bucher, M Burigana, C Butler, RC Calabrese, E Cardoso, JF Casaponsa, B Catalano, A Challinor, A Chamballu, A Chiang, HC Christensen, PR Church, S Clements, DL Colombi, S Colombo, LPL Combet, C Contreras, D Couchot, F Coulais, A Crill, BP Cruz, M Curto, A Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Desert, FX Diego, JM Dole, H Donzelli, S Dore, O Douspis, M Ducout, A Dupac, X Efstathiou, G Elsner, F Ensslin, TA Eriksen, HK Fantaye, Y Ferguson, J Fernandez-Cobos, R Finelli, F Forni, O Frailis, M Fraisse, AA Franceschi, E Frejsel, A Frolov, A Galeotta, S Galli, S Ganga, K Gauthier, C Ghosh, T Giard, M Giraud-Heraud, Y Gjerlow, E Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Gudmundsson, JE Hansen, FK Hanson, D Harrison, DL Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huang, Z Huffenberger, KM Hurier, G Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihanen, E Keskitalo, R Kim, J Kisner, TS Knoche, J Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Lattanzi, M Lawrence, CR Leonardi, R Lesgourgues, J Levrier, F Liguori, M Lilje, PB Linden-Vornle, M Liu, H Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maggio, G Maino, D Mandolesi, N Mangilli, A Marinucci, D Maris, M Martin, PG Martinez-Gonzalez, E Masi, S Matarrese, S McGehee, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mikkelsen, K Mitra, S Miville-Deschenes, MA Molinari, D Moneti, A Montier, L Morgante, G Mortlock, D Moss, A Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Oxborrow, CA Paci, F Pagano, L Pajot, F Pant, N Paoletti, D Pasian, F Patanchon, G Pearson, TJ Perdereau, O Perotto, L Perrotta, F Pettorino, V Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Popa, L Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Rebolo, R Reinecke, M Remazeilles, M Renault, C Renzi, A Ristorcelli, I Rocha, G Rosset, C Rossetti, M Rotti, A Roudier, G Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savelainen, M Savini, G Scott, D Seiffert, MD Shellard, EPS Souradeep, T Spencer, LD Stolyarov, V Stompor, R Sudiwala, R Sunyaev, R Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Tristram, M Trombetti, T Tucci, M Tuovinen, J Valenziano, L Valiviita, J Van Tent, B Vielva, P Villa, F Wade, LA Wandelt, BD Wehus, IK Yvon, D Zacchei, A Zibin, JP Zonca, A AF Ade, P. A. R. Aghanim, N. Akrami, Y. Aluri, P. K. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartolo, N. Basak, S. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P Bersanelli, M. Bielewicz, P. Bock, J. J. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bucher, M. Burigana, C. Butler, R. C. Calabrese, E. Cardoso, J. -F. Casaponsa, B. Catalano, A. Challinor, A. Chamballu, A. Chiang, H. C. Christensen, P. R. Church, S. Clements, D. L. Colombi, S. Colombo, L. P. L. Combet, C. Contreras, D. Couchot, F. Coulais, A. Crill, B. P. Cruz, M. Curto, A. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Desert, F. -X. Diego, J. M. Dole, H. Donzelli, S. Dore, O. Douspis, M. Ducout, A. Dupac, X. Efstathiou, G. Elsner, F. Ensslin, T. A. Eriksen, H. K. Fantaye, Y. Ferguson, J. Fernandez-Cobos, R. Finelli, F. Forni, O. Frailis, M. Fraisse, A. A. Franceschi, E. Frejsel, A. Frolov, A. Galeotta, S. Galli, S. Ganga, K. Gauthier, C. Ghosh, T. Giard, M. Giraud-Heraud, Y. Gjerlow, E. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Gudmundsson, J. E. Hansen, F. K. Hanson, D. Harrison, D. L. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huang, Z. Huffenberger, K. M. Hurier, G. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kim, J. Kisner, T. S. Knoche, J. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Lattanzi, M. Lawrence, C. R. Leonardi, R. Lesgourgues, J. Levrier, F. Liguori, M. Lilje, P. B. Linden-Vornle, M. Liu, H. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maggio, G. Maino, D. Mandolesi, N. Mangilli, A. Marinucci, D. Maris, M. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Matarrese, S. McGehee, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mikkelsen, K. Mitra, S. Miville-Deschenes, M. -A. Molinari, D. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Moss, A. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Pant, N. Paoletti, D. Pasian, F. Patanchon, G. Pearson, T. J. Perdereau, O. Perotto, L. Perrotta, F. Pettorino, V. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Popa, L. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Renzi, A. Ristorcelli, I. Rocha, G. Rosset, C. Rossetti, M. Rotti, A. Roudier, G. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savelainen, M. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Souradeep, T. Spencer, L. D. Stolyarov, V. Stompor, R. Sudiwala, R. Sunyaev, R. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Trombetti, T. Tucci, M. Tuovinen, J. Valenziano, L. Valiviita, J. Van Tent, B. Vielva, P. Villa, F. Wade, L. A. Wandelt, B. D. Wehus, I. K. Yvon, D. Zacchei, A. Zibin, J. P. Zonca, A. CA Planck Collaboration TI Planck 2015 results XVI. Isotropy and statistics of the CMB SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology: observations; cosmic background radiation; polarization; methods: data analysis; methods: statistical ID MICROWAVE-ANISOTROPY-PROBE; OBSERVATIONS COSMOLOGICAL INTERPRETATION; PRIMORDIAL NON-GAUSSIANITY; 5-YEAR WMAP DATA; COLD SPOT; BACKGROUND ANISOTROPY; SKY MAPS; MINKOWSKI FUNCTIONALS; SPHERICAL WAVELETS; POWER ASYMMETRY AB We test the statistical isotropy and Gaussianity of the cosmic microwave background (CMB) anisotropies using observations made by the Planck satellite. Our results are based mainly on the full Planck mission for temperature, but also include some polarization measurements. In particular, we consider the CMB anisotropy maps derived from the multi-frequency Planck data by several component-separation methods. For the temperature anisotropies, we find excellent agreement between results based on these sky maps over both a wry large fraction of the sky and a broad range of angular scales, establishing that potential foreground residuals do not affect our studies. Tests of skewness, kurtosis, multi-normality, N-point functions, and Minkowski functionals indicate consistency with Gaussianity, while a power deficit at large angular scales is manifested in several ways, for example low map variance. The results of a peak statistics analysis are consistent with the expectations of a Gaussian random field. The "Cold Spot" is detected with several methods, including map kurtosis, peak statistics, and mean temperature profile. We thoroughly probe the large-scale dipolar power asymmetry, detecting it with several independent tests, and address the subject of a posteriori correction. Tests of directionality suggest the presence of angular clustering from large to small scales, but at a significance that is dependent on the details of the approach. We perform the first examination of polarization data, finding the morphology of stacked peaks to be consistent with the expectations of statistically isotropic simulations. Where they overlap, these results are consistent with the Planck 2013 analysis based on the nominal mission data and provide our most thorough view of the statistics of the CMB fluctuations to date. C1 [Bucher, M.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Gauthier, C.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Remazeilles, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, CNRS IN2P3, CEA Irfu, APC,AstroParticule & Cosmol,Observ Paris,Sorbonne, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France. [Lahteenmaki, A.] Aalto Univ, Metsahovi Radio Observ, POB 13000, Aalto 00076, Finland. [Lahteenmaki, A.] Dept Radio Sci & Engn, POB 13000, Aalto 00076, Finland. [Kunz, M.] African Inst Math Sci, 6-8 Melrose Rd, Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy. [Lagache, G.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Ashdown, M.; Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, Westville Campus,Private Bag X54001, ZA-4000 Durban, South Africa. [Bond, J. R.; Hanson, D.; Huang, Z.; Martin, P. G.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, 60 St George St, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.] CNRS, IRAP, 9 Av Colonel Roche,BP 44346, F-31028 Toulouse 4, France. [Tuovinen, J.] Trinity Coll Dublin, CRANN, Dublin, Ireland. [Bock, J. J.; 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.; Ferguson, J.; Shellard, E. P. S.] Univ Cambridge, Ctr Theoret Cosmol, DAMTP, Wilberforce Rd, Cambridge CB3 0WA, England. [Hernandez-Monteagudo, C.] CEFCA, Plaza San Juan 1,Planta 2, Teruel 44001, Spain. [Borrill, J.; Keskitalo, R.] Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA USA. [Rebolo, R.] CSIC, Madrid, Spain. [Chamballu, A.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. [Hornstrup, A.; Linden-Vornle, M.; Norgaard-Nielsen, H. U.; Oxborrow, C. A.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark. [Kunz, M.; Tucci, M.] Univ Geneva, Dept Phys Theor, 24 Quai E Ansermet, CH-1211 Geneva, Switzerland. [Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38206, Tenerife, Spain. [Gonzalez-Nuevo, J.; Toffolatti, L.] Univ Oviedo, Dept Fis, Avda Calvo Sotelo S-N, Oviedo 33003, Spain. [Cruz, M.] Univ Cantabria, Dept Matemat Estadist & Computac, Avda Castros S-N, E-39005 Santander, Spain. [Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON, Canada. [Rachen, J. P.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands. [Contreras, D.; Scott, D.; Zibin, J. P.] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC, Canada. [Colombo, L. P. L.; Pierpaoli, E.] Univ Southern Calif, Dana & David Dornsife Coll Letter Arts & Sci, Dept Phys & Astron, Los Angeles, CA 90089 USA. [Elsner, F.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Huffenberger, K. M.] Florida State Univ, Dept Phys, Keen Phys Bldg,77 Chieftan Way, Tallahassee, FL 32306 USA. [Juvela, M.; Keihanen, E.; Kurki-Suonio, H.; Savelainen, M.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Dept Phys, Gustaf Hallstromin Katu 2a, Helsinki 00100, Finland. [Chiang, H. C.; Fraisse, A. A.; Gudmundsson, J. E.; Jones, W. C.; Nati, F.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [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, 1110 West Green St, Urbana, IL USA. [Bartolo, N.; Liguori, M.; Matarrese, S.] Univ Padua, Dipartimento Fis & Astron G Galilei, Via Marzolo 8, I-35131 Padua, Italy. [Burigana, C.; Lattanzi, M.; Mandolesi, N.; Natoli, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, Via Saragat 1, I-44122 Ferrara, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Pagano, L.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, Ple A Moro 2, Rome, Italy. [Bersanelli, M.; Maino, D.; Mennella, A.; Rossetti, M.; Tomasi, M.] Univ Milan, Dipartimento Fis, Via Celoria 16, Milan, Italy. [Benoit-Levy, A.; Gregorio, A.] Univ Trieste, Dipartimento Fis, Via A Valerio 2, Trieste, Italy. [Fantaye, Y.; Marinucci, D.; Renzi, A.] Univ Roma Tor Vergata, Dipartimento Matemat, Via Ric Sci 1, Rome, Italy. [Christensen, P. R.; Liu, H.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, 17 Blegdamsvej, Copenhagen, Denmark. [Dupac, X.; Leonardi, R.; Lopez-Caniego, M.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Camino Bajo Castillo S-N, Madrid 28692, Spain. [Tauber, J. A.] European Space Agcy, Estec, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. [Terenzi, L.] Univ E Campus, Fac Ingn, Via Isimbardi 10, I-22060 Novedrate, CO, Italy. [Matarrese, S.] Ist Nazl Fis Nucl, Gran Sasso Sci Inst, Viale F Crispi 7, I-67100 Laquila, Italy. [Pettorino, V.] HGSFP, Philosophenweg 16, D-69120 Heidelberg, Germany. [Pettorino, V.] Heidelberg Univ, Dept Theoret Phys, Philosophenweg 16, D-69120 Heidelberg, Germany. [Kurki-Suonio, H.; Lahteenmaki, A.; Savelainen, M.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Helsinki Inst Phys, Gustaf Hallstromin Katu 2, Helsinki, Finland. [de Zotti, G.] Osserv Astron Padova, INAF, Vicolo Osservatorio 5, Padua, Italy. [Polenta, G.] Osserv Astron Roma, INAF, Via Frascati 33, Monte Porzio Catone, Italy. [Frailis, M.; Galeotta, S.; Gregorio, A.; Maggio, G.; Maris, M.; Pasian, F.; Zacchei, A.] Osserv Astron Trieste, INAF, Via GB Tiepolo 11, Trieste, Italy. [Burigana, C.; Butler, R. C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Molinari, D.; Morgante, G.; Natoli, P.; Paoletti, D.; Sandri, M.; Terenzi, L.; Toffolatti, L.; Trombetti, T.; Valenziano, L.; Villa, F.] IASF Bologna, INAF, Via Gobetti 101, Bologna, Italy. [Bersanelli, M.; Donzelli, S.; Maino, D.; Mennella, A.; Rossetti, M.; Tomasi, M.] IASF Milano, INAF, Via E Bassini 15, Milan, Italy. [Burigana, C.; Finelli, F.; Paoletti, D.] Ist Nazl Fis Nucl, Sez Bologna, Via Irnerio 46, I-40126 Bologna, Italy. [Melchiorri, A.; Pagano, L.] Univ Roma Sapienza, Ist Nazl Fis Nucl, Sez Roma 1, Piazzale Aldo Moro 2, I-00185 Rome, Italy. [Renzi, A.] Univ Roma Tor Vergata, Ist Nazl Fis Nucl, Sez Roma 2, Via Ric Sci 1, Rome, Italy. [Gregorio, A.] Ist Nazl Fis Nucl, Natl Inst Nucl Phys, Via Valerio 2, I-34127 Trieste, Italy. [Desert, F. -X.] Univ Grenoble Alpes, IPAG, CNRS, F-38000 Grenoble, France. [Aluri, P. K.; Mitra, S.; Pant, N.; Rotti, A.; Souradeep, T.] Pune Univ Campus, Post Bag 4, Pune 411007, Maharashtra, India. [Clements, D. L.; Ducout, A.; Jaffe, A. H.; Mortlock, D.] Imperial Coll London, Blackett Lab, Astrophys Grp, Prince Consort Rd, London SW7 2AZ, England. [McGehee, P.; Pearson, T. J.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, 25 Rue Martyrs, Grenoble, France. [Dole, H.] Inst Univ France, 103 Bd St Michel, F-75005 Paris, France. [Aghanim, N.; Aumont, J.; Boulanger, F.; Chamballu, A.; Dole, H.; Douspis, M.; Ghosh, T.; Hurier, G.; Kunz, M.; Lagache, G.; Mangilli, A.; Miville-Deschenes, M. -A.; Pajot, F.; Puget, J. -L.; Remazeilles, M.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR 8617, Batiment 121, F-91440 Orsay, France. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Ducout, A.; Elsner, F.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] CNRS, Inst Astrophys Paris, UMR 7095, 98 Bis Blvd Arago, F-75014 Paris, France. [Lesgourgues, J.] Rhein Westfal TH Aachen, Inst Theoret Teilchenphys & Kosmol, D-52056 Aachen, Germany. [Popa, L.] Inst Space Sci, Bucharest 077125, Romania. [Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D. L.; Migliaccio, M.; Sutton, D.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Akrami, Y.; Eriksen, H. K.; Gjerlow, E.; Hansen, F. K.; Lilje, P. B.; Mikkelsen, K.] Univ Oslo, Inst Theoret Astrophys, N-0371 Oslo, Norway. [Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, C Via Lactea S-N, San Cristobal la Laguna 38205, Tenerife, Spain. [Barreiro, R. B.; Bonavera, L.; Casaponsa, B.; Curto, A.; Diego, J. M.; Fernandez-Cobos, R.; Gonzalez-Nuevo, J.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Molinari, D.; Toffolatti, L.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, Avda Castros S-N, Santander 39005, Spain. [Bartolo, N.; Liguori, M.; Matarrese, S.] Ist Nazl Fis Nucl, Sez Padova, Via Marzolo 8, I-35131 Padua, Italy. [Bock, J. J.; Colombo, L. P. L.; Crill, B. P.; Dore, O.; Gorski, K. M.; Hanson, D.; Hildebrandt, S. R.; Holmes, W. A.; Lawrence, C. R.; Mitra, S.; Pietrobon, D.; Prezeau, G.; Rocha, G.; Roudier, G.; Seiffert, M. D.; Wade, L. A.; Wehus, I. K.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. [Bonaldi, A.; Davies, R. D.; Davis, R. J.; Noviello, F.; Remazeilles, M.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England. [Galli, S.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Ashdown, M.; Challinor, A.; Curto, A.; Gratton, S.; Harrison, D. L.; Lasenby, A.; Migliaccio, M.; Sutton, D.] Univ Cambridge, Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Stolyarov, V.] Kazan Fed Univ, 18 Kremlyovskaya St, Kazan 420008, Russia. [Couchot, F.; Henrot-Versille, S.; Mangilli, A.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, CNRS, IN2P3, LAL, Orsay, France. [Catalano, A.; Coulais, A.; Lamarre, J. -M.; Levrier, F.; Roudier, G.] CNRS, Observ Paris, LERMA, 61 Ave Observ, F-75014 Paris, France. [Arnaud, M.; Chamballu, A.; Pratt, G. W.] Univ Paris Diderot, CEA Saclay, CEA DSM CNRS, IRFU,Serv Astrophys,Lab AIM, Bat 709, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, Lab Traitement & Commun Informat, UMR 5141, 46 Rue Barrault, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom ParisTech, 46 Rue Barrault, F-75634 Paris 13, France. [Catalano, A.; Combet, C.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble Alpes, CNRS, IN2P3, Lab Phys Subatom & Cosmol, 53 Rue Martyrs, F-38026 Grenoble, France. [Van Tent, B.] Univ Paris 11, Lab Phys Theor, Batiment 210, F-91405 Orsay, France. [Van Tent, B.] CNRS, Batiment 210, F-91405 Orsay, France. [Kisner, T. S.] Lawrence Berkeley Natl Lab, Berkeley, CA USA. [Novikov, D.; Novikov, I.] Russian Acad Sci, Ctr Astro Space, Lebedev Phys Inst, 84-32 Profsoyuznaya St, Moscow 117997, Russia. [Gauthier, C.] Natl Taiwan Univ, Leung Ctr Cosmol & Particle Astrophys, Taipei 10617, Taiwan. [Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Kim, J.; Knoche, J.; Rachen, J. P.; Reinecke, M.; Sunyaev, R.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. [Hanson, D.] McGill Univ, McGill Phys, Ernest Rutherford Phys Bldg,3600 Rue Univ, Montreal, PQ H3A 2T8, Canada. [Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Bielewicz, P.] Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland. [Christensen, P. R.; Frejsel, A.; Liu, H.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, Blegdamsvej 17, DK-2100 Copenhagen, Denmark. [Savini, G.] UCL, Opt Sci Lab, Gower St, London, England. [Baccigalupi, C.; Basak, S.; Bielewicz, P.; Danese, L.; de Zotti, G.; Paci, F.; Perrotta, F.] SISSA, Astrophys Sect, Via Bonomea 265, I-34136 Trieste, Italy. [Ade, P. A. R.; Munshi, D.; Spencer, L. D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Queens Buildings, Cardiff CF24 3AA, S Glam, Wales. [Moss, A.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Frolov, A.] Simon Fraser Univ, Dept Phys, 8888 Univ Dr, Burnaby, BC, Canada. [Bouchet, F. R.] UPMC, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, 98 Bis Blvd Arago, F-75014 Paris, France. [Sunyaev, R.] Russian Acad Sci, Space Res Inst IKI, Profsoyuznaya Str 84-32, Moscow 117997, Russia. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz 369167, Zelenchukskiy R, Russia. [Church, S.] Stanford Univ, Dept Phys, Varian Phys Bldg,382 Via Pueblo Mall, Stanford, CA 94305 USA. [Calabrese, E.] Univ Oxford, Subdept Astrophys, Keble Rd, Oxford OX1 3RH, England. [Lesgourgues, J.] CERN, PH TH, Div Theory, CH-1211 Geneva 23, Switzerland. [Benabed, K.; Benoit-Levy, A.; Colombi, S.; Elsner, F.; Hivon, E.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UMR 7095, 98 Bis Blvd Arago, F-75014 Paris, France. [Banday, A. J.; Bernard, J. -P; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, E-18071 Granada, Spain. [Battaner, E.] Univ Granada, Inst Carlos Fis Teor & Computac 1, E-18071 Granada, Spain. [Akrami, Y.] Heidelberg Univ, Inst Theoret Phys, Philosophenweg 16, D-69120 Heidelberg, Germany. [Gorski, K. M.] Univ Warsaw Observ, Aleje Ujazdowskie 4, PL-00478 Warsaw, Poland. RP Banday, AJ (reprint author), CNRS, IRAP, 9 Av Colonel Roche,BP 44346, F-31028 Toulouse 4, France.; Banday, AJ (reprint author), Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. EM anthony.banday@irap.omp.eu RI Lahteenmaki, Anne/L-5987-2013; Barreiro, Rita Belen/N-5442-2014; bonavera, laura/E-9368-2017; Gonzalez-Nuevo, Joaquin/I-3562-2014; Herranz, Diego/K-9143-2014; Colombo, Loris/J-2415-2016; OI Juvela, Mika/0000-0002-5809-4834; Molinari, Diego/0000-0002-7799-3915; Zacchei, Andrea/0000-0003-0396-1192; Toffolatti, Luigi/0000-0003-2645-7386; Lilje, Per/0000-0003-4324-7794; Liu, Hao/0000-0003-4410-5827; Paoletti, Daniela/0000-0003-4761-6147; Nati, Federico/0000-0002-8307-5088; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Barreiro, Rita Belen/0000-0002-6139-4272; bonavera, laura/0000-0001-8039-3876; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Herranz, Diego/0000-0003-4540-1417; Colombo, Loris/0000-0003-4572-7732; Stolyarov, Vladislav/0000-0001-8151-828X; Valiviita, Jussi/0000-0001-6225-3693; Hurier, Guillaume/0000-0002-1215-0706; Huang, Zhiqi/0000-0002-1506-1063; Kurki-Suonio, Hannu/0000-0002-4618-3063 FU ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MINECO (Spain); JA (Spain); RES (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC; PRACE (EU) 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, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (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.cosmos.esaint/web/planck/planch-collaboration. Some of the results in this paper have been derived using the HEALPix package. NR 157 TC 1 Z9 1 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 OCT PY 2016 VL 594 AR Al6 DI 10.1051/0004-6361/201526681 PG 62 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4MG UT WOS:000385832200023 ER PT J AU Zhao, KL Wang, RH Burleigh, SC Sabbagh, A Wu, WW De Sanctis, M AF Zhao, Kanglian Wang, Ruhai Burleigh, Scott C. Sabbagh, Alaa Wu, Wenwei De Sanctis, Mauro TI Performance of Bundle Protocol for Deep-Space Communications SO IEEE TRANSACTIONS ON AEROSPACE AND ELECTRONIC SYSTEMS LA English DT Article ID FILE-DELIVERY PROTOCOL; TOLERANT NETWORKING; INTERPLANETARY INTERNET; DELAY; DTN; CHALLENGES; LINKS; TIME AB Delay/disruption tolerant networking (DTN) was developed to enable automated network communications despite frequent and lengthy link disruptions and long link delay. DTN communications rely heavily on a bundle protocol (BP) that uses the well-known approach of store and forward with optional custody transfer for which a node agrees to hold BP data units, bundles, in memory (or storage) until its successful reception is acknowledged by the next node. However, in the presence of long link disruptions, little work has been done regarding performance modeling of BP for reliable data transfer in deep-space communications. In this paper, we present a study of BP over a relay-based deep-space communications system, characterized by lengthy link disruptions accompanied by an extremely long propagation delay, lossy data links, and asymmetric channel rates. An analytical model is built to estimate the total delivery time of a file (message) that is transmitted as the contents of one or more BP bundles over a deep-space channel. A model is also built to characterize the dynamics of memory occupancy and release when BP is used for reliable data delivery in the presence of link disruptions. The constructed models are validated by running experiments using a test bed. C1 [Zhao, Kanglian] Nanjing Univ, Sch Elect Sci & Engn, Nanjing 210093, Jiangsu, Peoples R China. [Wang, Ruhai; Sabbagh, Alaa] Lamar Univ, Elect Engn, POB 10029, Beaumont, TX 77710 USA. [Burleigh, Scott C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wu, Wenwei] Soochow Univ, Sch Elect & Informat Engn, 1 Shizi St, Suzhou 215006, Jiangsu, Peoples R China. [De Sanctis, Mauro] Univ Roma Tor Vergata, Dept Elect Engn, Via Politecn 1, I-00175 Rome, Italy. RP Wang, RH (reprint author), Lamar Univ, Elect Engn, POB 10029, Beaumont, TX 77710 USA. EM rwang@lamar.edu FU Future Networks Innovation Institute of Jiangsu Province, China [BY2013039-3-10]; National Natural Science Foundation of China [61401194]; Satellite Communication and Navigation Collaborative Innovation Center of Jiangsu Province, China [SatCN-201410, SatCN-201407] FX The research described in this paper was performed, in part, at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Government sponsorship is acknowledged. This work was supported, in part, by the Future Networks Innovation Institute of Jiangsu Province, China, for a Prospective Research Project on Future Networks under Grant BY2013039-3-10 and by the National Natural Science Foundation of China under Grant 61401194. This work was also supported, in part, by the Satellite Communication and Navigation Collaborative Innovation Center of Jiangsu Province, China, under Grants SatCN-201410 and SatCN-201407. NR 31 TC 0 Z9 0 U1 0 U2 0 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9251 EI 1557-9603 J9 IEEE T AERO ELEC SYS JI IEEE Trans. Aerosp. Electron. Syst. PD OCT PY 2016 VL 52 IS 5 BP 2347 EP 2361 DI 10.1109/TAES.2016.150462 PG 15 WC Engineering, Aerospace; Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA EK5TM UT WOS:000393988800021 ER PT J AU Grecu, M Olson, WS Munchak, SJ Ringerud, S Liao, L Haddad, Z Kelley, BL McLaughlin, SF AF Grecu, Mircea Olson, William S. Munchak, Stephen Joseph Ringerud, Sarah Liao, Liang Haddad, Ziad Kelley, Bartie L. McLaughlin, Steven F. TI The GPM Combined Algorithm SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID RAIN-PROFILING ALGORITHM; TRMM PRECIPITATION RADAR; MICROWAVE RADIATIVE PROPERTIES; DROP SIZE DISTRIBUTION; PART II; MULTIPLE-SCATTERING; MELTING-LAYER; RADIOMETER; FREQUENCIES; RETRIEVALS AB In this paper, the operational Global Precipitation Measurement (GPM) mission combined radar-radiometer algorithm is thoroughly described. The operational combined algorithm is designed to reduce uncertainties in GPM Core Observatory precipitation estimates by effectively integrating complementary information from the GPM Dual-Frequency Precipitation Radar (DPR) and the GPM Microwave Imager (GMI) into an optimal, physically consistent precipitation product. Although similar in many respects to previously developed combined algorithms, the GPM combined algorithm has several unique features that are specifically designed to meet the GPM objectives of deriving, based on GPM Core Observatory information, accurate and physically consistent precipitation estimates from multiple spaceborne instruments, and ancillary environmental data from reanalyses. The algorithm features an optimal estimation framework based on a statistical formulation of the Gauss-Newton method, a parameterization for the nonuniform distribution of precipitation within the radar fields of view, a methodology to detect and account for multiple scattering in Ka-band DPR observations, and a statistical deconvolution technique that allows for an efficient sequential incorporation of radiometer information into DPR precipitation retrievals. C1 [Grecu, Mircea; Liao, Liang] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21239 USA. [Grecu, Mircea] NASA GSFC, Atmospheres Lab, Greenbelt, MD USA. [Olson, William S.] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21201 USA. [Olson, William S.; Munchak, Stephen Joseph; Ringerud, Sarah; Liao, Liang] NASA GSFC, Mesoscale Atmospher Proc Lab, 8800 Greenbelt Rd,MC 612, Greenbelt, MD 20771 USA. [Ringerud, Sarah] Oak Ridge Associated Univ, Oak Ridge, TN USA. [Haddad, Ziad] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Kelley, Bartie L.; McLaughlin, Steven F.] Sci Syst & Applicat Inc, Lanham, MD USA. RP Grecu, M (reprint author), NASA GSFC, Mesoscale Atmospher Proc Lab, 8800 Greenbelt Rd,MC 612, Greenbelt, MD 20771 USA. EM mircea.grecu-1@nasa.gov FU NASA PMM project [NNX13AF85G] FX This work was supported by the NASA PMM project (NNX13AF85G). The authors thank Drs. Ramesh Kakar (NASA headquarters) and Gail Skofronick-Jackson (GPM project scientist) for their support of this effort. The authors would also like to thank the PMM combined algorithm team members, Benjamin Johnson, Lin Tian, Kwo-Sen Kuo, and Hirohiko Masunaga, for their contributions to the overall algorithm development effort. In addition, the authors are grateful to Lawrence Woltz and NASA Precipitation Processing System personnel for their operational support, David Bolvin for his help with GPCP data, and Drs. Pierre Kirstetter and Chris Kidd for their insights into the use of MRMS and other ground validation products. The authors also thank Dr. Robin Hogan for making public the source code of the fast multiple-scattering model, and three anonymous reviewers for their comments and suggestions. NR 57 TC 0 Z9 0 U1 1 U2 1 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD OCT PY 2016 VL 33 IS 10 BP 2225 EP 2245 DI 10.1175/JTECH-D-16-0019.1 PG 21 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA EL3RG UT WOS:000394536000005 ER PT J AU Jain, RK Yeo, H Ho, JC Bhagwat, M AF Jain, Rohit K. Yeo, Hyeonsoo Ho, Jimmy C. Bhagwat, Mahendra TI An Assessment of RCAS Performance Prediction for Conventional and Advanced Rotor Configurations SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY LA English DT Article ID AIRLOADS; DYNAMICS; MODEL; WAKE AB The U.S. Army's Rotorcraft Comprehensive Analysis System (RCAS) version 15.07 was validated for aerodynamic performance prediction for a variety of isolated rotor configurations in hover and forward flight. Validation cases included a wide variety of key rotor configurations, covering model scale and full scale, twist distributions (zero twist, moderate linear twist, nonlinear twist, and high nonlinear twist), tip shapes (rectangular, swept, swept-tapered, tapered, and anhedral), and flight conditions (hover to high-speed forward flight). A free-vortex wake model was used for hover performance, whereas a prescribed-vortex wake model was sufficient for moderate-to-high advance ratios. At low advance ratios, the increased rotor-wake interactions yielded less-accurate results using the prescribed wake. The validation study showed good correlation with test data using the best practices for the vortex wake modeling parameters. C1 [Jain, Rohit K.; Yeo, Hyeonsoo; Bhagwat, Mahendra] US Army Aviat Dev Directorate AFDD, Aviat & Missile Res Dev & Engn Ctr, Res Dev & Engn Command RDECOM, Moffett Field, CA 94035 USA. [Ho, Jimmy C.] Sci & Technol Corp, Ames Res Ctr, Moffett Field, CA USA. RP Jain, RK (reprint author), US Army Aviat Dev Directorate AFDD, Aviat & Missile Res Dev & Engn Ctr, Res Dev & Engn Command RDECOM, Moffett Field, CA 94035 USA. EM rkj238@gmail.com NR 51 TC 1 Z9 1 U1 0 U2 0 PU AMER HELICOPTER SOC INC PI ALEXANDRIA PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA SN 0002-8711 EI 2161-6027 J9 J AM HELICOPTER SOC JI J. Am. Helicopter Soc. PD OCT PY 2016 VL 61 IS 4 AR 042005 DI 10.4050/JAHS.61.042005 PG 12 WC Engineering, Aerospace SC Engineering GA EK7PY UT WOS:000394118900006 ER PT J AU Srivastava, PK Islam, T Singh, SK Petropoulos, GP Gupta, M Dai, Q AF Srivastava, Prashant K. Islam, Tanvir Singh, Sudhir K. Petropoulos, George P. Gupta, Manika Dai, Qiang TI Forecasting Arabian Sea level rise using exponential smoothing state space models and ARIMA from TOPEX and Jason satellite radar altimeter data SO METEOROLOGICAL APPLICATIONS LA English DT Article DE sea level rise; forecasting; exponential models; ARIMA; Arabian Sea ID CLIMATE-CHANGE; MARINE ECOSYSTEMS; MANGROVE FORESTS; FUTURE; THREATS AB Sea level rise is a threat to coastal habitation and is corroborating evidence for global warming. The present study investigated the combined use of quantitative forecasting methods for sea level rise using exponential smoothing state space models (ESMs) and an autoregressive integrated moving average (ARIMA) model fed with sea level data over 17 years (1994-2010). Two levels of ESMs were employed: double (model levels with trend) and triple (model levels, trend and seasonal decomposition). The overall data analysis revealed the better performance of ARIMA in terms of index of agreement (d = 0.79), root-mean-square error (RMSE = 32.8 mm) and mean absolute error (MAE = 25.55 mm) than the triple ESM (d = 0.76; RMSE = 39.86 mm; MAE = 35.02 mm) and double ESM(d = 0.14; RMSE = 52.71 mm; MAE = 45.99 mm) models. The present study results suggest that the rate of Arabian Sea level rise is high, and if this is not taken into consideration many coastal areas may become subject to climate-change-induced habitat loss in future. C1 [Srivastava, Prashant K.; Gupta, Manika] NASA, Hydrol Sci, Goddard Space Flight Ctr, Code 617,Room G208,Bldg 33, Greenbelt, MD 20771 USA. [Srivastava, Prashant K.] Banaras Hindu Univ, Inst Environm & Sustainable Dev, Varanasi, Uttar Pradesh, India. [Islam, Tanvir] NASA, Jet Prop Lab, Pasadena, CA USA. [Islam, Tanvir] CALTECH, Pasadena, CA 91125 USA. [Singh, Sudhir K.] Univ Allahabad, K Banerjee Ctr Atmospher & Ocean Studies, Nehru Sci Ctr, IIDS, Allahabad, Uttar Pradesh, India. [Petropoulos, George P.] Aberystwyth Univ, Dept Geog & Earth Sci, Aberystwyth, Dyfed, Wales. [Dai, Qiang] Nanjing Normal Univ, Sch Geog Sci, Nanjing, Jiangsu, Peoples R China. RP Srivastava, PK (reprint author), NASA, Hydrol Sci, Goddard Space Flight Ctr, Code 617,Room G208,Bldg 33, Greenbelt, MD 20771 USA. EM prashant.k.srivastava@nasa.gov FU Banaras Hindu University FX The authors are grateful to the anonymous reviewers for their valuable feedback. Authors are also thankful to Colorado Center for Astrodynamics Research at the University of Colorado at Boulder, USA, for providing the altimeter data sets. The first author would like to acknowledge Banaras Hindu University for providing a seed grant. The views expressed here are those of the authors solely and do not constitute a statement of policy, decision, or position on behalf of NASA or the authors' affiliated institutions. NR 41 TC 0 Z9 0 U1 2 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1350-4827 EI 1469-8080 J9 METEOROL APPL JI Meteorol. Appl. PD OCT PY 2016 VL 23 IS 4 BP 633 EP 639 DI 10.1002/met.1585 PG 7 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EJ3VJ UT WOS:000393140000007 ER PT J AU Lew, BWP Apai, D Zhou, Y Schneider, G Burgasser, AJ Karalidi, T Yang, H Marley, MS Cowan, NB Bedin, LR Metchev, SA Radigan, J Lowrance, PJ AF Lew, Ben W. P. Apai, Daniel Zhou, Yifan Schneider, Glenn Burgasser, Adam J. Karalidi, Theodora Yang, Hao Marley, Mark S. Cowan, Nicolas B. Bedin, Luigi R. Metchev, Stanimir A. Radigan, Jacqueline Lowrance, Patrick J. TI CLOUD ATLAS: DISCOVERY OF PATCHY CLOUDS AND HIGH-AMPLITUDE ROTATIONAL MODULATIONS IN A YOUNG, EXTREMELY RED L-TYPE BROWN DWARF SO Astrophysical Journal Letters LA English DT Article DE brown dwarfs; stars: atmospheres; stars: individual (WISEP J004701.06+680352.1); stars: low-mass ID HUBBLE-SPACE-TELESCOPE; PROPER-MOTION SURVEY; DOR MOVING GROUP; L/T TRANSITION; BAND VARIABILITY; T DWARFS; WISE J104915.57-531906.1AB; PHOTOMETRIC VARIABILITY; SURFACE GRAVITY; MASS OBJECT AB Condensate clouds fundamentally impact the atmospheric structure and spectra of exoplanets and brown dwarfs, but the connections between surface gravity, cloud structure, dust in the upper atmosphere, and the red colors of some brown dwarfs remain poorly understood. Rotational modulations enable the study of different clouds in the same atmosphere, thereby providing a method to isolate the effects of clouds. Here, we present the discovery of high peak-to-peak amplitude (8%) rotational modulations in a low-gravity, extremely red (J-K-s = 2.55) L6 dwarf WISEP J004701.06+680352.1 (W0047). Using the Hubble Space Telescope (HST) time-resolved grism spectroscopy, we find a best-fit rotational period (13.20 +/- 0.14 hr) with a larger amplitude at 1.1 mu m than at 1.7 mu m. This is the third-largest near-infrared variability amplitude measured in a brown dwarf, demonstrating that large-amplitude variations are not limited to the L/T transition but are present in some extremely red L-type dwarfs. We report a tentative trend between the wavelength dependence of relative amplitude, possibly proxy for small dust grains lofted in the upper atmosphere, and the likelihood of large-amplitude variability. By assuming forsterite as a haze particle, we successfully explain the wavelength-dependent amplitude with submicron-sized haze particle sizes of around 0.4 mu m. W0047 links the earlier spectral and later spectral type brown dwarfs in which rotational modulations have been observed; the large amplitude variations in this object make this a benchmark brown dwarf for the study of cloud properties close to the L/T transition. C1 [Lew, Ben W. P.; Apai, Daniel] Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, 1640 E Univ Blvd, Tucson, AZ 85718 USA. [Apai, Daniel; Zhou, Yifan; Schneider, Glenn; Karalidi, Theodora; Yang, Hao] Univ Arizona, Dept Astron, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. [Apai, Daniel] NASA Nexus Exoplanet Syst Sci, Earths Other Solar Syst Team, 933 N Cherry Ave, Tucson, AZ 85721 USA. [Burgasser, Adam J.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Marley, Mark S.] NASA, Ames Res Ctr, Naval Air Stn, Mountain View, CA 94035 USA. [Cowan, Nicolas B.] Amherst Coll, Dept Phys & Astron, Amherst, MA 01002 USA. [Bedin, Luigi R.] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy. [Metchev, Stanimir A.] Univ Western Ontario, Dept Phys & Astron, 1151 Richmond Ave, London, ON N6A 3K7, Canada. [Radigan, Jacqueline] Utah Valley Univ, Dept Phys, 800 West Univ Pkwy, Orem, UT 84058 USA. [Lowrance, Patrick J.] CALTECH, Infrared Proc & Anal Ctr, MS 100-22, Pasadena, CA 91125 USA. RP Lew, BWP (reprint author), Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, 1640 E Univ Blvd, Tucson, AZ 85718 USA. EM wplew@lpl.arizona.edu OI Yang, Hao/0000-0002-9423-2333; Zhou, Yifan/0000-0003-2969-6040; Marley, Mark/0000-0002-5251-2943 FU Technology Research Initiative Fund (TRIF) Imaging Fellowship, University of Arizona; NASA through a grant from the Space Telescope Science Institute [14241]; NASA [NAS5-26555]; Space Telescope Science Institute [14241]; National Aeronautics and Space Administration; National Science Foundation FX We thank the anonymous referee for useful comments that improved the manuscript. We would like to thank Min Fang, Alex Bixel, Kevin Wagner, Belle Yu-Ya Huang, and Carol Yang for providing useful comments. Ben W.P. Lew is supported in part by the Technology Research Initiative Fund (TRIF) Imaging Fellowship, University of Arizona. Support for Program number 14241 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. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained in GO program 14241 at the Space Telescope Science Institute. 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. NR 49 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2016 VL 829 IS 2 AR L32 DI 10.3847/2041-8205/829/2/L32 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EJ7XH UT WOS:000393435500001 ER PT J AU Holst, M Sarbach, O Tiglio, M Vallisneri, M AF Holst, Michael Sarbach, Olivier Tiglio, Manuel Vallisneri, Michele TI THE EMERGENCE OF GRAVITATIONAL WAVE SCIENCE: 100 YEARS OF DEVELOPMENT OF MATHEMATICAL THEORY, DETECTORS, NUMERICAL ALGORITHMS, AND DATA ANALYSIS TOOLS SO BULLETIN OF THE AMERICAN MATHEMATICAL SOCIETY LA English DT Article ID EINSTEIN CONSTRAINT EQUATIONS; MEAN-CURVATURE SOLUTIONS; BOUNDARY-VALUE-PROBLEMS; BLACK-HOLE COLLISIONS; GENERAL-RELATIVITY; INITIAL DATA; CLOSED MANIFOLDS; FIELD-EQUATIONS; STABILITY; RADIATION AB On September 14, 2015, the newly upgraded Laser Interferometer Gravitational-wave Observatory (LIGO) recorded a loud gravitational-wave (GW) signal, emitted a billion light-years away by a coalescing binary of two stellar-mass black holes. The detection was announced in February 2016, in time for the hundredth anniversary of Einstein's prediction of GWs within the theory of general relativity (GR). The signal represents the first direct detection of GWs, the first observation of a black-hole binary, and the first test of GR in its strong-field, high-velocity, nonlinear regime. In the remainder of its first observing run, LIGO observed two more signals from black-hole binaries, one moderately loud, another at the boundary of statistical significance. The detections mark the end of a decades-long quest and the beginning of GW astronomy: finally, we are able to probe the unseen, electromagnetically dark Universe by listening to it. In this article, we present a short historical overview of GW science: this young discipline combines GR, arguably the crowning achievement of classical physics, with record-setting, ultra-low-noise laser interferometry, and with some of the most powerful developments in the theory of differential geometry, partial differential equations, high-performance computation, numerical analysis, signal processing, statistical inference, and data science. Our emphasis is on the synergy between these disciplines and how mathematics, broadly understood, has historically played, and continues to play, a crucial role in the development of GW science. We focus on black holes, which are very pure mathematical solutions of Einstein's gravitational-field equations that are nevertheless realized in Nature and that provided the first observed signals. C1 [Holst, Michael] Univ Calif San Diego, Dept Phys, Dept Math, La Jolla, CA 92093 USA. Univ Michoacana, Inst Fis & Matemat, Edificio C-3,Ciudad Univ, Morelia 58040, Michoacan, Mexico. Univ Calif San Diego, Ctr Astrophys & Space Sci, Ctr Computat Math, La Jolla, CA 92093 USA. Univ Calif San Diego, San Diego Supercomp Ctr, La Jolla, CA 92093 USA. CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. CALTECH, TAPIR Grp, MC 350-17, Pasadena, CA 91125 USA. RP Holst, M (reprint author), Univ Calif San Diego, Dept Phys, Dept Math, La Jolla, CA 92093 USA. FU NSF [PHY-1500818, DMS/FRG-1262982, DMS/CM-1217175, PHY-1404569]; CONACyT [271904]; CIC grant; National Aeronautics and Space Administration FX We thank the reviewers as well as David Shoemaker, who read preliminary drafts, for their feedback and comments. This work was supported in part by NSF grants PHY-1500818, DMS/FRG-1262982, and DMS/CM-1217175 to the University of California at San Diego, by NSF grant PHY-1404569 to the California Institute of Technology, by CONACyT grant No. 271904, and by a CIC grant to Universidad Michoacana. Part of this research was performed at the Jet Propulsion Laboratory, under contract with the National Aeronautics and Space Administration. NR 154 TC 1 Z9 1 U1 1 U2 1 PU AMER MATHEMATICAL SOC PI PROVIDENCE PA 201 CHARLES ST, PROVIDENCE, RI 02940-2213 USA SN 0273-0979 EI 1088-9485 J9 B AM MATH SOC JI Bull. Amer. Math. Soc. PD OCT PY 2016 VL 53 IS 4 BP 513 EP 554 DI 10.1090/bull/1544 PG 42 WC Mathematics SC Mathematics GA EI8GY UT WOS:000392745400001 ER PT J AU de Fleurian, B Morlighem, M Seroussi, H Rignot, E van den Broeke, MR Munneke, PK Mouginot, J Smeets, PCJP Tedstone, AJ AF de Fleurian, Basile Morlighem, Mathieu Seroussi, Helene Rignot, Eric van den Broeke, Michiel R. Munneke, Peter Kuipers Mouginot, Jeremie Smeets, Paul C. J. P. Tedstone, Andrew J. TI A modeling study of the effect of runoff variability on the effective pressure beneath Russell Glacier, West Greenland SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE LA English DT Article ID ICE-SHEET MOTION; SUBGLACIAL DRAINAGE; MASS-BALANCE; WATER-FLOW; ACCELERATION; TEMPERATURE; MECHANISMS; EVOLUTION; BOREHOLES; INTERIOR AB Basal sliding is a main control on glacier flow primarily driven by water pressure at the glacier base. The ongoing increase in surface melting of the Greenland Ice Sheet warrants an examination of its impact on basal water pressure and in turn on basal sliding. Here we examine the case of Russell Glacier, in West Greenland, where an extensive set of observations has been collected. These observations suggest that the recent increase in melt has had an equivocal impact on the annual velocity, with stable flow on the lower part of the drainage basin but accelerated flow above the Equilibrium Line Altitude (ELA). These distinct behaviors have been attributed to different evolutions of the subglacial draining system during and after the melt season. Here we use a high-resolution subglacial hydrological model forced by reconstructed surface runoff for the period 2008 to 2012 to investigate the cause of these distinct behaviors. We find that the increase in meltwater production at low elevation yields a more efficient drainage system compatible with the observed stagnation of the mean annual flow below the ELA. At higher elevation, the model indicates that the drainage system is mostly inefficient and is therefore strongly sensitive to an increase in meltwater availability, which is consistent with the observed increase in ice velocity. C1 [de Fleurian, Basile; Morlighem, Mathieu; Rignot, Eric; Mouginot, Jeremie] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Seroussi, Helene; Rignot, Eric] CALTECH, Jet Prop Lab, Pasadena, CA USA. [van den Broeke, Michiel R.; Munneke, Peter Kuipers; Smeets, Paul C. J. P.] Univ Utrecht, Inst Marine & Atmospher Res, Utrecht, Netherlands. [Tedstone, Andrew J.] Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland. RP de Fleurian, B (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. EM basile.defleurian@uib.no RI Van den Broeke, Michiel/F-7867-2011 OI Van den Broeke, Michiel/0000-0003-4662-7565 FU National Aeronautics and Space Administration FX This work was performed at the University of California Irvine and at the California Institute of Technology's Jet Propulsion Laboratory under a contract with the National Aeronautics and Space Administration. We acknowledge data from NASA's Operation IceBridge mission. Request for data should be made respectively to C.J.P.P. Smeets (C.J.P.P.Smeets@uu.nl) for pressure data at SHR, M.R. van den Broeke (M.R.vandenBroeke@uu.nl) for RACMO2 output, and P.W. Nienow (pnienow@staffmail.ed.ac.uk) for GPS velocities on Russell Glacier. We thank the reviewers for their constructive comments that helped to improve the manuscript quality. NR 47 TC 0 Z9 0 U1 6 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9003 EI 2169-9011 J9 J GEOPHYS RES-EARTH JI J. Geophys. Res.-Earth Surf. PD OCT PY 2016 VL 121 IS 10 DI 10.1002/2016JF003842 PG 15 WC Geosciences, Multidisciplinary SC Geology GA EI9LS UT WOS:000392830200012 ER PT J AU Adam, R Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartolo, N Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bertincourt, B Bielewicz, P Bock, JJ Bonavera, L Bond, JR Borrill, J Bouchet, FR Boulanger, F Bucher, M Burigana, C Calabrese, E Cardoso, JF Catalano, A Challinor, A Chamballu, A Chary, RR Chiang, HC Christensen, PR Clements, DL Colombi, S Colombo, LPL Combet, C Couchot, F Coulais, A Crill, BP Curto, A Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Diego, JM Dole, H Donzelli, S Dure, O Douspis, M Ducout, A Dupac, X Efstathiou, G Elsner, F Ensslin, TA Eriksen, HK Falgarone, E Fergusson, J Finelli, F Forni, O Frailis, M Fraisse, AA Franceschi, E Frejser, A Galeotta, S Galli, S Ganga, K Ghosh, T Giard, M Giraud-Heraudl, Y Gjerlow, E Gonzalez-Nuevo, J Gorski, KM Gratton, S Gruppuso, A Gudmundsson, JE Hansen, FK Hanson, D Harrison, DL Henrot-Versille, S Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Hurier, G Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knoche, J Kunz, M Kurki-Suonio, H Lagache, G Lamarre, JM Lasenby, A Lattanzi, M Lawrence, CR Le Jenne, M Leahy, JP Lellouch, E Leonardi, R Lesgourgues, J Levrier, F Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maggie, G Maino', D Mandolesi, N Mangilli, A Maris, M Martin, PG Martinez-Gonzalez, E Masi, S Matarrese, S McGehee, P Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Moreno, R Morgante, G Mortlock, D Moss, A Mottet, S Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Oxborrow, CA Paci, F Pagano, L Pajot, F Paoletti, D Pasian, F Patanchon, G Pearson, TJ Perdereau, O Perotto, L Perrotta, F Pettorino, V Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Reinecke, M Remazeilles, M Renault, C Renzi, A Ristorcelli, I Rocha, G Rosset, C Rossetti, M Roudier, G Rowan-Robinson, M Rusholme, B Sandri, M Santos, D Sauve, A Savelainen, M Savini, G Scott, D Seiffert, MD Shellard, EPS Spencer, LD Stolyarov, V Stompor, R Sudiwala, R Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Tuovinen, J Valenziano, L Valiviita, J Van Tent, B Vibert, L Vielva, P Villa, F Wade, LA Wandelt, BD Watson, R Wehus, IK Yvon, D Zacchei, A Zonca, A AF Adam, R. Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartolo, N. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bertincourt, B. Bielewicz, P. Bock, J. J. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bucher, M. Burigana, C. Calabrese, E. Cardoso, J. -F. Catalano, A. Challinor, A. Chamballu, A. Chary, R. -R. Chiang, H. C. Christensen, P. R. Clements, D. L. Colombi, S. Colombo, L. P. L. Combet, C. Couchot, F. Coulais, A. Crill, B. P. Curto, A. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J. -M. Desert, F. -X. Diego, J. M. Dole, H. Donzelli, S. Dure, O. Douspis, M. Ducout, A. Dupac, X. Efstathiou, G. Elsner, F. Ensslin, T. A. Eriksen, H. K. Falgarone, E. Fergusson, J. Finelli, F. Forni, O. Frailis, M. Fraisse, A. A. Franceschi, E. Frejser, A. Galeotta, S. Galli, S. Ganga, K. Ghosh, T. Giard, M. Giraud-Heraudl, Y. Gjerlow, E. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gruppuso, A. Gudmundsson, J. E. Hansen, F. K. Hanson, D. Harrison, D. L. Henrot-Versille, S. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Hurier, G. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knoche, J. Kunz, M. Kurki-Suonio, H. Lagache, G. Lamarre, J. -M. Lasenby, A. Lattanzi, M. Lawrence, C. R. Le Jenne, M. Leahy, J. P. Lellouch, E. Leonardi, R. Lesgourgues, J. Levrier, F. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maggie, G. Maino', D. Mandolesi, N. Mangilli, A. Maris, M. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Matarrese, S. McGehee, P. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Moreno, R. Morgante, G. Mortlock, D. Moss, A. Mottet, S. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paoletti, D. Pasian, F. Patanchon, G. Pearson, T. J. Perdereau, O. Perotto, L. Perrotta, F. Pettorino, V. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Reinecke, M. Remazeilles, M. Renault, C. Renzi, A. Ristorcelli, I. Rocha, G. Rosset, C. Rossetti, M. Roudier, G. Rowan-Robinson, M. Rusholme, B. Sandri, M. Santos, D. Sauve, A. Savelainen, M. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Stolyarov, V. Stompor, R. Sudiwala, R. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Tucci, M. Tuovinen, J. Valenziano, L. Valiviita, J. Van Tent, B. Vibert, L. Vielva, P. Villa, F. Wade, L. A. Wandelt, B. D. Watson, R. Wehus, I. K. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2015 results VII. High Frequency Instrument data processing: Time-ordered information and beams SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: data analysis; cosmic background radiation; instrumentation: detectors ID PRE-LAUNCH STATUS AB The Planck High Frequency Instrument (HFI) has observed the full sky at six frequencies (100, 143, 217, 353, 545, and 857 GHz) in intensity and at four frequencies in linear polarization (100, 143, 217, and 353 GHz). In order to obtain sky maps, the time-ordered information (TOI) containing the detector and pointing samples must be processed and the angular response must be assessed. The full mission TOI is included in the Planck 2015 release. This paper describes the HFI TOI and beam processing for the 2015 release. HFI calibration and map making are described in a companion paper. The main pipeline has been modified since the last release (2013 nominal mission in intensity only), by including a correction for the nonlinearity of the warm readout and by improving the model of the bolometer time response. The beam processing is an essential tool that derives the angular response used in all the Planck science papers and we report an improvement in the effective beam window function uncertainty of more than a factor of 10 relative to the 2013 release. Noise correlations introduced by pipeline filtering function are assessed using dedicated simulations. Angular cross-power spectra using data sets that are decorrelated in time are immune to the main systematic effects. C1 [Bucher, M.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Giraud-Heraudl, Y.; Le Jenne, M.; Patanchon, G.; Piat, M.; Remazeilles, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, APC, CNRS IN2P3, CEA Lrfu,Observ Paris,Sorbonne Paris Cite, 10 Rue Alice Domon & Leonie, F-75205 Paris 13, France. [Kunz, M.] African Inst Math Sci, 6-8 Melrose Rd, ZA-7945 Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana, Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy. [Lagache, G.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Ashdown, M.; Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Astrophys Grp, Cavendish Lab, JJ Thomson Ave, Cambridge CB3 0HE, England. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, Westville Campus,Private Bag X54001, ZA-4000 Durban, South Africa. [Kneissl, R.] ALMA Santiago Cent Off, Atacama Large Millimeter Submillimeter Array, Alonso Cordova 3107,Vitacura,763 0355 Casilla, Santiago, Chile. [Bond, J. R.; Hanson, D.; Martin, P. G.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, 60 St George St, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Ristorcelli, I.; Sauve, A.] IRAP, CNRS, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France. [Tuovinen, J.] Trinity Coll Dublin, CRANN, Dublin, Ireland. [Bock, J. J.; Crill, B. P.; Dure, O.; Hildebrandt, S. R.; Pearson, T. J.; Prezeau, G.; Rocha, G.; Seiffert, M. D.] CALTECH, Pasadena, CA 91125 USA. [Challinor, A.; Fergusson, J.; Shellard, E. P. S.] Univ Cambridge, DAMTP, Ctr Theoret Cosmol, Wilberforce Rd, Cambridge CB3 0WA, England. [Borrill, J.; Keskitalo, R.] Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA USA. [Chamballu, A.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. [Hornstrup, A.; Linden-Vornle, M.; Norgaard-Nielsen, H. U.; Oxborrow, C. A.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark. [Kunz, M.; Tucci, M.] Univ Geneva, Dept Phys Theor, 24 Quai E Ansermet, CH-1211 Geneva 4, Switzerland. [Gonzalez-Nuevo, J.; Toffolatti, L.] Univ Oviedo, Dept Fis, Avda Calvo Sotelo S-N, Oviedo, Spain. [Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON, Canada. [Rachen, J. P.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Scott, D.] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z4, Canada. [Colombo, L. P. L.; Pierpaoli, E.] Univ Southern Calif, Dana & David Dornsife Coll Letter Arts & Sci, Dept Phys & Astron, Los Angeles, CA 90089 USA. [Benoit-Levy, A.; Elsner, F.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Huffenberger, K. M.] Florida State Univ, Dept Phys, Keen Phys Bldg,77 Chieftan Way, Tallahassee, FL 32306 USA. [Juvela, M.; Keihanen, E.; Kurki-Suonio, H.; Savelainen, M.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Dept Phys, Gustaf Hallstromin Katu 2a, Helsinki 00100, Finland. [Chiang, H. C.; Fraisse, A. A.; Gudmundsson, J. E.; Jones, W. C.; Nati, F.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Lubin, P. M.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wandelt, B. D.] Univ Illinois, Dept Phys, 1110 West Green St, Urbana, IL 61801 USA. [Bartolo, N.; Liguori, M.; Matarrese, S.] Univ Padua, Dipartimento Fis & Astron G Galilei, Via Marzolo 8, I-35131 Padua, Italy. [Burigana, C.; Lattanzi, M.; Mandolesi, N.; Natoli, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, Via Saragat 1, I-44122 Ferrara, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Pagano, L.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, Ple A Moro 2, I-00185 Rome, Italy. [Bersanelli, M.; Maino', D.; Mennella, A.; Rossetti, M.; Tomasi, M.] Univ Milan, Dipartimento Fis, Via Celoria 16, I-20122 Milan, Italy. [Renzi, A.] Univ Roma Tor Vergata, Dipartimento Matemat, Via Ric Sci 1, Rome, Italy. [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, 17 Blegdamsvej, Copenhagen, Denmark. [Kneissl, R.] European Southern Observ, ESO Vitacura, Alonso Cordova 3107,19001 Casilla, Santiago, Chile. [Dupac, X.; Leonardi, R.; Lopez-Caniego, M.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Camino Bajo Castillo S-N, Madrid 28692, Spain. [Remazeilles, M.; Tauber, J. A.] European Space Agcy, Estec, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. [Terenzi, L.] Univ E Campus, Fac Ingn, Via Isimbardi 10, I-22060 Novedrate, CO, Italy. [Matarrese, S.] Ist Nazl Fis Nucl, Gran Sasso Sci Inst, Viale F Crispi 7, I-67100 Laquila, Italy. [Pettorino, V.; Pointecouteau, E.] HGSFP, Philosophenweg 16, D-69120 Heidelberg, Germany. [Pettorino, V.; Pointecouteau, E.] Heidelberg Univ, Dept Theoret Phys, Philosophenweg 16, D-69120 Heidelberg, Germany. [Kurki-Suonio, H.; Savelainen, M.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Dept Theoret Phys, Gustaf Hallstromin Katu 2, Helsinki 00100, Finland. [de Zotti, G.] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35141 Padua, Italy. [Polenta, G.] INAF Osservatorio Astron Roma, Via Frascati 33, I-0036 Rome, Italy. [Frailis, M.; Galeotta, S.; Maggie, G.; Maris, M.; Pasian, F.; Zacchei, A.] INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34131 Trieste, Italy. [Burigana, C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Paoletti, D.; Sandri, M.; Terenzi, L.; Toffolatti, L.; Valenziano, L.; Villa, F.] INAF IASF Bologna, Via Gobetti 101, I-40147 Bologna, Italy. [Bersanelli, M.; Donzelli, S.; Maino', D.; Mennella, A.; Rossetti, M.; Tomasi, M.] INAF IASF Milano, Via E Bassini 15, I-20133 Milan, Italy. [Burigana, C.; Finelli, F.; Paoletti, D.] Ist Nazl Fis Nucl, Sez Bologna, Via Irnerio 46, I-40126 Bologna, Italy. [Melchiorri, A.; Pagano, L.] Univ Roma Sapienza, Sez Roma 1, Ist Nazl Fis Nucl, Piazzale Aldo Moro 2, I-00185 Rome, Italy. [Renzi, A.] Univ Roma Tor Vergata, Sez Roma 2, Ist Nazl Fis Nucl, Via Ric Sci 1, Rome, Italy. [Desert, F. -X.] Univ Grenoble Alpes, IPAG, CNRS, F-38000 Grenoble, France. [Mitra, S.] IUCAA, Post Bag 4,Pune Univ Campus, Pune 411007, Maharashtra, India. [Clements, D. L.; Ducout, A.; Jaffe, A. H.; Mortlock, D.; Rowan-Robinson, M.] Imperial Coll London, Astrophys Grp, Blackett Lab, Prince Consort Rd, London SW7 2AZ, England. [Chary, R. -R.; McGehee, P.; Pearson, T. J.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Benoit, A.] Univ Joseph Fourier Grenoble I, Inst Neel, CNRS, 25 Rue Martyrs, F-38042 Grenoble, France. [Dole, H.] Inst Univ France, 103 Bd St Michel, F-75005 Paris, France. [Aghanim, N.; Aumont, J.; Bertincourt, B.; Boulanger, F.; Chamballu, A.; Dole, H.; Douspis, M.; Ghosh, T.; Hurier, G.; Kunz, M.; Lagache, G.; Mangilli, A.; Miville-Deschenes, M. -A.; Pajot, F.; Puget, J. -L.; Remazeilles, M.; Vibert, L.] Univ Paris Sud 11, CNRS, Inst Astrophys Spatiale, UMR 8617, Batiment 121, F-91400 Orsay, France. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Ducout, A.; Elsner, F.; Hivon, E.; Moneti, A.; Mottet, S.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] Inst Astrophys Paris, CNRS, UMR 7095, 98 Bis Blvd Arago, F-75014 Paris, France. [Lesgourgues, J.] Rhein Westfal TH Aachen, Inst Theoret Teilchenphys & Kosmol, D-52056 Aachen, Germany. [Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D. L.; Migliaccio, M.; Sutton, D.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Eriksen, H. K.; Gjerlow, E.; Hansen, F. K.; Lilje, P. B.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway. [Barreiro, R. B.; Bonavera, L.; Curto, A.; Diego, J. M.; Gonzalez-Nuevo, J.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Toffolatti, L.; Vielva, P.] Univ Cantabria, Inst Fis Cantabria, CSIC, Avda Castros S-N, E-39005 Santander, Spain. [Bartolo, N.; Liguori, M.; Matarrese, S.] Ist Nazl Fis Nucl, Sez Padova, Via Marzolo 8, I-35131 Padua, Italy. [Bock, J. J.; Colombo, L. P. L.; Crill, B. P.; Dure, O.; Gorski, K. M.; Hanson, D.; Hildebrandt, S. R.; Holmes, W. A.; Lawrence, C. R.; Mitra, S.; Pietrobon, D.; Prezeau, G.; Rocha, G.; Roudier, G.; Seiffert, M. D.; Wade, L. A.; Wehus, I. K.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA. [Davies, R. D.; Davis, R. J.; Leahy, J. P.; Noviello, F.; Watson, R.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England. [Galli, S.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Ashdown, M.; Challinor, A.; Curto, A.; Gratton, S.; Harrison, D. L.; Lasenby, A.; Migliaccio, M.; Stolyarov, V.; Sutton, D.] Kavli Inst Cosmol Cambridge, Madingley Rd, Cambridge CB3 0HA, England. [Couchot, F.; Henrot-Versille, S.; Mangilli, A.; Moreno, R.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, LAL, CNRS IN2P3, F-91400 Orsay, France. [Catalano, A.; Coulais, A.; Falgarone, E.; Lamarre, J. -M.; Levrier, F.; Roudier, G.] CNRS, LERMA, 61 Ave Observ, F-75014 Paris, France. [Lellouch, E.; Moreno, R.] Univ Paris Diderot, CNRS, LESIA, Observ Paris, 5 Pl J Janssen, F-92195 Meudon, France. [Arnaud, M.; Chamballu, A.; Pratt, G. W.] Univ Paris Diderot, Lab AIM, IRFU Serv Astrophys, CEA DSM,CNRS,CEA Saclay, Bat 709, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, Lab Traitement & Commun Informat, UMR 5141, 46 Rue Barrault, F-75634 Paris 13, France. [Adam, R.; Catalano, A.; Combet, C.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble Alpes, CNRS IN2P3, Lab Phys Subat & Cosmol, 53 Rue Martyrs, F-38026 Grenoble, France. [Van Tent, B.] Univ Paris Sud 11, Lab Phys Theor, Batiment 210, F-91405 Orsay, France. [Van Tent, B.] CNRS, Batiment 210, F-91405 Orsay, France. [Kisner, T. S.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Novikov, D.; Novikov, I.] Russian Acad Sci, Lebedev Phys Inst, Ctr Astro Space, 84-32 Profsoyuznaya St,GSP 7, Moscow 117997, Russia. [Ensslin, T. A.; Hovest, W.; Knoche, J.; Rachen, J. P.; Reinecke, M.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. [Hanson, D.] McGill Univ, McGill Phys, Ernest Rutherford Phys Bldg,3600 Rue Univ, Montreal, PQ H3A 2T8, Canada. [Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Bielewicz, P.] Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland. [Christensen, P. R.; Frejser, A.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, Blegdamsvej 17, DK-2100 Copenhagen, Denmark. [Savini, G.] UCL, Opt Sci Lab, Gower St, London WC1E 6BT, England. [Baccigalupi, C.; Bielewicz, P.; Danese, L.; de Zotti, G.; Paci, F.; Perrotta, F.] SISSA, Astrophys Sect, Via Bonomea 265, I-34136 Trieste, Italy. [Ade, P. A. R.; Munshi, D.; Spencer, L. D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, Wales. [Moss, A.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Bouchet, F. R.] Sorbonne Univ UPMC, UMR 7095, Inst Astrophys Paris, 98 Bis Blvd Arago, F-75014 Paris, France. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Karachai Cherkessian Rep 369167, Zelenchukskiy R, Russia. [Calabrese, E.] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England. [Lesgourgues, J.] CERN, Div Theory, PH TH, CH-1211 Geneva 23, Switzerland. [Benabed, K.; Benoit-Levy, A.; Colombi, S.; Delouis, J. -M.; Elsner, F.; Hivon, E.; Prunet, S.; Wandelt, B. D.] UPMC Univ Paris 06, UMR 7095, 98 Bis Blvd Arago, F-75014 Paris, France. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.; Sauve, A.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, E-18071 Granada, Spain. [Battaner, E.] Univ Granada, Inst Carlos Fis Teor & Computac 1, Granada 18071, Spain. [Gorski, K. M.] Univ Warsaw Observ, Aleje Ujazdowskie 4, PL-00478 Warsaw, Poland. RP Crill, BP (reprint author), CALTECH, Pasadena, CA 91125 USA.; Desert, FX (reprint author), Univ Grenoble Alpes, IPAG, CNRS, F-38000 Grenoble, France.; Crill, BP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA. EM bcrill@jpl.nasa.gov; francois-xavier.desert@obs.ujf-grenoble.fr RI Gonzalez-Nuevo, Joaquin/I-3562-2014; Herranz, Diego/K-9143-2014; Colombo, Loris/J-2415-2016; Barreiro, Rita Belen/N-5442-2014; bonavera, laura/E-9368-2017 OI Toffolatti, Luigi/0000-0003-2645-7386; Lilje, Per/0000-0003-4324-7794; Nati, Federico/0000-0002-8307-5088; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Herranz, Diego/0000-0003-4540-1417; Colombo, Loris/0000-0003-4572-7732; Villa, Fabrizio/0000-0003-1798-861X; Zacchei, Andrea/0000-0003-0396-1192; Stolyarov, Vladislav/0000-0001-8151-828X; Watson, Robert/0000-0002-5873-0124; Paoletti, Daniela/0000-0003-4761-6147; TERENZI, LUCA/0000-0001-9915-6379; Valiviita, Jussi/0000-0001-6225-3693; Barreiro, Rita Belen/0000-0002-6139-4272; bonavera, laura/0000-0001-8039-3876 FU ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MINECO (Spain); JA (Spain); RES (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC (EU); PRACE (EU) 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, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (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.cosmos.esa.int/web/planck/planck-collaboration. NR 53 TC 0 Z9 0 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 OCT PY 2016 VL 594 AR A7 DI 10.1051/0004-6361/201525844 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4MG UT WOS:000385832200017 ER PT J AU Adam, R Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartolo, N Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bertincourt, B Bielewicz, P Bock, JJ Bonavera, L Bond, JR Borrill, J Bouchet, FR Boulanger, F Bucher, M Burigana, C Calabrese, E Cardoso, JF Catalano, A Challinor, A Chamballu, A Chiang, HC Christensen, PR Clements, DL Colombi, S Colombo, LPL Combet, C Couchot, F Coulais, A Crill, BP Curto, A Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Diego, JM Dole, H Donzelli, S Dore, O Douspis, M Ducout, A Dupac, X Efstathiou, G Elsner, F Ensslin, TA Eriksen, HK Falgarone, E Fergusson, J Finelli, F Forni, O Frailis, M Fraisse, AA Franceschi, E Frejsel, A Galeotta, S Galli, S Ganga, K Ghosh, T Giard, M Giraud-Heraud, Y Gjerlow, E Gonzalez-Nuevo, J Gorski, KM Gratton, S Gruppuso, A Gudmundsson, JE Hansen, FK Hanson, D Harrison, DL Henrot-Versille, S Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Hurier, G Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knoche, J Kunz, M Kurki-Suonio, H Lagache, G Lamarre, JM Lasenby, A Lattanzi, M Lawrence, CR Le Jeune, M Leahy, JP Lellouch, E Leonardi, R Lesgourgues, J Levrier, F Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maggio, G Maino, D Mandolesi, N Mangilli, A Maris, M Martin, PG Martinez-Gonzalez, E Masi, S Matarrese, S McGehee, P Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Moreno, R Morgante, G Mortlock, D Moss, A Mottet, S Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Oxborrow, CA Paci, F Pagano, L Pajot, F Paoletti, D Pasian, F Patanchon, G Pearson, TJ Perdereau, O Perotto, L Perrotta, F Pettorino, V Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Reinecke, M Remazeilles, M Renault, C Renzi, A Ristorcelli, I Rocha, G Rosset, C Rossetti, M Roudier, G Rusholme, B Sandri, M Santos, D Sauve, A Savelainen, M Savini, G Scott, D Seiffert, MD Shellard, EPS Spencer, LD Stolyarov, V Stompor, R Sudiwala, R Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Tuovinen, J Valenziano, L Valiviita, J Van Tent, B Vibert, L Vielva, P Villa, F Wade, LA Wandelt, BD Watson, R Wehus, IK Yvon, D Zacchei, A Zonca, A AF Adam, R. Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartolo, N. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bertincourt, B. Bielewicz, P. Bock, J. J. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bucher, M. Burigana, C. Calabrese, E. Cardoso, J. -F. Catalano, A. Challinor, A. Chamballu, A. Chiang, H. C. Christensen, P. R. Clements, D. L. Colombi, S. Colombo, L. P. L. Combet, C. Couchot, F. Coulais, A. Crill, B. P. Curto, A. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J. -M. Desert, F. -X. Diego, J. M. Dole, H. Donzelli, S. Dore, O. Douspis, M. Ducout, A. Dupac, X. Efstathiou, G. Elsner, F. Ensslin, T. A. Eriksen, H. K. Falgarone, E. Fergusson, J. Finelli, F. Forni, O. Frailis, M. Fraisse, A. A. Franceschi, E. Frejsel, A. Galeotta, S. Galli, S. Ganga, K. Ghosh, T. Giard, M. Giraud-Heraud, Y. Gjerlow, E. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gruppuso, A. Gudmundsson, J. E. Hansen, F. K. Hanson, D. Harrison, D. L. Henrot-Versille, S. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Hurier, G. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knoche, J. Kunz, M. Kurki-Suonio, H. Lagache, G. Lamarre, J. -M. Lasenby, A. Lattanzi, M. Lawrence, C. R. Le Jeune, M. Leahy, J. P. Lellouch, E. Leonardi, R. Lesgourgues, J. Levrier, F. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maggio, G. Maino, D. Mandolesi, N. Mangilli, A. Maris, M. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Matarrese, S. McGehee, P. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Moreno, R. Morgante, G. Mortlock, D. Moss, A. Mottet, S. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paoletti, D. Pasian, F. Patanchon, G. Pearson, T. J. Perdereau, O. Perotto, L. Perrotta, F. Pettorino, V. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Reinecke, M. Remazeilles, M. Renault, C. Renzi, A. Ristorcelli, I. Rocha, G. Rosset, C. Rossetti, M. Roudier, G. Rusholme, B. Sandri, M. Santos, D. Sauve, A. Savelainen, M. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Stolyarov, V. Stompor, R. Sudiwala, R. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Tucci, M. Tuovinen, J. Valenziano, L. Valiviita, J. Van Tent, B. Vibert, L. Vielva, P. Villa, F. Wade, L. A. Wandelt, B. D. Watson, R. Wehus, I. K. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2015 results VIII. High Frequency Instrument data processing: Calibration and maps SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology: observations; cosmic background radiation; surveys; methods: data analysis ID PRE-LAUNCH STATUS; MICROWAVE; POLARIZATION; MODEL AB This paper describes the processing applied to the cleaned, time-ordered information obtained from the Planck High Frequency Instrument (HFI) with the aim of producing photometrically calibrated maps in temperature and (for the first time) in polarization. The data from the entire 2.5-year HFI mission include almost five full-sky surveys. HFI observes the sky over a broad range of frequencies, from 100 to 857 GHz. To obtain the best accuracy on the calibration over such a large range, two different photometric calibration schemes have been used. The 545 and 857 GHz data are calibrated using models of planetary atmospheric emission. The lower frequencies (from 100 to 353 GHz) are calibrated using the time-variable cosmological microwave background dipole, which we call the orbital dipole. This source of calibration only depends on the satellite velocity with respect to the solar system. Using a CMB temperature of T-CMB = 2.7255 +/- 0.0006 K, it permits an independent measurement of the amplitude of the CMB solar dipole (3364.3 +/- 1.5 mu K), which is approximatively 1 sigma higher than the WMAP measurement with a direction that is consistent between the two experiments. We describe the pipeline used to produce the maps of intensity and linear polarization from the HFI timelines, and the scheme used to set the zero level of the maps a posteriori. We also summarize the noise characteristics of the HFI maps in the 2015 Planck data release and present some null tests to assess their quality. Finally, we discuss the major systematic effects and in particular the leakage induced by flux mismatch between the detectors that leads to spurious polarization signal. C1 [Bucher, M.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Le Jeune, M.; Patanchon, G.; Piat, M.; Remazeilles, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, Sorbonne Paris Cite, AstroParticule & Cosmol, APC,CNRS IN2P3,CEA Irfu,Observ Paris, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France. [Kunz, M.] African Inst Math Sci, 6-8 Melrose Rd, ZA-7945 Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana, Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy. [Lagache, G.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Ashdown, M.; Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Astrophys Grp, Cavendish Lab, JJ Thomson Ave, Cambridge CB3 0HE, England. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, Westville Campus,Private Bag X54001, ZA-4000 Durban, South Africa. [Kneissl, R.] ALMA Santiago Cent Off, Atacama Large Millimeter submillimeter Array, Alonso Cordova 3107, Santiago 7630355, Chile. [Bond, J. R.; Hanson, D.; Martin, P. G.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, 60 St George St, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.; Sauve, A.] CNRS, IRAP, 9 Av Colonel Roche,BP 44346, F-31028 Toulouse 4, France. [Tuovinen, J.] Trinity Coll Dublin, CRANN, Dublin 2, Ireland. [Bock, J. J.; 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.; Fergusson, J.; Shellard, E. P. S.] Univ Cambridge, DAMTP, Ctr Theoret Cosmol, Wilberforce Rd, Cambridge CB3 0WA, England. 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EM perdereau@lal.in2p3.fr; tristram@lal.in2p3.fr RI Barreiro, Rita Belen/N-5442-2014; bonavera, laura/E-9368-2017; Gonzalez-Nuevo, Joaquin/I-3562-2014; Herranz, Diego/K-9143-2014; Colombo, Loris/J-2415-2016; OI Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Nati, Federico/0000-0002-8307-5088; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Barreiro, Rita Belen/0000-0002-6139-4272; bonavera, laura/0000-0001-8039-3876; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Herranz, Diego/0000-0003-4540-1417; Colombo, Loris/0000-0003-4572-7732; Zacchei, Andrea/0000-0003-0396-1192; Stolyarov, Vladislav/0000-0001-8151-828X; TERENZI, LUCA/0000-0001-9915-6379; Valiviita, Jussi/0000-0001-6225-3693; Hurier, Guillaume/0000-0002-1215-0706; Hivon, Eric/0000-0003-1880-2733; Toffolatti, Luigi/0000-0003-2645-7386 FU ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MINECO (Spain); JA (Spain); RES (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC (EU); PRACE (EU) 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, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (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.cosmos.esa.int/web/planck/planck-collaboration. NR 52 TC 3 Z9 3 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2016 VL 594 AR A8 DI 10.1051/0004-6361/201525820 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4MG UT WOS:000385832200008 ER PT J AU Adam, R Ade, PAR Aghanim, N Alves, MIR Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartlett, JG Bartolo, N Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bock, JJ Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Boulanger, F Bucher, M Burigana, C Butler, RC Calabrese, E Cardoso, JF Catalano, A Challinor, A Chamballu, A Chary, RR Chiang, HC Christensen, PR Clements, DL Colombi, S Colombo, LPL Combet, C Couchot, F Coulais, A Crill, BP Curto, A Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Desert, FX Dickinson, C Diego, JM Dole, H Donzelli, S Dore, O Douspis, M Ducout, A Dupac, X Efstathiou, G Elsner, F Ensslin, TA Eriksen, HK Falgarone, E Fergusson, J Finelli, F Forni, O Frailis, M Fraisse, AA Franceschi, E Frejsel, A Galeotta, S Galli, S Ganga, K Ghosh, T Giard, M Giraud-Heraud, Y Gjerlow, E Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Gudmundsson, JE Hansen, FK Hanson, D Harrison, DL Helou, G Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, F Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Hurier, G Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihaen, E Keskitalo, R Kisner, TS Kneissl, R Knoche, J Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Lattanzi, M Lawrence, CR Le Jeune, M Leahy, JP Leonardi, R Lesgourgues, J Levrier, F Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maggio, G Maino, D Mandolesi, N Mangilli, A Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Matarrese, S McGehee, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Moss, A Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Orlando, E Oxborrow, CA Paci, F Pagano, L Pajot, F Paladini, R Paoletti, D Partridge, B Pasian, F Patanchon, G Pearson, TJ Perdereau, O Perotto, L Perrotta, F Pettorino, V Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Reach, WT Rebolo, R Reinecke, M Remazeilles, M Renault, C Renzi, A Ristorcelli, I Rocha, G Rosset, C Rossetti, M Roudier, G Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savelainen, M Savini, G Scott, D Seiffert, MD Shellard, EPS Spencer, LD Stolyarov, V Stompor, R Strong, AW Sudiwala, R Sunyaev, R Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Tuovinen, J Umana, G Valenziano, L Valiviita, J Van Tent, F Vielva, P Villa, F Wade, LA Wandelt, BD Wehus, IK Wilkinson, A Yvon, D Zacchei, A Zonca, A AF Adam, R. Ade, P. A. R. Aghanim, N. Alves, M. I. R. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Bartolo, N. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bock, J. J. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bucher, M. Burigana, C. Butler, R. C. Calabrese, E. Cardoso, J. -F. Catalano, A. Challinor, A. Chamballu, A. Chary, R. -R. Chiang, H. C. Christensen, P. R. Clements, D. L. Colombi, S. Colombo, L. P. L. Combet, C. Couchot, F. Coulais, A. Crill, B. P. Curto, A. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Desert, F. -X. Dickinson, C. Diego, J. M. Dole, H. Donzelli, S. Dore, O. Douspis, M. Ducout, A. Dupac, X. Efstathiou, G. Elsner, F. Ensslin, T. A. Eriksen, H. K. Falgarone, E. Fergusson, J. Finelli, F. Forni, O. Frailis, M. Fraisse, A. A. Franceschi, E. Frejsel, A. Galeotta, S. Galli, S. Ganga, K. Ghosh, T. Giard, M. Giraud-Heraud, Y. Gjerlow, E. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Gudmundsson, J. E. Hansen, F. K. Hanson, D. Harrison, D. L. Helou, G. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, F. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Hurier, G. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knoche, J. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Lattanzi, M. Lawrence, C. R. Le Jeune, M. Leahy, J. P. Leonardi, R. Lesgourgues, J. Levrier, F. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maggio, G. Maino, D. Mandolesi, N. Mangilli, A. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Matarrese, S. McGehee, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Moss, A. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Orlando, E. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paladini, R. Paoletti, D. Partridge, B. Pasian, F. Patanchon, G. Pearson, T. J. Perdereau, O. Perotto, L. Perrotta, F. Pettorino, V. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Reach, W. T. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Renzi, A. Ristorcelli, I. Rocha, G. Rosset, C. Rossetti, M. Roudier, G. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savelainen, M. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Stolyarov, V. Stompor, R. Strong, A. W. Sudiwala, R. Sunyaev, R. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Tucci, M. Tuovinen, J. Umana, G. Valenziano, L. Valiviita, J. Van Tent, F. Vielva, P. Villa, F. Wade, L. A. Wandelt, B. D. Wehus, I. K. Wilkinson, A. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2015 results X. Diffuse component separation: Foreground maps SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: general; cosmology: observations; polarization; cosmic background radiation; diffuse radiation; Galaxy: general ID MICROWAVE-ANISOTROPY-PROBE; POWER SPECTRUM ESTIMATION; COSMIC-RAY PROPAGATION; LATITUDE MOLECULAR GAS; WMAP OBSERVATIONS; GALACTIC PLANE; BACKGROUND-RADIATION; DUST EMISSION; DATA RELEASE; MILKY-WAY AB Planck has mapped the microwave sky in temperature over nine frequency bands between 30 and 857 GHz and in polarization over seven frequency bands between 30 and 353 GHz in polarization. In this paper we consider the problem of diffuse astrophysical component separation, and process these maps within a Bayesian framework to derive an internally consistent set of full-sky astrophysical component maps. Component separation dedicated to cosmic microwave background (CMB) reconstruction is described in a companion paper. For the temperature analysis, we combine the Planck observations with the 9-yr Wilkinson Microwave Anisotropy Probe (WMAP) sky maps and the Haslam et al. 408 MHz map, to derive a joint model of CMB, synchrotron, free-free, spinning dust, CO, line emission in the 94 and 100 GHz channels, and thermal dust emission. Full-sky maps are provided for each component, with an angular resolution varying between 7: 5 and 1 degrees. Global parameters (monopoles, dipoles, relative calibration, and bandpass errors) are fitted jointly with the sky model, and best-fit values are tabulated. For polarization, the model includes CMB, synchrotron, and thermal dust emission. These models provide excellent fits to the observed data, with rms temperature residuals smaller than 4pK over 93% of the sky for all Planck frequencies up to 353 GHz, and fractional errors smaller than 1% in the remaining 7% of the sky. The main limitations of the temperature model at the lower frequencies are internal degeneracies among the spinning dust, free-free, and synchrotron components; additional observations from external low-frequency experiments will be essential to break these degeneracies. The main limitations of the temperature model at the higher frequencies are uncertainties in the 545 and 857 GHz calibration and zero-points. For polarization, the main outstanding issues are instrumental systematics in the 100-353 GHz bands on large angular scales in the form of temperature-to-polarization leakage, uncertainties in the analogue-to-digital conversion, and corrections for the very long time constant of the bolometer detectors, all of which are expected to improve in the near future. C1 [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Le Jeune, M.; Patanchon, G.; Piat, M.; Remazeilles, M.; Rosset, C.; Stompor, R.] Univ Paris Diderot, CEA Irfu, CNRS IN2P3, APC,AstroParticule & Cosrnol,Sorbonne Paris Cite, 10 Rue Alice Domori & Leonia Duqutet, F-75205 Paris 13, France. [Lahteenmaki, A.] Aalto Univ, Metsahovi Radio Observ, POB 13000, Aalto 00076, Finland. [Lahteenmaki, A.] Dept Radio Sci & Engn, POB 13000, Aalto 00076, Finland. [Kunz, M.] African Inst Math Sci, 6-8 Melrose Rd, ZA-7945 Cape Town, South Africa. 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M.] Univ Warsaw Observ, Aleje Ujazdowskie 4, PL-00478 Warsaw, Poland. RP Wehus, IK (reprint author), Inst Astrofis Canarias, C Via Lactea S-N, Tenerife 38205, Spain.; Wehus, IK (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 31109 USA. EM i.k.wehus@astro.uio.no RI Lahteenmaki, Anne/L-5987-2013; Barreiro, Rita Belen/N-5442-2014; bonavera, laura/E-9368-2017; Gonzalez-Nuevo, Joaquin/I-3562-2014; Herranz, Diego/K-9143-2014; Colombo, Loris/J-2415-2016; OI Valiviita, Jussi/0000-0001-6225-3693; Toffolatti, Luigi/0000-0003-2645-7386; Lilje, Per/0000-0003-4324-7794; Nati, Federico/0000-0002-8307-5088; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Barreiro, Rita Belen/0000-0002-6139-4272; bonavera, laura/0000-0001-8039-3876; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Herranz, Diego/0000-0003-4540-1417; Colombo, Loris/0000-0003-4572-7732; Zacchei, Andrea/0000-0003-0396-1192; Stolyarov, Vladislav/0000-0001-8151-828X; Paoletti, Daniela/0000-0003-4761-6147; TERENZI, LUCA/0000-0001-9915-6379; Reach, William/0000-0001-8362-4094 FU ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MINECO (Spain); JA (Spain); RES (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC (EU); PRACE (EU) 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, MINECO, JA and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (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.cosmos.esa.int/web/planck/planck-collaboration. NR 126 TC 3 Z9 3 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2016 VL 594 AR A10 DI 10.1051/0004-6361/201525967 PG 63 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4MG UT WOS:000385832200021 ER PT J AU Adam, R Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartlett, JG Bartolo, N Basak, S Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bock, JJ Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Boulanger, F Bucher, M Burigana, C Butler, RC Calabrese, E Cardoso, JF Casaponsa, B Castex, G Catalano, A Challinor, A Chamballu, A Chary, RR Chiang, HC Christensen, PR Clements, DL Colombi, S Colombo, LPL Combet, C Couchot, F Coulais, A Crill, BP Curto, A Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Desert, FX Dickinson, C Diego, JM Dole, H Donzelli, S Dore, O Douspis, M Ducout, A Dupac, X Efstathiou, G Elsner, F Ensslin, TA Eriksen, HK Falgarone, E Fantaye, Y Fergusson, J Finelli, F Forni, O Frailis, M Fraisse, AA Francescht, E Frejsel, A Galeotta, S Galli, S Ganga, K Ghosh, T Giard, M Giraud-Heraud, Y Gjerlow, E Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Gudmundsson, JE Hansen, FK Hanson, D Harrison, DL Helou, G Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Hurier, G Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knoche, J Krachmalnicoff, N Kunz, M Kurki-Suonio, H Lagache, G Lamarre, JM Lasenby, A Lattanzi, M Lawrence, CR Le Jenne, M Leonardi, R Lesgourgues, J Levrier, F Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maggio, G Maino, D Mandolesi, N Mangilli, A Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Matarrese, S McGehee, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Miville-Deschenes, MA Molinari, D Moneti, A Montier, L Morgante, G Mortlock, D Moss, A Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Oxborrow, CA Paci, F Pagano, L Pajot, F Paladini, R Paoletti, D Pasian, F Patanchon, G Pearson, TJ Perdereau, O Perotto, L Perrotta, F Pettorino, V Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Racine, B Reach, WT Rebolo, R Reinecke, M Remazeilles, M Renault, C Renzi, A Ristorcelli, I Rocha, G Rosset, C Rossetti, M Roudier, G Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savelainen, M Savini, G Scott, D Seiffert, MD Shellard, EPS Spencer, LD Stolyarov, V Stompor, R Sudiwala, R Sunyaev, R Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Tristram, M Trombetti, T Tucci, M Tuovinen, J Valenziano, L Valiviita, J Van Tent, F Vielva, P Villa, F Wade, LA Wandelt, BD Wehus, IK Yvon, D Zacchei, A Zonca, A AF Adam, R. Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Bartolo, N. Basak, S. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bock, J. J. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bucher, M. Burigana, C. Butler, R. C. Calabrese, E. Cardoso, J. -F. Casaponsa, B. Castex, G. Catalano, A. Challinor, A. Chamballu, A. Chary, R-R. Chiang, H. C. Christensen, P. R. Clements, D. L. Colombi, S. Colombo, L. P. L. Combet, C. Couchot, F. Coulais, A. Crill, B. P. Curto, A. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Desert, F. -X. Dickinson, C. Diego, J. M. Dole, H. Donzelli, S. Dore, O. Douspis, M. Ducout, A. Dupac, X. Efstathiou, G. Elsner, F. Ensslin, T. A. Eriksen, H. K. Falgarone, E. Fantaye, Y. Fergusson, J. Finelli, F. Forni, O. Frailis, M. Fraisse, A. A. Francescht, E. Frejsel, A. Galeotta, S. Galli, S. Ganga, K. Ghosh, T. Giard, M. Giraud-Heraud, Y. Gjerlow, E. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Gudmundsson, J. E. Hansen, F. K. Hanson, D. Harrison, D. L. Helou, G. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Hurier, G. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knoche, J. Krachmalnicoff, N. Kunz, M. Kurki-Suonio, H. Lagache, G. Lamarre, J. -M. Lasenby, A. Lattanzi, M. Lawrence, C. R. Le Jenne, M. Leonardi, R. Lesgourgues, J. Levrier, F. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maggio, G. Maino, D. Mandolesi, N. Mangilli, A. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Matarrese, S. McGehee, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Miville-Deschenes, M. -A. Molinari, D. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Moss, A. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paladini, R. Paoletti, D. Pasian, F. Patanchon, G. Pearson, T. J. Perdereau, O. Perotto, L. Perrotta, F. Pettorino, V. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Racine, B. Reach, W. T. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Renzi, A. Ristorcelli, I. Rocha, G. Rosset, C. Rossetti, M. Roudier, G. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savelainen, M. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Stolyarov, V. Stompor, R. Sudiwala, R. Sunyaev, R. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Trombetti, T. Tucci, M. Tuovinen, J. Valenziano, L. Valiviita, J. Van Tent, F. Vielva, P. Villa, F. Wade, L. A. Wandelt, B. D. Wehus, I. K. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2015 results IX. Diffuse component separation: CMB maps SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology: observations; polarization; cosmic background radiation; diffuse radiation ID PROBE WMAP OBSERVATIONS; POWER SPECTRUM ESTIMATION; POLARIZATION DATA; SKY MAPS; FULL-SKY; MICROWAVE; PLANCK; PARAMETERS; VARIANCE; TEMPLATE AB We present foreground-reduced cosmic microwave background (CMB) maps derived from the full Planck data set in both temperature and polarization. Compared to the corresponding Planck 2013 temperature sky maps, the total data volume is larger by a factor of 3.2 for frequencies between 30 and 70 GHz, and by 1.9 for frequencies between 100 and 857 GHz. In addition, systematic errors in the forms of temperature-topolarization leakage, analogue-to-digital conversion uncertainties, and very long time constant errors have been dramatically reduced, to the extent that the cosmological polarization signal may now be robustly recovered on angular scales l greater than or similar to 40. On the very largest scales, instrumental systematic residuals are still non-negligible compared to the expected cosmological signal, and modes with l < 20 are accordingly suppressed in the current polarization maps by high-pass filtering. As in 2013, four different CMB component separation algorithms are applied to these observations, providing a measure of stability with respect to algorithmic and modelling choices. The resulting polarization maps have rms instrumental noise ranging between 0.21 and 0.27 mu K averaged over 55' pixels, and between 4.5 and 6.1 mu K averaged over 3.'4 pixels. The cosmological parameters derived from the analysis of temperature power spectra are in agreement at the 1 sigma level with the Planck 2015 likelihood. Unresolved mismatches between the noise properties of the data and simulations prevent a satisfactory description of the higher-order statistical properties of the polarization maps. Thus, the primary applications of these polarization maps are those that do not require massive simulations for accurate estimation of uncertainties, for instance estimation of cross-spectra and cross-correlations, or stacking analyses. However, the amplitude of primordial non-Gaussianity is consistent with zero within 2 sigma for all local, equilateral, and orthogonal configurations of the bispectrum, including for polarization E-modes. Moreover, excellent agreement is found regarding the lensing B-mode power spectrum, both internally among the various component separation codes and with the best-fit Planck 2015 Lambda cold dark matter model. 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[Adam, R.; Catalano, A.; Combet, C.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble Alpes, Lab Phys Subat & Cosmol, CNRS IN2P3, 53 Rue Martyrs, F-38026 Grenoble, France. [Van Tent, F.] Univ Paris Sud 11, Lab Phys Theor, Batiment 210, F-91405 Orsay, France. [Van Tent, F.] CNRS, Batiment 210, F-91405 Orsay, France. [Kisner, T. S.] Lawrence Berkeley Natl Lab, Berkeley, CA USA. [Novikov, D.; Novikov, I.] Russian Acad Sci, Lebedev Phys Inst, Ctr Astro Space, 84-32 Profsoyuznaya St, Moscow 117997, Russia. [Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Knoche, J.; Rachen, J. P.; Reinecke, M.; Sunyaev, R.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. [Hanson, D.] McGill Univ, McGill Phys, Ernest Rutherford Phys Bldg,3600 Rue Univ, Montreal, PQ H3A 2T8, Canada. [Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Bielewicz, P.] Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland. [Christensen, P. R.; Frejsel, A.; Novikov, I.] Niels Bohr Inst, Blegdamsvej 17, DK-1165 Copenhagen, Denmark. [Naselsky, P.] Univ Copenhagen, Niels Bohr Inst, Blegdamsvej 17, DK-1165 Copenhagen, Denmark. [Gudmundsson, J. E.] Nordita Nord Inst Theoret Phys, Roslagstullsbacken 23, S-10691 Stockholm, Sweden. [Savini, G.] UCL, Opt Sci Lab, Gower St, London, England. [Baccigalupi, C.; Basak, S.; Bielewicz, P.; Danese, L.; de Zotti, G.; Paci, F.; Perrotta, F.] SISSA, Astrophys Sect, Via Bonomea 265, I-34136 Trieste, Italy. [Terenzi, L.] Univ E Campus, SMARTEST Res Ctr, Via Isimbardi 10, I-22060 Novedrate, CO, Italy. [Ade, P. A. R.; Munshi, D.; Spencer, L. D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales. [Moss, A.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Bouchet, F. R.] Sorbonne Univ UPMC, Inst Astrophys Paris, UMR 7095, 98bis Blvd Arago, F-75014 Paris, France. [Sunyaev, R.] Russian Acad Sci, Space Res Inst IKI, Profsoyuznaya Str 84-32, Moscow 117997, Russia. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Karachai Cherkessian Rep 369167, Zelenchukskiy R, Russia. [Calabrese, E.] Univ Oxford, Subdept Astrophys, Keble Rd, Oxford OX1 3RH, England. [Gudmundsson, J. E.] Stockholm Univ, Dept Phys, Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, S-10691 Stockholm, Sweden. [Lesgourgues, J.] CERN, PH TH, Div Theory, CH-1211 Geneva 23, Switzerland. [Benabed, K.; Benoit-Levy, A.; Colombi, S.; Elsner, F.; Hivon, E.; Prunet, S.; Wandelt, B. D.] UPMC Univ Paris 06, UMR 7095, 98bis Blvd Arago, F-75014 Paris, France. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Jaffe, T. R.; 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, MS 232-11, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Dept Fis Teer & Cosmos, Fac Ciencias, E-18071 Granada, Spain. [Battaner, E.] Univ Granada, Inst Carlos Fis Teor & Computac 1, Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, Aleje Ujazdowskie 4, PL-00478 Warsaw, Poland. RP Ashdown, M (reprint author), Univ Cambridge, Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England.; Ashdown, M (reprint author), Kavli Inst Cosmol Cambridge, Madingley Rd, Cambridge CB3 0HA, England. EM maja1@mrao.cam.acuk RI Barreiro, Rita Belen/N-5442-2014; bonavera, laura/E-9368-2017; Gonzalez-Nuevo, Joaquin/I-3562-2014; Herranz, Diego/K-9143-2014; Colombo, Loris/J-2415-2016; OI Barreiro, Rita Belen/0000-0002-6139-4272; bonavera, laura/0000-0001-8039-3876; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Herranz, Diego/0000-0003-4540-1417; Colombo, Loris/0000-0003-4572-7732; Zacchei, Andrea/0000-0003-0396-1192; Stolyarov, Vladislav/0000-0001-8151-828X; TERENZI, LUCA/0000-0001-9915-6379; Reach, William/0000-0001-8362-4094; Valiviita, Jussi/0000-0001-6225-3693; Hurier, Guillaume/0000-0002-1215-0706; Piacentini, Francesco/0000-0002-5444-9327; Molinari, Diego/0000-0002-7799-3915; Toffolatti, Luigi/0000-0003-2645-7386; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Nati, Federico/0000-0002-8307-5088; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993 FU ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MINECO (Spain); JA (Spain); RES (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC (EU); PRACE (EU) 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, MINECO, JA and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (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.cosmos.esa.int/web/planck/planck-collaboration. Some of the results in this paper have been derived using the HEALPix package. NR 64 TC 5 Z9 5 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2016 VL 594 AR A9 DI 10.1051/0004-6361/201525936 PG 42 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4MG UT WOS:000385832200019 ER PT J AU Adam, R Ade, PAR Aghanim, N Akrami, Y Alves, MIR Argueso, F Arnaud, M Arroja, F Ashdown, M Aumont, J Baccigalupi, C Ballardini, M Banday, AJ Barreiro, RB Bartlett, JG Bartolo, N Basak, S Battaglia, P Battaner, E Battye, R Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bertincourt, B Bielewicz, P Bikmaev, I Bock, JJ Bohringer, H Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Boulanger, F Bucher, M Burenin, R Burigana, C Butler, RC Calabrese, E Cardoso, JF Carvalho, P Casaponsa, B Castex, G Catalano, A Challinor, A Chamballu, A Chary, RR Chiang, HC Chluba, J Chon, G Christensen, PR Church, S Clemens, M Clements, DL Colombi, S Colombo, LPL Combet, C Comis, B Contreras, D Couchot, F Coulais, A Crill, BP Cruz, M Curto, A Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Di Valentino, E Dickinson, C Diego, JM Dolag, K Dole, H Donzelli, S Dore, O Douspis, M Ducout, A Dunkley, J Dupac, X Efstathiou, G Eisenhardt, PRM Elsner, F Ensslin, TA Eriksen, HK Falgarone, E Fantaye, Y Farhang, M Feeney, S Fergusson, J Fernandez-Cobos, R Feroz, F Finelli, F Florido, E Forni, O Frailis, M Fraisse, AA Franceschet, C Franceschi, E Frejsel, A Frolov, A Galeotta, S Galli, S Ganga, K Gauthier, C Genova-Santos, RT Gerbino, M Ghosh, T Giard, M Giraud-Heraud, Y Giusarma, E Gjerlow, E Gonzalez-Nuevo, J Gorski, KM Grainge, KJB Gratton, S Gregorio, A Gruppuso, A Gudmundsson, JE Hamann, J Handley, W Hansen, FK Hanson, D Harrison, DL Heavens, A Helou, G Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huang, Z Huffenberger, KM Hurier, G Ilic, S Jaffe, AH Jaffe, TR Jin, T Jones, WC Juvela, M Karakci, A Keihanen, E Keskitalo, R Khamitov, I Kiiveri, K Kim, J Kisner, TS Kneissl, R Knoche, J Knox, L Krachmalnicoff, N Kunz, M Kurki-Suonio, H Lacasa, F Lagache, G Lahteenmaki, A Lamarre, JM Langer, M Lasenby, A Lattanzi, M Lawrence, CR Jeune, M Leahy, JP Lellouch, E Leonardi, R Leon-Tavares, J Lesgourgues, J Levrier, F Lewis, A Liguori, M Lilje, PB Lilley, M Linden-Vornle, M Lindholm, V Liu, H Lopez-Caniego, M Lubin, PM Ma, YZ Macias-Perez, JF Maggio, G Maino, D Mak, DSY Mandolesi, N Mangilli, A Marchini, A Marcos-Caballero, A Marinucci, D Maris, M Marshall, DJ Martin, PG Martinelli, M Martinez-Gonzalez, E Masi, S Matarrese, S Mazzotta, P McEwen, JD McGehee, P Mei, S Meinhold, PR Melchiorri, A Melin, JB Mendes, L Mennella, A Migliaccio, M Mikkelsen, K Millea, M Mitra, S Miville-Deschenes, MA Molinari, D Moneti, A Montier, L Moreno, R Morgante, G Mortlock, D Moss, A Mottet, S Munchmeyer, M Munshi, D Murphy, JA Narimani, A Naselsky, P Nastasi, A Nati, F Natoli, P Negrello, M Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Olamaie, M Oppermann, N Orlando, E Oxborrow, CA Paci, F Pagano, L Pajot, F Paladini, R Pandolfi, S Paoletti, D Partridge, B Pasian, F Patanchon, G Pearson, TJ Peel, M Peiris, HV Pelkonen, VM Perdereau, O Perotto, L Perrott, YC Perrotta, F Pettorino, V Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pogosyan, D Pointecouteau, E Polenta, G Popa, L Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Racine, B Reach, WT Rebolo, R Reinecke, M Remazeilles, M Renault, C Renzi, A Ristorcelli, I Rocha, G Roman, M Romelli, E Rosset, C Rossetti, M Rotti, A Roudier, G d'Orfeuil, BR Rowan-Robinson, M Rubino-Martin, JA Ruiz-Granados, B Rumsey, C Rusholme, B Said, N Salvatelli, V Salvati, L Sandri, M Sanghera, HS Santos, D Saunders, RDE Sauve, A Savelainen, M Savini, G Schaefer, BM Schammel, MP Scott, D Seiffert, MD Serra, P Shellard, EPS Shimwell, TW Shiraishi, M Smith, K Souradeep, T Spencer, LD Spinelli, M Stanford, SA Stern, D Stolyarov, V Stompor, R Strong, AW Sudiwala, R Sunyaev, R Sutter, P Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Tavagnacco, D Terenzi, L Texier, D Toffolatti, L Tomasi, M Tornikoski, M Tramonte, D Tristram, M Troja, A Trombetti, T Tucci, M Tuovinen, J Turler, M Umana, G Valenziano, L Valiviita, J Van Tent, F Vassallo, T Vibert, L Vidal, M Viel, M Vielva, P Villa, F Wade, LA Walter, B Wandelt, BD Watson, R Wehus, IK Welikala, N Weller, J White, M White, SDM Wilkinson, A Yvon, D Zacchei, A Zibin, JP Zonca, A AF Adam, R. Ade, P. A. R. Aghanim, N. Akrami, Y. Alves, M. I. R. Argueeso, F. Arnaud, M. Arroja, F. Ashdown, M. Aumont, J. Baccigalupi, C. Ballardini, M. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Bartolo, N. Basak, S. Battaglia, P. Battaner, E. Battye, R. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bertincourt, B. Bielewicz, P. Bikmaev, I. Bock, J. J. Boehringer, H. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bucher, M. Burenin, R. Burigana, C. Butler, R. C. Calabrese, E. Cardoso, J. -F. Carvalho, P. Casaponsa, B. Castex, G. Catalano, A. Challinor, A. Chamballu, A. Chary, R. -R. Chiang, H. C. Chluba, J. Chon, G. Christensen, P. R. Church, S. Clemens, M. Clements, D. L. Colombi, S. Colombo, L. P. L. Combet, C. Comis, B. Contreras, D. Couchot, F. Coulais, A. Crill, B. P. Cruz, M. Curto, A. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J. -M. Desert, F. -X. Di Valentino, E. Dickinson, C. Diego, J. M. Dolag, K. Dole, H. Donzelli, S. Dore, O. Douspis, M. Ducout, A. Dunkley, J. Dupac, X. Efstathiou, G. Eisenhardt, P. R. M. Elsner, F. Ensslin, T. A. Eriksen, H. K. Falgarone, E. Fantaye, Y. Farhang, M. Feeney, S. Fergusson, J. Fernandez-Cobos, R. Feroz, F. Finelli, F. Florido, E. Forni, O. Frailis, M. Fraisse, A. A. Franceschet, C. Franceschi, E. Frejsel, A. Frolov, A. Galeotta, S. Galli, S. Ganga, K. Gauthier, C. Genova-Santos, R. T. Gerbino, M. Ghosh, T. Giard, M. Giraud-Heraud, Y. Giusarma, E. Gjerlow, E. Gonzalez-Nuevo, J. Gorski, K. M. Grainge, K. J. B. Gratton, S. Gregorio, A. Gruppuso, A. Gudmundsson, J. E. Hamann, J. Handley, W. Hansen, F. K. Hanson, D. Harrison, D. L. Heavens, A. Helou, G. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huang, Z. Huffenberger, K. M. Hurier, G. Ilic, S. Jaffe, A. H. Jaffe, T. R. Jin, T. Jones, W. C. Juvela, M. Karakci, A. Keihanen, E. Keskitalo, R. Khamitov, I. Kiiveri, K. Kim, J. Kisner, T. S. Kneissl, R. Knoche, J. Knox, L. Krachmalnicoff, N. Kunz, M. Kurki-Suonio, H. Lacasa, F. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Langer, M. Lasenby, A. Lattanzi, M. Lawrence, C. R. Le Jeune, M. Leahy, J. P. Lellouch, E. Leonardi, R. Leon-Tavares, J. Lesgourgues, J. Levrier, F. Lewis, A. Liguori, M. Lilje, P. B. Lilley, M. Linden-Vornle, M. Lindholm, V. Liu, H. Lopez-Caniego, M. Lubin, P. M. Ma, Y. -Z. Macias-Perez, J. F. Maggio, G. Maino, D. Mak, D. S. Y. Mandolesi, N. Mangilli, A. Marchini, A. Marcos-Caballero, A. Marinucci, D. Maris, M. Marshall, D. J. Martin, P. G. Martinelli, M. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Mazzotta, P. McEwen, J. D. McGehee, P. Mei, S. Meinhold, P. R. Melchiorri, A. Melin, J. -B. Mendes, L. Mennella, A. Migliaccio, M. Mikkelsen, K. Millea, M. Mitra, S. Miville-Deschenes, M. -A. Molinari, D. Moneti, A. Montier, L. Moreno, R. Morgante, G. Mortlock, D. Moss, A. Mottet, S. Muenchmeyer, M. Munshi, D. Murphy, J. A. Narimani, A. Naselsky, P. Nastasi, A. Nati, F. Natoli, P. Negrello, M. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Olamaie, M. Oppermann, N. Orlando, E. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paladini, R. Pandolfi, S. Paoletti, D. Partridge, B. Pasian, F. Patanchon, G. Pearson, T. J. Peel, M. Peiris, H. V. Pelkonen, V. -M. Perdereau, O. Perotto, L. Perrott, Y. C. Perrotta, F. Pettorino, V. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pogosyan, D. Pointecouteau, E. Polenta, G. Popa, L. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Racine, B. Reach, W. T. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Renzi, A. Ristorcelli, I. Rocha, G. Roman, M. Romelli, E. Rosset, C. Rossetti, M. Rotti, A. Roudier, G. d'Orfeuil, B. Rouille Rowan-Robinson, M. Rubino-Martin, J. A. Ruiz-Granados, B. Rumsey, C. Rusholme, B. Said, N. Salvatelli, V. Salvati, L. Sandri, M. Sanghera, H. S. Santos, D. Saunders, R. D. E. Sauve, A. Savelainen, M. Savini, G. Schaefer, B. M. Schammel, M. P. Scott, D. Seiffert, M. D. Serra, P. Shellard, E. P. S. Shimwell, T. W. Shiraishi, M. Smith, K. Souradeep, T. Spencer, L. D. Spinelli, M. Stanford, S. A. Stern, D. Stolyarov, V. Stompor, R. Strong, A. W. Sudiwala, R. Sunyaev, R. Sutter, P. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Tavagnacco, D. Terenzi, L. Texier, D. Toffolatti, L. Tomasi, M. Tornikoski, M. Tramonte, D. Tristram, M. Troja, A. Trombetti, T. Tucci, M. Tuovinen, J. Turler, M. Umana, G. Valenziano, L. Valiviita, J. Van Tent, F. Vassallo, T. Vibert, L. Vidal, M. Viel, M. Vielva, P. Villa, F. Wade, L. A. Walter, B. Wandelt, B. D. Watson, R. Wehus, I. K. Welikala, N. Weller, J. White, M. White, S. D. M. Wilkinson, A. Yvon, D. Zacchei, A. Zibin, J. P. Zonca, A. CA Planck Collaboration TI Planck 2015 results I. Overview of products and scientific results SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology: observations; cosmic background radiation; surveys; space vehicles: instruments; instrumentation: detectors ID ANGULAR POWER SPECTRUM; PROBE WMAP OBSERVATIONS; MICROWAVE BACKGROUND TEMPERATURE; PRE-LAUNCH STATUS; COMPONENT SEPARATION; SKY MAPS; INTERSTELLAR DUST; POLARIZATION DATA; MAGNETIC-FIELD; ANISOTROPY AB The European Space Agency's Planck satellite, which is dedicated to studying the early Universe and its subsequent evolution, was launched on 14 May 2009. It scanned the microwave and submillimetre sky continuously between 12 August 2009 and 23 October 2013. In February 2015, ESA and the Planck Collaboration released the second set of cosmology products based on data from the entire Planck mission, including both temperature and polarization, along with a set of scientific and technical papers and a web-based explanatory supplement. This paper gives an overview of the main characteristics of the data and the data products in the release, as well as the associated cosmological and astrophysical science results and papers. The data products include maps of the cosmic microwave background (CMB), the thermal Sunyaev-Zeldovich effect, diffuse foregrounds in temperature and polarization, catalogues of compact Galactic and extragalactic sources (including separate catalogues of Sunyaev-Zeldovich clusters and Galactic cold clumps), and extensive simulations of signals and noise used in assessing uncertainties and the performance of the analysis methods. The likelihood code used to assess cosmological models against the Planck data is described, along with a CMB lensing likelihood. Scientific results include cosmological parameters derived from CMB power spectra, gravitational lensing, and cluster counts, as well as constraints on inflation, non-Gaussianity, primordial magnetic fields, dark energy, and modified gravity, and new results on low-frequency Galactic foregrounds. C1 [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Castex, G.; Delabrouille, J.; Ganga, K.; Gauthier, C.; Giraud-Heraud, Y.; Karakci, A.; Le Jeune, M.; Patanchon, G.; Piat, M.; Remazeilles, M.; Roman, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, APC AstroParticule & Cosmol, CNRS IN2P3, CEA Irfu,Observ Paris,Sorbonne Paris Cite, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France. [Lahteenmaki, A.; Leon-Tavares, J.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, POB 13000, Aalto 00076, Finland. [Lahteenmaki, A.] Dept Radio Sci & Engn, POB 13000, Aalto 00076, Finland. [Bikmaev, I.] Acad Sci Tatarstan, Bauman Str 20, Kazan 420111, Republic Of Tat, Russia. [Fantaye, Y.; Kunz, M.] African Inst Math Sci, 6-8 Melrose Rd, Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy. [Lagache, G.] Aix Marseille Univ, CNRS, LAM Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France. [Ilic, S.; Salvatelli, V.] Aix Marseille Univ, Ctr Phys Theor, 163 Ave Luminy, F-13288 Marseille, France. [Ashdown, M.; Curto, A.; Feroz, F.; Grainge, K. J. B.; Handley, W.; Hobson, M.; Jin, T.; Lasenby, A.; Olamaie, M.; Perrott, Y. C.; Rumsey, C.; Saunders, R. D. E.; Schammel, M. P.; Shimwell, T. W.; Stolyarov, V.] Univ Cam bridge, Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, Westville Campus,Private Bag X54001, ZA-4000 Durban, South Africa. 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S.] Univ Cambridge, Ctr Theoret Cosmol, DAMTP, Wilberforce Rd, Cambridge CB3 0WA, England. [Hernandez-Monteagudo, C.] CEFCA, Plaza San Juan,1 Planta 2, Teruel 44001, Spain. [Borrill, J.; Keskitalo, R.] Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA USA. [Rebolo, R.] CSIC, Madrid, Spain. [Chamballu, A.; Melin, J. -B.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. [Linden-Vornle, M.; Norgaard-Nielsen, H. U.; Oxborrow, C. A.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark. [Kunz, M.; Tucci, M.] Univ Geneva, Dept Phys Theor, 24 Quai E Ansermet, CH-1211 Geneva 4, Switzerland. [Pandolfi, S.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Manes Vej 30, DK-2100 Copenhagen, Denmark. [Genova-Santos, R. T.; Rebolo, R.; Rubino-Martin, J. A.; Tramonte, D.] Univ La Laguna ULL, Dept Astrofis, San Cristobal la Laguna 38206, Tenerife, Spain. 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[Bersanelli, M.; Franceschet, C.; Krachmalnicoff, N.; Maino, D.; Mennella, A.; Rossetti, M.; Tomasi, M.; Troja, A.] Univ Milan, Dipartimento Fis, Via Celoria 16, Milan, Italy. [Battaglia, P.; Gregorio, A.; Romelli, E.; Tavagnacco, D.] Univ Trieste, Dipartimento Fis, Via A Valerio 2, Trieste, Italy. [Mazzotta, P.] Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, Rome, Italy. [Fantaye, Y.; Marinucci, D.; Renzi, A.] Univ Roma Tor Vergata, Dipartimento Matemat, Via Ric Sci 1, Rome, Italy. [Christensen, P. R.; Liu, H.] Niels Bohr Inst, Discovery Ctr, Blegdamsvej 17, Copenhagen, Denmark. Univ Copenhagen, Niels Bohr Inst, Discovery Ctr, Blegdamsvej 17, Copenhagen, Denmark. [Kneissl, R.] ESO Vitacura, European Southern Observ, Alonso de Cordova 3107,Vitacura,Casilla 19001, Santiago, Chile. [Texier, D.] ESAC, European Space Agcy, Camino Bajo del Castillo S-N, Madrid, Spain. 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[Lacasa, F.] Univ Estadual Paulista, Inst Fis Teor, ICTP South Amer Inst Fundamental Res, Sao Paulo, Brazil. [Umana, G.] INAF, Osservatorio Astrofis Catania, Via S Sofia 78, Catania, Italy. [Clemens, M.; de Zotti, G.; Negrello, M.] INAF, Osservatorio Astron Padova, Vicolo Osservatorio 5, Padua, Italy. [Polenta, G.] INAF, Osservatorio Astron Roma, Via Frascati 33, Monte Porzio Catone, Italy. [Frailis, M.; Galeotta, S.; Gregorio, A.; Maggio, G.; Maris, M.; Romelli, E.; Tavagnacco, D.; Viel, M.; Zacchei, A.] INAF, Osservatorio Astron Trieste, Via GB Tiepolo 11, Trieste, Italy. [Ballardini, M.; Burigana, C.; Butler, R. C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Molinari, D.; Morgante, G.; Paoletti, D.; Sandri, M.; Terenzi, L.; Toffolatti, L.; Trombetti, T.; Valenziano, L.; Villa, F.] IASF Bologna, INAF, Via Gobetti 101, Bologna, Italy. 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L.; Ducout, A.; Feeney, S.; Heavens, A.; Jaffe, A. H.; Mortlock, D.; Rowan-Robinson, M.] Imperial Coll London, Astrophys Grp, Blackett Lab, Prince Consort Rd, London SW7 2AZ, England. [Chary, R. -R.; McGehee, P.; Paladini, R.; Pearson, T. J.; Pelkonen, V. -M.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Benoit, A.] Univ Joseph Fourier Grenoble I, CNRS, Inst Neel, 25 Rue Martyrs, Grenoble, France. [Dole, H.] Inst Univ France, 103 Bd St Michel, F-75005 Paris, France. [Aghanim, N.; Alves, M. I. R.; Aumont, J.; Bertincourt, B.; Boulanger, F.; Chamballu, A.; Dole, H.; Douspis, M.; Ghosh, T.; Hurier, G.; Kunz, M.; Lacasa, F.; Lagache, G.; Langer, M.; Mangilli, A.; Miville-Deschenes, M. -A.; Nastasi, A.; Pajot, F.; Puget, J. -L.; Remazeilles, M.; Serra, P.; Vibert, L.] Univ Paris Saclay, Univ Paris Sud, CNRS, Inst Astrophys Spatiale, Bat 121, F-91405 Orsay, France. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Di Valentino, E.; Ducout, A.; Elsner, F.; Hivon, E.; Lilley, M.; Moneti, A.; Mottet, S.; Muenchmeyer, M.; Prunet, S.; Sutter, P.; Sygnet, J. -F.; Wandelt, B. D.] Inst Astrophys Paris, CNRS, UMR 7095, 98bis Blvd Arago, F-75014 Paris, France. [Lesgourgues, J.] Rhein Westfal TH Aachen, Inst Theoret Teilchenphys & Kosmol, D-52056 Aachen, Germany. [Popa, L.] Inst Space Sci, Bucharest, Romania. [Carvalho, P.; Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D. L.; Mak, D. S. Y.; Migliaccio, M.; Sanghera, H. S.; Sutton, D.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Akrami, Y.; Eriksen, H. K.; Gjerlow, E.; Hansen, F. K.; Lilje, P. B.; Mikkelsen, K.; Racine, B.; Wehus, I. K.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway. [Leon-Tavares, J.] INAOE, Apartado Postal 51 & 216, Puebla 72000, Mexico. [Genova-Santos, R. T.; Rebolo, R.; Rubino-Martin, J. 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[Catalano, A.; Coulais, A.; Falgarone, E.; Lamarre, J. -M.; Levrier, F.; Roudier, G.] Observ Paris, CNRS, LERMA, 61 Ave Observ, Paris, France. [Lellouch, E.; Moreno, R.] Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris, 5 Pl J Janssen, F-92195 Meudon, France. [Arnaud, M.; Chamballu, A.; Marshall, D. J.; Pratt, G. W.] Univ Paris Diderot, CEA Saclay, CNRS, Lab AIM,IRFU Serv Astrophys CEA DSM, Bat 709, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, UMR 5141, Lab Traitement & Commun Informat, 46 Rue Barrault, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom ParisTech, 46 Rue Barrault, F-75634 Paris 13, France. [Adam, R.; Catalano, A.; Combet, C.; Comis, B.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble Alpes, CNRS IN2P3, Lab Phys Subat & Cosmol, 53 Rue Martyrs, F-38026 Grenoble, France. [Van Tent, F.] Univ Paris Sud 11, Lab Phys Theor, Batiment 210, F-91405 Orsay, France. [Van Tent, F.] CNRS, Batiment 210, F-91405 Orsay, France. [Kisner, T. 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T.] Stratospher Observ Infrared Astron, Univ Space Res Assoc, MS 232-11, Moffett Field, CA 94035 USA. [Dolag, K.; Weller, J.] Ludwig Maximilian Univ Munich, Univ Observ, Scheinerstr 1, D-81679 Munich, Germany. [Battaner, E.; Florido, E.; Ruiz-Granados, B.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Battaner, E.] Univ Granada, Inst Carlos I Fis Teor & Computac, Granada, Spain. [Akrami, Y.; Martinelli, M.] Heidelberg Univ, Inst Theoret Phys, Philosophenweg 16, D-69120 Heidelberg, Germany. [Orlando, E.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Orlando, E.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Gorski, K. M.] Univ Warsaw Observ, Aleje Ujazdowskie 4, PL-00478 Warsaw, Poland. RP Lawrence, CR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM charles.lawrence@jpl.nasa.gov RI Lahteenmaki, Anne/L-5987-2013; Gerbino, Martina/E-4029-2017; Barreiro, Rita Belen/N-5442-2014; Mazzotta, Pasquale/B-1225-2016; bonavera, laura/E-9368-2017; Gonzalez-Nuevo, Joaquin/I-3562-2014; Herranz, Diego/K-9143-2014; Colombo, Loris/J-2415-2016; OI Savini, Giorgio/0000-0003-4449-9416; Martinelli, Matteo/0000-0002-6943-7732; Pierpaoli, Elena/0000-0002-7957-8993; Paoletti, Daniela/0000-0003-4761-6147; Huang, Zhiqi/0000-0002-1506-1063; TERENZI, LUCA/0000-0001-9915-6379; Reach, William/0000-0001-8362-4094; Valiviita, Jussi/0000-0001-6225-3693; Kurki-Suonio, Hannu/0000-0002-4618-3063; Juvela, Mika/0000-0002-5809-4834; Molinari, Diego/0000-0002-7799-3915; Toffolatti, Luigi/0000-0003-2645-7386; Nati, Federico/0000-0002-8307-5088; Gerbino, Martina/0000-0002-3538-1283; Barreiro, Rita Belen/0000-0002-6139-4272; Mazzotta, Pasquale/0000-0002-5411-1748; bonavera, laura/0000-0001-8039-3876; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Herranz, Diego/0000-0003-4540-1417; Colombo, Loris/0000-0003-4572-7732; Liu, Hao/0000-0003-4410-5827; Hivon, Eric/0000-0003-1880-2733; Zacchei, Andrea/0000-0003-0396-1192; Stolyarov, Vladislav/0000-0001-8151-828X FU CNES; CNRS/INSU-IN2P3; ASI; Danish Natural Research Council; ESA; CNES (France); CNRS/INSU-IN2P3INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MINECO (Spain); JA (Spain); RES (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC (EU); PRACE (EU); LFI; HFI FX Planck is a project of the European Space Agency in cooperation with the scientific community, which started in 1993. ESA led the project, developed the satellite, integrated the payload into it, and launched and operated the satellite. Two Consortia, comprising around 100 scientific institutes within Europe, the USA, and Canada, and funded by agencies from the participating countries, developed and operated the scientific instruments LFI and HFI. 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. These three Consortia, together with ESA's Planck Science Office, form the Planck Collaboration. 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.cosmos.esa.int/web/planck/planck-collaboration. The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). We thank Diego Falceta-Goncalves for providing the technique for making the line-integral-convolution maps presented in Figs. 23 and 25. NR 127 TC 16 Z9 16 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2016 VL 594 AR A1 DI 10.1051/0004-6361/201527101 PG 38 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4MG UT WOS:000385832200030 ER PT J AU Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartlett, JG Bartolo, N Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bock, JJ Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Boulanger, F Bucher, M Burigana, C Butler, RC Calabrese, E Cardoso, JF Castex, G Catalano, A Challinor, A Chamballu, A Chiang, HC Christensen, PR Clements, DL Colombi, S Colombo, LPL Combet, C Couchot, F Coulais, A Crill, BP Curto, A Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Dickinson, C Diego, JM Dolag, K Dole, H Donzelli, S Dore, O Douspis, M Ducout, A Dupac, X Efstathiou, G Elsner, F Ensslin, TA Eriksen, HK Fergusson, J Finelli, F Forni, O Frailis, M Fraisse, AA Franceschi, E Frejsel, A Galeotta, S Galli, S Ganga, K Ghosh, T Giard, M Giraud-Heraud, Y Gjerlow, E Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Gudmundsson, JE Hansen, FK Hanson, D Harrison, DL Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Hurier, G Jaffe, AH Jaffe, TR Jones, WC Juvela, M Karakei, A Keihanen, E Keskitalo, R Kiiveri, K Kisner, TS Kneissl, R Knoche, J Kunz, M Kurki-Suonio, H Lagache, G Lamarre, JM Lasenby, A Lattanzi, M Lawrence, CR Leonardi, R Lesgourgues, J Levrier, F Liguori, M Lilje, PB Linden-Vornle, M Lindholm, V Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maggio, G Maino, D Mandolesi, N Mangilli, A Maris, M Martin, PG Martinez-Gonzalez, E Masi, S Matarrese, S McGehee, P Meinhold, PR Melchiorri, A Melin, JB Mendes, L Mennella, A Migliaccio, M Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Moss, A Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Oxborrow, CA Paci, F Pagano, L Pajot, F Paoletti, D Pasian, F Patanchon, G Pearson, TJ Perdereau, O Perotto, L Perrotta, F Pettorino, V Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Rebolo, R Reinecke, M Remazeilles, M Renault, C Renzi, A Ristorcelli, I Rocha, G Roman, M Rosset, C Rossetti, M Roudier, G Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savelainen, M Scott, D Seiffert, MD Shellard, EPS Spencer, LD Stolyarov, V Stompor, R Sudiwala, R Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Tuovinen, J Valenziano, L Valiviita, J Van Tent, B Vielva, P Villa, F Wade, LA Wandelt, BD Wehus, IK Welikala, N Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Bartolo, N. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bock, J. J. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bucher, M. Burigana, C. Butler, R. C. Calabrese, E. Cardoso, J. -F. Castex, G. Catalano, A. Challinor, A. Chamballu, A. Chiang, H. C. Christensen, P. R. Clements, D. L. Colombi, S. Colombo, L. P. L. Combet, C. Couchot, F. Coulais, A. Crill, B. P. Curto, A. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J. -M. Desert, F. -X. Dickinson, C. Diego, J. M. Dolag, K. Dole, H. Donzelli, S. Dore, O. Douspis, M. Ducout, A. Dupac, X. Efstathiou, G. Elsner, F. Ensslin, T. A. Eriksen, H. K. Fergusson, J. Finelli, F. Forni, O. Frailis, M. Fraisse, A. A. Franceschi, E. Frejsel, A. Galeotta, S. Galli, S. Ganga, K. Ghosh, T. Giard, M. Giraud-Heraud, Y. Gjerlow, E. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Gudmundsson, J. E. Hansen, F. K. Hanson, D. Harrison, D. L. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Hurier, G. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Karakei, A. Keihanen, E. Keskitalo, R. Kiiveri, K. Kisner, T. S. Kneissl, R. Knoche, J. Kunz, M. Kurki-Suonio, H. Lagache, G. Lamarre, J. -M. Lasenby, A. Lattanzi, M. Lawrence, C. R. Leonardi, R. Lesgourgues, J. Levrier, F. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lindholm, V. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maggio, G. Maino, D. Mandolesi, N. Mangilli, A. Maris, M. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Matarrese, S. McGehee, P. Meinhold, P. R. Melchiorri, A. Melin, J. -B. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Moss, A. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paoletti, D. Pasian, F. Patanchon, G. Pearson, T. J. Perdereau, O. Perotto, L. Perrotta, F. Pettorino, V. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Renzi, A. Ristorcelli, I. Rocha, G. Roman, M. Rosset, C. Rossetti, M. Roudier, G. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savelainen, M. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Stolyarov, V. Stompor, R. Sudiwala, R. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Tucci, M. Tuovinen, J. Valenziano, L. Valiviita, J. Van Tent, B. Vielva, P. Villa, F. Wade, L. A. Wandelt, B. D. Wehus, I. K. Welikala, N. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2015 results XII. Full focal plane simulations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: data analysis; methods: numerical; cosmic background radiation ID MICROWAVE-ANISOTROPY-PROBE; STATISTICAL PROPERTIES; GALAXY CLUSTERS; BACKGROUND MAPS; SPINNING DUST; SKY MAPS; EMISSION; CATALOG; SEPARATION; MODEL AB We present the 8th full focal plane simulation set (FFP8), deployed in support of the Planck 2015 results. FFP8 consists of 10 fiducial mission realizations reduced to 18 144 maps, together with the most massive suite of Monte Carlo realizations of instrument noise and CMB ever generated, comprising 104 mission realizations reduced to about 106 maps. The resulting maps incorporate the dominant instrumental, scanning, and data analysis effects, and the remaining subdominant effects will be included in future updates. 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A.] Inst Astrofis Canarias, C Via Lactea S-N, San Cristobal la Laguna 38205, Tenerife, Spain. [Barreiro, R. B.; Bonavera, L.; Curto, A.; Diego, J. M.; Gonzalez-Nuevo, J.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Toffolatti, L.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, Avda Los Castros S-N, Santander, Spain. [Bartolo, N.; Liguori, M.; Matarrese, S.] Ist Nazl Fis Nucl, Sez Padova, Via Marzolo 8, I-35131 Padua, Italy. [Bartlett, J. G.; Bock, J. J.; Colombo, L. P. L.; Crill, B. P.; Dore, O.; Gorski, K. M.; Hanson, D.; Hildebrandt, S. R.; Holmes, W. A.; Lawrence, C. R.; Mitra, S.; Pietrobon, D.; Prezeau, G.; Rocha, G.; Roudier, G.; Seiffert, M. D.; Wade, L. A.; Wehus, I. K.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA. [Bonaldi, A.; Davies, R. D.; Davis, R. J.; Dickinson, C.; Noviello, F.; Remazeilles, M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England. [Galli, S.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Ashdown, M.; Challinor, A.; Curto, A.; Gratton, S.; Harrison, D. L.; Lasenby, A.; Migliaccio, M.; Sutton, D.] Kavli Inst Cosmol Cambridge, Madingley Rd, Cambridge CB3 0HA, England. [Stolyarov, V.] Kazan Fed Univ, 18 Kremlyovskaya St, Kazan 420008, Russia. [Couchot, F.; Henrot-Versille, S.; Mangilli, A.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, LAL, CNRS IN2P3, F-91898 Orsay, France. [Catalano, A.; Coulais, A.; Lamarre, J. -M.; Levrier, F.; Roudier, G.] Observ Paris, CNRS, LERMA, 61 Ave Observ, F-75000 Paris, France. [Arnaud, M.; Chamballu, A.; Pratt, G. W.] Univ Paris Diderot, CEA Saclay, CNRS, Lab AIM IRFU,Serv Astrophys,CEA,DSM, Bat 709, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, UMR 5141, Lab Traitement & Commun Informat, 46 Rue Barrault, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom ParisTech, 46 Rue Barrault, F-75634 Paris 13, France. [Catalano, A.; Combet, C.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble Alpes, CNRS IN2P3, Lab Phys Subat & Cosmol, 53 Rue Martyrs, F-38026 Grenoble, France. [Van Tent, B.] Univ Paris Sud 11, Lab Phys Theor, Batiment 210, F-91405 Orsay, France. [Van Tent, B.] CNRS, Batiment 210, F-91405 Orsay, France. [Kisner, T. S.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Novikov, D.; Novikov, I.] Russian Acad Sci, Astro Space Ctr, Lebedev Phys Inst, 84-32 Profsoyuznaya St,GSP-7, Moscow 117997, Russia. [Dolag, K.; Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Knoche, J.; Rachen, J. P.; Reinecke, M.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. [Hanson, D.] McGill Univ, McGill Phys, Ernest Rutherford Phys Bldg,3600 Rue Univ, Montreal, PQ H3A 2T8, Canada. [Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Co Kildare, Ireland. [Bielewicz, P.] Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland. [Christensen, P. R.; Frejsel, A.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, Blegdamsvej 17, DK-1165 Copenhagen, Denmark. [Baccigalupi, C.; Bielewicz, P.; Danese, L.; de Zotti, G.; Paci, F.; Perrotta, F.] SISSA, Astrophys Sect, Via Bonomea 265, I-34136 Trieste, Italy. [Ade, P. A. R.; Munshi, D.; Spencer, L. D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales. [Moss, A.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Bouchet, F. R.] UPMC, Sorbonne Univ, UMR7095, Inst Astrophys Paris, 98 Bis Blvd Arago, F-75014 Paris, France. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Karachai Cherkessian Rep 369167, Russia. [Calabrese, E.; Welikala, N.] Univ Oxford, Subdept Astrophys, Keble Rd, Oxford OX1 3RH, England. [Lesgourgues, J.] CERN, Div Theory, PH TH, CH-1211 Geneva 23, Switzerland. [Benabed, K.; Benoit-Levy, A.; Colombi, S.; Delouis, J. -M.; Elsner, F.; Hivon, E.; Prunet, S.; Wandelt, B. D.] UPMC Univ Paris 06, UMR7095, 98 Bis Blvd Arago, F-75014 Paris, France. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Dolag, K.] Ludwig Maximilian Univ Munich, Univ Observ, Scheinerstr 1, D-81679 Munich, Germany. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada 18010, Spain. [Battaner, E.] Univ Granada, Inst Carlos I Fis Teor & Computac, E-18071 Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, Aleje Ujazdowskie 4, PL-00478 Warsaw, Poland. RP Borrill, J (reprint author), Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 92093 USA.; Borrill, J (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM jdborrill@lbl.gov RI Gonzalez-Nuevo, Joaquin/I-3562-2014; Herranz, Diego/K-9143-2014; Colombo, Loris/J-2415-2016; Barreiro, Rita Belen/N-5442-2014; bonavera, laura/E-9368-2017 OI Valiviita, Jussi/0000-0001-6225-3693; Toffolatti, Luigi/0000-0003-2645-7386; Lilje, Per/0000-0003-4324-7794; Nati, Federico/0000-0002-8307-5088; Pierpaoli, Elena/0000-0002-7957-8993; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Herranz, Diego/0000-0003-4540-1417; Colombo, Loris/0000-0003-4572-7732; Kurki-Suonio, Hannu/0000-0002-4618-3063; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Stolyarov, Vladislav/0000-0001-8151-828X; Paoletti, Daniela/0000-0003-4761-6147; TERENZI, LUCA/0000-0001-9915-6379; Barreiro, Rita Belen/0000-0002-6139-4272; bonavera, laura/0000-0001-8039-3876 FU ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MINECO (Spain); JA (Spain); RES (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC (EU); PRACE (EU) 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, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (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.cosmos.esa.int/web/planck/planck-collaboration. Particular thanks are due to the extraordinary NERSC staff, who have supported the Planck mission for over a decade and who facilitated the production and distribution of FFP8 in numerous ways. NR 105 TC 0 Z9 0 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 OCT PY 2016 VL 594 AR A12 DI 10.1051/0004-6361/201527103 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4MG UT WOS:000385832200031 ER PT J AU Ade, PAR Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartolo, N Basak, S Battaglia, P Battaner, E Benabed, K Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bonaldi, A Bonavera, L Bond, JR Borrill, J Burigana, C Butler, RC Calabrese, E Catalano, A Christensen, PR Colombo, LPL Cruz, M Curto, A Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Dickinson, C Diego, JM Dore, O Ducout, A Dupac, X Elsner, F Ensslin, TA Eriksen, HK Finelli, F Frailis, M Franceschet, C Franceschi, E Galeotta, S Galli, S Ganga, K Ghosh, T Giard, M Giraud-Heraud, Y Gjerlow, E Gonzalez-Nuevo, J Gorski, KM Gregorio, A Gruppuso, A Hansen, FK Harrison, DL Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Hornstrup, A Hovest, W Huffenberger, KM Hurier, G Jaffe, AH Jaffe, TR Keihanen, E Keskitalo, R Kiiveri, K Kisner, TS Knoche, J Krachmalnicoff, N Kunz, M Kurki-Suonio, H Lagache, G Lamarre, JM Lasenby, A Lattanzi, M Lawrence, CR Leahy, JP Leonardi, R Levrier, F Liguori, M Lilje, PB Linden-Vornle, M Lindholm, V Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maggio, G Maino, D Mandolesi, N Mangilli, A Maris, M Martin, PG Martinez-Gonzalez, E Masi, S Matarrese, S Meinhold, PR Mennella, A Migliaccio, M Mitra, S Montier, L Morgante, G Mortlock, D Munshi, D Murphy, JA Nati, F Natoli, P Noviello, F Paci, F Pagano, L Pajot, F Paoletti, D Partridge, B Pasian, F Pearson, TJ Perdereau, O Pettorino, V Piacentini, F Pointecouteau, E Polenta, G Pratt, GW Puget, JL Rachen, JP Reinecke, M Remazeilles, M Renzi, A Ristorcelli, I Rocha, G Rosset, C Rossetti, M Roudier, G Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savelainen, M Scott, D Stolyarov, V Stompor, R Suur-Uski, AS Sygnet, JF Tauber, JA Tavagnacco, D Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Umana, G Valenziano, L Valiviita, J Van Tent, B Vassallo, T Vielva, P Villa, F Wade, LA Wandelt, BD Watson, R Wehus, IK Yvon, D Zacchei, A Zibin, JP Zonca, A AF Ade, P. A. R. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartolo, N. Basak, S. Battaglia, P. Battaner, E. Benabed, K. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Burigana, C. Butler, R. C. Calabrese, E. Catalano, A. Christensen, P. R. Colombo, L. P. L. Cruz, M. Curto, A. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Dickinson, C. Diego, J. M. Dore, O. Ducout, A. Dupac, X. Elsner, F. Ensslin, T. A. Eriksen, H. K. Finelli, F. Frailis, M. Franceschet, C. Franceschi, E. Galeotta, S. Galli, S. Ganga, K. Ghosh, T. Giard, M. Giraud-Heraud, Y. Gjerlow, E. Gonzalez-Nuevo, J. Gorski, K. M. Gregorio, A. Gruppuso, A. Hansen, F. K. Harrison, D. L. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Hornstrup, A. Hovest, W. Huffenberger, K. M. Hurier, G. Jaffe, A. H. Jaffe, T. R. Keihanen, E. Keskitalo, R. Kiiveri, K. Kisner, T. S. Knoche, J. Krachmalnicoff, N. Kunz, M. Kurki-Suonio, H. Lagache, G. Lamarre, J. -M. Lasenby, A. Lattanzi, M. Lawrence, C. R. Leahy, J. P. Leonardi, R. Levrier, F. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lindholm, V. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maggio, G. Maino, D. Mandolesi, N. Mangilli, A. Maris, M. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Meinhold, P. R. Mennella, A. Migliaccio, M. Mitra, S. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, J. A. Nati, F. Natoli, P. Noviello, F. Paci, F. Pagano, L. Pajot, F. Paoletti, D. Partridge, B. Pasian, F. Pearson, T. J. Perdereau, O. Pettorino, V. Piacentini, F. Pointecouteau, E. Polenta, G. Pratt, G. W. Puget, J. -L. Rachen, J. P. Reinecke, M. Remazeilles, M. Renzi, A. Ristorcelli, I. Rocha, G. Rosset, C. Rossetti, M. Roudier, G. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savelainen, M. Scott, D. Stolyarov, V. Stompor, R. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Tavagnacco, D. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Tucci, M. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Vassallo, T. Vielva, P. Villa, F. Wade, L. A. Wandelt, B. D. Watson, R. Wehus, I. K. Yvon, D. Zacchei, A. Zibin, J. P. Zonca, A. CA Planck Collaboration TI Planck 2015 results III. LFI systematic uncertainties SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmic background radiation; cosmology: observations; space vehicles: instruments; methods: data analysis ID LOW-FREQUENCY INSTRUMENT; PRIMORDIAL NON-GAUSSIANITY; STRAYLIGHT CONTAMINATION; ANGULAR RESOLUTION; TRADE-OFF; SKY MAPS; POLARIZATION; BISPECTRUM; MISSION AB We present the current accounting of systematic effect uncertainties for the Low Frequency Instrument (LFI) that are relevant to the 2015 release of the Planck cosmological results, showing the robustness and consistency of our data set, especially for polarization analysis. We use two complementary approaches: (i) simulations based on measured data and physical models of the known systematic effects; and (ii) analysis of difference maps containing the same sky signal ("null-maps"). The LFI temperature data are limited by instrumental noise. At large angular scales the systematic effects are below the cosmic microwave background (CMB) temperature power spectrum by several orders of magnitude. In polarization the systematic uncertainties are dominated by calibration uncertainties and compete with the CMB E-modes in the multipole range 10-20. Based on our model of all known systematic effects, we show that these effects introduce a slight bias of around 0.2 sigma on the reionization optical depth derived from the 70 GHz EE spectrum using the 30 and 353 GHz channels as foreground templates. At 30 GHz the systematic effects are smaller than the Galactic foreground at all scales in temperature and polarization, which allows us to consider this channel as a reliable template of synchrotron emission. We assess the residual uncertainties due to LFI effects on CMB maps and power spectra after component separation and show that these effects are smaller than the CMB amplitude at all scales. We also assess the impact on non-Gaussianity studies and find it to be negligible. Some residuals still appear in null maps from particular sky survey pairs, particularly at 30 GHz, suggesting possible straylight contamination due to an imperfect knowledge of the beam far sidelobes. C1 [Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Remazeilles, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, CNRS IN2P3, APC AstroParticule & Cosmol, CEA Irfu,Observ Paris,Sorbonne Paris Cite, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France. [Kunz, M.] African Inst Math Sci, 6-8 Melrose Rd, ZA-7945 Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy. [Lagache, G.] Aix Marseille Univ, CNRS, LAM Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France. [Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England. [Leonardi, R.] CGEE, SCS Qd 9,Lote C,Tone C,4 Andar, BR-70308200 Brasilia, DF, Brazil. [Bond, J. R.; Martin, P. G.] Univ Toronto, CITA, 60 St George St, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] IRAP, CNRS, 9 Av Colonel Roche,BP 44346, F-31028 Toulouse 4, France. [Dore, O.; Hildebrandt, S. R.; Pearson, T. J.; Rocha, G.] CALTECH, Pasadena, CA 91125 USA. 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[Matarrese, S.] INFN, Gran Sasso Sci Inst, Viale F Crispi 7, I-67100 Laquila, Italy. [Pettorino, V.] HGSFP, Philosophenweg 16, D-69120 Heidelberg, Germany. [Pettorino, V.] Heidelberg Univ, Dept Theoret Phys, Philosophenweg 16, D-69120 Heidelberg, Germany. [Partridge, B.] Haverford Coll, Dept Astron, 370 Lancaster Ave, Haverford, PA USA. [Kiiveri, K.; Kurki-Suonio, H.; Lindholm, V.; Savelainen, M.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Helsinki Inst Phys, Gustaf Hallstromin Katu 2, Helsinki 00100, Finland. [Umana, G.] INAF, Osservatorio Astrofis Catania, Via S Sofia 78, Catania, Italy. [de Zotti, G.] INAF, Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy. [Polenta, G.] INAF, Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy. [Frailis, M.; Galeotta, S.; Gregorio, A.; Maggio, G.; Maris, M.; Pasian, F.; Tavagnacco, D.; Vassallo, T.; Zacchei, A.] INAF, Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34131 Trieste, Italy. [Burigana, C.; Butler, R. C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Paoletti, D.; Sandri, M.; Terenzi, L.; Toffolatti, L.; Valenziano, L.; Villa, F.] INAF, IASF Bologna, Via Gobetti 101, I-40127 Bologna, Italy. [Bersanelli, M.; Maino, D.; Mennella, A.; Rossetti, M.; Tomasi, M.] INAF, IASF Milano, Via E Bassini 15, I-20133 Milan, Italy. [Burigana, C.; Finelli, F.; Paoletti, D.] INFN, Sez Bologna, Via Irnerio 46, I-40126 Bologna, Italy. [Pagano, L.] Univ Roma Sapienza, INFN, Sez Roma 1, Ple Aldo Moro 2, I-00185 Rome, Italy. [Renzi, A.] Univ Roma Tor Vergata, INFN, Sez Roma 2, Via Ric Sci 1, Rome, Italy. [Gregorio, A.] INFN, Natl Inst Nucl Phys, Via Valerio 2, I-34127 Trieste, Italy. [Mitra, S.] IUCAA, Post Bag 4,Pune Univ Campus, Pune 411007, Maharashtra, India. [Ducout, A.; Jaffe, A. H.; Mortlock, D.] Imperial Coll London, Blackett Lab, Astrophys Grp, Prince Consort Rd, London SW7 2AZ, England. [Pearson, T. J.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Aumont, J.; Ghosh, T.; Hurier, G.; Kunz, M.; Lagache, G.; Mangilli, A.; Pajot, F.; Puget, J. -L.; Remazeilles, M.] Univ Paris Saclay, Univ Paris Sud, CNRS, Inst Astrophys Spatiale, Bat 121, F-91405 Orsay, France. [Benabed, K.; Benoit-Levy, A.; Ducout, A.; Elsner, F.; Hivon, E.; Sygnet, J. -F.; Wandelt, B. D.] Inst Astrophys Paris, CNRS, UMR 7095, 98bis Blvd Arago, F-75014 Paris, France. [Harrison, D. L.; Migliaccio, M.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Eriksen, H. K.; Gjerlow, E.; Hansen, F. K.; Lilje, P. B.; Wehus, I. K.] Univ Oslo, Inst Theoret Astrophys, N-0371 Oslo, Norway. [Rubino-Martin, J. A.] Inst Astrofis Canarias, C Via Lactea S-N, San Cristobal la Laguna 38205, Tenerife, Spain. [Barreiro, R. B.; Bonavera, L.; Curto, A.; Diego, J. M.; Gonzalez-Nuevo, J.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Toffolatti, L.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, Avda Los Castros S-N, E-39005 Santander, Spain. [Bartolo, N.; Liguori, M.; Matarrese, S.] Ist Nazl Fis Nucl, Sez Padova, Via Marzolo 8, I-35131 Padua, Italy. [Colombo, L. P. L.; Dore, O.; Gorski, K. M.; Hildebrandt, S. R.; Lawrence, C. R.; Mitra, S.; Rocha, G.; Roudier, G.; Wade, L. A.; Wehus, I. K.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA. [Bonaldi, A.; Davies, R. D.; Davis, R. J.; Dickinson, C.; Leahy, J. P.; Maffei, B.; Noviello, F.; Remazeilles, M.; Watson, R.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England. [Galli, S.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Curto, A.; Harrison, D. L.; Lasenby, A.; Migliaccio, M.] Kavli Inst Cosmol Cambridge, Madingley Rd, Cambridge CB3 0HA, England. [Stolyarov, V.] Kazan Fed Univ, 18 Kremlyovskaya St, Kazan 420008, Russia. [Mangilli, A.; Perdereau, O.; Tristram, M.] Univ Paris 11, CNRS, LAL, IN2P3, Orsay, France. [Catalano, A.; Lamarre, J. -M.; Levrier, F.; Roudier, G.] LERMA, CNRS, Observ Paris, 61 Ave Observ, F-75104 Paris, France. [Pratt, G. W.] Univ Paris Diderot, CEA Saclay, CNRS, CEA DSM,Lab AIM,IRFU Serv Astrophys, Bat 709, F-91191 Gif Sur Yvette, France. [Catalano, A.; Macias-Perez, J. F.; Santos, D.] Univ Grenoble Alpes, IN2P3, CNRS, Lab Phys Subat & Cosmol, 53 Rue Martyrs, F-38026 Grenoble, France. [Van Tent, B.] Univ Paris Sud 11, Lab Phys Theor, Batiment 210, F-91405 Orsay, France. [Van Tent, B.] CNRS, Batiment 210, F-91405 Orsay, France. [Kisner, T. S.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Knoche, J.; Rachen, J. P.; Reinecke, M.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. [Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Co Kildare, Ireland. [Bielewicz, P.] Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland. [Christensen, P. R.] Niels Bohr Inst, Blegdamsvej 17, Copenhagen, Denmark. [Baccigalupi, C.; Basak, S.; Bielewicz, P.; Danese, L.; de Zotti, G.; Paci, F.] SISSA, Astrophys Sect, Via Bonomea 265, I-34136 Trieste, Italy. [Terenzi, L.] Univ E Campus, SMARTEST Res Ctr, Via Isimbardi 10, I-22060 Novedrate, CO, Italy. [Ade, P. A. R.; Munshi, D.] Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Karachai Cherkessian Rep 369167, Russia. [Calabrese, E.] Univ Oxford, Subdept Astrophys, Keble Rd, Oxford OX1 3RH, England. [Benabed, K.; Benoit-Levy, A.; Elsner, F.; Hivon, E.; Wandelt, B. D.] UPMC Univ Paris 06, UMR 7095, 98bis Blvd Arago, F-75014 Paris, France. [Banday, A. J.; Benoit-Levy, A.; Bernard, J. -P.; Giard, M.; 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 18010, Spain. [Battaner, E.] Univ Granada, Inst Carlos I Fis Teor & Computac, Granada 18010, Spain. [Gorski, K. M.] Univ Warsaw Observ, Aleje Ujazdowskie 4, PL-00478 Warsaw, Poland. RP Ade, PAR (reprint author), Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales. RI Colombo, Loris/J-2415-2016; Barreiro, Rita Belen/N-5442-2014; bonavera, laura/E-9368-2017; Gonzalez-Nuevo, Joaquin/I-3562-2014; Herranz, Diego/K-9143-2014 OI Piacentini, Francesco/0000-0002-5444-9327; Toffolatti, Luigi/0000-0003-2645-7386; Paoletti, Daniela/0000-0003-4761-6147; Nati, Federico/0000-0002-8307-5088; Colombo, Loris/0000-0003-4572-7732; Valiviita, Jussi/0000-0001-6225-3693; Kurki-Suonio, Hannu/0000-0002-4618-3063; Zacchei, Andrea/0000-0003-0396-1192; Stolyarov, Vladislav/0000-0001-8151-828X; TERENZI, LUCA/0000-0001-9915-6379; Hurier, Guillaume/0000-0002-1215-0706; Barreiro, Rita Belen/0000-0002-6139-4272; bonavera, laura/0000-0001-8039-3876; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Herranz, Diego/0000-0003-4540-1417 FU ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MINECO (Spain); JA (Spain); RES (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC (EU); PRACE (EU) 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, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (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.cosmos.esa.int/web/planck/planck_collaboration. Some of the results in this paper have been derived using the HEALPix package. NR 59 TC 0 Z9 0 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 OCT PY 2016 VL 594 AR A3 DI 10.1051/0004-6361/201526998 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4MG UT WOS:000385832200027 ER PT J AU Ade, PAR Aghanim, N Argueso, F Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartolo, N Battaner, E Beichman, C Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bock, JJ Bohringer, H Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Boulanger, F Bucher, M Burigana, C Butler, RC Calabrese, E Cardoso, JF Carvalho, P Catalano, A Challinor, A Chamballu, A Chary, RR Chiang, HC Christensen, PR Clemens, M Clements, DL Colombi, S Colombo, LPL Combet, C Couchot, F Coulais, A Crill, BP Curto, A Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Desert, FX Dickinson, C Diego, JM Dole, H Donzelli, S Dore, O Douspis, M Ducout, A Dupac, X Efstathiou, G Elsner, F Ensslin, TA Eriksen, HK Falgarone, E Fergusson, J Finelli, F Forni, O Frailis, M Fraisse, AA Franceschi, E Frejsel, A Galeotta, S Galli, S Ganga, K Giard, M Giraud-Heraud, Y Gjerlow, E Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Gudmundsson, JE Hansen, FK Hanson, D Harrison, DL Helou, G Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Hurier, G Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knoche, J Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Lattanzi, M Lawrence, CR Leahy, JP Leonardi, R Leon-Tavares, J Lesgourgues, J Levrier, F Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maggio, G Maino, D Mandolesi, N Mangilli, A Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Matarrese, S McGehee, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Moss, A Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Negrello, M Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Oxborrow, CA Paci, F Pagano, L Pajot, F Paladini, R Paoletti, D Partridge, B Pasian, F Patanchon, G Pearson, TJ Perdereau, O Perotto, L Perrotta, F Pettorino, V Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Reach, WT Rebolo, R Reinecke, M Remazeilles, M Renault, C Renzi, A Ristorcelli, I Rocha, G Rosset, C Rossetti, M Roudier, G Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Sandri, M Sanghera, HS Santos, D Savelainen, M Savini, G Scott, D Seiffert, MD Shellard, EPS Spencer, LD Stolyarov, V Sudiwala, R Sunyaev, R Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Tornikoski, M Tristram, M Tucci, M Tuovinen, J Turler, M Umana, G Valenziano, L Valiviita, J Van Tent, B Vielva, P Villa, F Wade, LA Walter, B Wandelt, BD Wehus, IK Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Argueeso, F. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartolo, N. Battaner, E. Beichman, C. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bock, J. J. Boehringer, H. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bucher, M. Burigana, C. Butler, R. C. Calabrese, E. Cardoso, J. -F. Carvalho, P. Catalano, A. Challinor, A. Chamballu, A. Chary, R. -R. Chiang, H. C. Christensen, P. R. Clemens, M. Clements, D. L. Colombi, S. Colombo, L. P. L. Combet, C. Couchot, F. Coulais, A. Crill, B. P. Curto, A. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Desert, F. -X. Dickinson, C. Diego, J. M. Dole, H. Donzelli, S. Dore, O. Douspis, M. Ducout, A. Dupac, X. Efstathiou, G. Elsner, F. Ensslin, T. A. Eriksen, H. K. Falgarone, E. Fergusson, J. Finelli, F. Forni, O. Frailis, M. Fraisse, A. A. Franceschi, E. Frejsel, A. Galeotta, S. Galli, S. Ganga, K. Giard, M. Giraud-Heraud, Y. Gjerlow, E. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Gudmundsson, J. E. Hansen, F. K. Hanson, D. Harrison, D. L. Helou, G. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Hurier, G. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knoche, J. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Lattanzi, M. Lawrence, C. R. Leahy, J. P. Leonardi, R. Leon-Tavares, J. Lesgourgues, J. Levrier, F. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maggio, G. Maino, D. Mandolesi, N. Mangilli, A. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Matarrese, S. McGehee, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Moss, A. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Negrello, M. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paladini, R. Paoletti, D. Partridge, B. Pasian, F. Patanchon, G. Pearson, T. J. Perdereau, O. Perotto, L. Perrotta, F. Pettorino, V. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Reach, W. T. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Renzi, A. Ristorcelli, I. Rocha, G. Rosset, C. Rossetti, M. Roudier, G. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Sanghera, H. S. Santos, D. Savelainen, M. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Stolyarov, V. Sudiwala, R. Sunyaev, R. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Tornikoski, M. Tristram, M. Tucci, M. Tuovinen, J. Turler, M. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Vielva, P. Villa, F. Wade, L. A. Walter, B. Wandelt, B. D. Wehus, I. K. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2015 results XXVI. The Second Planck Catalogue of Compact Sources SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE catalogs; cosmology: observations; radio continuum: general; submillimeter: general ID POINT-SOURCE DETECTION; DISCRETE OBJECT DETECTION; HERSCHEL REFERENCE SURVEY; ACTIVE GALACTIC NUCLEI; ASTRONOMICAL DATA SETS; FAST BAYESIAN-APPROACH; FLUX-DENSITY SCALE; ALL-SKY SURVEY; EXTRAGALACTIC SOURCES; NUMBER COUNTS AB The Second Planck Catalogue of Compact Sources is a list of discrete objects detected in single-frequency maps from the full duration of the Planck mission and supersedes previous versions. It consists of compact sources, both Galactic and extragalactic, detected over the entire sky. Compact sources detected in the lower frequency channels are assigned to the PCCS2, while at higher frequencies they are assigned to one of two subcatalogues, the PCCS2 or PCCS2E, depending on their location on the sky. The first of these (PCCS2) covers most of the sky and allows the user to produce subsamples at higher reliabilities than the target 80% integral reliability of the catalogue. The second ( PCCS2E) contains sources detected in sky regions where the diffuse emission makes it difficult to quantify the reliability of the detections. Both the PCCS2 and PCCS2E include polarization measurements, in the form of polarized flux densities, or upper limits, and orientation angles for all seven polarization-sensitive Planck channels. The improved data-processing of the full-mission maps and their reduced noise levels allow us to increase the number of objects in the catalogue, improving its completeness for the target 80% reliability as compared with the previous versions, the PCCS and the Early Release Compact Source Catalogue (ERCSC). C1 [Bucher, M.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Remazeilles, M.; Rosset, C.; Roudier, G.] Univ Paris Diderot, APC AstroParticule & Cosmol, CNRS IN2P3, CEA Irfu,Observ Paris,Sorbonne Paris Site, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France. [Leon-Tavares, J.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, POB 13000, Aalto 00076, Finland. [Lahteenmaki, A.] Dept Radio Sci & Engn, POB 13000, Aalto 00076, Finland. [Kunz, M.] African Inst Math Sci, 6-8 Melrose Rd, Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy. [Lagache, G.] Aix Marseille Univ, CNRS, LAM Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France. [Ashdown, M.; Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England. [Chiang, H. C.] Univ KwaZulu Natal, Sch Mathe Stat & Comp Sci, Astrophys & Cosmol Res Unit, Westville Campus,Private Bag X54001, ZA-4000 Durban, South Africa. [Kneissl, R.] ALMA Santiago Cent Off, Atacama Large Millimeter Submillimeter Array, Alonso de Cordova 3107, Santiago 7630355, Chile. [Leonardi, R.] CGEE, SCS Qd 9,Lote C,Torre C,4 Andar, BR-70308200 Brasilia, DF, Brazil. [Bond, J. R.; Hanson, D.; Martin, P. G.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, 60 St George St, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] IRAP, CNRS, 9 Av Colonel Roche,BP 44346, F-31028 Toulouse 4, France. [Tuovinen, J.] Trinity Coll Dublin, CRANN, Dublin, Ireland. [Beichman, C.; Bock, J. J.; Crill, B. P.; Dore, O.; Helou, G.; Hildebrandt, S. R.; Pearson, T. J.; Prezeau, G.; Rocha, G.; Seiffert, M. D.] CALTECH, Pasadena, CA 91125 USA. [Challinor, A.; Fergusson, J.; Shellard, E. P. S.] Univ Cambridge, Ctr Theoret Cosmol, DAMTP, Wilberforce Rd, Cambridge CB3 0WA, England. [Hernandez-Monteagudo, C.] Ctr Estudios Fis Cosmos Aragon CEFCA, Plaza San Juan 1,Planta 2, Teruel 44001, Spain. [Borrill, J.; Keskitalo, R.] Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA USA. [Rebolo, R.] CSIC, Madrid, Spain. [Chamballu, A.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. [Hornstrup, A.; Linden-Vornle, M.; Norgaard-Nielsen, H. U.; Oxborrow, C. A.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark. [Kunz, M.; Tucci, M.] Univ Geneva, Dept Phys Theor, 24 Quai E Ansermet, CH-1211 Geneva 4, Switzerland. [Rebolo, R.; Rubino-Martin, J. 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T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, MS 232-11, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Battaner, E.] Univ Granada, Inst Carlos I Fis Teor & Computac, Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, Aleje Ujazdowskie 4, PL-00478 Warsaw, Poland. RP Lopez-Caniego, M (reprint author), European Space Agcy ESAC, Planck Sci Off, Camino Bajo Castillo S-N, Madrid, Spain.; Harrison, DL (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.; Lopez-Caniego, M (reprint author), Univ Cantabria, CSIC, Inst Fis Cantabria, Avda Los Castros S-N, Santander, Spain.; Harrison, DL (reprint author), Kavli Inst Cosmol Cambridge, Madingley Rd, Cambridge CB3 OHA, England. EM dlh@ast.cam.ac.uk; mlopez@sciops.esa.int RI Barreiro, Rita Belen/N-5442-2014; bonavera, laura/E-9368-2017; Gonzalez-Nuevo, Joaquin/I-3562-2014; Herranz, Diego/K-9143-2014; Colombo, Loris/J-2415-2016; Lahteenmaki, Anne/L-5987-2013; OI Barreiro, Rita Belen/0000-0002-6139-4272; bonavera, laura/0000-0001-8039-3876; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Herranz, Diego/0000-0003-4540-1417; Colombo, Loris/0000-0003-4572-7732; TERENZI, LUCA/0000-0001-9915-6379; Stolyarov, Vladislav/0000-0001-8151-828X; Valiviita, Jussi/0000-0001-6225-3693; Hurier, Guillaume/0000-0002-1215-0706; Kurki-Suonio, Hannu/0000-0002-4618-3063; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Toffolatti, Luigi/0000-0003-2645-7386; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Nati, Federico/0000-0002-8307-5088; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993 FU ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MINECO (Spain); JA (Spain); RES (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC (EU); PRACE (EU); HEFCE 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, MINECO, JA, and, RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (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.cosmos.esa.int/web/planck/planck-collaboration. We are grateful to the H-ATLAS Executive Committee and primarily to the PIs, S. Eales and L. Dunne, for permission to use the unpublished H-ATLAS catalogue for the validation of the present catalogue. This research has made use of the "Aladin sky atlas" (Bonnarel et al. 2000), developed at CDS, Strasbourg Observatory, France. Part of this work was performed using the Darwin Supercomputer of the University of Cambridge High Performance Computing Service (http://www.hpc.cam.ac.uk/), provided by Dell Inc. using Strategic Research Infrastructure Funding from the HEFCE and funding from the STFC. 