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
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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
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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
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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
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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
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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
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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.
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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
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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.
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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.
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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.
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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
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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.
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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.
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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
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U1 5
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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).
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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
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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
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U1 5
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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
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U1 6
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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
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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
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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
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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
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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
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U1 3
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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
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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
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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
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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
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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
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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
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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
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Baldaccini, F
Ballardin, G
Ballmer, SW
Barayoga, JC
Barclay, SE
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Barker, D
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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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Bizouard, MA
Blackburn, JK
Blair, CD
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Blair, RM
Bloemen, S
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Cheeseboro, BD
Chen, HY
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Chow, JH
Christensen, N
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Countryman, ST
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Cowart, MJ
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Cunningham, L
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Devine, RC
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Diaz, MC
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Di Pace, S
Di Palma, I
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Downes, TP
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Everett, R
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Fang, Q
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Farr, WM
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Fehrmann, H
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Ferrini, F
Fidecaro, F
Fiori, I
Fiorucci, D
Fisher, RP
Flaminio, R
Fletcher, M
Fong, H
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Frasca, S
Frasconi, F
Frei, Z
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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
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Gonzalez, G
Castro, JMG
Gopakumar, A
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Guo, X
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Hall, ED
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Hardwick, T
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Heurs, M
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Hofman, D
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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
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Jacqmin, T
Jang, H
Jani, K
Jaranowski, P
Jawahar, S
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Johnson, WW
Johnson-McDaniel, NK
Jones, DI
Jones, R
Jonker, RJG
Ju, L
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Kalogera, V
Kandhasamy, S
Kang, G
Kanner, JB
Kapadia, SJ
Karki, S
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Katzman, W
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Kefelian, F
Kehl, MS
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Kelley, DB
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Khan, S
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Kim, W
Kim, YM
Kimbrell, SJ
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King, PJ
Kissel, JS
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Kleybolte, L
Klimenko, S
Koehlenbeck, SM
Koley, S
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Kontos, A
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Korth, WZ
Kowalska, I
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Kringel, V
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Kumar, R
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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.
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[Dasgupta, A.; Gaur, G.; Gupta, M. K.; Khan, Z.; Kumar, R.; Srivastava, A. K.; Sunil, S.] Inst Plasma Res, Bhat 382428, Gandhinagar, India.
[Daw, E. J.; Edo, T. B.; Kennedy, R.; Tomlinson, C.] Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England.
[Diaz, M. C.; Geng, P.; Key, J. S.; Morriss, S. R.; Mukherjee, S.; Normandin, M. E. N.; Quetschke, V.; Rakhmanov, M.; Romano, J. D.; Stone, R.; Torres, C. V.; Tuyenbayev, D.; Valdes, G.] Univ Texas Rio Grande Valley, Brownsville, TX 78520 USA.
[Di Giovanni, M.; Leonardi, M.; Prodi, G. A.; Tringali, M. C.] Univ Trento, Dipartimento Fis, I-38123 Povo, Trento, Italy.
[Di Giovanni, M.; Leonardi, M.; Prodi, G. A.; Tiwari, S.; Tringali, M. C.] Ist Nazl Fis Nucl, Trento Inst Fundamental Phys & Applicat, I-38123 Povo, Trento, Italy.
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[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.
[Fong, H.; Kehl, M. S.; Kumar, P.; Pfeiffer, H. P.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto M5S 3H8, ON, Canada.
[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.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA.
[Gopakumar, A.; Haney, M.; Unnikrishnan, C. S.] Tata Inst Fundamental Res, Mumbai 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.
[Hamilton, H.; Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA.
[Healy, J.; Henry, J.; Lange, J.; Lousto, C.; 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.
[Ain, A.; Haris, K.; Pai, A.; Saleem, M.] IISER TVM, CET Campus, Trivandrum 695016, Kerala, India.
[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.
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[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.] CNRS, ESPCI, 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.
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[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.
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RP Abbott, BP (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
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
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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.
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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
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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
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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
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U1 3
U2 3
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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
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AR 150
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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
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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
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U1 9
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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
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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
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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
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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.
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[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.
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[Bartolo, N.; Liguori, M.; Matarrese, S.] Ist Nazl Fis Nucl, Sez Padova, Via Marzolo 8, I-35131 Padua, Italy.
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[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.
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RP Perdereau, O; Tristram, M (reprint author), Univ Paris 11, LAL, CNRS, IN2P3, Orsay, France.
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.
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[Terenzi, L.] Univ E Campus, SMARTEST Res Ctr, Via Isimbardi 10, I-22060 Novedrate, CO, Italy.
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, Inst Astrophys Paris, UMR 7095, 98bis Blvd Arago, F-75014 Paris, France.
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.
[Calabrese, E.] Univ Oxford, Subdept Astrophys, Keble Rd, Oxford OX1 3RH, England.
[Gudmundsson, J. E.] Univ Stockholm, AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, Dept Phys, S-10691 Stockholm, Sweden.
[Lesgourgues, J.] CERN, PH TH, Div Theory, Geneva 23, Switzerland.
[Benabed, K.; Benoit-Levy, A.; Colombi, S.; Elsner, F.; Hivon, F.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UMR 7095, 98bis Blvd Arago, F-75014 Paris, France.
[Alves, M. I. R.; Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, TRAP, 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, Fac Ciencias, Dept Fis Teor & Cosmos, E-18071 Granada, Spain.
[Battaner, E.] Univ Granada, Inst Carlos Fis Teor & Computac 1, E-18071 Granada, Spain.
[Orlando, E.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, 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 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.
C1 [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Castex, G.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Le Jenne, M.; Patanchon, G.; Piat, M.; Racine, B.; 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-75205 Paris 13, France.
[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.
[Kneissl, R.] ALMA Santiago Cent Off, Atacama Large Millimeter Submillimeter Array, Alonso Cordova 3107,Vitacura,Casilla 763 0355, Santiago, Chile.
[Leonardi, R.] CGEE, SCS Qd 9,Lote C,Tone 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 Ave Colonel Roche,BP 44346, F-31028 Toulouse, France.
[Tuovinen, J.] Trinity Coll Dublin, CRANN, Dublin, Ireland.
[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, DAMTP, Ctr Theoret Cosmol, 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, CH-1211 Geneva 4, Switzerland.
[Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[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, POB 9010, NL-6500 GL Nijmegen, Netherlands.
[Scott, D.] 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.
[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 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 0065, 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 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.; Molinari, D.; Natoli, P.; Trombetti, T.] 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-00133 Rome, Italy.
[Bersanelli, M.; Krachmalnicoff, N.; 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.
[Fantaye, Y.; 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, DK-1165 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,Vitacura,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, D-69120 Heidelberg, Germany.
[Pettorino, V.] Heidelberg Univ, Dept Theoret Phys, D-69120 Heidelberg, Germany.
[Kurki-Suonio, H.; Savelainen, M.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Helsinki Inst Phys, Gustaf Hallstromin Katu 2, Helsinki 0065, Finland.
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[Barreiro, R. B.; Bonavera, L.; Casaponsa, B.; 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, Spain.
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[Stolyarov, V.] Kazan Fed Univ, 18 Kremlyovskaya St, Kazan 420008, Russia.
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[Christensen, P. R.; Frejsel, A.; Novikov, I.] Niels Bohr Inst, Blegdamsvej 17, DK-1165 Copenhagen, Denmark.
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[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.
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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
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Sanghera, HS
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Saunders, RDE
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Schaefer, BM
Schammel, MP
Scott, D
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Serra, P
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Shimwell, TW
Shiraishi, M
Smith, K
Souradeep, T
Spencer, LD
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Viel, M
Vielva, P
Villa, F
Wade, LA
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Wandelt, BD
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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.
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Masi, S.
Matarrese, S.
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McGehee, P.
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Melchiorri, A.
Melin, J. -B.
Mendes, L.
Mennella, A.
Migliaccio, M.
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Miville-Deschenes, M. -A.
Molinari, D.
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Shimwell, T. W.
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Souradeep, T.
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Stanford, S. A.
Stern, D.
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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.
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[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. S.] Lawrence Berkeley Natl Lab, Berkeley, CA USA.
[Novikov, D.; Novikov, I.] Russian Acad Sci, Ctr Astro Space, Lebedev Phys Inst, 84-32 Prof St,GSP-7, Moscow 117997, Russia.
[Arroja, F.; Gauthier, C.] Natl Taiwan Univ, Leung Ctr Cosmol & Particle Astrophys, Taipei 10617, Taiwan.
[Dolag, K.; Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Kim, J.; 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.
[Boehringer, H.; Chon, G.; Strong, A. W.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
[Hanson, D.] McGill Univ, McGill Phys, Ernest Rutherford Phys Bldg,3600 Rue Univ, Montreal, PQ H3A 2T8, Canada.
[Burenin, R.] Moscow Inst Phys & Technol, Inst Per 9, Dolgoprudnyi 141700, Russia.
[McEwen, J. D.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[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.; Liu, H.; Novikov, I.] Niels Bohr Inst, Blegdamsvej 17, Copenhagen, Denmark.
[Naselsky, P.] Univ Copenhagen, Niels Bohr Inst, Blegdamsvej 17, Copenhagen, Denmark.
[Gerbino, M.; Gudmundsson, J. E.] Nordita Nord Inst Theoret Phys, Roslagstullsbacken 23, S-10691 Stockholm, Sweden.
[Savini, G.] UCL, Opt Sci Lab, Gower St, London, England.
[Smith, K.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.
[Farhang, M.] Shahid Beheshti Univ, Dept Phys, Tehran, Iran.
[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.
[Ma, Y. -Z.] Univ KwaZulu Natal, Sch Chem & Phys, Westville Campus,Private Bag X54001, ZA-4000 Durban, South Africa.
[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.
[Frolov, A.] Simon Fraser Univ, Dept Phys, 8888 Univ Dr, Burnaby, BC, Canada.
[Bouchet, F. R.; Di Valentino, E.; Lilley, M.; Mottet, S.] UPMC, Sorbonne Univ, UMR7095, Inst Astrophys Paris, 98bis Blvd Arago, F-75014 Paris, France.
[Burenin, R.; 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, Russia.
[Church, S.] Stanford Univ, Dept Phys, Varian Phys Bldg,382 Via Pueblo Mall, Stanford, CA 94305 USA.
[Shimwell, T. W.] Sterrewacht Leiden, POB 9513, NL-2300 RA Leiden, Netherlands.
[Calabrese, E.; Dunkley, J.; Welikala, N.] Univ Oxford, Subdept Astrophys, Keble Rd, Oxford OX1 3RH, England.
[Hamann, J.] Univ Sydney, Sydney Inst Astron, Sch Phys, A28, Sydney, NSW 2006, Australia.
[Khamitov, I.] TUBITAK Natl Observ, Akdeniz Univ Campus, TR-07058 Antalya, Turkey.
[Gerbino, M.; Gudmundsson, J. E.] Stockholm Univ, AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, Dept Phys, S-10691 Stockholm, Sweden.
[Hamann, J.; Lesgourgues, J.] CERN, PH TH, Div Theory, 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, 98bis Blvd Arago, F-75014 Paris, France.
[Schaefer, B. M.] Heidelberg Univ, Inst Theoret Astrophys, Philosophenweg 12, D-69120 Heidelberg, Germany.
[Mei, S.] Univ Denis Diderot Paris 7, F-75205 Paris 13, France.
[Alves, M. I. R.; Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Ilic, S.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.; Sauve, A.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France.
[Reach, W. 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. Generated at a cost of some 25 million CPU-hours spread across multiple high-performance-computing (HPC) platforms, FFP8 is used to validate and verify analysis algorithms and their implementations, and to remove biases from and quantify uncertainties in the results of analyses of the real data.
C1 [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Castex, G.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Karakei, A.; 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.
[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.
[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 de Cordova 3107,Vitacura,Casilla 763 0355, 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.; Pointecouteau, E.; Ristorcelli, I.] CNRS, IRAP, 9 Av Colonel Roche,BP 44346, F-31028 Toulouse 4, France.
[Tuovinen, J.] Trinity Coll Dublin, CRANN, 91125 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.; Fergusson, 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 92093 USA.
[Rebolo, R.] CSIC, Madrid 0424, Spain.
[Chamballu, A.; Melin, J. -B.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France.
[Hornstrup, A.; Linden-Vornle, M.] 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. A.] Univ La Laguna ULL, Dept Astrofis, San Cristobal la Laguna 38206, Tenerife, Spain.
[Gonzalez-Nuevo, J.; Toffolatti, L.] Univ Oviedo, Dept Fis, Avda Calvo Sotelo S-N, E-33007 Oviedo, Spain.
[Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada.
[Rachen, J. P.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC, Canada.
[Colombo, L. P. L.; Pierpaoli, E.] Univ Southern Calif, Dept Phys & Astron, Dana & David Dornsife Coll Letter Arts & Sci, 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.; Kiiveri, K.; Kurki-Suonio, H.; Lindholm, V.; Savelainen, M.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Dept Phys, Gustaf Hallstromin Katu 2a, Helsinki 00560, Finland.
[Chiang, H. C.; Fraisse, A. A.; Gudmundsson, J. E.; Jones, W. C.; Nati, F.] Princeton Univ, Dept Phys, Princeton, CA 93106 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, I-00133 Rome, Italy.
[Bersanelli, M.; Maino, D.; Mennella, A.; Rossetti, M.; Tomasi, M.] Univ Milan, Dipartimento Fis, Via Celoria 16, I-00133 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-000138 Rome, Italy.
[Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, Blegdamsvej 17, DK-1165 Copenhagen, Denmark.
[Kneissl, R.] European Southern Observ ESO Vitacura, Alonso de Cordova 3107,Casilla 19001, Santiago, Chile.
[Dupac, X.; Leonardi, R.; Lopez-Caniego, M.; Mendes, L.] European Space Agcy ESAC, Planck Sci Off, Camino Bajo del Castillo S-N, Madrid 28692, Spain.
[Tauber, J. A.] ESTEC, European Space Agcy, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands.
[Terenzi, L.] Univ E Campus, Fac Ingn, Via Isimbardi 10, I-22060 Novedrate, CO, Italy.
[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.
[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 00560, Finland.
[de Zotti, G.] Osserv Astron Padova, INAF, Vicolo Osservatorio 5, I-35131 Padua, Italy.
[Polenta, G.] Osservatorio Astronom Roma, INAF, Via Frascati 33, Monte Porzio Catone, Italy.
[Frailis, M.; Galeotta, S.; Gregorio, A.; Maggio, G.; Maris, M.; Pasian, F.; Zacchei, A.] Osservatorio Astronom Trieste, INAF, Via GB Tiepolo 11, I-34127 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.] IASF Bologna, INAF, Via Gobetti 101, I-40127 Bologna, Italy.
[Bersanelli, M.; Donzelli, S.; Maino, D.; Mennella, A.; Rossetti, M.; Tomasi, M.] IASF Milano, INAF, Via E Bassini 15, I-20133 Milan, Italy.
[Burigana, C.; Finelli, F.; Paoletti, D.] INFN, Sez Bologna, Via Irnerio 46, I-40126 Bologna, Italy.
[Melchiorri, A.; Pagano, L.] Univ Roma Sapienza, INFN, Sez Roma 1, Piazzale Aldo Moro 2, I-00185 Rome, Italy.
[Renzi, A.] Univ Roma Tor Vergata, INFN, Sez Roma 2, Via Ric Sci 1, I-00185 Rome, Italy.
[Gregorio, A.] Natl Inst Nucl Phys, INFN, Via Valerio 2, I-34127 Trieste, Italy.
[Desert, F. -X.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
[Desert, F. -X.] IPAG, CNRS, F-38000 Grenoble, France.
[Mitra, S.] IUCAA, Post Bag 4,Ganeshkhind,Pune Univ Campus, 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 Joseph Fourier Grenoble I, CNRS, Inst Neel, 25 Rue Martyrs, F-38000 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 Sud 11, CNRS, Inst Astrophys Spatiale, UMR8617, Batiment 121, F-91898 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.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] Inst Astrophys Paris, CNRS, UMR7095, 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, 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.; 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.
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[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.
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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).
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[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.
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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. G.; 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, CNRS 1N2P3, 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.
[Kneissl, R.] ALMA Santiago Cent Off, Atacama Large Millimeter Submillimeter Array, Alonso Cordova 3107,Vitacura,Casilla 763 0355, Santiago, Chile.
[Leonardi, R.] CGEE, SCS Qd 9, Lote C,Torre C,4 Andar,Ed Parque Cidade Corp, 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.
[Alves, M. I. R.; Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] 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.; 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.] 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, DTU Space, Natl Space Inst, Elektrovej 327, DK-2800 Lyngby, Denmark.
[Kunz, M.; Tucci, M.] Univ Geneva, Dept Phys, 24 Quai E Ansermet, CH-1211 Geneva 4, 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, 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.
[Scott, D.] 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.
[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 USA.
[Juvela, M.; Keihanen, E.; Kurki-Suonio, H.; Savelainen, M.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Dept Phys, Gustaf Hallstromin Katu 2a, 00560 Helsinki, 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, I-00185 Rome, Italy.
[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-00185 Rome, Italy.
[Christensen, P. R.] Niels Bohr Inst, Discovery Ctr, Blegdamsvej 17, DK-1165 Copenhagen, Denmark.
[Kneissl, R.] European Southern Observ, ESO Vitacura, Alonso Cordova 3107,Vitacura,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 19041 USA.
[Kurki-Suonio, H.; Lahteenmaki, A.; Savelainen, M.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Helsinki Inst Phys, Gustaf Hallstromin Katu 2, Helsinki 00560, Finland.
[Umana, G.] Osserv Astrofis Catania, INAF, Via S Sofia 78, Catania, Italy.
[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.; Morgante, G.; Paoletti, D.; Sandri, M.; Terenzi, L.; Toffolatti, L.; 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, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
[Lattanzi, M.; Natoli, P.] Ist Nazl Fis Nucl, Sez Ferrara, Via Saragat 1, I-44122 Ferrara, 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, I-00185 Rome, Italy.
[Gregorio, A.] Natl Inst Nucl Phys, Ist Nazl Fis Nucl, Via Valerio 2, I-34127 Trieste, Italy.
[Desert, F. -X.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
[Desert, F. -X.] CNRS, IPAG, F-38000 Grenoble, France.
[Mitra, S.] Pune Univ Campus, IUCAA, Post Bag 4, 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.
[Chary, R. -R.; McGehee, P.; Paladini, R.; 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, F-38042 Grenoble, France.
[Dole, H.] Inst Univ France, 103 Bd St Michel, F-75005 Paris, France.
[Aghanim, N.; Alves, M. I. R.; 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, 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.; Delouis, J. -M.; Ducout, A.; Elsner, F.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] CNRS, Inst Astrophys Paris, UMR7095, 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.; 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, San Cristobal la Laguna 38200, 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 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.; 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.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England.
[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, CNRS, IN2P3, LAL, F-91898 Orsay, France.
[Catalano, A.; Coulais, A.; Falgarone, E.; Lamarre, J. -M.; Levrier, F.; Roudier, G.] Observ Paris, CNRS, LERMA, 61 Ave Observ, Paris, France.
[Arnaud, M.; Chamballu, A.; Marshall, D. J.; 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, F.] Univ Paris 11, CNRS, Phys Theor Lab, 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.; 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.
[Strong, A. W.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 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.
[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.; 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 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.
[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.
[Calabrese, E.] Univ Oxford, Subdept Astrophys, Keble Rd, Oxford OX1 3RH, England.
[Gudmundsson, J. E.] Stockholm Univ, AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, Dept Phys, S-10691 Stockholm, Sweden.
[Lesgourgues, J.] CERN, PH TH, Div Theory, CH-1211 Geneva 23, Switzerland.
[Benabed, K.; Benoit-Levy, A.; Colombi, S.; Delouis, J. -M.; Elsner, F.; Hivon, E.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UMR7095, 98 Bis Blvd Arago, F-75014 Paris, France.
[Alves, M. I. R.; Banday, A. J.; Bernard, J. -P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, TRAP, F-31028 Toulouse, France.
[Reach, W. 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, E-18071 Granada, Spain.
[Battaner, E.] Univ Granada, Inst Carlos Fis Teor & Computac 1, E-18071 Granada, Spain.
[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 Dickinson, C; Leahy, JP (reprint author), Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England.
EM Clive.dickinson@manchester.ac.uk; 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.
[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.
[Leonardi, R.] CGEE, SCS Qd 9, Lote C,Torre C,4 Andar,Ed Parque Cidade Corp, BR-70308200 Brasilia, DF, Brazil.
[Bond, J. R.; Hanson, D.; Martin, P. G.] 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.
[Fergusson, J.; Shellard, E. P. S.] Univ Cambridge, Ctr Theoret Cosmol, DAMTP, Wilberforce Rd, Cambridge CB3 0WA, England.
[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.] 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. 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, 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.
[Scott, D.] 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.
[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, Finland.
[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.
[Battaglia, P.; 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.; Krachmalnicoff, N.; Kunz, M.; Maino, D.; Mennella, A.; Rossetti, M.; Tomasi, M.] Univ Milan, Dipartimento Fis, Via Celoria 16, I-20133 Milan, Italy.
[Battaglia, P.; Gregorio, A.; Romelli, E.; Tavagnacco, D.] 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-00185 Rome, Italy.
[Christensen, P. R.] Niels Bohr Inst, Discovery Ctr, Blegdamsvej 17, DK-1165 Copenhagen, Denmark.
[Naselsky, P.] Univ Copenhagen, Niels Bohr Inst, Discovery Ctr, Blegdamsvej 17, DK-1165 Copenhagen, Denmark.
[Dupac, X.; Lopez-Caniego, M.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Camino Bajo Castillo S-N, Madrid 68692, 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.; Lahteenmaki, A.; Savelainen, M.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Helsinki Inst Phys, Gustaf Hallstromin Katu 2, Helsinki 02540, Finland.
[Umana, G.] Osserv Astrofis Catania, INAF, Via S Sofia 78, I-95123 Catania, Italy.
[de Zotti, G.] Osserv Astron Padova, INAF, Vicolo Osserv 5, I-35131 Padua, Italy.
[Polenta, G.] Osserv Astron Roma, INAF, Via Frascati 33, I-00185 Rome, Italy.
[Frailis, M.; Galeotta, S.; Gregorio, A.; Maggio, G.; Maris, M.; Pasian, F.; Romelli, E.; Tavagnacco, D.; Vassallo, T.; Zacchei, A.] Osserv Astron Trieste, INAF, Via GB Tiepolo 11, I-43127 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.] IASF Bologna, INAF, Via Gobetti 101, I-40127 Bologna, Italy.
[Bersanelli, M.; Donzelli, S.; Maino, D.; Mennella, A.; Rossetti, M.; Tomasi, M.] IASF Milano, INAF, 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, 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, I-00185 Rome, Italy.
[Gregorio, A.] Ist Nazl Fis Nucl, Natl Inst Nucl Phys, Via Valerio 2, I-34127 Trieste, Italy.
[Turler, M.] Univ Geneva, ISDC, Dept Astron, Ch Ecogia 16, CH-1290 Versoix, Switzerland.
[Mitra, S.] Pune Univ Campus, IUCAA, Post Bag 4, 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.
[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, F-38042 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.; Kunz, M.; Lagache, G.; Mangilli, A.; Pajot, F.; Puget, J. -L.; Remazeilles, M.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, Batiment 121, Orsay, France.
[Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Ducout, A.; Elsner, F.; Hivon, E.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] CNRS, Inst Astrophys Paris, UMR7095, 98 Bis Blvd Arago, F-75014 Paris, France.
[Lesgourgues, J.] Rhein Westfal TH Aachen, Inst Theoret Teilchenphys & Kosmol, D-52056 Aachen, Germany.
[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.; 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, San Cristobal la Laguna 38200, 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 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.
[Ashdown, M.; 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.
[Henrot-Versille, S.; Mangilli, A.; Perdereau, O.; Tristram, M.] Univ Paris 11, CNRS, IN2P3, LAL, Orsay, France.
[Catalano, A.; Lamarre, J. -M.; Levrier, F.; Roudier, G.] Observ Paris, CNRS, LERMA, 61 Ave Observ, F-75000 Paris, France.
[Chamballu, A.; Pratt, G. W.] Univ Paris Diderot, CEA DSM CNRS, CEA Saclay, IRFU,Serv Astrophys,ab 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.; Macias-Perez, J. F.; Perotto, L.; Santos, D.] Univ Grenoble Alpes, CNRS, IN2P3, Lab Phys Subatom & Cosmol, 53 Rue Martyrs, F-38026 Grenoble, France.
[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.
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[Lahteennmaki, A.] Aalto Univ, Metsahovi Radio Observ, POB 13000, Aalto 00076, Finland.
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[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.
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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.
[Lagache, G.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Ashdown, M.; Challinor, A.; 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.
[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.; Montier, L.; Pointecouteau, E.] IRAP, CNRS, 9 Ave 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.; 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.
[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 94720 USA.
[Rebolo, R.] CSIC, Plaza Murillo 2, E-28006 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. A.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Bonavera, L.; Gonzalez-Nuevo, J.; Toffolatti, L.] Univ Oviedo, Dept Fis, Avda Calvo Sotelo S-N, Oviedo 33003, Spain.
[Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON, Canada.
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[Scott, D.] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC, Canada.
[Colombo, L. P. L.; Pierpaoli, E.] Univ Southern Calif, Dept Phys & Astron, Dana & David Dornsife Coll Letter Arts & Sci, Los Angeles, CA 90089 USA.
[Benoit-Levy, A.; Elsner, F.; Peiris, H. V.] 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.
[Scott, D.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Pogosyan, D.] Univ Alberta, Dept Phys, 11322-89 Ave, Edmonton, AB T6G 2G7, Canada.
[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 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, Rome, Italy.
[Bersanelli, M.; Maino, D.; Mennella, A.; Rossetti, M.; Tomasi, M.] Univ Milan, Dipartimento Fis, Via Celoria 16, Milan, Italy.
[Gregorio, A.] Univ Trieste, Dipartimento Fis, Via A Valerio 2, Trieste, Italy.
[Renzi, A.] Univ Roma Tor Vergata, Dipartimento Matemat, Via Ric Sci 1, 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, Copenhagen, Denmark.
[Dupac, X.; 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.
[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.
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[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.] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, Padua, Italy.
[Polenta, G.] INAF Osservatorio Astron Roma, Via Frascati 33, Monte Porzio Catone, Italy.
[Finelli, F.; Frailis, M.; Galeotta, S.; Gregorio, A.; Maggio, G.; Maris, M.; Pasian, F.; Zacchei, A.] INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, Trieste, Italy.
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[Bersanelli, M.; Donzelli, S.; Maino, D.; Mennella, A.; Rossetti, M.; Tomasi, M.] INAF IASF Milano, Via E Bassini 15, Milan, Italy.
[Burigana, C.; Finelli, F.; Gruppuso, A.; Paoletti, D.] Ist Nazl Fis Nucl, Sez Bologna, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
[Lattanzi, M.; Natoli, P.] Ist Nazl Fis Nucl, Sez Ferrara, Via Saragat 1, I-44122 Ferrara, 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, Sez Roma 2, Ist Nazl Fis Nucl, 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.
[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.
[McGehee, P.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Benoit, A.] Univ Joseph Fourier Grenoble I, Inst Neel, CNRS, 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.; Kunz, M.; Lagache, G.; Mangilli, A.; Miville-Deschenes, M. -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.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Ducout, A.; Elsner, F.; Hivon, E.; Moneti, A.; 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.
[Popa, L.] Inst Space Sci, Bucharest 077125, Romania.
[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.; Wehus, I. K.] Univ Oslo, Inst Theoret Astrophys, N-1072 Oslo, Norway.
[Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, C Via Lactea S-N, Tenerife 38205, Spain.
[Barreiro, R. B.; Curto, A.; Diego, J. M.; Gonzalez-Nuevo, J.; Herranz, D.; 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.
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[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.
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[Stolyarov, V.] Kazan Fed Univ, 18 Kremlyovskaya St, Kazan 420008, Russia.
[Ashdown, M.; Couchot, F.; Henrot-Versille, S.; Mangilli, A.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, LAL, CNRS IN2P3, Orsay, France.
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[Cardoso, J. -F.] CNRS, Lab Traitement & Commun Informat, UMR 5141, 46 Rue Barrault, F-75634 Paris 13, France.
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[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 94720 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.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany.
[Feeney, S.; Hanson, D.] McGill Univ, McGill Phys, Ernest Rutherford Phys Bldg,3600 Rue Univ, Montreal, PQ H3A 2T8, Canada.
[McEwen, J. D.] Univ Coll London, Mullard Space Sci Lab, Surrey RH5 6NT, England.
[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.; Frejse, A.; Novikov, I.] Niels Bohr Inst, Blegdamsvej 17, Copenhagen, Denmark.
[Naselsky, P.] Univ Copenhagen, Niels Bohr Inst, Blegdamsvej 17, 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 WC 1E6BT, 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, 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.
[Church, S.] Stanford Univ, Dept Phys, Varian Phys Bldg,382 Via Pueblo Mall, Stanford, CA USA.
[Calabrese, E.] Univ Oxford, Subdept Astrophys, Keble Rd, Oxford OX1 3RH, England.
[Gudmundsson, J. E.] Stockholm Univ, AlbaNova, Dept Phys, Oskar Klein Ctr Cosmoparticle Phys, S-10691 Stockholm, Sweden.
[Lesgourgues, J.] CERN, PH TH, Div Theory, CH-1211 Geneva 23, Switzerland.
[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, Granada 18010, Spain.
[Battaner, E.; Benabed, K.] Univ Granada, Inst Carlos Fis Teor & Computac 1, Granada, Spain.
[Gorski, K. M.] Univ Warsaw Observ, Aleje Ujazdowskie 4, PL-00478 Warsaw, Poland.
RP Jaffe, AH (reprint author), Imperial Coll London, Astrophys Grp, Blackett Lab, Prince Consort Rd, London SW7 2AZ, England.
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