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 85 TC 1 Z9 1 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2016 VL 594 AR A26 DI 10.1051/0004-6361/201526914 PG 39 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4MG UT WOS:000385832200025 ER PT J AU Ade, PAR Aghanim, N Alves, MIR Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartlett, JG Bartolo, N Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bock, JJ Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Boulanger, F Bucher, M Burigana, C Butler, RC Calabrese, E Cardoso, JF Catalano, A Challinor, A Chamballu, A Chary, RR Chiang, HC Christensen, PR Colombi, S Colombo, LPL Combet, C Couchot, F Coulais, A Crill, BP Curto, A Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Dickinson, C Diego, JM Dole, H Donzelli, S Dore, O Douspis, M Ducout, A Dupac, X Efstathiou, G Elsner, F Ensslin, TA Eriksen, HK Falgarone, E Fergusson, J Finelli, F Forni, O Frailis, M Fraisse, AA Franceschi, E Frejsel, A Galeotta, S Galli, S Ganga, K Ghosh, T Giard, M Giraud-Heraud, Y Gjerlow, E Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Gudmundsson, JE Hansen, FK Hanson, D Harrison, DL Helou, G Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Hurier, G Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knoche, J Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Lattanzi, M Lawrence, CR Leahy, JP Leonardi, R Lesgourgues, J Levrier, F Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maggio, G Maino, D Mandolesi, N Mangilli, A Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Matarrese, S McGehee, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Moss, A Munshi, D Murphy, JA Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Orlando, E Oxborrow, CA Paci, F Pagano, L Pajot, F Paladini, R Paoletti, D Partridge, B Pasian, F Patanchon, G Pearson, TJ Peel, M Perdereau, O Perotto, L Perrotta, F Pettorino, V Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Reach, WT Rebolo, R Reinecke, M Remazeilles, M Renault, C Renzi, A Ristorcelli, I Rocha, G Rosset, C Rossetti, M Roudier, G Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savelainen, M Savini, G Scott, D Seiffert, MD Shellard, EPS Spencer, LD Stolyarov, V Stompor, R Strong, AW Sudiwala, R Sunyaev, R Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Tuovinen, J Umana, G Valenziano, L Valiviita, J Van Tent, F Vidal, M Vielva, P Villa, F Wade, LA Wandelt, BD Watson, R Wehus, IK Wilkinson, A Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Alves, M. I. R. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Bartolo, N. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bock, J. J. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bucher, M. Burigana, C. Butler, R. C. Calabrese, E. Cardoso, J. -F. Catalano, A. Challinor, A. Chamballu, A. Chary, R. -R. Chiang, H. C. Christensen, P. R. Colombi, S. Colombo, L. P. L. Combet, C. Couchot, F. Coulais, A. Crill, B. P. Curto, A. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J. -M. Desert, F. -X. Dickinson, C. Diego, J. M. Dole, H. Donzelli, S. Dore, O. Douspis, M. Ducout, A. Dupac, X. Efstathiou, G. Elsner, F. Ensslin, T. A. Eriksen, H. K. Falgarone, E. Fergusson, J. Finelli, F. Forni, O. Frailis, M. Fraisse, A. A. Franceschi, E. Frejsel, A. Galeotta, S. Galli, S. Ganga, K. Ghosh, T. Giard, M. Giraud-Heraud, Y. Gjerlow, E. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Gudmundsson, J. E. Hansen, F. K. Hanson, D. Harrison, D. L. Helou, G. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Hurier, G. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knoche, J. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Lattanzi, M. Lawrence, C. R. Leahy, J. P. Leonardi, R. Lesgourgues, J. Levrier, F. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maggio, G. Maino, D. Mandolesi, N. Mangilli, A. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Matarrese, S. McGehee, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Moss, A. Munshi, D. Murphy, J. A. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Orlando, E. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paladini, R. Paoletti, D. Partridge, B. Pasian, F. Patanchon, G. Pearson, T. J. Peel, M. Perdereau, O. Perotto, L. Perrotta, F. Pettorino, V. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Reach, W. T. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Renzi, A. Ristorcelli, I. Rocha, G. Rosset, C. Rossetti, M. Roudier, G. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savelainen, M. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Stolyarov, V. Stompor, R. Strong, A. W. Sudiwala, R. Sunyaev, R. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Tucci, M. Tuovinen, J. Umana, G. Valenziano, L. Valiviita, J. Van Tent, F. Vidal, M. Vielva, P. Villa, F. Wade, L. A. Wandelt, B. D. Watson, R. Wehus, I. K. Wilkinson, A. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2015 results XXV. Diffuse low-frequency Galactic foregrounds SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE diffuse radiation; ISM: general; radiation mechanisms: general; radio continuum: ISM; polarization; local insterstellar matter ID MICROWAVE-ANISOTROPY-PROBE; NORTH-POLAR SPUR; LARGE-MAGELLANIC-CLOUD; PERSEUS MOLECULAR-COMPLEX; BAYESIAN COMPONENT SEPARATION; CENTIMETER-WAVE CONTINUUM; COSMIC-RAY PROPAGATION; LAMBDA-ORIONIS RING; ALL-SKY SURVEY; RADIO-CONTINUUM AB We discuss the Galactic foreground emission between 20 and 100 GHz based on observations by Planck and WMAP. The total intensity in this part of the spectrum is dominated by free-free and spinning dust emission, whereas the polarized intensity is dominated by synchrotron emission. The Commander component-separation tool has been used to separate the various astrophysical processes in total intensity. Comparison with radio recombination line templates verifies the recovery of the free-free emission along the Galactic plane. Comparison of the high-latitude H alpha emission with our free-free map shows residuals that correlate with dust optical depth, consistent with a fraction (approximate to 30%) of H alpha having been scattered by high-latitude dust. We highlight a number of diffuse spinning dust morphological features at high latitude. There is substantial spatial variation in the spinning dust spectrum, with the emission peak (in I-v) ranging from below 20 GHz to more than 50 GHz. There is a strong tendency for the spinning dust component near many prominent H Pi regions to have a higher peak frequency, suggesting that this increase in peak frequency is associated with dust in the photo-dissociation regions around the nebulae. The emissivity of spinning dust in these diffuse regions is of the same order as previous detections in the literature. Over the entire sky, the Commander solution finds more anomalous microwave emission (AME) than the WMAP component maps, at the expense of synchrotron and free-free emission. This can be explained by the difficulty in separating multiple broadband components with a limited number of frequency maps. Future surveys, particularly at 5-20 GHz, will greatly improve the separation by constraining the synchrotron spectrum. We combine Planck and WMAP data to make the highest signal-to-noise ratio maps yet of the intensity of the all-sky polarized synchrotron emission at frequencies above a few GHz. Most of the high-latitude polarized emission is associated with distinct large-scale loops and spurs, and we re-discuss their structure. We argue that nearly all the emission at 40 degrees > l > -90 degrees is part of the Loop I structure, and show that the emission extends much further in to the southern Galactic hemisphere than previously recognised, giving Loop I an ovoid rather than circular outline. However, it does not continue as far as the "Fermi bubble/microwave haze", making it less probable that these are part of the same structure. We identify a number of new faint features in the polarized sky, including a dearth of polarized synchrotron emission directly correlated with a narrow, roughly 20 degrees long filament seen in H alpha at high Galactic latitude. Finally, we look for evidence of polarized AME, however many AME regions are significantly contaminated by polarized synchrotron emission, and we find a 2 sigma upper limit of 1.6% in the Perseus region. C1 [Bartlett, J. 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EM Clive.dickinson@manchester.ac.uk; j.p.leahy@manchester.ac.uk RI Lahteenmaki, Anne/L-5987-2013; Barreiro, Rita Belen/N-5442-2014; bonavera, laura/E-9368-2017; Gonzalez-Nuevo, Joaquin/I-3562-2014; Herranz, Diego/K-9143-2014; Colombo, Loris/J-2415-2016; OI Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Toffolatti, Luigi/0000-0003-2645-7386; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Nati, Federico/0000-0002-8307-5088; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Barreiro, Rita Belen/0000-0002-6139-4272; bonavera, laura/0000-0001-8039-3876; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Herranz, Diego/0000-0003-4540-1417; Colombo, Loris/0000-0003-4572-7732; TERENZI, LUCA/0000-0001-9915-6379; Stolyarov, Vladislav/0000-0001-8151-828X; Valiviita, Jussi/0000-0001-6225-3693; Hurier, Guillaume/0000-0002-1215-0706; Kurki-Suonio, Hannu/0000-0002-4618-3063 FU ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MINECO (Spain); JA (Spain); RES (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC (EU); PRACE (EU); ERC [307209]; STFC Consolidated Grant [ST/L000768/1] FX This paper is dedicated to the memory of the late Professor Rodney Deane Davies CBE FRS and Professor Richard John Davis OBE, both of whom contributed greatly to the Planck project. 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, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (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.cosmos.esa.int/web/planck/planck-collaboration. This research was supported by an ERC Starting (Consolidator) Grant (no. 307209) and STFC Consolidated Grant (no. ST/L000768/1). We have made extensive use of the HEALPix package and the IDL astronomy library. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 227 TC 1 Z9 1 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 OCT PY 2016 VL 594 AR A25 DI 10.1051/0004-6361/201526803 PG 45 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4MG UT WOS:000385832200024 ER PT J AU Ade, PAR Aghanim, N Ashdown, M Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartolo, N Battaglia, P Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bock, JJ Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Bucher, M Burigana, C Butler, RC Calabrese, E Cardoso, JF Catalano, A Chamballu, A Christensen, PR Colombi, S Colombo, LPL Crill, BP Curto, A Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Dickinson, C Diego, JM Dole, H Donzelli, S Dore, O Douspis, M Ducout, A Dupac, X Efstathiou, G Elsner, F Ensslin, TA Eriksen, HK Fergusson, J Finelli, F Forni, O Frailis, M Franceschi, E Frejsel, A Galeotta, S Galli, S Ganga, K Giard, M Giraud-Heraud, Y Gjerlow, E Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Hanson, D Harrison, DL Henrot-Versille, S Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Hurier, G Jaffe, AH Jaffe, TR Juvela, M Keihanen, E Keskitalo, R Kisner, TS Knoche, J Krachmalnicoff, N Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Lattanzi, M Lawrence, CR Leahy, JP Leonardi, R Lesgourgues, J Levrier, F Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maggio, G Maino, D Mandolesi, N Mangilli, A Maris, M Martin, PG Martinez-Gonzalez, E Masi, S Matarrese, S McGehee, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Montier, L Morgante, G Mortlock, D Moss, A Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Novikov, D Novikov, I Paci, F Pagano, L Pajot, F Paoletti, D Partridge, B Pasian, F Patanchon, G Pearson, TJ Peel, M Perdereau, O Perotto, L Perrotta, F Pettorino, V Piacentini, F Pierpaoli, E Pietrobon, D Pointecouteau, E Polenta, G Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Rebolo, R Reinecke, M Remazeilles, M Renzi, A Rocha, G Romelli, E Rosset, C Rossetti, M Roudier, G Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savelainen, M Scott, D Seiffert, MD Shellard, EPS Spencer, LD Stolyarov, V Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Tavagnacco, D Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Tuovinen, J Turler, M Umana, G Valenziano, L Valiviita, J Van Tent, B Vassallo, T Vielva, P Villa, F Wade, LA Wandelt, BD Watson, R Wehus, IK Wilkinson, A Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Ashdown, M. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartolo, N. Battaglia, P. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bock, J. J. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Bucher, M. Burigana, C. Butler, R. C. Calabrese, E. Cardoso, J. -F. Catalano, A. Chamballu, A. Christensen, P. R. Colombi, S. Colombo, L. P. L. Crill, B. P. Curto, A. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Dickinson, C. Diego, J. M. Dole, H. Donzelli, S. Dore, O. Douspis, M. Ducout, A. Dupac, X. Efstathiou, G. Elsner, F. Ensslin, T. A. Eriksen, H. K. Fergusson, J. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Frejsel, A. Galeotta, S. Galli, S. Ganga, K. Giard, M. Giraud-Heraud, Y. Gjerlow, E. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Hanson, D. Harrison, D. L. Henrot-Versille, S. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Hurier, G. Jaffe, A. H. Jaffe, T. R. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Knoche, J. Krachmalnicoff, N. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Lattanzi, M. Lawrence, C. R. Leahy, J. P. Leonardi, R. Lesgourgues, J. Levrier, F. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maggio, G. Maino, D. Mandolesi, N. Mangilli, A. Maris, M. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Matarrese, S. McGehee, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Montier, L. Morgante, G. Mortlock, D. Moss, A. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Novikov, D. Novikov, I. Paci, F. Pagano, L. Pajot, F. Paoletti, D. Partridge, B. Pasian, F. Patanchon, G. Pearson, T. J. Peel, M. Perdereau, O. Perotto, L. Perrotta, F. Pettorino, V. Piacentini, F. Pierpaoli, E. Pietrobon, D. Pointecouteau, E. Polenta, G. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Rebolo, R. Reinecke, M. Remazeilles, M. Renzi, A. Rocha, G. Romelli, E. Rosset, C. Rossetti, M. Roudier, G. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savelainen, M. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Stolyarov, V. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Tavagnacco, D. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Tucci, M. Tuovinen, J. Turler, M. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Vassallo, T. Vielva, P. Villa, F. Wade, L. A. Wandelt, B. D. Watson, R. Wehus, I. K. Wilkinson, A. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2015 results V. LFI calibration SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmic background radiation; instrumentation: polarimeters; methods: data analysis ID PROBE WMAP OBSERVATIONS; SYSTEMATIC-ERROR LIMITS; PRE-LAUNCH STATUS; BEAM PROFILES; MICROWAVE; MAPS AB We present a description of the pipeline used to calibrate the Planck Low Frequency Instrument (LFI) timelines into thermodynamic temperatures for the Planck 2015 data release, covering four years of uninterrupted operations. As in the 2013 data release, our calibrator is provided by the spin-synchronous modulation of the cosmic microwave background dipole, but we now use the orbital component, rather than adopting the Wilkinson Microwave Anisotropy Probe (WMAP) solar dipole. This allows our 2015 LFI analysis to provide an independent Solar dipole estimate, which is in excellent agreement with that of HFI and within 1 sigma (0.3% in amplitude) of the WMAP value. This 0.3% shift in the peak-to-peak dipole temperature from WMAP and a general overhaul of the iterative calibration code increases the overall level of the LFI maps by 0.45% (30 GHz), 0.64% (44 GHz), and 0.82% (70 GHz) in temperature with respect to the 2013 Planck data release, thus reducing the discrepancy with the power spectrum measured by WMAP. We estimate that the LFI calibration uncertainty is now at the level of 0.20% for the 70 GHz map, 0.26% for the 44 GHz map, and 0.35% for the 30 GHz map. We provide a detailed description of the impact of all the changes implemented in the calibration since the previous data release. C1 [Bucher, M.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Remazeilles, M.; Rosset, C.; Roudier, G.] Univ Paris Diderot, CNRS IN2P3, CEA Irfu, APC AstroParticule & Cosmol,Observ Paris,Sorbonne, 10 rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France. 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B.; Bonavera, L.; Curto, A.; Diego, J. M.; Gonzalez-Nuevo, J.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Toffolatti, L.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, Avda Castros S-N, Santander 39005, Spain. [Bartolo, N.; Liguori, M.; Matarrese, S.] Ist Nazl Fis Nucl, Sez Padova, Via Marzolo 8, I-35131 Padua, Italy. [Bock, J. J.; Colombo, L. P. L.; Crill, B. P.; Dore, O.; Gorski, K. M.; Hanson, D.; Hildebrandt, S. R.; Holmes, W. A.; Lawrence, C. R.; Mitra, S.; Pietrobon, D.; Prezeau, G.; Rocha, G.; Roudier, G.; Seiffert, M. D.; Wade, L. A.; Wehus, I. K.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA. [Bonaldi, A.; Davies, R. D.; Davis, R. J.; Dickinson, C.; Leahy, J. P.; Peel, M.; Remazeilles, M.; Watson, R.; Wilkinson, A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England. [Galli, S.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. 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[Van Tent, B.] Univ Paris 11, Phys Theor Lab, Batiment 210, F-91405 Orsay, France. [Van Tent, B.] CNRS, Batiment 210, F-91405 Orsay, France. [Kisner, T. S.] Lawrence Berkeley Natl Lab, Berkeley, CA USA. [Novikov, D.; Novikov, I.] Russian Acad Sci, Ctr Astro Space, Lebedev Phys Inst, 84-32 Profsoyuznaya St,GSP-7, Moscow 117997, Russia. [Ensslin, T. A.; Hovest, W.; Knoche, J.; Rachen, J. P.; Reinecke, M.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. [Hanson, D.] McGill Univ, McGill Phys, Ernest Rutherford Phys Bldg,3600 Rue Univ, Montreal, PQ H3A 2T8, Canada. [Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Bielewicz, P.] Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland. [Christensen, P. R.; Frejsel, A.; Novikov, I.] Niels Bohr Inst, Blegdamsvej 17, DK-1165 Copenhagen, Denmark. [Naselsky, P.] Univ Copenhagen, Niels Bohr Inst, Blegdamsvej 17, DK-1165 Copenhagen, Denmark. [Baccigalupi, C.; Bielewicz, P.; Danese, L.; de Zotti, G.; Paci, F.; Perrotta, F.] SISSA, Astrophys Sect, Via Bonomea 265, I-34136 Trieste, Italy. [Terenzi, L.] Univ E Campus, SMARTEST Res Ctr, Via Isimbardi 10, I-22060 Novedrate, CO, Italy. [Ade, P. A. R.; Munshi, D.; Spencer, L. D.] Cardiff Univ, Sch Phys & Astron, Queens Buildings, Cardiff CF24 3AA, S Glam, Wales. [Moss, A.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Bouchet, F. R.] UPMC, Sorbonne Univ, Inst Astrophys Paris, UMR7095, 98 Bis Blvd Arago, F-75014 Paris, France. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz 369167, Zelenchukskiy R, Russia. [Calabrese, E.] Univ Oxford, Subdept Astrophys, Keble Rd, Oxford OX1 3RH, England. [Lesgourgues, J.] CERN, PH TH, Div Theory, CH-1211 Geneva 23, Switzerland. [Benabed, K.; Benoit-Levy, A.; Colombi, S.; Elsner, F.; Hivon, E.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UMR7095, 98 Bis Blvd Arago, F-75014 Paris, France. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, E-18071 Granada, Spain. [Battaner, E.] Univ Granada, Inst Carlos Fis Teor & Computac 1, E-18071 Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, Aleje Ujazdowskie 4, PL-00478 Warsaw, Poland. RP Tomasi, M (reprint author), Univ Milan, Dipartimento Fis, Via Celoria 16, I-20133 Milan, Italy.; Tomasi, M (reprint author), IASF Milano, INAF, Via E Bassini 15, I-20133 Milan, Italy. EM maurizio.tomasi@unimi.it RI Colombo, Loris/J-2415-2016; Lahteenmaki, Anne/L-5987-2013; Barreiro, Rita Belen/N-5442-2014; bonavera, laura/E-9368-2017; Gonzalez-Nuevo, Joaquin/I-3562-2014; Herranz, Diego/K-9143-2014; OI Colombo, Loris/0000-0003-4572-7732; Valiviita, Jussi/0000-0001-6225-3693; Kurki-Suonio, Hannu/0000-0002-4618-3063; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Stolyarov, Vladislav/0000-0001-8151-828X; Barreiro, Rita Belen/0000-0002-6139-4272; bonavera, laura/0000-0001-8039-3876; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Herranz, Diego/0000-0003-4540-1417; TERENZI, LUCA/0000-0001-9915-6379; Hurier, Guillaume/0000-0002-1215-0706; Toffolatti, Luigi/0000-0003-2645-7386; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Nati, Federico/0000-0002-8307-5088; Pierpaoli, Elena/0000-0002-7957-8993 FU ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MINECO (Spain); JA (Spain); RES (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC (EU); PRACE (EU) 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, MINECO, JA and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (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.cosmos.esa.int/web/planck/planck_collaboration NR 45 TC 1 Z9 1 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 OCT PY 2016 VL 594 AR A5 DI 10.1051/0004-6361/201526632 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4MG UT WOS:000385832200022 ER PT J AU Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartlett, JG Bartolo, N Battaner, E Battye, R Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bock, JJ Bonaldi, A Bonavera, L Bond, JR Borrinll, J Bouchet, FR Bucher, M Burigana, C Butler, RC Calabrese, E Cardoso, JF Catalano, A Challinor, A Chamballu, A Chary, RR Chiang, HC Christensen, PR Church, S Clements, DL Colombi, S Colombo, LPL Combet, C Comis, B Couchot, F Coulais, A Crill, BP Curto, A Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Desert, FX Diego, JM Dolag, K Dole, H Donzelli, S Dore, O Douspis, M Ducout, A Dupac, X Efstathiou, G Elsner, F Ensslin, TA Eriksen, HK Falgarone, E Fergusson, J Finelli, F Forni, O Frailis, M Fraisse, AA Franceschi, E Frejsel, A Galeotta, S Galli, S Ganga, K Giard, M Giraud-Heraud, Y Gjerlow, E Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Gudmundsson, JE Hansen, FK Hanson, D Harrison, DL Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Hurier, G Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knoche, J Kunzo, M Kurki-Suonio, H Lagache, G Lahteennmaki, A Lamarre, JM Lasenby, A Lattanzi, M Lawrence, CR Leonardi, R Lesgourgues, J Levrier, F Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maggio, G Maino, D Mandolesi, N Mangilli, A Maris, M Martin, PG Martinez-Gonzalez, E Masi, S Matarrese, S McGehee, P Meinhold, PR Melchiorri', A Melin, JB Mendes, L Mennella, A Migliaccio, M Mitrao, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Moss, A Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Oxborrow, CA Paci, F Pagano, L Pajot, F Paoletti, D Partridge, B Pasian, F Patanchon, G Pearson, TJ Perdereau, O Perotto, L Perrotta, F Pettorino, V Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Popa, L Prate, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Rebolo, R Reinecke, M Remazeilles, M Renault, C Renzi, A Ristorcelli, I Rocha, G Roman, M Rosset, C Rossetti, M Roudier, G Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savelainen, M Savini, G Scott, D Seiffert, MD Shellard, EPS Spencer, LD Stolyarov, V Stompor, R Sudiwala, R Sunyaev, R Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Tuovinen, J Turler, M Umana, G Valenziano, L Valiviita', J Van Tent, B Vielva, P Villa, F Wade, LA Wandelt, BD Wehus, IK Weller, J White, SDM Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Bartolo, N. Battaner, E. Battye, R. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bock, J. J. Bonaldi, A. Bonavera, L. Bond, J. R. Borrinll, J. Bouchet, F. R. Bucher, M. Burigana, C. Butler, R. C. Calabrese, E. Cardoso, J. -F. Catalano, A. Challinor, A. Chamballu, A. Chary, R. -R. Chiang, H. C. Christensen, P. R. Church, S. Clements, D. L. Colombi, S. Colombo, L. P. L. Combet, C. Comis, B. Couchot, F. Coulais, A. Crill, B. P. Curto, A. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Desert, F. -X. Diego, J. M. Dolag, K. Dole, H. Donzelli, S. Dore, O. Douspis, M. Ducout, A. Dupac, X. Efstathiou, G. Elsner, F. Ensslin, T. A. Eriksen, H. K. Falgarone, E. Fergusson, J. Finelli, F. Forni, O. Frailis, M. Fraisse, A. A. Franceschi, E. Frejsel, A. Galeotta, S. Galli, S. Ganga, K. Giard, M. Giraud-Heraud, Y. Gjerlow, E. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Gudmundsson, J. E. Hansen, F. K. Hanson, D. Harrison, D. L. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Hurier, G. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knoche, J. Kunzo, M. Kurki-Suonio, H. Lagache, G. Lahteennmaki, A. Lamarre, J. -M. Lasenby, A. Lattanzi, M. Lawrence, C. R. Leonardi, R. Lesgourgues, J. Levrier, F. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maggio, G. Maino, D. Mandolesi, N. Mangilli, A. Maris, M. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Matarrese, S. McGehee, P. Meinhold, P. R. Melchiorri', A. Melin, J. -B. Mendes, L. Mennella, A. Migliaccio, M. Mitrao, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Moss, A. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paoletti, D. Partridge, B. Pasian, F. Patanchon, G. Pearson, T. J. Perdereau, O. Perotto, L. Perrotta, F. Pettorino, V. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Popa, L. Prate, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Renzi, A. Ristorcelli, I. Rocha, G. Roman, M. Rosset, C. Rossetti, M. Roudier, G. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savelainen, M. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Stolyarov, V. Stompor, R. Sudiwala, R. Sunyaev, R. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Tucci, M. Tuovinen, J. Turler, M. Umana, G. Valenziano, L. Valiviita', J. Van Tent, B. Vielva, P. Villa, F. Wade, L. A. Wandelt, B. D. Wehus, I. K. Weller, J. White, S. D. M. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2015 results XXIV. Cosmology from Sunyaev-Zeldovich cluster counts SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmological parameters; large-scale structure of Universe ID BARYON ACOUSTIC-OSCILLATIONS; SOUTH-POLE TELESCOPE; HALO MASS FUNCTION; LOCAL GALAXY CLUSTERS; WEAK-LENSING MASSES; X-RAY; INTRACLUSTER MEDIUM; SCALING RELATIONS; PRECISION COSMOLOGY; HUBBLE CONSTANT AB We present cluster counts and corresponding cosmological constraints from the Planck full mission data set. Our catalogue consists of 439 clusters detected via their Sunyaev-Zeldovich (SZ) signal down to a signal-to-noise ratio of 6, and is more than a factor of 2 larger than the 2013 Planck cluster cosmology sample. The counts are consistent with those from 2013 and yield compatible constraints under the same modelling assumptions. Taking advantage of the larger catalogue, we extend our analysis to the two-dimensional distribution in redshift and signal-to-noise. We use mass estimates from two recent studies of gravitational lensing of background galaxies by Planck clusters to provide priors on the hydrostatic bias parameter, (1 - b). In addition, we use lensing of cosmic microwave background (CMB) temperature fluctuations by Planck clusters as an independent constraint on this parameter. These various calibrations imply constraints on the present-day amplitude of matter fluctuations in varying degrees of tension with those from the Planck analysis of primary fluctuations in the CMB; for the lowest estimated values of (1 b) the tension is mild, only a little over one standard deviation, while it remains substantial (3.7 sigma) for the largest estimated value. We also examine constraints on extensions to the base flat Lambda CDM model by combining the cluster and CMB constraints. The combination appears to favour non-minimal neutrino masses, but this possibility does little to relieve the overall tension because it simultaneously lowers the implied value of the Hubble parameter, thereby exacerbating the discrepancy with most current astrophysical estimates. Improving the precision of cluster mass calibrations from the current 10%-level to 1% would significantly strengthen these combined analyses and provide a stringent test of the base Lambda CDM model. C1 [Bartlett, J. G.; Bucher, M.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Remazeilles, M.; Roman, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, APC, CNRS IN2P3, CEA Lrfu,Observ Paris,Sorbonne Paris Cite, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France. [Lahteennmaki, A.] Aalto Univ, Metsahovi Radio Observ, POB 13000, Aalto 00076, Finland. [Lahteennmaki, A.] Aalto Univ, Dept Radio Sci & Engn, POB 13000, Aalto 00076, Finland. [Bartolo, N.; Kunzo, M.] African Inst Math Sci, 6-8 Melrose Rd, ZA-7945 Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana, Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy. [Lagache, G.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Ashdown, M.; Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, Westville Campus,Private Bag X54001, ZA-4000 Durban, South Africa. [Kneissl, R.] ALMA Santiago Cent Off, Atacama Large Millimeter Submillimeter Array, Alonso Cordova 3107,763 0355 Casilla, Santiago, Chile. [Leonardi, R.] CGEE, SCS Qd 9,Lote C,Torre C,4 Andar, BR-70308200 Brasilia, DF, Brazil. [Bond, J. R.; Hanson, D.; Martin, P. G.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, 60 St George St, Toronto, ON M5S 3H8, Canada. [Banday, A. 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[Bersanelli, M.; Maino, D.; Mennella, A.; Rossetti, M.; Tomasi, M.] Univ Milan, Dipartimento Fis, Via Celoria 16, I-20133 Milan, Italy. [Gregorio, A.] Univ Trieste, Dipartimento Fis, Via A Valerio 2, I-34127 Trieste, Italy. [Renzi, A.] Univ Roma Tor Vergata, Dipartimento Matemat, Via Ric Sci 1, I-00133 Rome, Italy. [Christensen, P. R.] Niels Bohr Inst, Discovery Ctr, Blegdamsvej 17, Copenhagen, Denmark. [Naselsky, P.] Univ Copenhagen, Niels Bohr Inst, Discovery Ctr, Blegdamsvej 17, DK-1165 Copenhagen, Denmark. [Kneissl, R.] European Southern Observ, ESO Vitacura, Alonso Cordova 3107,Casilla 19001, Santiago, Chile. [Dupac, X.; Lopez-Caniego, M.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Camino Bajo Castillo S-N, Madrid, Spain. [Tauber, J. A.] European Space Agcy, Estec, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. [Matarrese, S.] Ist Nazl Fis Nucl, Gran Sasso Sci Inst, Viale F Crispi 7, I-67100 Laquila, Italy. [Pettorino, V.] HGSFP, Philosophenweg 16, D-69120 Heidelberg, Germany. [Pettorino, V.] Heidelberg Univ, Dept Theoret Phys, Philosophenweg 16, D-69120 Heidelberg, Germany. [Partridge, B.] Haverford Coll, Dept Astron, 370 Lancaster Ave, Haverford, PA USA. [Kurki-Suonio, H.; Lahteennmaki, A.; Savelainen, M.; Suur-Uski, A. -S.; Valiviita', J.] Univ Helsinki, Helsinki Inst Phys, Gustaf Hallstromin Katu 2, Helsinki 00560, Finland. [Umana, G.] INAF Osservatorio Astrofis Catania, Via S Sofia 78, Catania, Italy. [de Zotti, G.] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35131 Padua, Italy. [Polenta, G.] INAF Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy. [Frailis, M.; Galeotta, S.; Gregorio, A.; Maggio, G.; Maris, M.; Pasian, F.; Zacchei, A.] INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, I-40127 Trieste, Italy. [Burigana, C.; Butler, R. C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Paoletti, D.; Sandri, M.; Terenzi, L.; Toffolatti, L.; Valenziano, L.; Villa, F.] INAF IASF Bologna, Via Gobetti 101, I-40129 Bologna, Italy. [Bersanelli, M.; Donzelli, S.; Maino, D.; Mennella, A.; Rossetti, M.; Tomasi, M.] INAF IASF Milano, Via E Bassini 15, I-20133 Milan, Italy. [Burigana, C.; Finelli, F.] Ist Nazl Fis Nucl, Sez Bologna, Via Irnerio 46, I-40126 Bologna, Italy. [Melchiorri', A.; Pagano, L.] Univ Roma Sapienza, Sez Roma 1, Ist Nazl Fis Nucl, Piazzale Aldo Moro 2, I-00185 Rome, Italy. [Renzi, A.] Univ Roma Tor Vergata, Sez Roma 2, Ist Nazl Fis Nucl, Via Ric Sci 1, I-00185 Rome, Italy. [Gregorio, A.] INFN Natl Inst Nucl Phys, Via Valerio 2, I-34127 Trieste, Italy. [Desert, F. -X.] Univ Grenoble Alpes, IPAG, CNRS, F-38000 Grenoble, France. [Turler, M.] Univ Geneva, Dept Astron, ISDC, Ch Ecogia 16, CH-1290 Versoix, Switzerland. [Mitrao, S.] IUCAA, Post Bag 4,Pune Univ Campus, Pune 411007, Maharashtra, India. [Clements, D. L.; Ducout, A.; Jaffe, A. H.; Mortlock, D.] Imperial Coll London, Astrophys Grp, Blackett Lab, Prince Consort Rd, London SW7 2AZ, England. [Chary, R. -R.; McGehee, P.; Pearson, T. J.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Benoit, A.] Univ Joseph Fourier Grenoble I, CNRS, Inst Neel, 25 Rue Martyrs, Grenoble, France. [Dole, H.] Inst Univ France, 103 Bd St Michel, F-75005 Paris, France. [Aghanim, N.; Aumont, J.; Chamballu, A.; Dole, H.; Douspis, M.; Hurier, G.; Kunzo, M.; Lagache, G.; Mangilli, A.; Miville-Deschenes, M. -A.; Pajot, F.; Puget, J. -L.; Remazeilles, M.] Univ Paris Saclay, CNRS, Inst Astrophys Spatiale, Bat 121, F-91405 Orsay, France. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Ducout, A.; Elsner, F.; Hivon, E.; Migliaccio, M.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] CNRS, Inst Astrophys Paris, UMR7095, 98bis Blvd Arago, F-75014 Paris, France. [Lesgourgues, J.] Rhein Westfal TH Aachen, Inst Theoret Teilchenphys & Kosmol, D-52056 Aachen, Germany. [Popa, L.] Inst Space Sci, Bucharest, Romania. [Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D. L.; Sutton, D.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Eriksen, H. K.; Gjerlow, E.; Hansen, F. K.; Lilje, P. B.; Wehus, I. K.] Univ Oslo, Inst Theoret Astrophys, N-0371 Oslo, Norway. [Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, C Via Lactea S-N, Tenerife 38205, Spain. [Barreiro, R. B.; Bonavera, L.; Curto, A.; Diego, J. M.; Gonzalez-Nuevo, J.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Toffolatti, L.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, Avda Castros S-N, Santander 39005, Spain. [Bartolo, N.; Liguori, M.; Matarrese, S.] Ist Nazl Fis Nucl, Sez Padova, Via Marzolo 8, I-35131 Padua, Italy. [Bartlett, J. G.; Colombo, L. P. L.; Crill, B. P.; Dore, O.; Gorski, K. M.; Hanson, D.; Hildebrandt, S. R.; Holmes, W. A.; Lawrence, C. R.; Mitrao, S.; Pietrobon, D.; Prezeau, G.; Rocha, G.; Roudier, G.; Seiffert, M. D.; Wade, L. A.; Wehus, I. K.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA. [Battye, R.; Bock, J. J.; Bonaldi, A.; Davies, R. D.; Davis, R. J.; Noviello, F.; Remazeilles, M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England. [Galli, S.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Ashdown, M.; Challinor, A.; Curto, A.; Gratton, S.; Harrison, D. L.; Lasenby, A.; Migliaccio, M.; Sutton, D.] Kavli Inst Cosmol Cambridge, Madingley Rd, Cambridge CB3 0HA, England. [Stolyarov, V.] Kazan Fed Univ, 18 Kremlyovskaya St, Kazan 420008, Russia. [Couchot, F.; Henrot-Versille, S.; Mangilli, A.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, LAL, CNRS IN2P3, F-91898 Orsay, France. [Catalano, A.; Coulais, A.; Falgarone, E.; Lamarre, J. -M.; Levrier, F.; Roudier, G.] Observ Paris, CNRS, LERMA, 61 Ave Observ, F-75000 Paris, France. [Arnaud, M.; Chamballu, A.; Prate, G. W.] Univ Paris Diderot, CEA DSM, IRFU Serv Astrophys, Lab AIM,CNRS, Bat 709, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, Lab Traitement & Commun Informat, UMR 5141, 46 Rue Barrault, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom ParisTech, 46 Rue Barrault, F-75634 Paris 13, France. [Catalano, A.; Combet, C.; Comis, B.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble Alpes, Lab Phys Subat & Cosmol, CNRS IN2P3, 53 Rue Martyrs, F-38026 Grenoble, France. [Van Tent, B.] Univ Paris Sud 11, Lab Phys Theor, Batiment 210, F-91405 Orsay, France. [Van Tent, B.] CNRS, Batiment 210, F-91405 Orsay, France. [Kisner, T. S.] Lawrence Berkeley Natl Lab, Berkeley, CA USA. [Novikov, D.; Novikov, I.] Russian Acad Sci, Lebedev Phys Inst, Ctr Astro Space, 84-32 Profsoyuznaya St,GS7, Moscow 117997, Russia. [Dolag, K.; Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Knoche, J.; Rachen, J. P.; Reinecke, M.; Sunyaev, R.; White, S. D. M.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. [Hanson, D.] McGill Univ, McGill Phys, Ernest Rutherford Phys Bldg,3600 Rue Univ, Montreal, PQ H3A 2T8, Canada. [Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Bielewicz, P.] Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland. [Christensen, P. R.; Frejsel, A.; Novikov, I.] Niels Bohr Inst, Blegdamsvej 17, DK-1165 Copenhagen, Denmark. [Naselsky, P.] Univ Copenhagen, Niels Bohr Inst, Blegdamsvej 17, DK-1165 Copenhagen, Denmark. [Gudmundsson, J. E.] Nordita Nord Inst Theoret Phys, Roslagstullsbacken 23, S-10691 Stockholm, Sweden. [Savini, G.] UCL, Opt Sci Lab, Gower St, London, England. [Baccigalupi, C.; Bielewicz, P.; de Zotti, G.; Paci, F.; Perrotta, F.] SISSA, Astrophys Sect, Via Bonomea 265, I-34136 Trieste, Italy. [Terenzi, L.] Univ E Campus, SMARTEST Res Ctr, Via Isimbardi 10, I-22060 Novedrate, CO, Italy. [Ade, P. A. R.; Danese, L.; Munshi, D.; Spencer, L. D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales. [Moss, A.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Bouchet, F. R.] Sorbonne Univ UPMC, UMR7095, Inst Astrophys Paris, 98bis Blvd Arago, F-75014 Paris, France. [Sunyaev, R.] Russian Acad Sci, Space Res Inst IKI, Profsoyuznaya Str 84-32, Moscow 117997, Russia. [Borrinll, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Karachai Cherkessian Rep 369167, Zelenchukskiy R, Russia. [Church, S.] Stanford Univ, Dept Phys, Varian Phys Bldg,382 Via Pueblo Mall, Stanford, CA USA. [Calabrese, E.] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England. [Gudmundsson, J. E.] Stockholm Univ, Oskar Klein Ctr Cosmoparticle Phys, Dept Phys, AlbaNova, S-10691 Stockholm, Sweden. [Lesgourgues, J.] CERN, PH TH, Div Theory, CH-1211 Geneva 23, Switzerland. [Benabed, K.; Benoit-Levy, A.; Colombi, S.; Elsner, F.; Hivon, E.; Prunet, S.; Wandelt, B. D.] UPMC Univ Paris 06, UMR7095, 98bis Blvd Arago, F-75014 Paris, France. [Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Dolag, K.; Weller, J.] Ludwig Maximilian Univ Munich, Univ Observ, Scheinerstr 1, D-81679 Munich, Germany. [Battaner, E.] Univ Granada, Dept Fis Teor & Cosmos, Fac Ciencias, Granada 81679, Spain. [Battaner, E.] Univ Granada, Inst Carlos Fis Teor & Computac 1, Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, Aleje Ujazdowskie 4, PL-00478 Warsaw, Poland. RP Bonaldi, A (reprint author), Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England. EM anna.bonaldi@manchester.ac.uk RI Gonzalez-Nuevo, Joaquin/I-3562-2014; Herranz, Diego/K-9143-2014; Colombo, Loris/J-2415-2016; Barreiro, Rita Belen/N-5442-2014; bonavera, laura/E-9368-2017 OI Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Toffolatti, Luigi/0000-0003-2645-7386; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Nati, Federico/0000-0002-8307-5088; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Herranz, Diego/0000-0003-4540-1417; Colombo, Loris/0000-0003-4572-7732; TERENZI, LUCA/0000-0001-9915-6379; Stolyarov, Vladislav/0000-0001-8151-828X; Valiviita, Jussi/0000-0001-6225-3693; Hurier, Guillaume/0000-0002-1215-0706; Kurki-Suonio, Hannu/0000-0002-4618-3063; Juvela, Mika/0000-0002-5809-4834; Barreiro, Rita Belen/0000-0002-6139-4272; bonavera, laura/0000-0001-8039-3876 FU ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MINECO (Spain); JA (Spain); RES (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC (EU); PRACE (EU) 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, MINECO, JA and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (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.cosmos.esa.int/web/planck/planck-collaboration. NR 103 TC 3 Z9 3 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2016 VL 594 AR A24 DI 10.1051/0004-6361/201525833 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4MG UT WOS:000385832200015 ER PT J AU Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartolo, N Basak, S Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bock, JJ Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Bucher, M Burigana, C Butler, RC Calabrese, E Cardoso, JF Catalano, A Challinor, A Chamballu, A Chiang, HC Christensen, PR Church, S Clements, DL Colombi, S Colombo, LPL Combet, C Couchot, F Coulais, A Crill, BP Curto, A Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Desert, FX Diego, JM Dole, H Donzelli, S Dore, O Douspis, M Ducout, A Dupac, X Efstathiou, G Elsner, F Ensslin, TA Eriksen, HK Feeney, S Fergusson, J Finelli, F Forni, O Frailis, M Fraisse, AA Franceschi, E Frejse, A Galeotta, S Galli, S Ganga, K Giard, M Giraud-Heraud, Y Gjerlow, E Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Gudmundsson, JE Hansen, FK Hanson, D Harrison, DL Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Hurier, G Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Knoche, J Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Lattanzi, M Lawrence, CR Leonardi, R Lesgourgues, J Levrier, F Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maggio, G Maino, D Mandolesi, N Mangilli, A Maris, M Martin, PG Martinez-Gonzalez, E Masi, S Matarrese, S McEwen, JD McGehee, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Moss, A Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Oxborrow, CA Paci, F Pagano, L Pajot, F Paoletti, D Pasian, F Patanchon, G Peiris, HV Perdereau, O Perotto, L Perrotta, F Pettorino, V Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pogosyan, D Pointecouteau, E Polenta, G Popa, L Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Rebolo, R Reinecke, M Remazeilles, M Renault, C Renzi, A Ristorcelli, I Rocha, G Rosset, C Rossetti, M Roudier, G Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savelainen, M Savini, G Scott, D Seiffert, MD Shellard, EPS Spencer, LD Stolyarov, V Stompor, R Sudiwala, R Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Tuovinen, J Valenziano, L Valiviita, J Van Tent, F Vielva, P Villa, F Wade, LA Wandelt, BD Wehus, IK Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartolo, N. Basak, S. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J-P. Bersanelli, M. Bielewicz, P. Bock, J. J. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Bucher, M. Burigana, C. Butler, R. C. Calabrese, E. Cardoso, J. -F. Catalano, A. Challinor, A. Chamballu, A. Chiang, H. C. Christensen, P. R. Church, S. Clements, D. L. Colombi, S. Colombo, L. P. L. Combet, C. Couchot, F. Coulais, A. Crill, B. P. Curto, A. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Desert, F. -X. Diego, J. M. Dole, H. Donzelli, S. Dore, O. Douspis, M. Ducout, A. Dupac, X. Efstathiou, G. Elsner, F. Ensslin, T. A. Eriksen, H. K. Feeney, S. Fergusson, J. Finelli, F. Forni, O. Frailis, M. Fraisse, A. A. Franceschi, E. Frejse, A. Galeotta, S. Galli, S. Ganga, K. Giard, M. Giraud-Heraud, Y. Gjerlow, E. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Gudmundsson, J. E. Hansen, F. K. Hanson, D. Harrison, D. L. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Hurier, G. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Knoche, J. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Lattanzi, M. Lawrence, C. R. Leonardi, R. Lesgourgues, J. Levrier, F. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maggio, G. Maino, D. Mandolesi, N. Mangilli, A. Maris, M. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Matarrese, S. McEwen, J. D. McGehee, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Moss, A. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paoletti, D. Pasian, F. Patanchon, G. Peiris, H. V. Perdereau, O. Perotto, L. Perrotta, F. Pettorino, V. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pogosyan, D. Pointecouteau, E. Polenta, G. Popa, L. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Renzi, A. Ristorcelli, I. Rocha, G. Rosset, C. Rossetti, M. Roudier, G. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savelainen, M. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Stolyarov, V. Stompor, R. Sudiwala, R. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Tucci, M. Tuovinen, J. Valenziano, L. Valiviita, J. Van Tent, F. Vielva, P. Villa, F. Wade, L. A. Wandelt, B. D. Wehus, I. K. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2015 results XVIII. Background geometry and topology of the Universe SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmic background radiation; cosmology: observations; cosmological parameters; gravitation; methods: data analysis; methods:statistical ID DODECAHEDRAL SPACE TOPOLOGY; BIANCHI-VIIH MODELS; WMAP DATA; SKY MAPS; COBE-DMR; COSMIC CRYSTALLOGRAPHY; COSMOLOGICAL MODELS; TOROIDAL UNIVERSE; CMB ANISOTROPY; MICROWAVE AB Maps of cosmic microwave background (CMB) temperature and polarization from the 2015 release of Planck data provide the highest quality full-sky view of the surface of last scattering available to date. This enables us to detect possible departures from a globally isotropic cosmology. We present the first searches using CMB polarization for correlations induced by a possible non-trivial topology with a fundamental domain that intersects, or nearly intersects, the last-scattering surface (at comoving distance chi(rec)), both via a direct scan for matched circular patterns at the intersections and by an optimal likelihood calculation for specific topologies. We specialize to flat spaces with cubic toroidal (T3) and slab (T1) topologies, finding that explicit searches for the latter are sensitive to other topologies with antipodal symmetry. These searches yield no detection of a compact topology with a scale below the diameter of the last-scattering surface. The limits on the radius R-i of the largest sphere inscribed in the fundamental domain (at log-likelihood ratio Delta ln L > -5 relative to a simply-connected flat Planck best-fit model) are: R-i > 0.97 chi(rec) for the T3 cubic torus; and R-i > 0.56 chi(rec) for the T1 slab. The limit for the T3 cubic torus from the matched-circles search is numerically equivalent, R-i > 0.97 chi(rec) at 99% confidence level from polarization data alone. We also perform a Bayesian search for an anisotropic global Bianchi VIIh geometry. In the non-physical setting, where the Bianchi cosmology is decoupled from the standard cosmology, Planck temperature data favour the inclusion of a Bianchi component with a Bayes factor of at least 2.3 units of log-evidence. However, the cosmological parameters that generate this pattern are in strong disagreement with those found from CMB anisotropy data alone. Fitting the induced polarization pattern for this model to the Planck data requires an amplitude of -0.10 +/- 0.04 compared to the value of + 1 if the model were to be correct. In the physically motivated setting, where the Bianchi parameters are coupled and fitted simultaneously with the standard cosmological parameters, we find no evidence for a Bianchi VIIh cosmology and constrain the vorticity of such models to (omega/H)(0) < 7.6 x 10(-10) (95% CL). C1 [Bucher, M.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Remazeilles, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, APC, CNRS IN2P3, CEA Lrfu,Observ Paris,Sorbonne Paris Cite, 10 Rue Alice Domon & Leonie Duquet, F-13 Paris, France. [Lahteenmaki, A.] Aalto Univ, Metsahovi Radio Observ, POB 13000, Aalto 00076, Finland. [Lahteenmaki, A.] Aalto Univ, Dept Radio Sci & Engn, POB 13000, Aalto 00076, Finland. [Kunz, M.] African Inst Math Sci, 6-8 Melrose Rd, Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci, Ctr Data, Via Politecn Snc, I-00133 Rome, Italy. 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EM a.jaffe@imperial.ac.uk RI Lahteenmaki, Anne/L-5987-2013; Barreiro, Rita Belen/N-5442-2014; bonavera, laura/E-9368-2017; Gonzalez-Nuevo, Joaquin/I-3562-2014; Herranz, Diego/K-9143-2014; Colombo, Loris/J-2415-2016; OI Kurki-Suonio, Hannu/0000-0002-4618-3063; Barreiro, Rita Belen/0000-0002-6139-4272; bonavera, laura/0000-0001-8039-3876; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Herranz, Diego/0000-0003-4540-1417; Colombo, Loris/0000-0003-4572-7732; Hivon, Eric/0000-0003-1880-2733; TERENZI, LUCA/0000-0001-9915-6379; Stolyarov, Vladislav/0000-0001-8151-828X; Valiviita, Jussi/0000-0001-6225-3693; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Toffolatti, Luigi/0000-0003-2645-7386; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Nati, Federico/0000-0002-8307-5088; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993 FU ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MINECO (Spain); JA (Spain); RES (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC (EU); PRACE (EU); Canada Foundation for Innovation under Compute Canada; Government of Ontario; Ontario Research Fund Research Excellence; University of Toronto 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, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (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.cosmos.esa.int/web/planck/planck-collaboration. The authors thank Andrew Pontzen for computing Bianchi VIIh polarization templates for the best-fit models resulting from the analysis of temperature data. We acknowledge the UCL Legion High Performance Computing Facility (Legion@UCL) and associated support services in the completion of this work. Parts of the computations were performed on the Andromeda and Perseus clusters of the University of Geneva, as well as the Carver IBM iDataPlex, the Hopper Cray XE6, and the Edison Cray XC30 at NERSC, and 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. NR 107 TC 0 Z9 0 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2016 VL 594 AR A18 DI 10.1051/0004-6361/201525829 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics