FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Hashmi, AJ Eftekhar, AA Adibi, A Amoozegar, F AF Hashmi, Ali J. Eftekhar, Ali A. Adibi, Ali Amoozegar, Farid TI Analysis of adaptive optics-based telescope arrays in a deep-space inter-planetary optical communications link between Earth and Mars SO OPTICS COMMUNICATIONS LA English DT Article DE Deep space optical communication; Optical array receivers; Free space optical communication; Earth-Mars communication; Atmospheric turbulence; Adaptive optics ID LASER COMMUNICATIONS; RECEIVER; TELEMETRY AB Earth-based telescope array receivers employing optical communications have the potential to fulfill the communication needs of technologically sophisticated, deep-space exploration missions. Atmospheric turbulence is the chief restrictive factor in an optical deep-space channel (ODSC). In this paper, investigation and design of adaptive optics (AO) subsystems are presented for the compensation of the coupled effects of optical turbulence and background noise in telescope array receivers. An end-to-end simulation platform for an ODSC between Mars and Earth is implemented, which incorporates pulse-position modulation (PPM), direct-detection receivers, and detectors with the capability of detection of single photon. The extreme conditions of atmospheric turbulence and background noise are also modeled in the analysis. AO subsystems are incorporated at individual telescopes in the array receiver to mitigate the turbulence effects. The performance of array receivers is evaluated in terms of the probability of error and communication throughput. The analysis in this research depicts that in worst-case turbulence and background noise conditions, inclusion of AO systems results in 8.5 dB performance improvement in communication data rates. The performance improvement of 5.6 dB is achievable in moderate channel conditions. Comparison of performance of array receivers with that of a large monolithic telescope shows that incorporation of AO systems is more feasible in arrays comprising telescopes with relatively smaller diameters. (C) 2014 Elsevier B.V. All rights reserved. C1 [Hashmi, Ali J.] Natl Univ Sci & Technol, Islamabad, Pakistan. [Eftekhar, Ali A.; Adibi, Ali] Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. [Amoozegar, Farid] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. RP Hashmi, AJ (reprint author), Natl Univ Sci & Technol, H 12, Islamabad, Pakistan. EM hashmi@gatech.edu NR 29 TC 2 Z9 2 U1 3 U2 24 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0030-4018 EI 1873-0310 J9 OPT COMMUN JI Opt. Commun. PD DEC 15 PY 2014 VL 333 BP 120 EP 128 DI 10.1016/j.optcom.2014.07.077 PG 9 WC Optics SC Optics GA AR1YT UT WOS:000343381200023 ER PT J AU Wilson, MA Nguyen, TH Pohorille, A AF Wilson, Michael A. Thuy Hien Nguyen Pohorille, Andrew TI Combining molecular dynamics and an electrodiffusion model to calculate ion channel conductance SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID FREE-ENERGY DIFFERENCES; BROWNIAN DYNAMICS; EQUATION APPROACH; ALPHA-HEMOLYSIN; DRUG DISCOVERY; LIPID-MEMBRANE; SIMULATIONS; WATER; TRANSPORT; FORCE AB Establishing the relation between the structures and functions of protein ion channels, which are protein assemblies that facilitate transmembrane ion transport through water-filled pores, is at the forefront of biological and medical sciences. A reliable way to determine whether our understanding of this relation is satisfactory is to reproduce the measured ionic conductance over a broad range of applied voltages. This can be done in molecular dynamics simulations by way of applying an external electric field to the system and counting the number of ions that traverse the channel per unit time. Since this approach is computationally very expensive we develop a markedly more efficient alternative in which molecular dynamics is combined with an electrodiffusion equation. This alternative approach applies if steady-state ion transport through channels can be described with sufficient accuracy by the one-dimensional diffusion equation in the potential given by the free energy profile and applied voltage. The theory refers only to line densities of ions in the channel and, therefore, avoids ambiguities related to determining the surface area of the channel near its endpoints or other procedures connecting the line and bulk ion densities. We apply the theory to a simple, model system based on the trichotoxin channel. We test the assumptions of the electrodiffusion equation, and determine the precision and consistency of the calculated conductance. We demonstrate that it is possible to calculate current/voltage dependence and accurately reconstruct the underlying (equilibrium) free energy profile, all from molecular dynamics simulations at a single voltage. The approach developed here applies to other channels that satisfy the conditions of the electrodiffusion equation. (C) 2014 AIP Publishing LLC. C1 [Wilson, Michael A.; Pohorille, Andrew] NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. [Wilson, Michael A.; Pohorille, Andrew] San Francisco State Univ, Dept Pharmaceut Chem, San Francisco, CA 94132 USA. [Thuy Hien Nguyen] Univ Penn, Dept Chem & Biochem, Philadelphia, PA 19104 USA. RP Wilson, MA (reprint author), NASA, Exobiol Branch, Ames Res Ctr, MS 239-4, Moffett Field, CA 94035 USA. EM Michael.A.Wilson@nasa.gov; Andrew.Pohorille@nasa.gov FU NASA Exobiology and Astrobiology Programs FX This work was supported by the NASA Exobiology and Astrobiology Programs. All simulations were performed at the NASA Advanced Supercomputing (NAS) Division and on the Anton computer at the Pittsburgh Supercomputer Center. NR 66 TC 1 Z9 1 U1 4 U2 27 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD DEC 14 PY 2014 VL 141 IS 22 AR 22D519 DI 10.1063/1.4900879 PG 14 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA AW4TH UT WOS:000346272800066 PM 25494790 ER PT J AU Bishop, JL Englert, PAJ Patel, S Tirsch, D Roy, AJ Koeberl, C Bottger, U Hanke, F Jaumann, R AF Bishop, Janice L. Englert, Peter A. J. Patel, Shital Tirsch, Daniela Roy, Alex J. Koeberl, Christian Boettger, Ute Hanke, Franziska Jaumann, Ralf TI Mineralogical analyses of surface sediments in the Antarctic Dry Valleys: coordinated analyses of Raman spectra, reflectance spectra and elemental abundances SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Article DE Antarctic Dry Valleys; sediments; Raman spectra; reflectance spectra; chemistry ID COVERED LAKE-HOARE; MOSSBAUER-SPECTROSCOPY; GEOCHEMICAL ANALYSES; VICTORIA LAND; ICE COVER; IN-SITU; MARS; ANALOG; SPECTROMETER; ENVIRONMENT AB Surface sediments at Lakes Fryxell, Vanda and Brownworth in the Antarctic Dry Valleys (ADV) were investigated as analogues for the cold, dry environment on Mars. Sediments were sampled from regions surrounding the lakes and from the ice cover on top of the lakes. The ADV sediments were studied using Raman spectra of individual grains and reflectance spectra of bulk particulate samples and compared with previous analyses of subsurface and lakebottom sediments. Elemental abundances were coordinated with the spectral data in order to assess trends in sediment alteration. The surface sediments in this study were compared with lakebottom sediments (Bishop JL et al. 2003 Int. J. Astrobiol. 2, 273-287 (doi:10.1017/S1473550403001654)) and samples from soil pits (Englert P et al. 2013 In European Planetary Science Congress, abstract no. 96; Englert P et al. 2014 In 45th Lunar and Planetary Science Conf., abstract no. 1707). Feldspar, quartz and pyroxene are common minerals found in all the sediments. Minor abundances of carbonate, chlorite, actinolite and allophane are also found in the surface sediments, and are similar to minerals found in greater abundance in the lakebottom sediments. Surface sediment formation is dominated by physical processes; a few centimetres below the surface chemical alteration sets in, whereas lakebottom sediments experience biomineralization. Characterizing the mineralogical variations in these samples provides insights into the alteration processes occurring in the ADV and supports understanding alteration in the cold and dry environment on Mars. C1 [Bishop, Janice L.; Patel, Shital] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Bishop, Janice L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Englert, Peter A. J.] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Patel, Shital] San Jose State Univ, Dept Chem, San Jose, CA 95192 USA. [Tirsch, Daniela; Boettger, Ute; Hanke, Franziska; Jaumann, Ralf] German Aerosp Ctr DLR, Berlin, Germany. [Roy, Alex J.] Dept Land & Nat Resources, Honolulu, HI USA. [Koeberl, Christian] Univ Vienna, Dept Lithospher Res, A-1090 Vienna, Austria. [Koeberl, Christian] Nat Hist Museum, A-1010 Vienna, Austria. [Hanke, Franziska] Tech Univ Berlin, Berlin, Germany. RP Bishop, JL (reprint author), SETI Inst, Carl Sagan Ctr, 189 Bernardo Ave, Mountain View, CA 94043 USA. EM jbishop@seti.org OI Tirsch, Daniela/0000-0001-5905-5426 NR 71 TC 2 Z9 2 U1 0 U2 14 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1364-503X EI 1471-2962 J9 PHILOS T R SOC A JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci. PD DEC 13 PY 2014 VL 372 IS 2030 SI SI AR 20140198 DI 10.1098/rsta.2014.0198 PG 26 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AT5OK UT WOS:000344991900006 ER PT J AU Conrad, PG AF Conrad, Pamela G. TI Scratching the surface of martian habitability SO SCIENCE LA English DT Editorial Material ID MARS C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Conrad, PG (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM pamela.g.conrad@nasa.gov NR 11 TC 1 Z9 1 U1 0 U2 13 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 DEC 12 PY 2014 VL 346 IS 6215 BP 1288 EP 1289 DI 10.1126/science.1259943 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AW3MA UT WOS:000346189600020 PM 25504700 ER PT J AU Tiburzi, C Johnston, S Bailes, M Bates, SD Bhat, NDR Burgay, M Burke-Spolaor, S Champion, D Coster, P D'Amico, N Keith, MJ Kramer, M Levin, L Milia, S Ng, C Possenti, A Stappers, BW Thornton, D van Straten, W AF Tiburzi, C. Johnston, S. Bailes, M. Bates, S. D. Bhat, N. D. R. Burgay, M. Burke-Spolaor, S. Champion, D. Coster, P. D'Amico, N. Keith, M. J. Kramer, M. Levin, L. Milia, S. Ng, C. Possenti, A. Stappers, B. W. Thornton, D. van Straten, W. TI The High Time Resolution Universe survey - IX. Polarimetry of long-period pulsars (vol 436, pg 3557, 2013) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Correction DE errata, addenda; magnetic fields; polarization; methods: observational; pulsars: general C1 [Tiburzi, C.; Burgay, M.; D'Amico, N.; Milia, S.; Possenti, A.] INAF Osservatorio Astron Cagliari, I-09047 Selargius, CA, Italy. [Tiburzi, C.; D'Amico, N.] Univ Cagliari, Dipartimento Fis, I-09042 Monserrato, CA, Italy. [Johnston, S.; Coster, P.; Thornton, D.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Bailes, M.; Bhat, N. D. R.; Coster, P.; van Straten, W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Bailes, M.; Bhat, N. D. R.; van Straten, W.] ARC Ctr Excellence All Sky Astrophys, Sydney, NSW 2016, Australia. [Bates, S. D.; Levin, L.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. [Bhat, N. D. R.] Curtin Univ Technol, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Burke-Spolaor, S.] NASA, Jet Prop Lab, Pasadena, CA 91106 USA. [Champion, D.; Kramer, M.; Ng, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Keith, M. J.; Kramer, M.; Stappers, B. W.; Thornton, D.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. RP Tiburzi, C (reprint author), INAF Osservatorio Astron Cagliari, Via Sci, I-09047 Selargius, CA, Italy. EM ctiburzi@oa-cagliari.inaf.it NR 1 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 DEC 11 PY 2014 VL 445 IS 3 BP 3009 EP 3010 DI 10.1093/mnras/stu1930 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AX5JT UT WOS:000346962900069 ER PT J AU Inglis, AR Gilbert, HR AF Inglis, A. R. Gilbert, H. R. TI HARD X-RAY AND ULTRAVIOLET EMISSION DURING THE 2011 JUNE 7 SOLAR FLARE (vol 777, 30, 2013) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Inglis, A. R.; Gilbert, H. R.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP Inglis, AR (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Heliophys Sci Div, Greenbelt, MD 20771 USA. EM a.r.inglis@gmail.com NR 1 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2014 VL 797 IS 1 AR 72 DI 10.1088/0004-637X/797/1/72 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU9LT UT WOS:000345915000072 ER PT J AU Kopytova, TG Crossfield, IJM Deacon, NR Brandner, W Buenzli, E Bayo, A Schlieder, JE Manjavacas, E Biller, BA Kopon, D AF Kopytova, Taisiya G. Crossfield, Ian J. M. Deacon, Niall R. Brandner, Wolfgang Buenzli, Esther Bayo, Amelia Schlieder, Joshua E. Manjavacas, Elena Biller, Beth A. Kopon, Derek TI DEEP z-BAND OBSERVATIONS OF THE COOLEST Y DWARF SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; stars: individual (WISE J085510.83-071442.5); stars: low-mass ID SURVEY-EXPLORER WISE; BROWN DWARF; WATER CLOUDS; T-DWARFS; TRANSITION; EXOPLANETS; DISCOVERY; SPECTRA; STARS AB WISE J085510.83-071442.5 (hereafter, WISE 0855-07) is the coolest Y dwarf known to date and is located at a distance of 2.31 +/- 0.08 pc, giving it the fourth largest parallax of any known star or brown dwarf system. We report deep z-band observations of WISE 0855-07 using FORS2 on UT1/Very Large Telescope. We do not detect any counterpart to WISE 0855-07 in our z-band images and estimate a brightness upper limit of AB mag > 24.8 (F. < 0.45 mu Jy) at 910 +/- 65 nm with 3 sigma confidence. We combine our z-band upper limit with previous near-and mid-infrared photometry to place constraints on the atmospheric properties of WISE 0855-07 via comparison to models which implement water clouds in the atmospheres of T-eff < 300 K substellar objects. We find that none of the available models that implement water clouds can completely reproduce the observed spectral energy distribution of WISE 0855-07. Every model significantly disagrees with the (3.6 mu m/4.5 mu m) flux ratio and at least one other bandpass. Since methane is predicted to be the dominant absorber at 3-4 mu m, these mismatches might point to an incorrect or incomplete treatment of methane in current models. We conclude that (a) WISE0855-07 has Teff similar to 200-250 K, (b) < 80% of its surface is covered by clouds, and (c) deeper observations, and improved models of substellar evolution, atmospheres, clouds, and opacities will be necessary to better characterize this object. C1 [Kopytova, Taisiya G.; Crossfield, Ian J. M.; Deacon, Niall R.; Brandner, Wolfgang; Buenzli, Esther; Bayo, Amelia; Schlieder, Joshua E.; Manjavacas, Elena; Kopon, Derek] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kopytova, Taisiya G.; Manjavacas, Elena] Int Max Planck Res Sch Astron & Space Phys, D-69117 Heidelberg, Germany. [Kopytova, Taisiya G.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Crossfield, Ian J. M.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Deacon, Niall R.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Bayo, Amelia] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile. [Schlieder, Joshua E.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Biller, Beth A.] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. RP Kopytova, TG (reprint author), Amer Museum Nat Hist, New York, NY 10024 USA. EM kopytova@mpia.de OI Buenzli, Esther/0000-0003-3306-1486 FU Annette Kade Graduate Student Fellowship Program of the RGGS at the American Museum of Natural History, through Annette Kade Charitable Trust; Swiss National Science Foundation (SNSF); NASA Postdoctoral Program at NASA Ames Research Center FX T.K. is partly supported by the Annette Kade Graduate Student Fellowship Program of the RGGS at the American Museum of Natural History, through generous contributions of the Annette Kade Charitable Trust. E.B. is supported by the Swiss National Science Foundation (SNSF). A portion of the research of J.E.S. was supported by an appointment to the NASA Postdoctoral Program at NASA Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. T.K. is grateful to Juan Carlos Beamin and Jackie Faherty for helpful discussions regarding WISE 0855-07. NR 25 TC 5 Z9 5 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2014 VL 797 IS 1 AR 3 DI 10.1088/0004-637X/797/1/3 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU9LT UT WOS:000345915000003 ER PT J AU Meneghetti, M Rasia, E Vega, J Merten, J Postman, M Yepes, G Sembolini, F Donahue, M Ettori, S Umetsu, K Balestra, I Bartelmann, M Benitez, N Biviano, A Bouwens, R Bradley, L Broadhurst, T Coe, D Czakon, N De Petris, M Ford, H Giocoli, C Gottlober, S Grillo, C Infante, L Jouvel, S Kelson, D Koekemoer, A Lahav, O Lemze, D Medezinski, E Melchior, P Mercurio, A Molino, A Moscardini, L Monna, A Moustakas, J Moustakas, LA Nonino, M Rhodes, J Rosati, P Sayers, J Seitz, S Zheng, W Zitrin, A AF Meneghetti, M. Rasia, E. Vega, J. Merten, J. Postman, M. Yepes, G. Sembolini, F. Donahue, M. Ettori, S. Umetsu, K. Balestra, I. Bartelmann, M. Benitez, N. Biviano, A. Bouwens, R. Bradley, L. Broadhurst, T. Coe, D. Czakon, N. De Petris, M. Ford, H. Giocoli, C. Gottloeber, S. Grillo, C. Infante, L. Jouvel, S. Kelson, D. Koekemoer, A. Lahav, O. Lemze, D. Medezinski, E. Melchior, P. Mercurio, A. Molino, A. Moscardini, L. Monna, A. Moustakas, J. Moustakas, L. A. Nonino, M. Rhodes, J. Rosati, P. Sayers, J. Seitz, S. Zheng, W. Zitrin, A. TI THE MUSIC OF CLASH: PREDICTIONS ON THE CONCENTRATION-MASS RELATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: clusters: general; gravitation lensing: weak; gravitational lensing: strong ID COLD DARK-MATTER; SIMULATED GALAXY CLUSTERS; STAR-FORMING GALAXIES; HALO DENSITY PROFILES; WEAK LENSING ANALYSIS; X-RAY; COSMOLOGICAL SIMULATIONS; IMPROVED CONSTRAINTS; ENERGY COSMOLOGIES; MACS J1206.2-0847 AB We present an analysis of the MUSIC-2 N-body/hydrodynamical simulations aimed at estimating the expected concentration-mass relation for the CLASH (Cluster Lensing and Supernova Survey with Hubble) cluster sample. We study nearly 1,400 halos simulated at high spatial and mass resolution. We study the shape of both their density and surface-density profiles and fit them with a variety of radial functions, including the Navarro-Frenk-White (NFW), the generalized NFW, and the Einasto density profiles. We derive concentrations and masses from these fits. We produce simulated Chandra observations of the halos, and we use them to identify objects resembling the X-ray morphologies and masses of the clusters in the CLASH X-ray-selected sample. We also derive a concentration-mass relation for strong-lensing clusters. We find that the sample of simulated halos that resembles the X-ray morphology of the CLASH clusters is composed mainly of relaxed halos, but it also contains a significant fraction of unrelaxed systems. For such a heterogeneous sample we measure an average two-dimensional concentration that is similar to 11% higher than is found for the full sample of simulated halos. After accounting for projection and selection effects, the average NFW concentrations of CLASH clusters are expected to be intermediate between those predicted in three dimensions for relaxed and super-relaxed halos. Matching the simulations to the individual CLASH clusters on the basis of the X-ray morphology, we expect that the NFW concentrations recovered from the lensing analysis of the CLASH clusters are in the range [3-6], with an average value of 3.87 and a standard deviation of 0.61. C1 [Meneghetti, M.; Rhodes, J.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Meneghetti, M.; Merten, J.; Ettori, S.; Moustakas, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Meneghetti, M.; Ettori, S.] INFN, Sez Bologna, I-40127 Bologna, Italy. [Rasia, E.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Vega, J.; Yepes, G.; Sembolini, F.] Univ Autonoma Madrid, Dept Fs Ter, E-28049 Madrid, Spain. [Vega, J.] CNRS, LERMA, Observ Paris, UMR 8112, F-75014 Paris, France. [Merten, J.; Koekemoer, A.; Rhodes, J.; Sayers, J.; Zitrin, A.] CALTECH, Pasadena, CA 91125 USA. [Postman, M.; Coe, D.; Zheng, W.] Space Telescope Sci Inst, Baltimore, MD 21208 USA. [Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Umetsu, K.; Czakon, N.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Balestra, I.; Mercurio, A.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Balestra, I.; Biviano, A.; Nonino, M.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy. [Bartelmann, M.] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, D-69120 Heidelberg, Germany. [Benitez, N.; Molino, A.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Bouwens, R.] Leiden Univ, Leiden Observ, NL-2333 Leiden, Netherlands. [Bradley, L.; Ford, H.; Lemze, D.; Medezinski, E.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Broadhurst, T.] Univ Basque Country, UPV EHU, Dept Theoret Phys & Hist Sci, E-48080 Bilbao, Spain. [Broadhurst, T.] Ikerbasque, Basque Fdn Sci, E-48011 Bilbao, Spain. [De Petris, M.] Sapienza Univ Roma, Dipartimento Fis, I-00185 Rome, Italy. [Giocoli, C.; Moscardini, L.] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy. [Gottloeber, S.] Leibniz Inst Astrophys, D-14482 Potsdam, Germany. [Grillo, C.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Infante, L.] Catholic Univ Chile, Ctr Astro Ingn, Dept Astron & Astrofis, Santiago, Chile. [Jouvel, S.] CSIC, IEEC, Inst Ciencies Espai, E-08193 Bellaterra, Barcelona, Spain. [Jouvel, S.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Kelson, D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Melchior, P.] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA. [Melchior, P.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Monna, A.] Univ Sternwarte, D-81679 Munich, Germany. [Monna, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Moustakas, J.] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. [Rosati, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy. [Zitrin, A.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. RP Meneghetti, M (reprint author), Osservatorio Astron Bologna, INAF, Via Ranzani 1, I-40127 Bologna, Italy. RI Grillo, Claudio/E-6223-2015; Yepes, Gustavo/A-7899-2010; Ettori, Stefano/N-5004-2015; Meneghetti, Massimo/O-8139-2015; OI Vega Ferrero, Jesus/0000-0003-2338-5567; rasia, elena/0000-0003-4175-002X; Umetsu, Keiichi/0000-0002-7196-4822; Grillo, Claudio/0000-0002-5926-7143; Yepes, Gustavo/0000-0001-5031-7936; Ettori, Stefano/0000-0003-4117-8617; Meneghetti, Massimo/0000-0003-1225-7084; Nonino, Mario/0000-0001-6342-9662; Balestra, Italo/0000-0001-9660-894X; Biviano, Andrea/0000-0002-0857-0732; Moustakas, Leonidas/0000-0003-3030-2360; Koekemoer, Anton/0000-0002-6610-2048; Benitez, Narciso/0000-0002-0403-7455; Donahue, Megan/0000-0002-2808-0853 FU National Aeronautics and Space Administration; ORAU; NASA [NAS8-03060]; ASI/INAF [I/023/12/0, INFN/PD51]; PRIN MIUR; National Science Foundation [AST-1210973]; SAO [TM3-14008X]; project GLENCO under the European Seventh Framework Programme, Ideas, grant [259349]; National Science Council of Taiwan [NSC100-2112-M-001-008-MY3]; Academia Sinica Career Development Award; NASA through Hubble Fellowship grant [HST-HF-51334.01-A]; STScI; SFBTransregio 33 The Dark Universe by the Deutsche Forschungsgemeinschaft (DFG); DFG cluster of excellence Origin and Structure of the Universe; Baden Wurttemberg Stiftung; DNRF; Norris Foundation CCAT Postdoctoral Fellowship; MINECO [AYA2012-31101, FPA2012-34694]; MultiDark [CSD2009-00064]; [NSF/AST1313447]; [NASA/NNX11AB07G] FX The research was in part carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. M.M. thanks ORAU and NASA for supporting his research at JPL. M.M., C.G., and L.M. acknowledge support from the contracts ASI/INAF I/023/12/0, INFN/PD51, and the PRIN MIUR 2010-2011 "The dark universe and the cosmic evolution of baryons: From current surveys to Euclid." E.R. acknowledges support from the National Science Foundation AST-1210973, SAO TM3-14008X (issued under NASA Contract No. NAS8-03060). C.G.'s research is part of the project GLENCO, funded under the European Seventh Framework Programme, Ideas, grant agreement No. 259349. K.U. acknowledges support from the National Science Council of Taiwan (grant NSC100-2112-M-001-008-MY3) and from the Academia Sinica Career Development Award. Support for A.Z. is provided by NASA through Hubble Fellowship grant #HST-HF-51334.01-A awarded by STScI. D.G., S.S., and P.R. were supported by SFBTransregio 33 The Dark Universe by the Deutsche Forschungsgemeinschaft (DFG) and the DFG cluster of excellence Origin and Structure of the Universe. This work was supported in part by contract research "Internationale Spitzenforschung II/2-6" of the Baden Wurttemberg Stiftung. The Dark Cosmology Centre is funded by the DNRF. J.S. was supported by NSF/AST1313447, NASA/NNX11AB07G, and the Norris Foundation CCAT Postdoctoral Fellowship. The MUSIC simulations were performed at the Barcelona Supercomputing Center (BSC), and the initial conditions were done at the Leibniz Rechenzentrum Munich (LRZ). G.Y. and F.S. acknowledge support from MINECO under research grants AYA2012-31101, FPA2012-34694, and MultiDark CSD2009-00064. We thank Stefano Borgani and the whole computational astrophysics group at the University of Trieste and at INAF-OATS for giving us access to their set of hydrodynamical simulations. NR 99 TC 37 Z9 37 U1 3 U2 19 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2014 VL 797 IS 1 AR 34 DI 10.1088/0004-637X/797/1/34 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU9LT UT WOS:000345915000034 ER PT J AU Piner, BG Edwards, PG AF Piner, B. Glenn Edwards, Philip G. TI FIRST-EPOCH VLBA IMAGING OF 20 NEW TeV BLAZARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: general; galaxies: active; galaxies: jets; radio continuum: galaxies ID GAMMA-RAY EMISSION; BL LACERTAE OBJECT; ACTIVE GALACTIC NUCLEI; EXTRAGALACTIC RADIO-SOURCES; LARGE-AREA TELESCOPE; SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS; INTRINSIC BRIGHTNESS TEMPERATURES; SPECTRAL ENERGY-DISTRIBUTION; PARSEC-SCALE STRUCTURE; MAGIC TELESCOPES AB We present Very Long Baseline Array (VLBA) images of 20 TeV blazars not previously well studied on the parsec scale. All 20 of these sources are high-frequency peaked BL Lac objects (HBLs). Observations were made between August and December of 2013 at a frequency of 8.4 GHz. These observations represent the first epoch of a VLBA monitoring campaign on these blazars, and they significantly increase the fraction of TeV HBLs studied with high-resolution imaging. The peak very long baseline interferometry (VLBI) flux densities of these sources range from similar to 10 to similar to 100 mJy bm(-1), and parsec-scale jet structure is detected in all sources. About half of the VLBI cores are resolved, with brightness temperature upper limits of a few times 10(10) K, and we find that a brightness temperature of similar to 2 x 10(10) K is consistent with the VLBI data for all but one of the sources. Such brightness temperatures do not require any relativistic beaming to reduce the observed value below commonly invoked intrinsic limits; however, the lack of detection of counterjets does place a modest limit on the bulk Lorentz factor of gamma greater than or similar to 2. These data are thus consistent with a picture where weak-jet sources like the TeV HBLs develop significant velocity structures on parsec scales. We also extend consideration to the full sample of TeV HBLs by combining the new VLBI data with VLBI and gamma-ray data from the literature. By comparing measured VLBI and TeV fluxes to samples with intrinsically uncorrelated luminosities generated by Monte Carlo simulations, we find a marginally significant correlation between the VLBI and TeV fluxes for the full TeV HBL sample. C1 [Piner, B. Glenn] Whittier Coll, Dept Phys & Astron, Whittier, CA 90608 USA. [Piner, B. Glenn] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA. [Edwards, Philip G.] Australia Telescope Natl Facil, CSIRO, Astron & Space Sci, Epping, NSW 1710, Australia. RP Piner, BG (reprint author), Whittier Coll, Dept Phys & Astron, 13406 E Philadelphia St, Whittier, CA 90608 USA. EM gpiner@whittier.edu FU Associated Universities, Inc.; National Aeronautics and Space Administration; Fermi Guest Investigator grant [NNX13AO82G] FX The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. 2009). Part of this research was carried out at the Jet Propulsion Laboratory, Caltech, under a contract with the National Aeronautics and Space Administration. This work was supported by Fermi Guest Investigator grant NNX13AO82G. We also acknowledge helpful comments from the anonymous referee. NR 126 TC 14 Z9 15 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2014 VL 797 IS 1 AR 25 DI 10.1088/0004-637X/797/1/25 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU9LT UT WOS:000345915000025 ER PT J AU Vreeswijk, PM Savaglio, S Gal-Yam, A De Cia, A Quimby, RM Sullivan, M Cenko, SB Perley, DA Filippenko, AV Clubb, KI Taddia, F Sollerman, J Leloudas, G Arcavi, I Rubin, A Kasliwal, MM Cao, Y Yaron, O Tal, D Ofek, EO Capone, J Kutyrev, AS Toy, V Nugent, PE Laher, R Surace, J Kulkarni, SR AF Vreeswijk, Paul M. Savaglio, Sandra Gal-Yam, Avishay De Cia, Annalisa Quimby, Robert M. Sullivan, Mark Cenko, S. Bradley Perley, Daniel A. Filippenko, Alexei V. Clubb, Kelsey I. Taddia, Francesco Sollerman, Jesper Leloudas, Giorgos Arcavi, Iair Rubin, Adam Kasliwal, Mansi M. Cao, Yi Yaron, Ofer Tal, David Ofek, Eran O. Capone, John Kutyrev, Alexander S. Toy, Vicki Nugent, Peter E. Laher, Russ Surace, Jason Kulkarni, Shrinivas R. TI THE HYDROGEN-POOR SUPERLUMINOUS SUPERNOVA iPTF 13ajg AND ITS HOST GALAXY IN ABSORPTION AND EMISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: atoms; supernovae: general; supernovae: individual (iPTF 13ajg) ID GAMMA-RAY BURSTS; DIFFUSE INTERSTELLAR BANDS; MASS-METALLICITY RELATION; CORE-COLLAPSE SUPERNOVAE; LYMAN-ALPHA ABSORBERS; SHOCK-BREAKOUT; LUMINOUS SUPERNOVAE; LIGHT-CURVES; ULTRALUMINOUS SUPERNOVAE; METAL ABUNDANCES AB We present imaging and spectroscopy of a hydrogen-poor superluminous supernova (SLSN) discovered by the intermediate Palomar Transient Factory, iPTF 13ajg. At a redshift of z = 0.7403, derived from narrow absorption lines, iPTF 13ajg peaked at an absolute magnitude of M-u,M-AB = -22.5, one of the most luminous supernovae to date. The observed bolometric peak luminosity of iPTF 13ajg is 3.2 x 10(44) erg s(-1), while the estimated total radiated energy is 1.3 x 10(51) erg. We detect narrow absorption lines of Mg I, Mg II, and Fe II, associated with the cold interstellar medium in the host galaxy, at two different epochs with X-shooter at the Very Large Telescope. From Voigt profile fitting, we derive the column densities log N(Mg I) = 11.94 +/- 0.06, log N(Mg II) = 14.7 +/- 0.3, and log N(Fe II) = 14.25 +/- 0.10. These column densities, as well as the Mg I and Mg II equivalent widths of a sample of hydrogen-poor SLSNe taken from the literature, are at the low end of those derived for gamma-ray bursts (GRBs) whose progenitors are also thought to be massive stars. This suggests that the environments of hydrogen-poor SLSNe and GRBs are different. From the nondetection of Fe II fine-structure absorption lines, we derive a lower limit on the distance between the supernova and the narrow-line absorbing gas of 50 pc. The neutral gas responsible for the absorption in iPTF 13ajg exhibits a single narrow component with a low velocity width, Delta V = 76 km s(-1), indicating a low-mass host galaxy. No host galaxy emission lines are detected, leading to an upper limit on the unobscured star formation rate (SFR) of SFR[O II] < 0.07 M-circle dot yr(-1). Late-time imaging shows the iPTF 13ajg host galaxy to be faint, with g(AB) approximate to 27.0 and R-AB >= 26.0 mag, corresponding to M-B,M-Vega greater than or similar to -17.7 mag. C1 [Vreeswijk, Paul M.; Gal-Yam, Avishay; De Cia, Annalisa; Rubin, Adam; Yaron, Ofer; Tal, David; Ofek, Eran O.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-7610001 Rehovot, Israel. [Savaglio, Sandra] Max Planck Inst Extraterrestrial Phys, D-85748 Garching, Germany. [Savaglio, Sandra] European So Observ, D-85748 Garching, Germany. [Savaglio, Sandra] Univ Calabria, Dept Phys, I-87036 Arcavacata Di Rende, Italy. [Quimby, Robert M.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. [Quimby, Robert M.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Sullivan, Mark] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Cenko, S. Bradley; Filippenko, Alexei V.; Clubb, Kelsey I.; Nugent, Peter E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Kulkarni, Shrinivas R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Taddia, Francesco; Sollerman, Jesper; Leloudas, Giorgos] Stockholm Univ, Oskar Klein Ctr, Dept Astron, S-10691 Stockholm, Sweden. [Leloudas, Giorgos] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Arcavi, Iair] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Arcavi, Iair] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Kasliwal, Mansi M.] Carnegie Inst Sci, Pasadena, CA 91101 USA. [Capone, John; Toy, Vicki] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Kutyrev, Alexander S.; Nugent, Peter E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Laher, Russ; Surace, Jason] CALTECH, Jet Prop Lab, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Vreeswijk, PM (reprint author), Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-7610001 Rehovot, Israel. EM paul.vreeswijk@weizmann.ac.il OI Sollerman, Jesper/0000-0003-1546-6615; Sullivan, Mark/0000-0001-9053-4820; Gal-Yam, Avishay/0000-0002-3653-5598; Savaglio, Sandra/0000-0003-2354-3238 FU W. M. Keck Foundation; Discovery Communications; NSF [AST-1005313, AST-1211916]; EU/FP7 via ERC [307260]; Israeli Committee; ISF; GIF; Minerva; Kimmel award; ARCHES award; TABASGO Foundation; Christopher R. Redlich Fund; Royal Society; NASA by Space Telescope Science Institute [HST-HF-51296.01-A]; NASA [NAS 5-26555]; DNRF; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; WIS-UK "making connections" FX This paper is based on observations collected at the Palomar 48 and 60 inch telescopes, the Nordic Optical Telescope (NOT), the Discovery Channel Telescope (DCT), the Very Large Telescope (VLT) under proposal No. 291.D-5009, and the Keck-I and Keck-II telescopes. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration (NASA); it was made possible by the generous financial support of the W. M. Keck Foundation. We are grateful to Ori D. Fox, Isaac Shivvers, Patrick L. Kelly, WeiKang Zheng, Sumin Tang, W. Kao, and Joel Johansson for performing part of the Keck observations presented in this paper, and to ESO's User Support Department and Paranal observing staff for arranging and securing the VLT DDT observations. These results made use of Lowell Observatory's Discovery Channel Telescope; Lowell operates the DCT in partnership with Boston University, Northern Arizona University, the University of Maryland, and the University of Toledo. Partial support of the DCT was provided by Discovery Communications. The LMI at the DCT was built by Lowell Observatory using funds from the NSF grant AST-1005313. We wish to thank Sylvain Veilleux, Antonino Cucchiara, Suvi Gezari, and Eleonora Troja for assistance in obtaining the DCT data. It is a pleasure to thank Daniele Malesani for providing his handy finder-chart routine, and Melina Bersten for interesting discussions. A.G.-Y. is supported by the EU/FP7 via ERC grant No. 307260, the Quantum Universe I-Core program by the Israeli Committee for planning and funding, and the ISF, GIF, Minerva, and ISF grants, WIS-UK "making connections," and Kimmel and ARCHES awards. A.V.F.'s supernova group at UC Berkeley is supported through NSF grant AST-1211916, the TABASGO Foundation, and the Christopher R. Redlich Fund. M. S. acknowledges support from the Royal Society. Support for D. A. P. was provided by NASA through Hubble Fellowship grant HST-HF-51296.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. The Dark Cosmology Centre is funded by the DNRF. The National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231, provided staff, computational resources, and data storage for this project. NR 100 TC 24 Z9 25 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2014 VL 797 IS 1 AR 24 DI 10.1088/0004-637X/797/1/24 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU9LT UT WOS:000345915000024 ER PT J AU Zahnle, KJ Marley, MS AF Zahnle, Kevin J. Marley, Mark S. TI METHANE, CARBON MONOXIDE, AND AMMONIA IN BROWN DWARFS AND SELF-LUMINOUS GIANT PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; brown dwarfs; planets and satellites: gaseous planets ID T-DWARFS; ATMOSPHERIC CHEMISTRY; CHEMICAL-EQUILIBRIUM; GLIESE 229B; HD 209458B; Y DWARFS; GJ 504; JUPITER; NITROGEN; PHOTOCHEMISTRY AB We address disequilibrium abundances of some simple molecules in the atmospheres of solar composition brown dwarfs and self-luminous extrasolar giant planets using a kinetics-based one-dimensional atmospheric chemistry model. Our approach is to use the full kinetics model to survey the parameter space with effective temperatures between 500 K and 1100 K. In all of these worlds, equilibrium chemistry favors CH4 over CO in the parts of the atmosphere that can be seen from Earth, but in most disequilibrium favors CO. The small surface gravity of a planet strongly discriminates against CH4 when compared to an otherwise comparable brown dwarf. If vertical mixing is like Jupiter's, the transition from methane to CO occurs at 500 K in a planet. Sluggish vertical mixing can raise this to 600 K, but clouds or more vigorous vertical mixing could lower this to 400 K. The comparable thresholds in brown dwarfs are 1100 +/- 100 K. Ammonia is also sensitive to gravity, but, unlike CH4/CO, the NH3/N-2 ratio is insensitive to mixing, which makes NH3 a potential proxy for gravity. HCN may become interesting in high-gravity brown dwarfs with very strong vertical mixing. Detailed analysis of the CO-CH4 reaction network reveals that the bottleneck to CO hydrogenation goes through methanol, in partial agreement with previous work. Simple, easy to use quenching relations are derived by fitting to the complete chemistry of the full ensemble of models. These relations are valid for determining CO, CH4, NH3, HCN, and CO2 abundances in the range of self-luminous worlds we have studied, but may not apply if atmospheres are strongly heated at high altitudes by processes not considered here (e.g., wave breaking). C1 [Zahnle, Kevin J.; Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Zahnle, KJ (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA. EM Kevin.J.Zahnle@NASA.gov; Mark.S.Marley@NASA.gov OI Marley, Mark/0000-0002-5251-2943 FU NASA Planetary Atmospheres Program FX The authors thank Richard Freedman, Caroline Morley, Julianne Moses, Didier Saumon, and Channon Visscher for many insightful discussions and occasional course corrections. The authors thank the NASA Planetary Atmospheres Program for support of this work. NR 60 TC 21 Z9 21 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 10 PY 2014 VL 797 IS 1 AR 41 DI 10.1088/0004-637X/797/1/41 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU9LT UT WOS:000345915000041 ER PT J AU Cordiner, MA Remijan, AJ Boissier, J Milam, SN Mumma, MJ Charnley, SB Paganini, L Villanueva, G Bockelee-Morvan, D Kuan, YJ Chuang, YL Lis, DC Biver, N Crovisier, J Minniti, D Coulson, IM AF Cordiner, M. A. Remijan, A. J. Boissier, J. Milam, S. N. Mumma, M. J. Charnley, S. B. Paganini, L. Villanueva, G. Bockelee-Morvan, D. Kuan, Y. -J. Chuang, Y. -L. Lis, D. C. Biver, N. Crovisier, J. Minniti, D. Coulson, I. M. TI MAPPING THE RELEASE OF VOLATILES IN THE INNER COMAE OF COMETS C/2012 F6 (LEMMON) AND C/2012 S1 (ISON) USING THE ATACAMA LARGE MILLIMETER/SUBMILLIMETER ARRAY (vol 792, L2, 2014) SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Correction C1 [Cordiner, M. A.; Milam, S. N.; Mumma, M. J.; Charnley, S. B.; Paganini, L.; Villanueva, G.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [Cordiner, M. A.; Paganini, L.; Villanueva, G.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Remijan, A. J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Boissier, J.] IRAM, F-38406 St Martin Dheres, France. [Bockelee-Morvan, D.; Biver, N.; Crovisier, J.] UPMC, Univ Paris Diderot, CNRS, LEISA,Observat Paris, F-92195 Meudon, France. [Kuan, Y. -J.; Chuang, Y. -L.] Natl Taiwan Normal Univ, Taipei 116, Taiwan. [Kuan, Y. -J.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Lis, D. C.] Univ Paris 06, Sorbonne Univ, CNRS, Observat Paris,LERMA,UMR 8112, F-75014 Paris, France. [Lis, D. C.] CALTECH, Pasadena, CA 91125 USA. [Minniti, D.] Pontificia Univ Catolica Chile, Santiago, Chile. [Minniti, D.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. [Coulson, I. M.] Joint Astron Ctr, Hilo, HI 96720 USA. RP Cordiner, MA (reprint author), NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM martin.cordiner@nasa.gov RI Milam, Stefanie/D-1092-2012 OI Milam, Stefanie/0000-0001-7694-4129 NR 1 TC 0 Z9 0 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 10 PY 2014 VL 797 IS 1 AR L11 DI 10.1088/2041-8205/797/1/L11 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU3HU UT WOS:000345504000011 ER PT J AU Troja, E Segreto, A La Parola, V Hartmann, D Baumgartner, W Markwardt, C Barthelmy, S Cusumano, G Gehrels, N AF Troja, E. Segreto, A. La Parola, V. Hartmann, D. Baumgartner, W. Markwardt, C. Barthelmy, S. Cusumano, G. Gehrels, N. TI SWIFT/BAT DETECTION OF HARD X-RAYS FROM TYCHO'S SUPERNOVA REMNANT: EVIDENCE FOR TITANIUM-44 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma rays: general; ISM: individual objects (SN 1572, Tycho's SNR); ISM: supernova remnants; nuclear reactions, nucleosynthesis, abundances ID CHANDRASEKHAR MASS MODELS; DELAYED-DETONATION MODELS; BRAHES 1572 SUPERNOVA; IA SUPERNOVAE; LINE EMISSION; WHITE-DWARF; NUCLEOSYNTHESIS; CASSIOPEIA; SPECTRUM; MISSION AB We report Swift/Burst Alert Telescope survey observations of the Tycho's supernova remnant, performed over a period of 104 months since the mission's launch. The remnant is detected with high significance (> 10 sigma) below 50 keV. We detect significant hard X-ray emission in the 60-85 keV band, above the continuum level predicted by a simple synchrotron model. The location of the observed excess is consistent with line emission from radioactive titanium-44, so far reported only for Type II supernova explosions. We discuss the implications of these results in the context of the galactic supernova rate, and nucleosynthesis in Type Ia supernova. C1 [Troja, E.; Baumgartner, W.; Markwardt, C.; Barthelmy, S.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Troja, E.] Univ Maryland, Dept Phys & Astron, College Pk, MD 20742 USA. [Segreto, A.; La Parola, V.; Cusumano, G.] INAF IASF Palermo, I-90146 Palermo, Italy. [Hartmann, D.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29631 USA. RP Troja, E (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM eleonora.troja@nasa.gov OI Troja, Eleonora/0000-0002-1869-7817; Segreto, Alberto/0000-0001-7341-6603; La Parola, Valentina/0000-0002-8087-6488; Cusumano, Giancarlo/0000-0002-8151-1990; Hartmann, Dieter/0000-0002-8028-0991 NR 42 TC 3 Z9 3 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 10 PY 2014 VL 797 IS 1 AR L6 DI 10.1088/2041-8205/797/1/L6 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU3HU UT WOS:000345504000006 ER PT J AU Werneth, CM Maung, KM Ford, WP Norbury, JW Vera, MD AF Werneth, Charles M. Maung, Khin M. Ford, William P. Norbury, John W. Vera, Michael D. TI Elastic differential cross sections for space radiation applications SO PHYSICAL REVIEW C LA English DT Article ID MULTIPLE-SCATTERING THEORY; PROTON-SCATTERING; IMPULSE APPROXIMATION; NUCLEAR REACTIONS; UNIFIED THEORY; OPTICAL-MODEL; ENERGY; POTENTIALS; DENSITIES AB The eikonal, partial wave (PW) Lippmann-Schwinger, and three-dimensional Lippmann-Schwinger (LS3D) methods are compared for nuclear reactions that are relevant for space radiation applications. Numerical convergence of the eikonal method is readily achieved when exact formulas of the optical potential are used for light nuclei (A <= 16), and the momentum-space representation of the optical potential is used for heavier nuclei. The PW solution method is known to be numerically unstable for systems that require a large number of partial waves, and, as a result, the LS3D method is employed. The effect of relativistic kinematics is studied with the PW and LS3D methods and is compared to eikonal results. It is recommended that the LS3D method be used for high-energy nucleon-nucleus reactions and nucleus-nucleus reactions at all energies because of its rapid numerical convergence and stability. C1 [Werneth, Charles M.; Norbury, John W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Maung, Khin M.; Ford, William P.; Vera, Michael D.] Univ So Mississippi, Hattiesburg, MS 39406 USA. RP Werneth, CM (reprint author), NASA, Langley Res Ctr, 2 West Reid St, Hampton, VA 23681 USA. FU Human Research Program under the Human Exploration and Operations Mission Directorate of NASA; NASA [NNX13AH31AS05] FX The authors thank Steve Blattnig, Ryan Norman, Jonathan Ransom, and Francis Badavi for reviewing this manuscript. This work was supported by the Human Research Program under the Human Exploration and Operations Mission Directorate of NASA and NASA Grant No. NNX13AH31AS05. Khin Maung Maung thanks Alexander Maung for his helpful conversations. NR 47 TC 1 Z9 1 U1 1 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0556-2813 EI 1089-490X J9 PHYS REV C JI Phys. Rev. C PD DEC 9 PY 2014 VL 90 IS 6 AR 064905 DI 10.1103/PhysRevC.90.064905 PG 11 WC Physics, Nuclear SC Physics GA AW6MR UT WOS:000346384100006 ER PT J AU Abeysekara, AU Alfaro, R Alvarez, C Alvarez, JD Arceo, R Arteaga-Velazquez, JC Solares, HAA Barber, AS Baughman, BM Bautista-Elivar, N Gonzalez, JB Belmont, E BenZvi, SY Berley, D Rosales, MB Braun, J Caballero-Lopez, RA Caballero-Mora, KS Carraminnana, A Castillo, M Cotti, U Cotzomi, J de la Fuente, E De Leon, C DeYoung, T Hernandez, RD Diaz-Cruz, L Diaz-Velez, JC Dingus, BL DuVernois, MA Ellsworth, RW Fiorino, DW Fraija, N Galindo, A Garfias, F Gonzalez, MM Goodman, JA Grabski, V Gussert, M Hampel-Arias, Z Harding, JP Hui, CM Huntemeyer, P Imran, A Iriarte, A Karn, P Kieda, D Kunde, GJ Lara, A Lauer, RJ Lee, WH Lennarz, D Vargas, HL Linares, EC Linnemann, JT Longo, M Luna-Garcia, R Marinelli, A Martinez, H Martinez, O Martinez-Castro, J Matthews, JAJ McEnery, J Torres, EM Miranda-Romagnoli, P Moreno, E Mostafa, M Nellen, L Newbold, M Noriega-Papaqui, R Oceguera-Becerra, T Patricelli, B Pelayo, R Perez-Perez, EG Pretz, J Riviere, C Rosa-Gonzalez, D Ryan, J Salazar, H Salesa, F Sanchez, FE Sandoval, A Schneider, M Silich, S Sinnis, G Smith, AJ Woodle, KS Springer, RW Taboada, I Toale, PA Tollefson, K Torres, I Ukwatta, TN Villasenor, L Weisgarber, T Westerhoff, S Wisher, IG Wood, J Yodh, GB Younk, PW Zaborov, D Zepeda, A Zhou, H Abazajian, KN AF Abeysekara, A. U. Alfaro, R. Alvarez, C. Alvarez, J. D. Arceo, R. Arteaga-Velazquez, J. C. Solares, H. A. Ayala Barber, A. S. Baughman, B. M. Bautista-Elivar, N. Gonzalez, J. Becerra Belmont, E. BenZvi, S. Y. Berley, D. Bonilla Rosales, M. Braun, J. Caballero-Lopez, R. A. Caballero-Mora, K. S. Carraminana, A. Castillo, M. Cotti, U. Cotzomi, J. de la Fuente, E. De Leon, C. DeYoung, T. Diaz Hernandez, R. Diaz-Cruz, L. Diaz-Velez, J. C. Dingus, B. L. DuVernois, M. A. Ellsworth, R. W. Fiorino, D. W. Fraija, N. Galindo, A. Garfias, F. Gonzalez, M. M. Goodman, J. A. Grabski, V. Gussert, M. Hampel-Arias, Z. Harding, J. P. Hui, C. M. Huentemeyer, P. Imran, A. Iriarte, A. Karn, P. Kieda, D. Kunde, G. J. Lara, A. Lauer, R. J. Lee, W. H. Lennarz, D. Leon Vargas, H. Linares, E. C. Linnemann, J. T. Longo, M. Luna-Garcia, R. Marinelli, A. Martinez, H. Martinez, O. Martinez-Castro, J. Matthews, J. A. J. McEnery, J. Mendoza Torres, E. Miranda-Romagnoli, P. Moreno, E. Mostafa, M. Nellen, L. Newbold, M. Noriega-Papaqui, R. Oceguera-Becerra, T. Patricelli, B. Pelayo, R. Perez-Perez, E. G. Pretz, J. Riviere, C. Rosa-Gonzalez, D. Ryan, J. Salazar, H. Salesa, F. Sanchez, F. E. Sandoval, A. Schneider, M. Silich, S. Sinnis, G. Smith, A. J. Woodle, K. Sparks Springer, R. W. Taboada, I. Toale, P. A. Tollefson, K. Torres, I. Ukwatta, T. N. Villasenor, L. Weisgarber, T. Westerhoff, S. Wisher, I. G. Wood, J. Yodh, G. B. Younk, P. W. Zaborov, D. Zepeda, A. Zhou, H. Abazajian, K. N. CA HAWC Collaboration TI Sensitivity of HAWC to high-mass dark matter annihilations SO PHYSICAL REVIEW D LA English DT Article ID DWARF SPHEROIDAL GALAXIES; GAMMA-RAY EMISSION; HALO; CONSTRAINTS; FERMI; SIMULATION; DETECTOR; SEARCH AB The High Altitude Water Cherenkov (HAWC) observatory is a wide field-of-view detector sensitive to gamma rays of 100 GeV to a few hundred TeV. Located in central Mexico at 19 degrees North latitude and 4100 m above sea level, HAWC will observe gamma rays and cosmic rays with an array of water Cherenkov detectors. The full HAWC array is scheduled to be operational in Spring 2015. In this paper, we study the HAWC sensitivity to the gamma-ray signatures of high-mass (multi-TeV) dark matter annihilation. The HAWC observatory will be sensitive to diverse searches for dark matter annihilation, including annihilation from extended dark matter sources, the diffuse gamma-ray emission from dark matter annihilation, and gamma-ray emission from nonluminous dark matter subhalos. Here we consider the HAWC sensitivity to a subset of these sources, including dwarf galaxies, the M31 galaxy, the Virgo cluster, and the Galactic center. We simulate the HAWC response to gamma rays from these sources in several well-motivated dark matter annihilation channels. If no gamma-ray excess is observed, we show the limits HAWC can place on the dark matter cross section from these sources. In particular, in the case of dark matter annihilation into gauge bosons, HAWC will be able to detect a narrow range of dark matter masses to cross sections below thermal. HAWC should also be sensitive to nonthermal cross sections for masses up to nearly 1000 TeV. The constraints placed by HAWC on the dark matter cross section from known sources should be competitive with current limits in the mass range where HAWC has similar sensitivity. HAWC can additionally explore higher dark matter masses than are currently constrained. C1 [Abeysekara, A. U.; Linnemann, J. T.; Tollefson, K.; Ukwatta, T. N.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Alfaro, R.; Belmont, E.; Grabski, V.; Leon Vargas, H.; Marinelli, A.; Oceguera-Becerra, T.; Sandoval, A.] Univ Nacl Autonoma Mexico, Inst Fis, Mexico City 04510, DF, Mexico. [Alfaro, R.; Alvarez, C.; Baughman, B. M.; Gonzalez, J. Becerra; Berley, D.; Braun, J.; Ellsworth, R. W.; Gonzalez, M. M.; Goodman, J. A.; Smith, A. J.; Wood, J.] Univ Maryland, Dept Phys, College Pk, MD 20740 USA. [Alvarez, C.; Arceo, R.] Univ Autonoma Chiapas, CEFyMAP, Chiapas, Mexico. [Alvarez, J. D.; Arteaga-Velazquez, J. C.; Cotti, U.; De Leon, C.; Linares, E. C.; Villasenor, L.] Univ Michoacana, Morelia, Michoacan, Mexico. [Solares, H. A. Ayala; Hui, C. M.; Huentemeyer, P.; Zhou, H.] Michigan Technol Univ, Dept Phys, Houghton, MI 49931 USA. [Barber, A. S.; Kieda, D.; Newbold, M.; Springer, R. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Bautista-Elivar, N.; Perez-Perez, E. G.] Univ Politecn Pachuca, Pachuca, Hgo, Mexico. [Gonzalez, J. Becerra] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [BenZvi, S. Y.; Diaz-Velez, J. C.; DuVernois, M. A.; Fiorino, D. W.; Hampel-Arias, Z.; Imran, A.; Weisgarber, T.; Westerhoff, S.; Wisher, I. G.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Bonilla Rosales, M.; Carraminana, A.; Diaz Hernandez, R.; Galindo, A.; Mendoza Torres, E.; Rosa-Gonzalez, D.; Silich, S.; Torres, I.] Inst Nacl Astrofis Opt & Electr, Puebla, Mexico. [Caballero-Lopez, R. A.; Lara, A.] Univ Nacl Autonoma Mexico, Inst Geofis, Mexico City 04510, DF, Mexico. [Caballero-Mora, K. S.; Martinez, H.; Sanchez, F. E.; Zepeda, A.] IPN, Ctr Invest & Estudios Avanzados, Dept Phys, Mexico City 07738, DF, Mexico. [Castillo, M.; Cotzomi, J.; Diaz-Cruz, L.; Martinez, O.; Moreno, E.; Salazar, H.] Benemerita Univ Autonoma Puebla, Fac Ciencias Fis & Matemat, Puebla, Mexico. [de la Fuente, E.; Oceguera-Becerra, T.] Ctr Univ Ciencias Exactas & Ingn, Dept Fis, Guadalajara, Jalisco, Mexico. [de la Fuente, E.; Oceguera-Becerra, T.] Univ Guadalajara, Ctr Univ Valles, Dept Ciencias Nat & Exactas, Guadalajara, Jalisco, Mexico. [DeYoung, T.; Mostafa, M.; Pretz, J.; Salesa, F.; Woodle, K. Sparks; Zaborov, D.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Dingus, B. L.; Harding, J. P.; Kunde, G. J.; Sinnis, G.; Younk, P. W.] Los Alamos Natl Lab, Div Phys, Los Alamos, NM 87545 USA. [Ellsworth, R. W.] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA. [Fraija, N.; Garfias, F.; Gonzalez, M. M.; Iriarte, A.; Lee, W. H.; Patricelli, B.; Riviere, C.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Gussert, M.; Longo, M.] Colorado State Univ, Dept Phys, Ft Collins, CO 80523 USA. [Karn, P.; Yodh, G. B.; Abazajian, K. N.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Lauer, R. J.; Matthews, J. A. J.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Lennarz, D.; Taboada, I.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Lennarz, D.; Taboada, I.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Luna-Garcia, R.; Martinez-Castro, J.; Pelayo, R.] Inst Politecn Nacl, Ctr Invest Computac, Mexico City, DF, Mexico. [McEnery, J.] Univ Autonoma Estado Hidalgo, Pachuca, Hidalgo, Mexico. [Miranda-Romagnoli, P.; Noriega-Papaqui, R.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. [Nellen, L.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Ryan, J.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Schneider, M.; Toale, P. A.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. RP Abeysekara, AU (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. EM bbaugh@umdgrb.umd.edu; jpharding@lanl.gov; kevork@uci.edu OI Dingus, Brenda/0000-0001-8451-7450; Lara, Alejandro/0000-0001-6336-5291; Becerra Gonzalez, Josefa/0000-0002-6729-9022 FU U.S. National Science Foundation (NSF); U.S. Department of Energy, Office of High-Energy Physics; Laboratory Directed Research and Development (LDRD) program of Los Alamos National Laboratory; Consejo Nacional de Ciencia y Tecnologia (CONACyT), Mexico; Red de Fisica de Altas Energias, Mexico; DGAPA-UNAM, Mexico [IN108713 IG100414-3]; Luc-Binette Foundation UNAM Postdoctoral Fellowship; University of Wisconsin Alumni Research Foundation; NSF CAREER [PHY-11-59224] FX We acknowledge the support from U.S. National Science Foundation (NSF); U.S. Department of Energy, Office of High-Energy Physics; The Laboratory Directed Research and Development (LDRD) program of Los Alamos National Laboratory; Consejo Nacional de Ciencia y Tecnologia (CONACyT), Mexico; Red de Fisica de Altas Energias, Mexico; DGAPA-UNAM IN108713 IG100414-3, Mexico; Luc-Binette Foundation UNAM Postdoctoral Fellowship; and the University of Wisconsin Alumni Research Foundation. K. N. A. is supported by NSF CAREER Grant No. PHY-11-59224. NR 69 TC 13 Z9 13 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD DEC 8 PY 2014 VL 90 IS 12 AR 122002 DI 10.1103/PhysRevD.90.122002 PG 14 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AW1KN UT WOS:000346048500001 ER PT J AU Holt, AL Vahidinia, S Gagnon, YL Morse, DE Sweeney, AM AF Holt, Amanda L. Vahidinia, Sanaz Gagnon, Yakir Luc Morse, Daniel E. Sweeney, Alison M. TI Photosymbiotic giant clams are transformers of solar flux SO JOURNAL OF THE ROYAL SOCIETY INTERFACE LA English DT Article DE photosymbiosis; giant clams; solar energy conversion; Symbiodinium; energy efficiency ID LIGHT MEASUREMENTS; POLARIZED-LIGHT; SCATTERING; CORALS; PHOTOSYNTHESIS; IRIDOPHORES; SYMBIOSIS; TRIDACNA; HOST AB 'Giant' tridacnid clams have evolved a three-dimensional, spatially efficient, photodamage-preventing system for photosymbiosis. We discovered that the mantle tissue of giant clams, which harbours symbiotic nutrition-providing microalgae, contains a layer of iridescent cells called iridocytes that serve to distribute photosynthetically productive wavelengths by lateral and forward-scattering of light into the tissue while back-reflecting non-productive wavelengths with a Bragg mirror. The wavelength-and angle-dependent scattering from the iridocytes is geometrically coupled to the vertically pillared microalgae, resulting in an even re-distribution of the incoming light along the sides of the pillars, thus enabling photosynthesis deep in the tissue. There is a physical analogy between the evolved function of the clam system and an electric transformer, which changes energy flux per area in a system while conserving total energy. At incident light levels found on shallow coral reefs, this arrangement may allow algae within the clam system to both efficiently use all incident solar energy and avoid the photodamage and efficiency losses due to non-photochemical quenching that occur in the reef-building coral photosymbiosis. Both intra-tissue radiometry andmultiscale optical modelling support our interpretation of the system's photophysics. This highly evolved 'three-dimensional' biophotonic system suggests a strategy for more efficient, damage-resistant photovoltaic materials and more spatially efficient solar production of algal biofuels, foods and chemicals. C1 [Holt, Amanda L.; Morse, Daniel E.; Sweeney, Alison M.] Univ Calif Santa Barbara, Ctr Energy Efficiency, Santa Barbara, CA 93106 USA. [Holt, Amanda L.; Morse, Daniel E.; Sweeney, Alison M.] Univ Calif Santa Barbara, Dept Mol Cellular & Dev Biol, Santa Barbara, CA 93106 USA. [Vahidinia, Sanaz] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Mountain View, CA 94035 USA. [Gagnon, Yakir Luc] Duke Univ, Dept Biol, Durham, NC 27708 USA. [Holt, Amanda L.; Sweeney, Alison M.] Univ Penn, David Rittenhouse Labs, Dept Phys & Astron, Philadelphia, PA 19104 USA. RP Morse, DE (reprint author), Univ Calif Santa Barbara, Ctr Energy Efficiency, 3155 Marine Biotechnol Bldg, Santa Barbara, CA 93106 USA. EM d_morse@lifesci.ucsb.edu; alisonsw@physics.upenn.edu RI Gagnon, Yakir/C-2665-2008 OI Gagnon, Yakir/0000-0003-2512-4520 FU Army Research Office [W911NF-10-1-0139]; Office of Naval Research (through MURI) [N00014-09-1-1053] FX This research was supported by grants from the Army Research Office (no. W911NF-10-1-0139) and the Office of Naval Research (through MURI award no. N00014-09-1-1053 to Duke University). NR 33 TC 6 Z9 6 U1 10 U2 69 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1742-5689 EI 1742-5662 J9 J R SOC INTERFACE JI J. R. Soc. Interface PD DEC 6 PY 2014 VL 11 IS 101 AR UNSP 20140678 DI 10.1098/rsif.2014.0678 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AR6DF UT WOS:000343672800003 PM 25401182 ER PT J AU Larsen, AB Wagner, JR Kandel, S Salomon-Ferrer, R Vaidehi, N Jain, A AF Larsen, Adrien B. Wagner, Jeffrey R. Kandel, Saugat Salomon-Ferrer, Romelia Vaidehi, Nagarajan Jain, Abhinandan TI GneimoSim: A Modular Internal Coordinates Molecular Dynamics Simulation Package SO JOURNAL OF COMPUTATIONAL CHEMISTRY LA English DT Article DE molecular dynamics; torsional MD; ICMD; GNEIMO; refinement; software; GneimoSim ID MASS OPERATOR METHOD; BIOMOLECULAR SIMULATION; CONFORMATIONAL DYNAMICS; STRUCTURE REFINEMENT; STRUCTURE PREDICTION; SMALL PROTEINS; RELAXATION; MODELS; EQUIPARTITION; ALGORITHMS AB The generalized Newton-Euler inverse mass operator (GNEIMO) method is an advanced method for internal coordinates molecular dynamics (ICMD). GNEIMO includes several theoretical and algorithmic advancements that address longstanding challenges with ICMD simulations. In this article, we describe the GneimoSim ICMD software package that implements the GNEIMO method. We believe that GneimoSim is the first software package to include advanced features such as the equipartition principle derived for internal coordinates, and a method for including the Fixman potential to eliminate systematic statistical biases introduced by the use of hard constraints. Moreover, by design, GneimoSim is extensible and can be easily interfaced with third party force field packages for ICMD simulations. Currently, GneimoSim includes interfaces to LAMMPS, OpenMM, and Rosetta force field calculation packages. The availability of a comprehensive Python interface to the underlying C++ classes and their methods provides a powerful and versatile mechanism for users to develop simulation scripts to configure the simulation and control the simulation flow. GneimoSim has been used extensively for studying the dynamics of protein structures, refinement of protein homology models, and for simulating large scale protein conformational changes with enhanced sampling methods. GneimoSim is not limited to proteins and can also be used for the simulation of polymeric materials. C1 [Larsen, Adrien B.; Wagner, Jeffrey R.; Kandel, Saugat; Salomon-Ferrer, Romelia; Vaidehi, Nagarajan] City Hope Natl Med Ctr, Beckman Res Inst, Div Immunol, Duarte, CA 91010 USA. [Jain, Abhinandan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Vaidehi, N (reprint author), City Hope Natl Med Ctr, Beckman Res Inst, Div Immunol, Duarte, CA 91010 USA. EM nvaidehi@coh.org; abhi.jain@jpl.nasa.gov FU National Institute of Health [RO1GM082896-01A2]; Jet Propulsion Laboratory (JPL); California Institute of Technology (National Aeronautics and Space Administration) FX Contract grant sponsor: National Institute of Health; Contract grant number: RO1GM082896-01A2; Contract grant sponsor: Jet Propulsion Laboratory (JPL) and California Institute of Technology (National Aeronautics and Space Administration) NR 52 TC 2 Z9 2 U1 4 U2 26 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0192-8651 EI 1096-987X J9 J COMPUT CHEM JI J. Comput. Chem. PD DEC 5 PY 2014 VL 35 IS 31 BP 2245 EP 2255 DI 10.1002/jcc.23743 PG 11 WC Chemistry, Multidisciplinary SC Chemistry GA AS5YC UT WOS:000344341400003 PM 25263538 ER PT J AU Yabuta, H Uesugi, M Naraoka, H Ito, M Kilcoyne, ALD Sandford, SA Kitajima, F Mita, H Takano, Y Yada, T Karouji, Y Ishibashi, Y Okada, T Abe, M AF Yabuta, Hikaru Uesugi, Masayuki Naraoka, Hiroshi Ito, Motoo Kilcoyne, A. L. David Sandford, Scott A. Kitajima, Fumio Mita, Hajime Takano, Yoshinori Yada, Toru Karouji, Yuzuru Ishibashi, Yukihiro Okada, Tatsuaki Abe, Masanao TI X-ray absorption near edge structure spectroscopic study of Hayabusa category 3 carbonaceous particles SO EARTH PLANETS AND SPACE LA English DT Article DE Hayabusa; Category 3 carbonaceous particles; STXM; XANES; Organic macromolecule ID INTERPLANETARY DUST PARTICLES; ISOTOPIC COMPOSITIONS; ITOKAWA REGOLITH; ORGANIC-MATTER; SAMPLES; ORIGIN; XANES; SPECTROMICROSCOPY; EVOLUTION; CHONDRITES AB Analyses with a scanning transmission x-ray microscope (STXM) using x-ray absorption near edge structure (XANES) spectroscopy were applied for the molecular characterization of two kinds of carbonaceous particles of unknown origin, termed category 3, which were collected from the Hayabusa spacecraft sample catcher. Carbon-XANES spectra of the category 3 particles displayed typical spectral patterns of heterogeneous organic macromolecules; peaks corresponding to aromatic/olefinic carbon, heterocyclic nitrogen and/or nitrile, and carboxyl carbon were all detected. Nitrogen-XANES spectra of the particles showed the presence of N-functional groups such as imine, nitrile, aromatic nitrogen, amide, pyrrole, and amine. An oxygen-XANES spectrum of one of the particles showed a ketone group. Differences in carbon-and nitrogen-XANES spectra of the category 3 particles before and after transmission electron microscopic (TEM) observations were observed, which demonstrates that the carbonaceous materials are electron beam sensitive. Calcium-XANES spectroscopy and elemental contrast mapping identified a calcium carbonate grain from one of the category 3 particles. No fluorine-containing molecular species were detected in fluorine-XANES spectra of the particles. The organic macromolecular features of the category 3 particles were distinct from commercial and/or biological 'fresh (non degraded)' polymers, but the category 3 molecular features could possibly reflect degradation of contaminant polymer materials or polymer materials used on the Hayabusa spacecraft. However, an extraterrestrial origin for these materials cannot currently be ruled out. C1 [Yabuta, Hikaru] Osaka Univ, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. [Uesugi, Masayuki; Yada, Toru; Karouji, Yuzuru; Ishibashi, Yukihiro; Okada, Tatsuaki; Abe, Masanao] Japan Aerosp Explorat Agcy JAXA, ISAS, Sagamihara, Kanagawa 2525210, Japan. [Naraoka, Hiroshi; Kitajima, Fumio] Kyushu Univ, Fac Sci, Dept Earth & Planetary Sci, Fukuoka 8128581, Japan. [Ito, Motoo] Japan Agcy Marine Earth Sci Technol JAMSTEC, Kochi Inst Core Sample Res, Nankoku, Kochi 7838502, Japan. [Kilcoyne, A. L. David] Adv Light Source, Berkeley, CA 94720 USA. [Sandford, Scott A.] NASA, Ames Res Ctr Moffett Field, Mountain View, CA 94035 USA. [Mita, Hajime] Fukuoka Inst Technol, Fukuoka 8110295, Japan. [Takano, Yoshinori] Japan Agcy Marine Earth Sci & Technol JAMSTEC, Dept Biogeochem, Yokosuka, Kanagawa 2370061, Japan. RP Yabuta, H (reprint author), Osaka Univ, Dept Earth & Space Sci, 1-1 Machikaneyama, Toyonaka, Osaka 5600043, Japan. EM hyabuta@ess.sci.osaka-u.ac.jp RI U-ID, Kyushu/C-5291-2016; Yabuta, Hikaru/M-9041-2014; Kilcoyne, David/I-1465-2013 OI Yabuta, Hikaru/0000-0002-4625-5362; FU Office of Science, Office of Basic Energy Sciences, and the US Department of Energy [DE-AC02-05CH11231] FX We appreciate Daniel Glavin, an anonymous reviewer, and official editor Michael Zolensky for their constructive comments, attentive corrections, and helpful editorial assistance. The STXM at the beam line 5.3.2.2 ALS facility is supported by the Director, Office of Science, Office of Basic Energy Sciences, and the US Department of Energy under Contract No. DE-AC02-05CH11231. NR 36 TC 3 Z9 3 U1 0 U2 9 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1880-5981 J9 EARTH PLANETS SPACE JI Earth Planets Space PD DEC 3 PY 2014 VL 66 AR 156 DI 10.1186/s40623-014-0156-0 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AZ7IY UT WOS:000348394000001 ER PT J AU Aasi, J Abbott, BP Abbott, R Abbott, T Abernathy, MR Accadia, T Acernese, F Ackley, K Adams, C Adams, T Addesso, P Adhikari, RX Affeldt, C Agathos, M Aggarwal, N Aguiar, OD Ain, A Ajith, P Alemic, A Allen, B Allocca, A Amariutei, D Andersen, M Anderson, R Anderson, SB Anderson, WG Arai, K Araya, MC Arceneaux, C Areeda, J Aston, SM Astone, P Aufmuth, P Aulbert, C Austin, L Aylott, BE Babak, S Baker, PT Ballardin, G Ballmer, SW Barayoga, JC Barbet, M Barish, BC Barker, D Barone, F Barr, B Barsotti, L Barsuglia, M Barton, MA Bartos, I Bassiri, R Basti, A Batch, JC Bauchrowitz, J Bauer, TS Behnke, B Bejger, M Beker, MG Belczynski, C Bell, AS Bell, C Bergmann, G Bersanetti, D Bertolini, A Betzwieser, J Beyersdorf, PT Bilenko, IA Billingsley, G Birch, J Biscans, S Bitossi, M Bizouard, MA Black, E Blackburn, JK Blackburn, L Blair, D Bloemen, S Blom, M Bock, O Bodiya, TP Boer, M Bogaert, G Bogan, C Bond, C Bondu, F Bonelli, L Bonnand, R Bork, R Born, M Boschi, V Bose, S Bosi, L Bradaschia, C Brady, PR Braginsky, VB Branchesi, M Brau, JE Briant, T Bridges, DO Brillet, A Brinkmann, M Brisson, V Brooks, AF Brown, DA Brown, DD Bruckner, F Buchman, S Bulik, T Bulten, HJ Buonanno, A Burman, R Buskulic, D Buy, C Cadonati, L Cagnoli, G Bustillo, JC Calloni, E Camp, JB Campsie, P Cannon, KC Canuel, B Cao, J Capano, CD Carbognani, F Carbone, L Caride, S Castiglia, A Caudill, S Cavaglia, M Cavalier, F Cavalieri, R Celerier, C Cella, G Cepeda, C Cesarini, E Chakraborty, R Chalermsongsak, T Chamberlin, SJ Chao, S Charlton, P Chassande-Mottin, E Chen, X Chen, Y Chincarini, A Chiummo, A Cho, HS Chow, J Christensen, N Chu, Q Chua, SSY Chung, S Ciani, G Clara, F 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Walker, M. Wallace, L. Wang, M. Wang, X. Ward, R. L. Was, M. Weaver, B. Wei, L. -W. Weinert, M. Weinstein, A. J. Weiss, R. Welborn, T. Wen, L. Wessels, P. West, M. Westphal, T. Wette, K. Whelan, J. T. White, D. J. Whiting, B. F. Wiesner, K. Wilkinson, C. Williams, K. Williams, L. Williams, R. Williams, T. Williamson, A. R. Willis, J. L. Willke, B. Wimmer, M. Winkler, W. Wipf, C. C. Wiseman, A. G. Wittel, H. Woan, G. Worden, J. Yablon, J. Yakushin, I. Yamamoto, H. Yancey, C. C. Yang, H. Yang, Z. Yoshida, S. Yvert, M. Zadrozny, A. Zanolin, M. Zendri, J. -P. Zhang, Fan Zhang, L. Zhao, C. Zhu, X. J. Zucker, M. E. Zuraw, S. Zweizig, J. CA LIGO & Virg Collaboration TI Improved Upper Limits on the Stochastic Gravitational-Wave Background from 2009-2010 LIGO and Virgo Data SO PHYSICAL REVIEW LETTERS LA English DT Article ID INFLATION; RADIATION; MAGNETARS AB Gravitational waves from a variety of sources are predicted to superpose to create a stochastic background. This background is expected to contain unique information from throughout the history of the Universe that is unavailable through standard electromagnetic observations, making its study of fundamental importance to understanding the evolution of the Universe. We carry out a search for the stochastic background with the latest data from the LIGO and Virgo detectors. Consistent with predictions from most stochastic gravitational-wave background models, the data display no evidence of a stochastic gravitational-wave signal. Assuming a gravitational-wave spectrum of Omega(GW)(f) = Omega(alpha)(f/f(ref))(alpha), we place 95% confidence level upper limits on the energy density of the background in each of four frequency bands spanning 41.5-1726 Hz. In the frequency band of 41.5-169.25 Hz for a spectral index of alpha = 0, we constrain the energy density of the stochastic background to be Omega(GW)(f) < 5.6 x 10(-6). For the 600-1000 Hz band, Omega(GW)(f) < 0.14(f/900 Hz)(3), a factor of 2.5 lower than the best previously reported upper limits. We find Omega(GW)(f) < 1.8 x 10(-4) using a spectral index of zero for 170-600 Hz and Omega(GW)(f) < 1.0(f/1300 Hz)(3) for 1000-1726 Hz, bands in which no previous direct limits have been placed. The limits in these four bands are the lowest direct measurements to date on the stochastic background. We discuss the implications of these results in light of the recent claim by the BICEP2 experiment of the possible evidence for inflationary gravitational waves. C1 [Aasi, J.; Abbott, B. P.; Abbott, R.; Abernathy, M. R.; Adhikari, R. X.; Anderson, R.; Anderson, S. B.; Arai, K.; Araya, M. C.; Austin, L.; Barayoga, J. C.; Barish, B. C.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cepeda, C.; Chakraborty, R.; Chalermsongsak, T.; Coyne, D. C.; Dergachev, V.; Drever, R. W. P.; Driggers, J. C.; Ehrens, P.; Etzel, T.; Gushwa, K.; Gustafson, E. 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[Ain, A.; Hosken, D. J.; King, E. J.; Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia. [Iyer, B. R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Jang, H.; Kang, G.; Kim, C.; Kim, N. G.] Korea Inst Sci & Technol Informat, Taejon 305806, South Korea. [Jaranowski, P.] Bialystok Univ, PL-15424 Bialystok, Poland. [Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [Haris, K.; Mazumder, N.; Mishra, C.; Pai, A.] IISER TVM, Trivandrum 695016, Kerala, India. [Khazanov, E. A.; Palashov, O.; Poteomkin, A.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia. [Kim, C.; Lee, H. M.] Seoul Natl Univ, Seoul 151742, South Korea. [Kim, K.; Lee, H. K.] Hanyang Univ, Seoul 133791, South Korea. [Krolak, A.] IM PAN, PL-00956 Warsaw, Poland. [Krolak, A.; Kutynia, A.; Zadrozny, A.] NCBJ, PL-05400 Otwock, Poland. [Kumar, A.] Inst Plasma Res, Bhat 382428, Gandhinagar, India. [Lasky, P. D.; Melatos, A.; Sammut, L.] Univ Melbourne, Parkville, Vic 3010, Australia. [Lazzaro, C.; Vedovato, G.; Zendri, J. -P.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Levin, Y.; Premachandra, S.] Monash Univ, Clayton, Vic 3800, Australia. [Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland. [Loriette, V.; Maksimovic, I.] CNRS, ESPCI, F-75005 Paris, France. [Maglione, C.; Quiroga, G.] Argentinian Gravitat Wave Grp, RA-5000 Cordoba, Argentina. [Marchesoni, F.] Univ Camerino, Dipartimento Fis, I-62032 Camerino, Italy. [Matzner, R. A.] Univ Texas Austin, Austin, TX 78712 USA. [McGuire, S. C.; Vincent-Finley, R.; Williams, K.] Southern Univ & A&M Coll, Baton Rouge, LA 70813 USA. [Mikhailov, E. E.; Romanov, G.] Coll William & Mary, Williamsburg, VA 23187 USA. [Nayak, R. K.] IISER Kolkata, Mohanpur 741252, W Bengal, India. [Oh, S. H.; Son, E. J.] Natl Inst Mat Sci, Taejon 305390, South Korea. [Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA. [Raja, S.] RRCAT, Indore 452013, Madhya Pradesh, India. [Reid, S.] Univ West Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland. [Rosinska, D.] Inst Astron, PL-65265 Zielona Gora, Poland. [Sengupta, A. S.] Indian Inst Technol, Ahmadabad 382424, Gujarat, India. [Sturani, R.] Univ Estadual Paulista, Int Ctr Theoret Phys, Inst Fis Teor, South Amer Inst Res, BR-01140070 Sao Paulo, Brazil. [Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA. [Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA. [Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA. [Williams, T.; Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA. [Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA. RP Aasi, J (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA. RI Costa, Cesar/G-7588-2012; Chow, Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Ciani, Giacomo/G-1036-2011; Di Virgilio, Angela Dora Vittoria/E-9078-2015; Sergeev, Alexander/F-3027-2017; Harms, Jan/J-4359-2012; Frasconi, Franco/K-1068-2016; Groot, Paul/K-4391-2016; Lazzaro, Claudia/L-2986-2016; Pinto, Innocenzo/L-3520-2016; Ferrante, Isidoro/F-1017-2012; Chen, Yanbei/A-2604-2013; Losurdo, Giovanni/K-1241-2014; Bondu, Francois/A-2071-2012; Travasso, Flavio/J-9595-2016; Bartos, Imre/A-2592-2017; Punturo, Michele/I-3995-2012; Cella, Giancarlo/A-9946-2012; Cesarini, Elisabetta/C-4507-2017; Shaddock, Daniel/A-7534-2011; Vicere, Andrea/J-1742-2012; Rocchi, Alessio/O-9499-2015; Martelli, Filippo/P-4041-2015; Branchesi, Marica/P-2296-2015; Strain, Kenneth/D-5236-2011; Miao, Haixing/O-1300-2013; Howell, Eric/H-5072-2014; Gehring, Tobias/A-8596-2016; Heidmann, Antoine/G-4295-2016; Nelemans, Gijs/D-3177-2012; Marchesoni, Fabio/A-1920-2008; Zhu, Xingjiang/E-1501-2016; prodi, giovanni/B-4398-2010; Strigin, Sergey/I-8337-2012; Leonardi, Matteo/G-9694-2015; Sigg, Daniel/I-4308-2015; Puppo, Paola/J-4250-2012; Tacca, Matteo/J-1599-2015; Graef, Christian/J-3167-2015; Bell, Angus/E-7312-2011; Ottaway, David/J-5908-2015; Garufi, Fabio/K-3263-2015; Deleglise, Samuel/B-1599-2015; Neri, Igor/F-1482-2010; Aggarwal, Nancy/M-7203-2015; Danilishin, Stefan/K-7262-2012; Khalili, Farit/D-8113-2012; Gammaitoni, Luca/B-5375-2009; Iyer, Bala R./E-2894-2012; Prokhorov, Leonid/I-2953-2012; Gemme, Gianluca/C-7233-2008; Lee, Chang-Hwan/B-3096-2015; Steinlechner, Sebastian/D-5781-2013; Gorodetsky, Michael/C-5938-2008; McClelland, David/E-6765-2010; Hild, Stefan/A-3864-2010; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Ward, Robert/I-8032-2014; OI Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Ciani, Giacomo/0000-0003-4258-9338; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Aulbert, Carsten/0000-0002-1481-8319; Coccia, Eugenio/0000-0002-6669-5787; Denker, Timo/0000-0003-1259-5315; O'Shaughnessy, Richard/0000-0001-5832-8517; Frasconi, Franco/0000-0003-4204-6587; Groot, Paul/0000-0002-4488-726X; Lazzaro, Claudia/0000-0001-5993-3372; Ferrante, Isidoro/0000-0002-0083-7228; Losurdo, Giovanni/0000-0003-0452-746X; Bondu, Francois/0000-0001-6487-5197; Travasso, Flavio/0000-0002-4653-6156; Punturo, Michele/0000-0001-8722-4485; Cella, Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167; Shaddock, Daniel/0000-0002-6885-3494; Vicere, Andrea/0000-0003-0624-6231; Rocchi, Alessio/0000-0002-1382-9016; Martelli, Filippo/0000-0003-3761-8616; Strain, Kenneth/0000-0002-2066-5355; Miao, Haixing/0000-0003-4101-9958; Howell, Eric/0000-0001-7891-2817; Gehring, Tobias/0000-0002-4311-2593; Heidmann, Antoine/0000-0002-0784-5175; Nelemans, Gijs/0000-0002-0752-2974; Marchesoni, Fabio/0000-0001-9240-6793; Zhu, Xingjiang/0000-0001-7049-6468; prodi, giovanni/0000-0001-5256-915X; Sigg, Daniel/0000-0003-4606-6526; Puppo, Paola/0000-0003-4677-5015; Tacca, Matteo/0000-0003-1353-0441; Graef, Christian/0000-0002-4535-2603; Bell, Angus/0000-0003-1523-0821; Garufi, Fabio/0000-0003-1391-6168; Deleglise, Samuel/0000-0002-8680-5170; Neri, Igor/0000-0002-9047-9822; Danilishin, Stefan/0000-0001-7758-7493; Gammaitoni, Luca/0000-0002-4972-7062; Iyer, Bala R./0000-0002-4141-5179; Gemme, Gianluca/0000-0002-1127-7406; Lee, Chang-Hwan/0000-0003-3221-1171; Steinlechner, Sebastian/0000-0003-4710-8548; Gorodetsky, Michael/0000-0002-5159-2742; McClelland, David/0000-0001-6210-5842; Vecchio, Alberto/0000-0002-6254-1617; Mandel, Ilya/0000-0002-6134-8946; Whiting, Bernard F/0000-0002-8501-8669; Murphy, David/0000-0002-8538-815X; Pitkin, Matthew/0000-0003-4548-526X; Veitch, John/0000-0002-6508-0713; Davies, Gareth/0000-0002-4289-3439; Allen, Bruce/0000-0003-4285-6256; Granata, Massimo/0000-0003-3275-1186; Kanner, Jonah/0000-0001-8115-0577; Leavey, Sean/0000-0001-8253-0272; Freise, Andreas/0000-0001-6586-9901; Nitz, Alexander/0000-0002-1850-4587; calloni, enrico/0000-0003-4819-3297; Scott, Jamie/0000-0001-6701-6515; Sorazu, Borja/0000-0002-6178-3198; Zweizig, John/0000-0002-1521-3397; Del Pozzo, Walter/0000-0003-3978-2030; Husa, Sascha/0000-0002-0445-1971; Pinto, Innocenzo M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200; Swinkels, Bas/0000-0002-3066-3601; Guidi, Gianluca/0000-0002-3061-9870; Collette, Christophe/0000-0002-4430-3703; Pierro, Vincenzo/0000-0002-6020-5521; Vetrano, Flavio/0000-0002-7523-4296; Addesso, Paolo/0000-0003-0895-184X; Naticchioni, Luca/0000-0003-2918-0730; Vocca, Helios/0000-0002-1200-3917; Drago, Marco/0000-0002-3738-2431; Ward, Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447; Whelan, John/0000-0001-5710-6576; Vedovato, Gabriele/0000-0001-7226-1320; Boschi, Valerio/0000-0001-8665-2293; Matichard, Fabrice/0000-0001-8982-8418 FU U.S. National Science Foundation; Science and Technology Facilities Council of the United Kingdom; Max-Planck-Society; State of Niedersachsen, Germany; Italian Istituto Nazionale di Fisica Nucleare; French Centre National de la Recherche Scientifique; Australian Research Council; International Science Linkages program of the Commonwealth of Australia; Council of Scientific and Industrial Research of India; Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de Economia y Competitividad; Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears; Netherlands Organisation for Scientific Research; Polish Ministry of Science and Higher Education; FOCUS Programme of Foundation for Polish Science; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; National Aeronautics and Space Administration; National Research Foundation of Korea; Industry Canada; Province of Ontario through the Ministry of Economic Development and Innovation; National Science and Engineering Research Council Canada; Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation; OTKA of Hungary; Science and Technologies Funding Council of the UK; Lyon Institute of Origins (LIO); Alfred P. Sloan Foundation FX The authors gratefully acknowledge the support of the U.S. National Science Foundation for the construction and operation of the LIGO Laboratory, the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of Niedersachsen, Germany for support of the construction and operation of the GEO600 detector, and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Economia y Competitividad, the Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the National Aeronautics and Space Administration, the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the National Science and Engineering Research Council Canada, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, the OTKA of Hungary, the Science and Technologies Funding Council of the UK, the Lyon Institute of Origins (LIO), and the Alfred P. Sloan Foundation. NR 55 TC 46 Z9 46 U1 3 U2 78 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD DEC 2 PY 2014 VL 113 IS 23 AR 231101 DI 10.1103/PhysRevLett.113.231101 PG 10 WC Physics, Multidisciplinary SC Physics GA AU9QK UT WOS:000345929600003 PM 25526109 ER PT J AU Roth, L Retherford, KD Saur, J Strobel, DF Feldman, PD McGrath, MA Nimmo, F AF Roth, Lorenz Retherford, Kurt D. Saur, Joachim Strobel, Darrell F. Feldman, Paul D. McGrath, Melissa A. Nimmo, Francis TI Orbital apocenter is not a sufficient condition for HST/STIS detection of Europa's water vapor aurora SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Europa; Hubble Space Telescope; aurora; water vapor plumes; Jupiter ID GALILEO ULTRAVIOLET SPECTROMETER; EXCITATION CROSS-SECTIONS; JOVIAN MAGNETOSPHERE; SUBSURFACE OCEAN; IOS ATMOSPHERE; ATOMIC OXYGEN; SOUTH-POLE; ENCELADUS; CONSTRAINTS; GANYMEDE AB We report far-ultraviolet observations of Jupiter's moon Europa taken by Space Telescope Imaging Spectrograph (STIS) of the Hubble Space Telescope (HST) in January and February 2014 to test the hypothesis that the discovery of a water vapor aurora in December 2012 by local hydrogen (H) and oxygen (O) emissions with the STIS originated from plume activity possibly correlated with Europa's distance from Jupiter through tidal stress variations. The 2014 observations were scheduled with Europa near the apocenter similar to the orbital position of its previous detection. Tensile stresses on south polar fractures are expected to be highest in this orbital phase, potentially maximizing the probability for plume activity. No local H and O emissions were detected in the new STIS images. In the south polar region where the emission surpluses were observed in 2012, the brightnesses are sufficiently low in the 2014 images to be consistent with any H2O abundance from(0-5)x10(15) cm(-2). Large high-latitude plumes should have been detectable by the STIS, independent of the observing conditions and geometry. Because electron excitation of water vapor remains the only viable explanation for the 2012 detection, the new observations indicate that although the same orbital position of Europa for plume activity may be a necessary condition, it is not a sufficient condition. However, the December 2012 detection of coincident HI Lyman-alpha and OI 1304-angstrom emission surpluses in an similar to 200-km high region well separated above Europa's limb is a firm result and not invalidated by our 2014 STIS observations. C1 [Roth, Lorenz; Retherford, Kurt D.] Southwest Res Inst, San Antonio, TX 78238 USA. [Roth, Lorenz] Royal Inst Technol, Sch Elect Engn, S-10044 Stockholm, Sweden. [Saur, Joachim] Univ Cologne, Inst Geophys & Meteorol, D-50969 Cologne, Germany. [Strobel, Darrell F.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Strobel, Darrell F.; Feldman, Paul D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [McGrath, Melissa A.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35811 USA. [Nimmo, Francis] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. RP Roth, L (reprint author), Southwest Res Inst, San Antonio, TX 78238 USA. EM lorenzr@kth.se OI Roth, Lorenz/0000-0003-0554-4691 FU NASA from the Space Telescope Science Institute [13619]; NASA [NAS5-26555, NNX10AB84G]; Verbundforschung Astronomie und Astrophysik FX The authors thank Wayne Pryor for providing the model results for the IPM Ly-alpha brightness. Support for Hubble Space Telescope Program 13619 was provided by the NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy under NASA Contract NAS5-26555. J.S. acknowledges support by Verbundforschung Astronomie und Astrophysik. D.F.S. was supported in part by NASA Grant NNX10AB84G. NR 65 TC 12 Z9 12 U1 3 U2 10 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 DEC 2 PY 2014 VL 111 IS 48 BP E5123 EP E5132 DI 10.1073/pnas.1416671111 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AU9NN UT WOS:000345920800001 PM 25404343 ER PT J AU Acker, J Soebiyanto, R Kiang, R Kempler, S AF Acker, James Soebiyanto, Radina Kiang, Richard Kempler, Steve TI Use of the NASA Giovanni Data System for Geospatial Public Health Research: Example of Weather-Influenza Connection SO ISPRS INTERNATIONAL JOURNAL OF GEO-INFORMATION LA English DT Article DE remote sensing; climate; weather; public health; disease; environment; atmosphere; ocean; biosphere; precipitation ID VISUALIZATION; TRANSMISSION; TEMPERATURE; CHOLERA; CLIMATE; VIRUS AB The NASA Giovanni data analysis system has been recognized as a useful tool to access and analyze many different types of remote sensing data. The variety of environmental data types has allowed the use of Giovanni for different application areas, such as agriculture, hydrology, and air quality research. The use of Giovanni for researching connections between public health issues and Earth's environment and climate, potentially exacerbated by anthropogenic influence, has been increasingly demonstrated. In this communication, the pertinence of several different data parameters to public health will be described. This communication also provides a case study of the use of remote sensing data from Giovanni in assessing the associations between seasonal influenza and meteorological parameters. In this study, logistic regression was employed with precipitation, temperature and specific humidity as predictors. Specific humidity was found to be associated (p < 0.05) with influenza activity in both temperate and tropical climate. In the two temperate locations studied, specific humidity was negatively correlated with influenza; conversely, in the three tropical locations, specific humidity was positively correlated with influenza. Influenza prediction using the regression models showed good agreement with the observed data (correlation coefficient of 0.5-0.83). C1 [Acker, James] NASA, Adnet Inc, Goddard Space Flight Ctr, Goddard Earth Sci Data & Informat Serv Ctr, Greenbelt, MD 20771 USA. [Soebiyanto, Radina] Univ Space Res Assoc, Goddard Earth Sci Technol & Res GESTAR, Columbia, MD 21046 USA. [Kiang, Richard] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kempler, Steve] NASA, Goddard Space Flight Ctr, Goddard Earth Sci Data & Informat Serv Ctr, Greenbelt, MD 20771 USA. RP Acker, J (reprint author), NASA, Adnet Inc, Goddard Space Flight Ctr, Goddard Earth Sci Data & Informat Serv Ctr, Code 6102, Greenbelt, MD 20771 USA. EM james.g.acker@nasa.gov; radina.p.soebiyanto@nasa.gov; richard.k.kiang@nasa.gov; steven.j.kempler@nasa.gov FU NASA Public Health Applications FX Richard Kiang and Radina P. Soebiyanto are grateful for the support from NASA Public Health Applications in initiating the global influenza feasibility project. NR 29 TC 1 Z9 1 U1 1 U2 7 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2220-9964 J9 ISPRS INT GEO-INF JI ISPRS Int. Geo-Inf. PD DEC PY 2014 VL 3 IS 4 BP 1372 EP 1386 DI 10.3390/ijgi3041372 PG 15 WC Geography, Physical; Remote Sensing SC Physical Geography; Remote Sensing GA CO1SA UT WOS:000358934300012 ER PT J AU Schwartz, SE Charlson, RJ Kahn, R Rodhe, H AF Schwartz, Stephen E. Charlson, Robert J. Kahn, Ralph Rodhe, Henning TI Earth's Climate Sensitivity: Apparent Inconsistencies in Recent Assessments SO EARTHS FUTURE LA English DT Article DE climate sensitivity; forcing; global mean surface temperature ID CMIP5 AB Earth's equilibrium climate sensitivity (ECS) and forcing of Earth's climate system over the industrial era have been re-examined in two new assessments: the Fifth Assessment Report (AR5) of the Intergovernmental Panel on Climate Change (IPCC), and a study by Otto et al. (2013). The ranges of these quantities given in these assessments and also in the Fourth (2007) IPCC Assessment are analyzed here within the framework of a planetary energy balance model, taking into account the observed increase in global mean surface temperature over the instrumental record together with best estimates of the rate of increase of planetary heat content. This analysis shows systematic differences among the several assessments and apparent inconsistencies within individual assessments. Importantly, the likely range of ECS to doubled CO2 given in AR5, 1.5-4.5 K/(3.7 W m(-2)) exceeds the range inferred from the assessed likely range of forcing, 1.2-2.9 K/(3.7 W m(-2)), where 3.7 W m(-2) denotes the forcing for doubled CO2. Such differences underscore the need to identify their causes and reduce the underlying uncertainties. Explanations might involve underestimated negative aerosol forcing, overestimated total forcing, overestimated climate sensitivity, poorly constrained ocean heating, limitations of the energy balance model, or a combination of effects. C1 [Schwartz, Stephen E.] Brookhaven Natl Lab, Biol Environm & Climate Sci Dept, Upton, NY 11973 USA. [Charlson, Robert J.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. [Kahn, Ralph] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rodhe, Henning] Stockholm Univ, Dept Meteorol, S-10691 Stockholm, Sweden. RP Schwartz, SE (reprint author), Brookhaven Natl Lab, Biol Environm & Climate Sci Dept, Upton, NY 11973 USA. EM ses@bnl.gov RI Schwartz, Stephen/C-2729-2008 OI Schwartz, Stephen/0000-0001-6288-310X FU U.S. Department of Energy's Atmospheric System Research Program (Office of Science, OBER) [DE-AC02-98CH10886] FX We thank several referees for valuable comments and Editor Guy Brasseur for encouragement. SES was supported by the U.S. Department of Energy's Atmospheric System Research Program (Office of Science, OBER) under Contract No. DE-AC02-98CH10886. All data and sources are given in Supporting Information. NR 16 TC 5 Z9 5 U1 1 U2 11 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2328-4277 J9 EARTHS FUTURE JI Earth Future PD DEC PY 2014 VL 2 IS 12 BP 601 EP 605 DI 10.1002/2014EF000273 PG 5 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA CN0XG UT WOS:000358137300002 ER PT J AU Saha, R Pohorille, A Chen, IA AF Saha, Ranajay Pohorille, Andrew Chen, Irene A. TI Molecular Crowding and Early Evolution SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES LA English DT Article; Proceedings Paper CT 4th Workshop on Open Questions on the Origin of Life (OQOL) CY JUL 12-13, 2014 CL Int Inst Adv Studies, Kizugawa, JAPAN HO Int Inst Adv Studies DE Crowding; Excluded volume effect; Protocell; Vesicle; Evolution; Fitness landscape; RNA; Neutral network; Evolutionary optimization ID INTRACELLULAR ENVIRONMENT; GLOBULAR-PROTEINS; ESCHERICHIA-COLI; EXCLUDED VOLUME; RNA; STABILITY; RIBOZYME; CONFINEMENT; REACTIVITY; VESICLES AB The environment of protocells might have been crowded with small molecules and functional and non-specific polymers. In addition to altering conformational equilibria, affecting reaction rates and changing the structure and activity of water, crowding might have enhanced the capabilities of protocells for evolutionary innovation through the creation of extended neutral networks in the fitness landscape. C1 [Saha, Ranajay; Chen, Irene A.] Univ Calif Santa Barbara, Dept Chem & Biochem, Santa Barbara, CA 93106 USA. [Pohorille, Andrew] NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. [Chen, Irene A.] Univ Calif Santa Barbara, Program Biomol Sci & Engn, Santa Barbara, CA 93106 USA. RP Chen, IA (reprint author), Univ Calif Santa Barbara, Program Biomol Sci & Engn, Santa Barbara, CA 93106 USA. EM chen@chem.ucsb.edu NR 36 TC 3 Z9 4 U1 1 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-6149 EI 1573-0875 J9 ORIGINS LIFE EVOL B JI Orig. Life Evol. Biosph. PD DEC PY 2014 VL 44 IS 4 BP 319 EP 324 DI 10.1007/s11084-014-9392-3 PG 6 WC Biology SC Life Sciences & Biomedicine - Other Topics GA CG0SZ UT WOS:000352980800011 PM 25585804 ER PT J AU Wilson, MA Wei, CY Pohorille, A AF Wilson, Michael A. Wei, Chenyu Pohorille, Andrew TI Towards Co-Evolution of Membrane Proteins and Metabolism SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES LA English DT Article; Proceedings Paper CT 4th Workshop on Open Questions on the Origin of Life (OQOL) CY JUL 12-13, 2014 CL Int Inst Adv Studies, Kizugawa, JAPAN HO Int Inst Adv Studies DE Membrane proteins; Permeation through membranes; Ion transport; Ion channels ID MOLECULAR-DYNAMICS; INFLUENZA-A; MECHANISM; LIFE; ANTIAMEBIN; TRANSPORT; PEPTAIBOL; CHANNELS; BILAYERS AB Primordial metabolism co-evolved with the earliest membrane peptides to produce more environmentally fit progeny. Here, we map a continuous, evolutionary path that connects nascent biochemistry with simple, membrane-bound oligopeptides, ion channels and, further, membrane proteins capable of energy transduction and utilization of energy for active transport. C1 [Wilson, Michael A.; Wei, Chenyu; Pohorille, Andrew] Univ Calif San Francisco, Dept Pharmaceut Chem, San Francisco, CA USA. [Wilson, Michael A.; Wei, Chenyu; Pohorille, Andrew] NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Pohorille, A (reprint author), NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Andrew.Pohorille@nasa.gov NR 19 TC 3 Z9 4 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-6149 EI 1573-0875 J9 ORIGINS LIFE EVOL B JI Orig. Life Evol. Biosph. PD DEC PY 2014 VL 44 IS 4 BP 357 EP 361 DI 10.1007/s11084-014-9393-2 PG 5 WC Biology SC Life Sciences & Biomedicine - Other Topics GA CG0SZ UT WOS:000352980800018 ER PT J AU Petry, FE Yager, RR AF Petry, Frederick E. Yager, Ronald R. TI Principles for organization of creative groups SO JOURNAL OF AMBIENT INTELLIGENCE AND HUMANIZED COMPUTING LA English DT Article DE Group creativity; Diversity; Generalization ID DECISION-MAKING; DIVERSITY CRITERION; HIERARCHIES; WORDS; LOGIC AB In this paper we first propose an outline for an overall organization of the group creative process. In particular two major components of the process are considered in detail. For group selection, diversity measures including those based on information theory and a species diversity measure are discussed and examples provided. The idea of a diversity space is also introduced to obtain some intuition on the issues relative to population diversity. The actual creative idea generation process is then considered with respect to the social interactions inside the selected creative group. Approaches to modeling the ways in which linguistic persuasion can occur are described. Finally approaches to the generalization of the ideas that evolved using concept hierarchies are presented. C1 [Petry, Frederick E.] Stennis Space Ctr, Naval Res Lab, Hancock, MS 39529 USA. [Yager, Ronald R.] Iona Coll, Inst Machine Intelligence, New Rochelle, NY 10801 USA. RP Yager, RR (reprint author), Iona Coll, Inst Machine Intelligence, New Rochelle, NY 10801 USA. EM yager@panix.com FU Naval Research Laboratory's Base Program [0602435N]; ONR Grant [N000141010121] FX We would like to thank the Naval Research Laboratory's Base Program, Program Element No. 0602435N and ONR Grant Award No. N000141010121 for sponsoring this research. NR 38 TC 0 Z9 0 U1 0 U2 3 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1868-5137 EI 1868-5145 J9 J AMB INTEL HUM COMP JI J. Ambient Intell. Humaniz. Comput. PD DEC PY 2014 VL 5 IS 6 BP 789 EP 797 DI 10.1007/s12652-013-0213-8 PG 9 WC Computer Science, Artificial Intelligence; Computer Science, Information Systems; Telecommunications SC Computer Science; Telecommunications GA CD7AH UT WOS:000351242100002 ER PT J AU Elmore, P Petry, F Yager, R AF Elmore, Paul Petry, Fred Yager, Ronald TI Comparative measures of aggregated uncertainty representations SO JOURNAL OF AMBIENT INTELLIGENCE AND HUMANIZED COMPUTING LA English DT Article DE Information theory; Decision making; Possibility theory; Shannon entropy; Gini index; Renyi entropy; Possibilistic conditioning; Consistency measures ID INFORMATION; ENTROPY AB Uncertainty must be taken into account in all aspects of ambient intelligence and human decisions and activities. We investigate how to utilize both probabilistic and possibilistic sources of information for use in humanized decision-making. In particular we examine aspects of the possibilistic conditioning of probability developed by Yager. To provide bounding of the resulting probability analysis of the cases of completely certain and uncertain probability and possibility distribution are carried out. Additionally the cases of intermediate uncertainty and a general case of possibilities are analyzed. The Zadeh consistency measure is also used to assess these cases. To consider whether the conditioned probability is more informative for decision-making, three measures, Shannon entropy, Gini index and Renyi entropy are used to compare the original probability distributions and the conditioned distribution for the cases described. C1 [Elmore, Paul; Petry, Fred] Naval Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. [Yager, Ronald] Iona Coll, Inst Machine Intelligence, New Rochelle, NY 10801 USA. RP Petry, F (reprint author), Naval Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. EM fpetry@nrlssc.navy.mil FU Naval Research Laboratory's Base Program [0602435 N]; ARO MURI grant [W911NF-09-1-0392] FX We would like to thank the Naval Research Laboratory's Base Program, Program Element No. 0602435 N for sponsoring this research. Ronald Yager has been in part supported by ARO MURI grant Number W911NF-09-1-0392. NR 25 TC 4 Z9 4 U1 1 U2 4 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1868-5137 EI 1868-5145 J9 J AMB INTEL HUM COMP JI J. Ambient Intell. Humaniz. Comput. PD DEC PY 2014 VL 5 IS 6 BP 809 EP 819 DI 10.1007/s12652-014-0228-9 PG 11 WC Computer Science, Artificial Intelligence; Computer Science, Information Systems; Telecommunications SC Computer Science; Telecommunications GA CD7AH UT WOS:000351242100004 ER PT J AU Califf, S Li, X Blum, L Jaynes, A Schiller, Q Zhao, H Malaspina, D Hartinger, M Wolf, RA Rowland, DE Wygant, JR Bonnell, JW AF Califf, S. Li, X. Blum, L. Jaynes, A. Schiller, Q. Zhao, H. Malaspina, D. Hartinger, M. Wolf, R. A. Rowland, D. E. Wygant, J. R. Bonnell, J. W. TI THEMIS measurements of quasi-static electric fields in the inner magnetosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MAGNETIC STORM; IONOSPHERE; CONVECTION; MODEL; MIDLATITUDE; CLUSTER; SECTOR; DRIFT AB We use 4 years of Time History of Events and Macroscale Interactions during Substorms (THEMIS) double-probe measurements to offer, for the first time, a complete picture of the dawn-dusk electric field covering all local times and radial distances in the inner magnetosphere based on in situ equatorial observations. This study is motivated by the results from the CRRES mission, which revealed a local maximum in the electric field developing near Earth during storm times, rather than the expected enhancement at higher L shells that is shielded near Earth as suggested by the Volland-Stern model. The CRRES observations were limited to the duskside, while THEMIS provides complete local time coverage. We show strong agreement with the CRRES results on the duskside, with a local maximum near L = 4 for moderate levels of geomagnetic activity and evidence of strong electric fields inside L = 3 during the most active times. The extensive data set from THEMIS also confirms the day/night asymmetry on the duskside, where the enhancement is closest to Earth in the dusk-midnight sector, and is farther away closer to noon. A similar, but smaller in magnitude, local maximum is observed on the dawnside near L = 4. The noon sector shows the smallest average electric fields, and for more active times, the enhancement develops near L = 7 rather than L = 4. We also investigate the impact of the uncertain boom-shorting factor on the results and show that while the absolute magnitude of the electric field may be underestimated, the trends with geomagnetic activity remain intact. C1 [Califf, S.; Li, X.; Blum, L.; Jaynes, A.; Schiller, Q.; Zhao, H.; Malaspina, D.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Hartinger, M.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Wolf, R. A.] Rice Univ, Dept Phys & Astron, Houston, TX USA. [Rowland, D. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wygant, J. R.] Univ Minnesota, Dept Phys & Astron, Minneapolis, MN 55455 USA. [Bonnell, J. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Califf, S (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA. EM califf@colorado.edu RI Hartinger, Michael/H-9088-2012; OI Hartinger, Michael/0000-0002-2643-2202; Blum, Lauren/0000-0002-4797-5476 FU NASA [NNX10AL04G] FX THEMIS data are publicly available at http://themis.ssl.berkeley.edu/, and the Kp index can be found at http://omni-web.gsfc.nasa.gov. Work at Rice was supported by NASA grant NNX10AL04G. NR 31 TC 9 Z9 9 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC PY 2014 VL 119 IS 12 DI 10.1002/2014JA020360 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA8IG UT WOS:000349161100042 ER PT J AU Clarke, TE Higgins, CA Skarda, J Imai, K Imai, M Reyes, F Thieman, J Jaeger, T Schmitt, H Dalal, NP Dowell, J Ellingson, SW Hicks, B Schinzel, F Taylor, GB AF Clarke, T. E. Higgins, C. A. Skarda, Jinhie Imai, Kazumasa Imai, Masafumi Reyes, Francisco Thieman, Jim Jaeger, Ted Schmitt, Henrique Dalal, Nagini Paravastu Dowell, Jayce Ellingson, S. W. Hicks, Brian Schinzel, Frank Taylor, G. B. TI Probing Jovian decametric emission with the long wavelength array station 1 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID COMPLETE POLARIZATION STATE; ELECTRON-CYCLOTRON MASER; IO-JUPITER INTERACTION; RADIO EMISSIONS; DYNAMIC SPECTRA; S-BURSTS; KILOMETRIC RADIATION; MILLISECOND BURSTS; MODULATION LANES; ARCS AB New observations of Jupiter's decametric radio emissions have been made with the Long Wavelength Array Station 1 (LWA1), which is capable of making high-quality observations as low as 11 MHz. Full Stokes parameters were determined for bandwidths of 16 MHz. Here we present the first LWA1 results for the study of six Io-related events at temporal resolutions as fine as 0.25 ms. LWA1 data show excellent spectral detail in Jovian DAM such as simultaneous left-hand circular (LHC) and right-hand circular (RHC) polarized Io-related arcs and source envelopes, modulation lane features, S-burst structures, narrow band N events, and interactions between S bursts and N events. The sensitivity of the LWA1 combined with the low-radio-frequency interference environment allow us to trace the start of the LHC Io-C source region to much earlier CML III than typically found in the literature. We find that the Io-C starts as early as CML III = 230 degrees at frequencies near 11 MHz. This early start of the Io-C emission may be valuable for refining models of the emission mechanism. We also detect modulation lane structures that appear continuous across LHC and RHC emissions, suggesting that both polarizations may originate from the same hemisphere of Jupiter. We present a study of rare S bursts detected during an Io-D event and show that drift rates are consistent with those from other Io-related sources. Finally, S-N burst events are seen in high spectral and temporal resolution and our data strongly support the cospatial origins of these events. C1 [Clarke, T. E.; Schmitt, Henrique; Hicks, Brian] Naval Res Lab, Washington, DC 20375 USA. [Higgins, C. A.] Middle Tennessee State Univ, Dept Phys & Astron, Murfreesboro, TN 37130 USA. [Skarda, Jinhie] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA. [Imai, Kazumasa] Kochi Natl Coll Technol, Dept Elect Engn & Informat Sci, Kochi, Japan. [Imai, Masafumi] Kyoto Univ, Dept Geophys, Kyoto, Japan. [Reyes, Francisco] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Thieman, Jim] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Jaeger, Ted] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Dalal, Nagini Paravastu] Naval Res Lab, ASEEE, Washington, DC 20375 USA. [Dowell, Jayce; Schinzel, Frank; Taylor, G. B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Ellingson, S. W.] Virginia Polytech Inst & State Univ, Bradley Dept Elect & Comp Engn, Blacksburg, VA 24061 USA. RP Clarke, TE (reprint author), Naval Res Lab, Washington, DC 20375 USA. EM tracy.clarke.ca@nrl.navy.mil RI Imai, Masafumi/S-8736-2016 OI Imai, Masafumi/0000-0002-2814-4036 FU 6.1 Base funding; Office of Naval Research [N00014-07-C-0147]; National Science Foundation of the University Radio Observatories program [AST-1139963, AST-1139974]; Tennessee Space Grant Consortium; JSPS KAK-ENHI [25400480]; Science and Engineering Apprenticeship Program (SEAP) at the Naval Research Laboratory; NSF [AST-1212162] FX We thank the referees for a careful reading of the manuscript and helpful comments. We also wish to thank the staff of the Long Wavelength Array. Basic research in radio astronomy at the Naval Research Laboratory is supported by 6.1 Base funding. Construction of LWA1 was supported by the Office of Naval Research under contract N00014-07-C-0147. Support for operations and continuing development of LWA1 is provided by the National Science Foundation under grants AST-1139963 and AST-1139974 of the University Radio Observatories program. C.A.H. acknowledges support from the Tennessee Space Grant Consortium. This research has been supported in part by JSPS KAK-ENHI grant 25400480. J.S. (a student at Montgomery Blair High School) was supported by the Science and Engineering Apprenticeship Program (SEAP) at the Naval Research Laboratory. G.B.T. acknowledges partial support for this work from NSF grant AST-1212162. Data used for this publication are available through request to the authors. NR 62 TC 1 Z9 1 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC PY 2014 VL 119 IS 12 DI 10.1002/2014JA020289 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA8IG UT WOS:000349161100015 ER PT J AU Liu, YH Birn, J Daughton, W Hesse, M Schindler, K AF Liu, Yi-Hsin Birn, Joachim Daughton, William Hesse, Michael Schindler, Karl TI Onset of reconnection in the near magnetotail: PIC simulations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID THIN CURRENT SHEETS; COLLISIONLESS MAGNETIC RECONNECTION; ION KINK INSTABILITY; EARTH PLASMA SHEET; NEUTRAL SHEETS; LINEAR-THEORY; SMALL-SCALE; STABILITY; CLUSTER; TAIL AB Using 2.5-dimensional particle-in-cell (PIC) simulations of magnetotail dynamics, we investigate the onset of reconnection in two-dimensional tail configurations with finite B-z. Reconnection onset is preceded by a driven phase, during which magnetic flux is added to the tail at the high-latitude boundaries, followed by a relaxation phase, during which the configuration continues to respond to the driving. We found a clear distinction between stable and unstable cases, dependent on deformation amplitude and ion/electron mass ratio. The threshold appears consistent with electron tearing. The evolution prior to onset, as well as the evolution of stable cases, are largely independent of the mass ratio, governed by integral flux tube entropy conservation as imposed in MHD. This suggests that ballooning instability in the tail should not be expected prior to the onset of tearing and reconnection. The onset time and other onset properties depend on the mass ratio, consistent with expectations for electron tearing. At onset, we found electron anisotropies T-perpendicular to/T-parallel to = 1.1-1.3, raising growth rates and wave numbers. Our simulations have provided a quantitative onset criterion that is easily evaluated in MHD simulations, provided the spatial resolution is sufficient. The evolution prior to onset and after the formation of a neutral line does not depend on the electron physics, which should permit an approximation by MHD simulations with appropriate dissipation terms. C1 [Liu, Yi-Hsin; Hesse, Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Birn, Joachim; Daughton, William] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Birn, Joachim] Space Sci Inst, Boulder, CO USA. [Schindler, Karl] Ruhr Univ Bochum, Inst Theoret Phys, Bochum, Germany. RP Birn, J (reprint author), Los Alamos Natl Lab, Los Alamos, NM 87545 USA. EM jbirn@spacescience.org RI Daughton, William/L-9661-2013; NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 FU NSF's GEM; NASA; NSF [OCI 07-25070]; state of Illinois FX Part of this work was performed at Los Alamos under the auspices of the U.S. Department of Energy, supported by the NSF's GEM and by NASA's MMS/SMART Theory and Modeling, SR&T, and Heliophysics Theory Programs. The simulations were performed using resources from the Los Alamos Institutional Computing Program, with further resources from the Blue Waters sustained-petascale computing project, which is supported by the NSF (OCI 07-25070) and the state of Illinois. NR 73 TC 10 Z9 10 U1 2 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC PY 2014 VL 119 IS 12 DI 10.1002/2014JA020492 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA8IG UT WOS:000349161100032 ER PT J AU Murphy, KR Mann, IR Rae, IJ Walsh, AP Frey, HU AF Murphy, Kyle R. Mann, Ian R. Rae, I. Jonathan Walsh, Andrew P. Frey, Harald U. TI Inner magnetospheric onset preceding reconnection and tail dynamics during substorms: Can substorms initiate in two different regions? SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID EARTHS MAGNETOTAIL; AURORAL SUBSTORMS; PRESSURE-GRADIENT; PLASMA SHEET; INSTABILITY; FLOW; MAGNETOMETER; BOUNDARY; MODEL; ARRAY AB We present a detailed ground-based and in situ examination of two substorms on 9 April 2011 providing one of the most detailed observations of a series of activations to date. Using auroral observations we demonstrate that the initial signature of substorm onset is a localized brightening on closed field lines. In both cases auroral onset precedes any geosynchronous indications of substorm onset. Despite excellent in situ coverage of the near-midnight plasma sheet there is no evidence of tail flows or topological changes which might indicate the initiation of reconnection and related disturbances prior to auroral onset. Similarly, no auroral streamers are observed prior to either onset. For the second substorm, following auroral onset and dipolarization of the geosynchronous field there is evidence of a rapid thinning of the plasma sheet followed by a secondary auroral activation and dipolarization of the magnetotail outside of geosynchronous orbit. This morphological change suggests that near-Earth neutral line reconnection is eventually triggered in the tail, but only following the earlier auroral onset. These observations demonstrate that expansion phase onset is not always initiated by reconnection in the tail. Finally, our observations suggest that activations at the near-Earth neutral line, or related to plasma instabilities and near-Earth onset, can develop independently during expansion phase onset. In this paradigm, free energy stored during the growth phase can be stored in the stretched tail and the inner magnetosphere where the dipole field begins to stretch. During expansion phase onset either region could become unstable, independent of the other, leading to substorm initiation and onset. C1 [Murphy, Kyle R.; Mann, Ian R.] Univ Alberta, Dept Phys, Edmonton, AB, Canada. [Murphy, Kyle R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rae, I. Jonathan] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Walsh, Andrew P.] ESAC, European Space Agcy, Sci & Robot Explorat Directorate, Madrid, Spain. [Frey, Harald U.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Murphy, KR (reprint author), Univ Alberta, Dept Phys, Edmonton, AB, Canada. EM kyle.r.murphy@nasa.gov OI Walsh, Andrew/0000-0002-1682-1212; Frey, Harald/0000-0001-8955-3282 FU Alberta Innovates Graduate Scholarship; Natural Science and Engineering Research Council of Canada Postdoctoral Fellowship; NASA [NAS5-02099]; NSF [AGS-1004736, AGS-1004814]; CSA [9F007-046101]; Canadian Space Agency FX K.R.M. is funded by an Alberta Innovates Graduate Scholarship and Natural Science and Engineering Research Council of Canada Postdoctoral Fellowship. We acknowledge NASA contract NAS5-02099 and V. Angelopoulos for the use of data from the THEMIS Mission, and NSF support of GIMNAST through grant AGS-1004736. Specifically, we thank S. Mende and E. Donovan for the use of the THEMIS ASI data. Deployment and data retrieval of the THEMIS ASIs was partly supported by CSA contract 9F007-046101 to the University of Calgary. We thank S. Mende and C.T. Russell for the use of the THEMIS ground-based magnetometer data and NSF for support through grant AGS-1004814. Operational support for NORSTAR is provided by the CSA and University of Calgary. We acknowledge Brian Jackel and the NORSTAR team for providing the MSP data used in this study. We acknowledge D.K. Milling and the rest of the CARISMA team for data use. CARISMA is operated by the University of Alberta, funded by the CSA. Funding for operation of the NORSTAR riometers is provided by the Canadian Space Agency. The NRCAN riometer operation and data processing were supported by Natural Resources Canada. The authors would like to thank D. Turner and L. Kepko for helpful discussions. NR 53 TC 4 Z9 4 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC PY 2014 VL 119 IS 12 DI 10.1002/2014JA019795 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA8IG UT WOS:000349161100026 ER PT J AU Omidi, N Zhang, H Chu, C Sibeck, D Turner, D AF Omidi, N. Zhang, H. Chu, C. Sibeck, D. Turner, D. TI Parametric dependencies of spontaneous hot flow anomalies SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID EARTHS BOW SHOCK; QUASI-PARALLEL SHOCKS; UPSTREAM SOLAR-WIND; MAGNETIC-FIELD; 2-DIMENSIONAL SIMULATIONS; DIAMAGNETIC CAVITIES; FORESHOCK CAVITONS; HYBRID SIMULATION; RE-FORMATION; ULF WAVES AB Parametric dependencies of spontaneous hot flow anomalies at the quasi-parallel bow shock are investigated using global hybrid (kinetic ions and fluid electron) simulations with a variety of solar wind Mach numbers and directions of the interplanetary magnetic field (IMF). Simulations with solar wind Alfvenic Mach number of 3 and small IMF cone angles (with the flow velocity) show sporadic formation of spontaneous hot flow anomalies (SHFAs). Increasing the Mach number shows the formation of copious number of SHFAs whose properties are examined in this study. It is shown that the duration of SHFAs does not show much variation with Mach number indicating that their size generally increases with Mach number. Additionally, the level of solar wind deceleration associated with SHFAs increases with Mach number as does the core ion temperature. It is also found that the edges of SHFAs are associated with jumps in magnetic field that increase with shock Mach number. The results also show that the rate of SHFA formation increases with increasing Mach number. Simulations with IMF cone angle of 90 degrees show that SHFAs form at the quasi-parallel bow shock provided the shock Alfven Mach number is similar to>3. This shows that SHFAs may form at all cone angles. C1 [Omidi, N.] Solana Sci Inc, Solana Beach, CA 92075 USA. [Zhang, H.; Chu, C.] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. [Sibeck, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Turner, D.] Univ Calif Los Angeles, IGPP, Los Angeles, CA USA. RP Omidi, N (reprint author), Solana Sci Inc, Solana Beach, CA 92075 USA. EM omidi@solanasci.com OI Chu, Christina/0000-0002-4468-7460 FU NSF [AGS-1007449, AGS-0963111, AGS-1303689]; NASA's THEMIS mission [NAS5-02099]; NASA [NNX14AC16G] FX Work for this project was supported by NSF grants AGS-1007449, AGS-0963111, and AGS-1303689. D.L. Turner is thankful for funding support from NASA's THEMIS mission (contract NAS5-02099) and a NASA grant (NNX14AC16G). Request for simulation data used in this study may be made to N. Omidi at omidi@solanasci.com. NR 53 TC 3 Z9 3 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC PY 2014 VL 119 IS 12 DI 10.1002/2014JA020382 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA8IG UT WOS:000349161100036 ER PT J AU Samsonov, AA Sibeck, DG Walsh, BM Zolotova, NV AF Samsonov, A. A. Sibeck, D. G. Walsh, B. M. Zolotova, N. V. TI Sudden impulse observations in the dayside magnetosphere by THEMIS SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID INTERPLANETARY MAGNETIC-FIELD; WIND DYNAMIC PRESSURE; NUMERICAL-SIMULATION; ULF WAVES; COMMENCEMENT; MAGNETOPAUSE; TIME; EXCITATION; VORTICES; EVENTS AB We present a study of the magnetospheric response to interplanetary shocks. We show eight events with simultaneous observations of sudden impulses in the dayside magnetosphere and interplanetary shocks in the solar wind. The spacecraft measurements in the equatorial plane, even those very close to the Earth, can be interpreted in terms of the vortices predicted by previous studies employing global MHD models. In fact, these vortices are velocity oscillations with the properties of Alfven waves. The amplitude and frequency of the oscillations depend on radial distance from the Earth. The amplitude of the velocity perturbations decreases with increase of the density and magnetic field magnitude, but the velocity amplitude shows no dependence on magnitude of the solar wind dynamic pressure change attending the interplanetary shocks. The oscillations are observed both in the outer magnetosphere and the plasmasphere, but they become less sinusoidal near the plasmapause, i.e., in the region with a large-density gradient. The amplitude of the magnetic field enhancement in the sudden impulses also depends on the radial distance. The MHD simulations successfully predict the amplitudes of magnetic field increase and the first cycles of the velocity oscillations in these events. C1 [Samsonov, A. A.; Zolotova, N. V.] St Petersburg State Univ, St Petersburg 199034, Russia. [Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Walsh, B. M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Samsonov, AA (reprint author), St Petersburg State Univ, St Petersburg 199034, Russia. EM andre.samsonov@gmail.com RI Zolotova, Nadezhda/I-7061-2012; Samsonov, Andrey/I-7057-2012 OI Zolotova, Nadezhda/0000-0002-0019-2415; Samsonov, Andrey/0000-0001-8243-1151 FU THEMIS Project funds; RFFI [14-05-00399]; NASA [NAS5-02099] FX This work was partly supported by THEMIS Project funds and by RFFI grant 14-05-00399. Simulation results have been provided by the Community Coordinated Modeling Center (http://ccmc.gsfc.nasa.gov) at Goddard Space Flight Center. We have used results of the runs "Andrey_Samsonov_120712_1," "Andrey_Samsonov_120712_3," "Andrey_Samsonov_111912_1," "Andrey_Samsonov_120512_1," and "Andrey_Samsonov_060513_2". We acknowledge NASA contract NAS5-02099 and V. Angelopoulos for the use of data from the THEMIS mission, specifically J.W. Bonnell and F.S. Mozer for the use of EFI data; C.W. Carlson and J.P. McFadden for the use of ESA data; and K.H. Glassmeier, U. Auster, and W. Baumjohann for the use of FGM data. THEMIS data are available from the Coordinated Data Analysis Web (CDAWeb) and THEMIS website (http://themis.igpp.ucla.edu). NR 52 TC 3 Z9 3 U1 0 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC PY 2014 VL 119 IS 12 DI 10.1002/2014JA020012 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CA8IG UT WOS:000349161100013 ER PT J AU Chien, S Morris, R AF Chien, Steve Morris, Robert TI Space Applications of Artificial Intelligence SO AI MAGAZINE LA English DT Editorial Material ID MARS AB We are pleased to introduce the space application issue articles in this issue of AI Magazine. The exploration of space is a testament to human curiosity and the desire to understand the universe that we inhabit. As many space agencies around the world design and deploy missions, it is apparent that there is a need for intelligent, exploring systems that can make decisions on their own in remote, potentially hostile environments. At the same time, the monetary cost of operating missions, combined with the growing complexity of the instruments and vehicles being deployed, make it apparent that substantial improvements can be made by the judicious use of automation in mission operations. C1 [Chien, Steve] CALTECH, Artificial Intelligence Grp, Pasadena, CA 91125 USA. [Chien, Steve] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Morris, Robert] NASA, Ames Res Center, Intelligent Syst Div, Explorat Technol Directorate, Mountain View, CA USA. RP Chien, S (reprint author), CALTECH, Artificial Intelligence Grp, Pasadena, CA 91125 USA. NR 27 TC 0 Z9 0 U1 1 U2 8 PU AMER ASSOC ARTIFICIAL INTELL PI MENLO PK PA 445 BURGESS DRIVE, MENLO PK, CA 94025-3496 USA SN 0738-4602 J9 AI MAG JI AI Mag. PD WIN PY 2014 VL 35 IS 4 BP 3 EP 6 PG 4 WC Computer Science, Artificial Intelligence SC Computer Science GA CA9XD UT WOS:000349277200001 ER PT J AU Johnston, MD Tran, D Arroyo, B Sorensen, S Tay, P Carruth, B Coffman, A Wallace, M AF Johnston, Mark D. Daniel Tran Arroyo, Belinda Sorensen, Sugi Tay, Peter Carruth, Butch Coffman, Adam Wallace, Mike TI Automated Scheduling for NASA's Deep Space Network SO AI MAGAZINE LA English DT Article AB This article describes the Deep Space Network (DSN) scheduling engine (DSE) component of a new scheduling system being deployed for NASA's Deep Space Network. The DSE provides core automation functionality for scheduling the network, including the interpretation of scheduling requirements expressed by users, their elaboration into tracking passes, and the resolution of conflicts and constraint violations. The DSE incorporates both systematic search- and repair-based algorithms, used for different phases and purposes in the overall system. It has been integrated with a web application that provides DSE functionality to all DSN users through a standard web browser, as part of a peer-to-peer schedule negotiation process for the entire network. The system has been deployed operationally and is in routine use, and is in the process of being extended to support long-range planning and forecasting and near real-time scheduling. C1 [Johnston, Mark D.] CALTECH, Jet Prop Lab, Planning & Execut Syst Sect, Pasadena, CA 91125 USA. [Arroyo, Belinda] NASA, Deep Space Network, Washington, DC USA. [Sorensen, Sugi; Tay, Peter] Jet Prop Lab, Flintridge, CA USA. [Sorensen, Sugi] JPL, Flintridge, CA USA. [Sorensen, Sugi] Adv Concepts Engn Grp, Albuquerque, NM USA. [Carruth, Butch] Innovat Prod Solut Inc, Charleston, SC USA. [Carruth, Butch] Deep Space Network, Jet Prop Lab, Paddys River, ACT, Australia. [Coffman, Adam] Innovat Prod Solut, Kissimmee, FL USA. IPS Inc, San Diego, CA USA. RP Johnston, MD (reprint author), JPL Deep Space Network, Serv Management Dev Team, Flintridge, CA 91011 USA. NR 18 TC 0 Z9 0 U1 0 U2 2 PU AMER ASSOC ARTIFICIAL INTELL PI MENLO PK PA 445 BURGESS DRIVE, MENLO PK, CA 94025-3496 USA SN 0738-4602 J9 AI MAG JI AI Mag. PD WIN PY 2014 VL 35 IS 4 BP 7 EP 25 PG 19 WC Computer Science, Artificial Intelligence SC Computer Science GA CA9XD UT WOS:000349277200002 ER PT J AU Knight, R Chouinard, C Jones, G Tran, D AF Knight, Russell Chouinard, Caroline Jones, Grailing Daniel Tran TI Leveraging Multiple Artificial Intelligence Techniques to Improve the Responsiveness in Operations Planning: ASPEN for Orbital Express SO AI MAGAZINE LA English DT Article AB The challenging timeline for DARPA's Orbital Express mission demanded a flexible, responsive, and (above all) safe approach to mission planning. Mission planning for space is challenging because of the mixture of goals and constraints. Every space mission tries to squeeze all of the capacity possible out of the spacecraft. For Orbital Express, this means performing as many experiments as possible, while still keeping the spacecraft safe. Keeping the spacecraft safe can be very challenging because we need to maintain the correct thermal environment (or batteries might freeze), we need to avoid pointing cameras and sensitive sensors at the sun, we need to keep the spacecraft batteries charged, and we need to keep the two spacecraft from colliding ... made more difficult as only one of the spacecraft had thrusters. Because the mission was a technology demonstration, pertinent planning information was learned during actual mission execution. For example, we didn't know for certain how long it would take to transfer propellant from one spacecraft to the other, although this was a primary mission goal. The only way to find out was to perform the task and monitor how long it actually took. This information led to amendments to procedures, which led to changes in the mission plan. In general, we used the ASPEN planner scheduler to generate and validate the mission plans. ASPEN is a planning system that allows us to enter all of the spacecraft constraints, the resources, the communications windows, and our objectives. ASPEN then could automatically plan our day. We enhanced ASPEN to enable it to reason about uncertainty. We also developed a model generator that would read the text of a procedure and translate it into an ASPEN model. Note that a model is the input to ASPEN that describes constraints, resources, and activities. These technologies had a significant impact on the success of the Orbital Express mission. Finally, we formulated a technique for converting procedural information to declarative information by transforming procedures into models of hierarchical task networks (HTNs). The impact of this effort on the mission was a significant reduction in (1) the execution time of the mission, (2) the daily staff required to produce plans, and (3) planning errors. Not a single misconfigured command was sent during operations. C1 [Knight, Russell] Automated Scheduing & Planning Environm ASPEN Pla, Aspen, CO USA. [Knight, Russell] Continuous Act Scheduling Planning Execut & Repla, Pasadena, CA USA. [Knight, Russell] Mission Data Syst, Pittsburgh, PA 15213 USA. [Chouinard, Caroline] Red Canyon Software, Denver, CO 80203 USA. [Chouinard, Caroline] Jet Prop Lab, Sequence Virtual Team Cassini, Pasadena, CA 91109 USA. RP Knight, R (reprint author), Automated Scheduing & Planning Environm ASPEN Pla, Aspen, CO USA. FU Defense Advanced Research Projects Agency FX Portions of this work were performed by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Portions of this work were performed by the Jet Propulsion Laboratory, California Institute of Technology, and were sponsored by the Defense Advanced Research Projects Agency. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise does not constitute or imply its endorsement by the United States government, or the Defense Advanced Research Projects Agency, or the Jet Propulsion Laboratory, California Institute of Technology. NR 11 TC 0 Z9 0 U1 2 U2 4 PU AMER ASSOC ARTIFICIAL INTELL PI MENLO PK PA 445 BURGESS DRIVE, MENLO PK, CA 94025-3496 USA SN 0738-4602 J9 AI MAG JI AI Mag. PD WIN PY 2014 VL 35 IS 4 BP 26 EP 36 PG 11 WC Computer Science, Artificial Intelligence SC Computer Science GA CA9XD UT WOS:000349277200003 ER PT J AU Wettergreen, D Foil, G Furlong, M Thompson, DR AF Wettergreen, David Foil, Greydon Furlong, Michael Thompson, David R. TI Science Autonomy for Rover Subsurface Exploration of the Atacama Desert SO AI MAGAZINE LA English DT Article ID EO-1; MISSION; ONBOARD AB As planetary rovers expand their capabilities, traveling longer distances, deploying complex tools, and collecting voluminous scientific data, the requirements for intelligent guidance and control also grow. This, coupled with limited bandwidth and latencies, motivates on-board autonomy that ensures the quality of the science data return. Increasing quality of the data requires better sample selection, data validation, and data reduction. Robotic studies in Mars-like desert terrain have advanced autonomy for long-distance exploration and seeded technologies for planetary rover missions. In these field experiments the remote science team uses a novel control strategy that intersperses preplanned activities with autonomous decision making. The robot performs automatic data collection, interpretation, and response at multiple spatial scales. Specific capabilities include instrument calibration, visual targeting of selected features, an on-board database of collected data, and a long-range path planner that guides the robot using analysis of current surface and prior satellite data. Field experiments in the Atacama Desert of Chile over the past decade demonstrate these capabilities and illustrate current challenges and future directions. C1 [Wettergreen, David; Foil, Greydon] Carnegie Mellon Univ, Inst Robot, Pittsburgh, PA 15213 USA. [Thompson, David R.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Wettergreen, D (reprint author), Carnegie Mellon Univ, Inst Robot, Pittsburgh, PA 15213 USA. FU NASA Astrobiology and Technology for Exploring Planets (ASTEP) program [NNX11AJ87G] FX A portion of this research was performed at the Jet Propulsion Laboratory, California Institute of Technology. The Landsat map in Figure 3 is courtesy Ken Tanaka (USGS). The geologic classification comes from Jeffery Moersch (UTenn). Copyright 2013. This research is funded by the NASA Astrobiology and Technology for Exploring Planets (ASTEP) program under grant NNX11AJ87G. NR 17 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC ARTIFICIAL INTELL PI MENLO PK PA 445 BURGESS DRIVE, MENLO PK, CA 94025-3496 USA SN 0738-4602 J9 AI MAG JI AI Mag. PD WIN PY 2014 VL 35 IS 4 BP 47 EP 60 PG 14 WC Computer Science, Artificial Intelligence SC Computer Science GA CA9XD UT WOS:000349277200005 ER PT J AU Yliniemi, L Agogino, AK Tumer, K AF Yliniemi, Logan Agogino, Adrian K. Tumer, Kagan TI Multirobot Coordination for Space Exploration SO AI MAGAZINE LA English DT Article ID SYSTEMS AB Teams of artificially intelligent planetary rovers have tremendous potential for space exploration, allowing for reduced cost, increased flexibility, and increased reliability. However, having these multiple autonomous devices acting simultaneously leads to a problem of coordination: to achieve the best results, they should work together. This is not a simple task. Due to the large distances and harsh environments, a rover must be able to perform a wide variety of tasks with a wide variety of potential teammates in uncertain and unsafe environments. Directly coding all the necessary rules that can reliably handle all of this coordination and uncertainty is problematic. Instead, this article examines tackling this problem through the use of coordinated reinforcement learning: rather than being programmed what to do, the rovers iteratively learn through trial and error to take take actions that lead to high overall system return. To allow for coordination, yet allow each agent to learn and act independently, we employ state-of-the-art reward-shaping techniques. This article uses visualization techniques to break down complex performance indicators into an accessible form and identifies key future research directions. C1 [Yliniemi, Logan; Tumer, Kagan] Oregon State Univ, Corvallis, OR 97331 USA. [Agogino, Adrian K.] NASA, Robust Software Engn Grp, Intelligent Syst Div, Kennedy Space Ctr, FL 32899 USA. RP Yliniemi, L (reprint author), Oregon State Univ, Corvallis, OR 97331 USA. NR 28 TC 1 Z9 1 U1 0 U2 1 PU AMER ASSOC ARTIFICIAL INTELL PI MENLO PK PA 445 BURGESS DRIVE, MENLO PK, CA 94025-3496 USA SN 0738-4602 J9 AI MAG JI AI Mag. PD WIN PY 2014 VL 35 IS 4 BP 61 EP 74 PG 14 WC Computer Science, Artificial Intelligence SC Computer Science GA CA9XD UT WOS:000349277200006 ER PT J AU Law, KS Stohl, A Quinn, PK Brock, CA Burkhart, JF Paris, JD Ancellet, G Singh, HB Roiger, A Schlager, H Dibb, J Jacob, DJ Arnold, SR Pelon, J Thomas, JL AF Law, Katharine S. Stohl, Andreas Quinn, Patricia K. Brock, Charles A. Burkhart, John F. Paris, Jean-Daniel Ancellet, Gerard Singh, Hanwant B. Roiger, Anke Schlager, Hans Dibb, Jack Jacob, Daniel J. Arnold, Steve R. Pelon, Jacques Thomas, Jennie L. TI ARCTIC AIR POLLUTION New Insights from POLARCAT-IPY SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID HIGH NORTHERN LATITUDES; STRATOSPHERE-TROPOSPHERE EXCHANGE; FOREST-FIRE EMISSIONS; LONG-TERM TRENDS; BLACK CARBON; AIRBORNE MEASUREMENTS; OPTICAL-PROPERTIES; SATELLITE-OBSERVATIONS; ATMOSPHERIC CHEMISTRY; SOURCE IDENTIFICATION AB Given the rapid nature of climate change occurring in the Arctic and the difficulty climate models have in quantitatively reproducing observed changes such as sea ice loss, it is important to improve understanding of the processes leading to climate change in this region, including the role of short-lived climate pollutants such as aerosols and ozone. It has long been known that pollution produced from emissions at midlatitudes can be transported to the Arctic, resulting in a winter/spring aerosol maximum known as Arctic haze. How-ever, many uncertainties remain about the composition and origin of Arctic pollution throughout the troposphere; for example, many climate-chemistry models fail to reproduce the strong seasonality of aerosol abundance observed at Arctic surface sites, the origin and deposition mechanisms of black carbon (soot) particles that darken the snow and ice surface in the Arctic is poorly understood, and chemical processes controlling the abundance of tropospheric ozone are not well quantified. The International Polar Year (IPY) Polar Study using Aircraft, Remote Sensing, Surface Measurements and Models, Climate, Chemistry, Aerosols and Transport (POLARCAT) core project had the goal to improve understanding about the origins of pollutants transported to the Arctic; to detail the chemical composition, optical properties, and climate forcing potential of Arctic aerosols; to evaluate the processes governing tropospheric ozone; and to quantify the role of boreal forest fires. This article provides a review of the many results now available based on analysis of data collected during the POLARCAT aircraft-, ship-, and ground-based field campaigns in spring and summer 2008. Major findings are highlighted and areas requiring further investigation are discussed. C1 [Law, Katharine S.; Ancellet, Gerard; Pelon, Jacques; Thomas, Jennie L.] Univ Paris 06, Sorbonne Univ, F-75252 Paris, France. [Law, Katharine S.; Ancellet, Gerard; Pelon, Jacques; Thomas, Jennie L.] Univ Versailles St Quentin, Paris, France. [Law, Katharine S.; Ancellet, Gerard; Pelon, Jacques; Thomas, Jennie L.] CNRS INSU, Paris, France. [Law, Katharine S.; Ancellet, Gerard; Pelon, Jacques; Thomas, Jennie L.] LATMOS IPSL, UMR 8190, Paris, France. [Stohl, Andreas] NILU Norwegian Inst Air Res, Kjeller, Norway. [Quinn, Patricia K.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. [Brock, Charles A.] NOAA, Earth Syst Res Lab, Boulder, CO USA. [Burkhart, John F.] Univ Oslo, Oslo, Norway. [Paris, Jean-Daniel] CNRS CEA UVSQ, IPSL, Lab Sci Climat & Environm, Gif Sur Yvette, France. [Singh, Hanwant B.] NASA, Ames Res Ctr, Mountain View, CA USA. [Roiger, Anke; Schlager, Hans] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Phys Atmosphare, Oberpfaffenhofen, Germany. [Dibb, Jack] Univ New Hampshire, Durham, NH 03824 USA. [Jacob, Daniel J.] Harvard Univ, Boston, MA 02115 USA. [Arnold, Steve R.] Univ Leeds, Sch Earth & Environm, Inst Climate & Atmospher Sci, Leeds, W Yorkshire, England. RP Law, KS (reprint author), Univ Paris 06, LATMOS IPSL, 4 Pl Jussieu, F-75252 Paris, France. EM kathy.law@latmos.ipsl.fr RI Stohl, Andreas/A-7535-2008; Burkhart, John/B-7095-2008; Quinn, Patricia/R-1493-2016; Manager, CSD Publications/B-2789-2015 OI Stohl, Andreas/0000-0002-2524-5755; Arnold, Steve/0000-0002-4881-5685; Burkhart, John/0000-0002-5587-1693; Quinn, Patricia/0000-0003-0337-4895; FU French Agence National de Recherche (ANR); CNRS-LEFE; CNES; Norwegian Research Council; NOAA Climate Change and Air Quality Programs; NASA Tropospheric Chemistry and Radiation Sciences Programs; CNRS; ANR; RFBR; SB-RAS; DLR; Deutsche Forschungsgemeinschaft (DFG) [SPP 1294 (SCHL1857/2-1), PAK 348 (SCHL1857/3-1)] FX French support is acknowledged for POLARCAT-France and CLIMSLIP projects from the French Agence National de Recherche (ANR), CNRS-LEFE, and CNES. POLARCAT-Norway was supported by the Norwegian Research Council. The ARCPAC project was supported by NOAA Climate Change and Air Quality Programs. ARCTAS was supported by NASA Tropospheric Chemistry and Radiation Sciences Programs. YAK-AEROSIB measurements were supported by CNRS, ANR, RFBR, and SB-RAS and rely on B. D. Belan, M. Yu. Arshinov, and colleagues at Institute of Atmospheric Optics, Tomsk, Russia, and P. Nedelec at Laboratoire d'Aerologie, Toulouse, France. The Falcon aircraft deployment for POLARCAT-GRACE was funded by DLR. HS and AR acknowledge support from Deutsche Forschungsgemeinschaft (DFG) under SPP 1294 (SCHL1857/2-1) and PAK 348 (SCHL1857/3-1). NR 120 TC 8 Z9 8 U1 8 U2 62 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD DEC PY 2014 VL 95 IS 12 BP 1873 EP + DI 10.1175/BAMS-D-13-00017.1 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CA8WP UT WOS:000349201900015 ER PT J AU de Lannoy, GJM Koster, RD Reichle, RH Mahanama, SPP Liu, Q AF de Lannoy, Gabrielle J. M. Koster, Randal D. Reichle, Rolf H. Mahanama, Sarith P. P. Liu, Qing TI An updated treatment of soil texture and associated hydraulic properties in a global land modeling system SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS LA English DT Article ID CLIMATE REFERENCE NETWORK; PEDOTRANSFER FUNCTIONS; ORGANIC-CARBON; SURFACE SCHEME; UNITED-STATES; DATA SET; MOISTURE; CONDUCTIVITY; PARAMETERS; EVAPOTRANSPIRATION AB The advent of new data sets describing soil texture and associated soil properties offers the promise of improved hydrological simulation. Here we describe the composition of a new soil texture data set and its implementation into a specific land surface modeling system, namely, the Catchment land surface model (LSM) of the NASA Goddard Earth Observing System version 5 (GEOS-5) modeling and assimilation framework. First, global soil texture composites are generated using data from the Harmonized World Soil Database version 1.21 (HWSD1.21) and the State Soil Geographic (STATSGO2) project, with explicit consideration of different levels of organic material. Then, the LSM's soil parameters are upgraded using the new texture data, with hydraulic parameters derived for the more extensive set of texture classes using pedotransfer functions. Other changes to the LSM parameters are included to further support simulations at increasingly fine resolutions. A suite of simulations with the original and new parameter versions shows modest yet significant improvements in the Catchment LSM's simulation of soil moisture and surface hydrological fluxes. The revised LSM parameters will be used for the forthcoming Soil Moisture Active Passive (SMAP) soil moisture assimilation product. C1 [de Lannoy, Gabrielle J. M.; Koster, Randal D.; Reichle, Rolf H.; Mahanama, Sarith P. P.; Liu, Qing] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [de Lannoy, Gabrielle J. M.] Univ Space Res Assoc, Columbia, MD USA. [Mahanama, Sarith P. P.; Liu, Qing] Sci Syst & Applicat, Lanham, MD USA. RP de Lannoy, GJM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Gabrielle.DeLannoy@nasa.gov RI Reichle, Rolf/E-1419-2012; Koster, Randal/F-5881-2012 OI Koster, Randal/0000-0001-6418-6383 FU NASA Soil Moisture Active Passive mission; NASA Modeling, Analysis, and Prediction program; NASA High-End Computing program FX The authors thank Mike Cosh for providing the USDA/ARS CalVal soil moisture validation data set, Narendra Das and Steven Chan for discussions on compositing texture databases, Lien Loosvelt, Henk Wosten, Keith Saxton, and Wim Cornelis for helpful discussions on the calculation of soil hydraulic parameters, and the anonymous reviewers for their helpful comments. The research was supported by the NASA Soil Moisture Active Passive mission, the NASA Modeling, Analysis, and Prediction program, and the NASA High-End Computing program. The soil texture data and soil hydraulic parameters used and developed for the baseline and revised simulations in this paper are available at the Global Modeling and Assimilation Office in NASA Goddard Space Flight Center, Maryland, USA. The STATSGO2 soil texture data are available from the USDA/NRCS (http://websoilsurvey.nrcs.usda.gov/), and the HWSD1.21 soil texture data are available from the International Institute for Applied Systems Analysis (IIASA) (http://webarchive.iiasa.ac.at/Research/LUC/External-World-soil-database /HTML/). NR 70 TC 15 Z9 15 U1 9 U2 25 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1942-2466 J9 J ADV MODEL EARTH SY JI J. Adv. Model. Earth Syst. PD DEC PY 2014 VL 6 IS 4 BP 957 EP 979 DI 10.1002/2014MS000330 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CA7FP UT WOS:000349083400001 ER PT J AU Zhang, CZ Wang, MH Morrison, H Somerville, RCJ Zhang, K Liu, XH Li, JLF AF Zhang, Chengzhu Wang, Minghuai Morrison, Hugh Somerville, Richard C. J. Zhang, Kai Liu, Xiaohong Li, Jui-Lin F. TI Investigating ice nucleation in cirrus clouds with an aerosol-enabled Multiscale Modeling Framework SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS LA English DT Article DE high resolution; global atmospheric modeling; extreme precipitation; tropical cyclones ID COMMUNITY ATMOSPHERE MODEL; GENERAL-CIRCULATION MODEL; TROPICAL CYCLONE CLIMATOLOGY; VOLUME DYNAMICAL CORE; PRECIPITATION EXTREMES; INTERCOMPARISON PROJECT; HORIZONTAL RESOLUTION; GRIDDED PRECIPITATION; VERSION 3; SIMULATIONS AB In this study, an aerosol-dependent ice nucleation scheme has been implemented in an aerosol-enabled Multiscale Modeling Framework (PNNL MMF) to study ice formation in upper troposphere cirrus clouds through both homogeneous and heterogeneous nucleation. The MMF model represents cloud scale processes by embedding a cloud-resolving model (CRM) within each vertical column of a GCM grid. By explicitly linking ice nucleation to aerosol number concentration, CRM-scale temperature, relative humidity and vertical velocity, the new MMF model simulates the persistent high ice supersaturation and low ice number concentration (10-100/L) at cirrus temperatures. The new model simulates the observed shift of the ice supersaturation PDF toward higher values at low temperatures following the homogeneous nucleation threshold. The MMF model predicts a higher frequency of midlatitude supersaturation in the Southern Hemisphere and winter hemisphere, which is consistent with previous satellite and in situ observations. It is shown that compared to a conventional GCM, the MMF is a more powerful model to simulate parameters that evolve over short time scales such as supersaturation. Sensitivity tests suggest that the simulated global distribution of ice clouds is sensitive to the ice nucleation scheme and the distribution of sulfate and dust aerosols. Simulations are also performed to test empirical parameters related to auto-conversion of ice crystals to snow. Results show that with a value of 250 mu m for the critical diameter, Dcs, that distinguishes ice crystals from snow, the model can produce good agreement with the satellite-retrieved products in terms of cloud ice water path and ice water content, while the total ice water is not sensitive to the specification of Dcs value. C1 [Zhang, Chengzhu; Somerville, Richard C. J.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Wang, Minghuai; Zhang, Kai] Pacific NW Natl Lab, Richland, WA 99352 USA. [Morrison, Hugh] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Liu, Xiaohong] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA. [Li, Jui-Lin F.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Zhang, CZ (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. EM c5zhang@ucsd.edu RI Liu, Xiaohong/E-9304-2011; Wang, Minghuai/E-5390-2011; Zhang, Kai/F-8415-2010 OI Liu, Xiaohong/0000-0002-3994-5955; Wang, Minghuai/0000-0002-9179-228X; Zhang, Kai/0000-0003-0457-6368 FU Center for Multiscale Modeling of Atmospheric Processes (CMMAP), a National Science Foundation (NSF) Science and Technology Center [ATM-0425247]; DOE Office of Science, Decadal and Regional Climate Prediction Earth System Models (EaSM) program; DOE [DE-AC06-76RLO 1830]; U.S. Department of Energy Atmospheric System Research Program; National Science Foundation [OCI-1053575]; National Science Foundation FX This research was supported by the Center for Multiscale Modeling of Atmospheric Processes (CMMAP), a National Science Foundation (NSF) Science and Technology Center managed by Colorado State University under Cooperative Agreement ATM-0425247. C. Zhang wants to thank Gabe Kooperman and Mike Pritchard for insightful discussions. M. Wang was supported by the DOE Office of Science, Decadal and Regional Climate Prediction using Earth System Models (EaSM) program. PNNL is operated by Battelle for the DOE under Contract DE-AC06-76RLO 1830. K. Zhang acknowledges the support from the U.S. Department of Energy Atmospheric System Research Program. We thank the anonymous reviewers for their extremely conscientious and constructive comments and suggestions, which greatly improved the manuscript. Our research used the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant number OCI-1053575. We also would like to acknowledge high-performance computing support from Yellowstone (ark:/85065/d7wd3xhc) provided by NCAR's Computational and Information Systems Laboratory, sponsored by the National Science Foundation. The original PNNL MMF model is available through the NCAR CESM repository at: https://svn-ccsmrelease.cgd.ucar.edu/model_development_releases/spcam2_0 -cesm1_1_1. The model with updated ice nucleation is available upon request to C. Zhang. NR 72 TC 2 Z9 2 U1 1 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1942-2466 J9 J ADV MODEL EARTH SY JI J. Adv. Model. Earth Syst. PD DEC PY 2014 VL 6 IS 4 BP 998 EP 1015 DI 10.1002/2014MS000343 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CA7FP UT WOS:000349083400003 ER PT J AU Shaevitz, DA Camargo, SJ Sobel, AH Jonas, JA Kim, D Kumar, A LaRow, TE Lim, YK Murakami, H Reed, KA Roberts, MJ Scoccimarro, E Vidale, PL Wang, H Wehner, MF Zhao, M Henderson, N AF Shaevitz, Daniel A. Camargo, Suzana J. Sobel, Adam H. Jonas, Jeffrey A. Kim, Daehyun Kumar, Arun LaRow, Timothy E. Lim, Young-Kwon Murakami, Hiroyuki Reed, Kevin A. Roberts, Malcolm J. Scoccimarro, Enrico Vidale, Pier Luigi Wang, Hui Wehner, Michael F. Zhao, Ming Henderson, Naomi TI Characteristics of tropical cyclones in high-resolution models in the present climate SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS LA English DT Article ID WESTERN NORTH PACIFIC; MADDEN-JULIAN OSCILLATION; INTERDECADAL VARIABILITY; EL-NINO; INTERANNUAL VARIABILITY; HURRICANE INTENSITY; DECADAL VARIATIONS; GENESIS LOCATION; STORM FORMATION; ENSO AB The global characteristics of tropical cyclones (TCs) simulated by several climate models are analyzed and compared with observations. The global climate models were forced by the same sea surface temperature (SST) fields in two types of experiments, using climatological SST and interannually varying SST. TC tracks and intensities are derived from each model's output fields by the group who ran that model, using their own preferred tracking scheme; the study considers the combination of model and tracking scheme as a single modeling system, and compares the properties derived from the different systems. Overall, the observed geographic distribution of global TC frequency was reasonably well reproduced. As expected, with the exception of one model, intensities of the simulated TC were lower than in observations, to a degree that varies considerably across models. C1 [Shaevitz, Daniel A.; Sobel, Adam H.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. [Camargo, Suzana J.; Sobel, Adam H.; Kim, Daehyun; Henderson, Naomi] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Sobel, Adam H.] Columbia Univ, Dept Earth & Environm Sci, New York, NY USA. [Jonas, Jeffrey A.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Jonas, Jeffrey A.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Kumar, Arun; Wang, Hui] NOAA NWS NCEP, Climate Predict Ctr, College Pk, MD USA. [LaRow, Timothy E.] Florida State Univ, Ctr Ocean Atmospher Predict Studies, Tallahassee, FL 32306 USA. [Lim, Young-Kwon] NASA, Goddard Space Flight Ctr, GMAO, Greenbelt, MD 20771 USA. [Lim, Young-Kwon] IM Syst Grp, Goddard Earth Sci Technol & Res, Greenbelt, MD USA. [Murakami, Hiroyuki] Univ Hawaii Manoa, Int Pacific Res Ctr, Honolulu, HI 96822 USA. [Reed, Kevin A.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Roberts, Malcolm J.] Met Off, Hadley Ctr, Exeter, Devon, England. [Scoccimarro, Enrico] Ist Nazl Geofis & Vulcanol, Bologna, Italy. [Scoccimarro, Enrico] Ctr Euromediterraneosui Cambiamenti Climatici, Bologna, Italy. [Vidale, Pier Luigi] Univ Reading, NCAS Climate, Reading, Berks, England. [Wehner, Michael F.] Lawrence Livermore Natl Lab, Berkeley, CA USA. [Zhao, Ming] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ USA. RP Camargo, SJ (reprint author), Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. EM suzana@ldeo.columbia.edu RI Camargo, Suzana/C-6106-2009; Reed, Kevin/C-4466-2012; Sobel, Adam/K-4014-2015; Murakami, Hiroyuki/L-5745-2015; Zhao, Ming/C-6928-2014; OI Camargo, Suzana/0000-0002-0802-5160; Reed, Kevin/0000-0003-3741-7080; Sobel, Adam/0000-0003-3602-0567; Vidale, Pier Luigi/0000-0002-1800-8460 FU NSF AGS [1143959]; NASA [NNX09AK34G]; Italian Ministry of Education, University and Research; Italian Ministry of Environment, Land and Sea under the GEMINA project; Office of Science, Office of Biological and Environmental Research of the U.S. Department of Energy as part of their Regional and Global Climate Modeling Program [DE-AC02-05CH11231]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231] FX The authors would like to thank all members of the U.S. CLIVAR Hurricane Working Group for their contribution to this significant effort. We also would like to thank Naomi Henderson for making the model data available for the working group and managing the data set. D.A.S., S.J.C., and A.H.S. acknowledge support of NSF AGS 1143959. S.J.C., A.H.S., and D.K. acknowledge support for the GISS model runs and analysis from NASA grant NNX09AK34G. E.S. acknowledges support from the Italian Ministry of Education, University and Research and the Italian Ministry of Environment, Land and Sea under the GEMINA project. M.W. was supported by the Director, Office of Science, Office of Biological and Environmental Research of the U.S. Department of Energy under contract DE-AC02-05CH11231 as part of their Regional and Global Climate Modeling Program. CAM5 simulations used resources of the National Energy Research Scientific Computing Center (NERSC), also supported by the Office of Science of the U.S. Department of Energy, under contract DE-AC02-05CH11231. The model data used in this paper are part of the U.S. CLIVAR Hurricane Working Group data set. Currently, the data are only available for Working Group members, in a near future, the data will be made available for the scientific community. NR 59 TC 21 Z9 21 U1 2 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1942-2466 J9 J ADV MODEL EARTH SY JI J. Adv. Model. Earth Syst. PD DEC PY 2014 VL 6 IS 4 BP 1154 EP 1172 DI 10.1002/2014MS000372 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CA7FP UT WOS:000349083400011 ER PT J AU Cohen, BA Miller, JS Li, ZH Swindle, TD French, RA AF Cohen, Barbara A. Miller, J. Scott Li, Zheng-Hua Swindle, Timothy D. French, Renee A. TI The Potassium-Argon Laser Experiment (KArLE): In Situ Geochronology for Planetary Robotic Missions SO GEOSTANDARDS AND GEOANALYTICAL RESEARCH LA English DT Article DE geochronology; mass spectrometry; laser ablation; Ar-Ar dating; in situ analysis ID FISH CANYON SANIDINE; X-RAY SPECTROMETER; INNER SOLAR-SYSTEM; K-AR; MARS; ROCKS; EVOLUTION; METEORITE; AGES; STRATIGRAPHY AB Geochronology is a fundamental measurement for planetary samples, providing global and solar system context for the conditions prevailing on the planet at the time of major geological events. The potassium (K)-Argon (Ar) laser experiment (KArLE) will make in situ noble gas geochronology measurements aboard planetary robotic missions such as rovers and landers. Laser-induced breakdown spectroscopy (LIBS) is used to measure the K abundance in a sample and to release its noble gases; the evolved Ar is measured by mass spectrometry, and relative K content is related to absolute Ar abundance by sample mass, determined by optical measurement of the ablated volume. This approach allows K and Ar to be measured on identical volumes multiple times to create an isochron, which improves the age determination and reveals irregularities in the rock if they exist. The KArLE technique measures a whole-rock K-Ar age with 10% uncertainty or better for rocks 2Ga or older, sufficient to resolve the absolute age of many planetary samples. The LIBS-mass spectrometry approach is attractive because the analytical components have been flight-proven, do not require further technical development and provide essential measurements (complete elemental abundance, evolved volatile analysis, micro-imaging) as well as in situ geochronology. C1 [Cohen, Barbara A.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Miller, J. Scott] Qualis Corp, Jacobs ESSSA Grp, Huntsville, AL 35806 USA. [Li, Zheng-Hua] Univ Alabama, Huntsville, AL 35805 USA. [Swindle, Timothy D.] Univ Arizona, Tucson, AZ 85721 USA. [French, Renee A.] Northwestern Univ, Evanston, IL 60208 USA. RP Cohen, BA (reprint author), NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM Barbara.A.Cohen@nasa.gov FU NASA Planetary Instrument Definition and Development Program FX This work was conducted under a grant from the NASA Planetary Instrument Definition and Development Program and used the NASA Astrophysical Data System Abstract Service. We thank Paul Sylvester for encouraging this submission and serving as its editor, along with two reviewers who strengthened the manuscript; Roger Wiens, Sam Clegg, Will Brinckerhoff, Paul Mahaffy, Ian Wright, Ariel Waldman and Ross Beyer for their collaboration and advice on instrument design, techniques and breadboard components; and Bill Hames and F. Scott Anderson for providing samples. BAC thanks Tim Swindle and Paul Lucey for convincing her of the utility of in situ dating during discussions at Los Portales in Mountain View CA and the Spy Bar in Washington DC. NR 76 TC 7 Z9 7 U1 0 U2 11 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1639-4488 EI 1751-908X J9 GEOSTAND GEOANAL RES JI Geostand. Geoanal. Res. PD DEC PY 2014 VL 38 IS 4 BP 421 EP 439 DI 10.1111/j.1751-908X.2014.00319.x PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AZ1YK UT WOS:000348031100003 ER PT J AU Zeng, LL Liu, WT Xue, HJ Xiu, P Wang, DX AF Zeng, Lili Liu, W. Timothy Xue, Huijie Xiu, Peng Wang, Dongxiao TI Freshening in the South China Sea during 2012 revealed by Aquarius and in situ data SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE Aquarius SSS; the South China Sea; freshening; in situ observation; surface salinity budget ID SURFACE SALINITY; BARRIER LAYER; INDIAN-OCEAN; PRECIPITATION; VALIDATION; CLIMATE; VARIABILITY; KUROSHIO; CURRENTS; FLUXES AB Newly available sea surface salinity (SSS) data from the Aquarius together with in situ hydrographic data are used to explore the spatial and temporal characteristics of SSS in the South China Sea (SCS). Using in situ observations as the reference, an evaluation of daily Aquarius data indicates that there exists a negative bias of 0.45 psu for the version 3.0 data set. The root-mean-square difference for daily Aquarius SSS is about 0.53 psu after correcting the systematic bias, and those for weekly and monthly Aquarius SSSs are 0.45 and 0.29 psu, respectively. Nevertheless, the Aquarius SSS shows a reliable freshening in the SCS in 2012, which is larger than the Aquarius uncertainty. The freshening of up to 0.4 psu in the upper-ocean of the northern SCS was confirmed by in situ observations. This freshening in 2012 was caused by a combined effect of abundant local freshwater flux and limited Kuroshio intrusion. By comparing the Kuroshio intrusion in 2012 with that in 2011, we found the reduction as a relatively important cause for the freshening over the northern SCS. In contrast to the northern SCS, reduced river discharge in 2012 played the leading role to the saltier surface in the region near the Mekong River mouth with respect to 2011. C1 [Zeng, Lili; Xue, Huijie; Xiu, Peng; Wang, Dongxiao] Chinese Acad Sci, South China Sea Inst Oceanol, State Key Lab Trop Oceanog, Guangzhou, Guangdong, Peoples R China. [Liu, W. Timothy] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Xue, Huijie; Xiu, Peng] Univ Maine, Sch Marine Sci, Orono, ME USA. RP Wang, DX (reprint author), Chinese Acad Sci, South China Sea Inst Oceanol, State Key Lab Trop Oceanog, Guangzhou, Guangdong, Peoples R China. EM dxwang@scsio.ac.cn RI WANG, DongXiao/B-4445-2012 FU National Natural Basic Research Program of China (973 Program) [2011CB403501]; "Strategic Priority Research Program'' of the Chinese Academy of Sciences [XDA11010203]; National Natural Science Foundation of China [41206011]; Recruitment Program of Global Experts; 100-Talent Program of Chinese Academy of Sciences [50601-112]; NASA Ocean Surface Salinity Science Team Program FX We appreciate valuable critiques from two anonymous whose input greatly improved this paper. Discussion with Xinxin Wang (Dalian Maritime University, China) helped to clarify issues related to the RFI sources. We benefited from numerous data sets made freely available, and those include Aquarius SSS (ftp://aqosst@podaac.jpl.nasa.gov), three precipitation products (http://apdrc.soest.hawaii.edu/data/), OSCAR currents (http://www.oscar.noaa.gov/datadisplay/datadownload.htm), OAFlux evaporation (ftp://ftp.whoi.edu/pub/science/oaflux/data_v3), Argo floats (http://www.usgodae.org/cgi-bin/argo_select.pl), and TRIP river pathways (http://hydro.iis.u-tokyo.ac.jp/similar to taikan/TRIPDATA/TRIPDATA.html#DATA). The records of Mekong River discharge are provided by the global river discharge data set from the Global Runoff Data Centre (GRDC). The in situ observations by SCSIO and the combined observational data set SCSOD14 are also available, and anyone who wants to get access to these data could contact the corresponding author, Dongxiao Wang. This study was supported by the National Natural Basic Research Program of China (973 Program; 2011CB403501), the "Strategic Priority Research Program'' of the Chinese Academy of Sciences (XDA11010203), the National Natural Science Foundation of China (41206011), the Recruitment Program of Global Experts, and the 100-Talent Program of Chinese Academy of Sciences (50601-112). The work of W. Timothy Liu was supported by NASA Ocean Surface Salinity Science Team Program. NR 40 TC 15 Z9 16 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD DEC PY 2014 VL 119 IS 12 BP 8296 EP 8314 DI 10.1002/2014JC010108 PG 19 WC Oceanography SC Oceanography GA AZ8GI UT WOS:000348452800006 ER PT J AU Lee, T Lagerloef, G Kao, HY McPhaden, MJ Willis, J Gierach, MM AF Lee, Tong Lagerloef, Gary Kao, Hsun-Ying McPhaden, Michael J. Willis, Joshua Gierach, Michelle M. TI The influence of salinity on tropical Atlantic instability waves SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE ocean salinity; remote sensing; tropical instability waves ID EASTERN EQUATORIAL PACIFIC; SEA-SURFACE TEMPERATURE; NORTH BRAZIL CURRENT; ROSSBY WAVES; MIXED-LAYER; WIND STRESS; OCEAN; ENERGETICS; IMPACT; VARIABILITY AB Sea surface salinity (SSS) data derived from the Aquarius/SAC-D satellite mission are analyzed along with other satellite and in situ data to assess Aquarius' capability to detect tropical instability waves (TIWs) and eddies in the tropical Atlantic Ocean and to investigate the influence that SSS has on the variability. Aquarius data show that the magnitude of SSS anomalies associated with the Atlantic TIWs is 0.25 practical salinity unit, which is weaker than those in the Pacific by 50%. In the central equatorial Atlantic, SSS contribution to the mean meridional density gradient is similar to sea surface temperature (SST) contribution. Consequently, SSS is important to TIW-related surface density anomalies and perturbation potential energy (PPE). In this region, SSS influences surface PPE significantly through the direct effect and the indirect effect associated with SSS-SST covariability. Ignoring SSS effects would underestimate TIW-related PPE by approximately three times in the surface layer. SSS also regulates the seasonality of the TIWs. The boreal-spring peak of the PPE due to SSS leads that due to SST by about one month. Therefore, SSS not only affects the spatial structure, but the seasonal variability of the TIWs in the equatorial Atlantic. In the northeast Atlantic near the Amazon outflow and the North Brazil Current retroflection region and in the southeast Atlantic near the Congo River outflow, SSS accounts for 80-90% of the contribution to mean meridional density gradient. Not accounting for SSS effect would underestimate surface PPE in these regions by a factor of 10 and 4, respectively. C1 [Lee, Tong; Willis, Joshua; Gierach, Michelle M.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Lagerloef, Gary; Kao, Hsun-Ying] Earth & Space Res, Seattle, WA USA. [McPhaden, Michael J.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. RP Lee, T (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Tong.Lee@jpl.nasa.gov RI McPhaden, Michael/D-9799-2016 FU National Aeronautics and Space Administration FX This research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This is PMEL contribution 4156. The gridded Aquarius data used in this study were provided by Gary Lagerloef (lager@esr.org) and Hsun-Ying Kao (hkao@esr.org) of Earth and Space Research. The links of all other data used in this study were provided in in section 2 "Data'' of this paper. We thank Xiaobin Yin of LOCEAN-IPSL for providing the Matlab script and instruction of Radon transform and Seymon Grodsky of University of Maryland for providing the source of the Congo River discharge. NR 61 TC 9 Z9 9 U1 2 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD DEC PY 2014 VL 119 IS 12 BP 8375 EP 8394 DI 10.1002/2014JC010100 PG 20 WC Oceanography SC Oceanography GA AZ8GI UT WOS:000348452800010 ER PT J AU Newman, T Farrell, SL Richter-Menge, J Connor, LN Kurtz, NT Elder, BC McAdoo, D AF Newman, Thomas Farrell, Sinead L. Richter-Menge, Jacqueline Connor, Laurence N. Kurtz, Nathan T. Elder, Bruce C. McAdoo, David TI Assessment of radar-derived snow depth over Arctic sea ice SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE snow; sea ice; remote sensing; instruments and techniques; wavelet transform ID THICKNESS; MISSION; LASER AB Knowledge of contemporaneous snow depth on Arctic sea ice is important both to constrain the regional climatology and to improve the accuracy of satellite altimeter estimates of sea ice thickness. We assess new data available from the NASA Operation IceBridge snow radar instrument and derive snow depth estimates across the western Arctic ice pack using a novel methodology based on wavelet techniques that define the primary reflecting surfaces within the snow pack. We assign uncertainty to the snow depth estimates based upon both the radar system parameters and sea ice topographic variability. The accuracy of the airborne snow depth estimates are examined via comparison with coincident measurements gathered in situ across a range of ice types in the Beaufort Sea. We discuss the effect of surface morphology on the derivation, and consequently the accuracy, of airborne snow depth estimates. We find that snow depths derived from the airborne snow radar using the wavelet-based technique are accurate to 1 cm over level ice. Over rougher surfaces including multiyear and ridged ice, the radar system is impacted by ice surface morphology. Across basin scales, we find the snow-radar-derived snow depth on first-year ice is at least approximate to 60% of the value reported in the snow climatology for the Beaufort Sea, Canada Basin, and parts of the central Arctic, since these regions were previously dominated by multiyear ice during the measurement period of the climatology. Snow on multiyear ice is more consistent with the climatology. C1 [Newman, Thomas; Farrell, Sinead L.; McAdoo, David] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Newman, Thomas; Farrell, Sinead L.; Connor, Laurence N.; McAdoo, David] NOAA, Lab Satellite Altimetry, Satellite Oceanog & Climatol Div, Ctr Weather & Climate Predict, College Pk, MD USA. [Richter-Menge, Jacqueline; Elder, Bruce C.] US Army Corps Engn, Engineer Res & Dev Ctr, Cold Reg Res & Engn Lab, Hanover, NH USA. [Kurtz, Nathan T.] NASA, Goddard Space Flight Ctr, Hydrospher & Biospher Sci Lab, Greenbelt, MD 20771 USA. RP Newman, T (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. EM tnewman3@umd.edu RI Connor, Laurence/E-7930-2011; McAdoo, Dave/F-5612-2010; Farrell, Sinead/F-5586-2010 OI Connor, Laurence/0000-0002-5276-6257; McAdoo, Dave/0000-0002-7533-5564; Farrell, Sinead/0000-0003-3222-2751 FU ONR Arctic grants [N000141210512, N0001412MP20150]; NOAA Ocean Remote Sensing Program FX Data used for the results of this paper are found at the National Snow and Ice Data Center (NSIDC, nsidc.org). IceBridge data utilized in this study are archived at the NSIDC: the IceBridge ATM Level-1B Elevation and Return Strength (ILATM1B) data set is available at http://nsidc.org/data/ilatm1b.html, the DMS L1B Geolocated and Orthorectified Images (IODMS1B) data set is available at http://nsidc.org/data/iodms1b.html, the NASA IceBridge Snow Radar Level-1B Geolocated Radar Echo Strength Profiles (IRSNO1B) data set is available at http://nsidc.org/data/irsno1b.html, and the IceBridge Sea Ice Freeboard, Snow Depth, and Thickness (IDCSI2) data set is available at http://nsidc.org/data/idcsi2.html. This work was supported by ONR Arctic grants N000141210512 and N0001412MP20150 and by the NOAA Ocean Remote Sensing Program. The authors thank Dr. L. Miller and two anonymous reviewers for their comments which helped to improve the text. The authors thank the IceBridge Instrument Teams, Science Team, and Project Science Office, as well as the aircraft support crew, for their diligent efforts in gathering and processing the OIB data. We acknowledge the significant work done by the CReSIS faculty, staff, and students in the design, development, operation, and data processing for the snow radar system. The authors thank the U.S. Army Cold Regions Research and Engineering Laboratory for collecting the in situ data. The authors thank the Naval Research Laboratory for their logistical support, including members of the field team. The authors thank the Arctic Submarine Laboratory for providing the ice camp that served as the base of operations for the in situ observation team and assisted in the coordination of the aircraft over flights. Data used in this paper were acquired by NASAs Operation IceBridge Project. The contents are solely the opinions of the authors and do not constitute a statement of policy, decision, or position on behalf of NOAA or the U.S. Government. NR 41 TC 7 Z9 7 U1 3 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD DEC PY 2014 VL 119 IS 12 BP 8578 EP 8602 DI 10.1002/2014JC010284 PG 25 WC Oceanography SC Oceanography GA AZ8GI UT WOS:000348452800022 ER PT J AU Mazarico, E Genova, A Goossens, S Lemoine, FG Neumann, GA Zuber, MT Smith, DE Solomon, SC AF Mazarico, Erwan Genova, Antonio Goossens, Sander Lemoine, Frank G. Neumann, Gregory A. Zuber, Maria T. Smith, David E. Solomon, Sean C. TI The gravity field, orientation, and ephemeris of Mercury from MESSENGER observations after three years in orbit SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE mercury; gravity field; MESSENGER; planetary orientation; Planetary Ephemeris ID LUNAR RECONNAISSANCE ORBITER; SPACE-TIME FRAME; INTERIOR STRUCTURE; COORDINATE TIME; PROPER TIME; ROTATION; MISSION; MODEL; TIDES; EARTH AB We have analyzed 3 years of radio tracking data from the MESSENGER spacecraft in orbit around Mercury and determined the gravity field, planetary orientation, and ephemeris of the innermost planet. With improvements in spatial coverage, force modeling, and data weighting, we refined an earlier global gravity field both in quality and resolution, and we present here a spherical harmonic solution to degree and order 50. In this field, termed HgM005, uncertainties in low-degree coefficients are reduced by an order of magnitude relative to earlier global fields, and we obtained a preliminary value of the tidal Love number k(2) of 0.451 0.014. We also estimated Mercury's pole position, and we obtained an obliquity value of 2.06 0.16 arcmin, in good agreement with analysis of Earth-based radar observations. From our updated rotation period (58.646146 0.000011 days) and Mercury ephemeris, we verified experimentally the planet's 3:2 spin-orbit resonance to greater accuracy than previously possible. We present a detailed analysis of the HgM005 covariance matrix, and we describe some near-circular frozen orbits around Mercury that could be advantageous for future exploration. C1 [Mazarico, Erwan; Genova, Antonio; Zuber, Maria T.; Smith, David E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Mazarico, Erwan; Genova, Antonio; Goossens, Sander; Lemoine, Frank G.; Neumann, Gregory A.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Goossens, Sander] Univ Maryland, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21201 USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA. RP Mazarico, E (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. EM erwan.m.mazarico@nasa.gov RI Neumann, Gregory/I-5591-2013; Lemoine, Frank/D-1215-2013; Mazarico, Erwan/N-6034-2014; Goossens, Sander/K-2526-2015; Genova, Antonio/M-1400-2016 OI Neumann, Gregory/0000-0003-0644-9944; Mazarico, Erwan/0000-0003-3456-427X; Goossens, Sander/0000-0002-7707-1128; Genova, Antonio/0000-0001-5584-492X FU NASA Discovery Program [NAS5-97271, NASW-00002] FX We thank the MESSENGER spacecraft and navigation teams for commanding and navigating the spacecraft during the interplanetary and orbital phases of the mission. The MESSENGER project is supported by the NASA Discovery Program under contracts NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of Washington. We thank David Rowlands for help with the GEODYN software, Mark Perry for his work with the NASA DSN to acquire the radio tracking data that made this work possible, and Steven Hauck for input on the implications of the new field to interior structure. We also appreciate constructive comments on an earlier version of the manuscript by two reviewers. The data used in this paper and the HgM005 gravity field (the spherical harmonics coefficients, their associated uncertainties, and the full covariance matrix) are available at http://geo.pds.nasa.gov/. Localized correlations were computed using the SHTOOLS library (http://shtools.ipgp.fr). Several figures were created with the Generic Mapping Tools (GMT) software [Wessel and Smith, 1991]. NR 62 TC 23 Z9 23 U1 1 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC PY 2014 VL 119 IS 12 BP 2417 EP 2436 DI 10.1002/2014JE004675 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AZ8GJ UT WOS:000348453000001 ER PT J AU Duxbury, TC Christensen, P Smith, DE Neumann, GA Kirk, RL Caplinger, MA Albee, AA Seregina, NV Neukum, G Archinal, BA AF Duxbury, T. C. Christensen, P. Smith, D. E. Neumann, G. A. Kirk, R. L. Caplinger, M. A. Albee, A. A. Seregina, N. V. Neukum, G. Archinal, B. A. TI The location of Airy-0, the Mars prime meridian reference, from stereo photogrammetric processing of THEMIS IR imaging and digital elevation data SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; prime meridian; Airy-0; cartography; THEMIS; MOLA ID ORBITER LASER ALTIMETER; ODYSSEY MISSION; SYSTEM AB The small crater Airy-0 was selected from Mariner 9 images to be the reference for the Mars prime meridian. Initial analyses in the year 2000 tied Viking Orbiter and Mars Orbiter Camera images of Airy-0 to the evolving Mars Orbiter Laser Altimeter global digital terrain model to update the location of Airy-0. Based upon this tie and radiometric tracking of landers/rovers from Earth, new expressions for the Mars spin axis direction, spin rate, and prime meridian epoch value were produced to define the orientation of the Martian surface in inertial space over time. Since the Mars Global Surveyor mission and Mars Orbiter Laser Altimeter global digital terrain model were completed some time ago, a more exhaustive study has been performed to determine the accuracy of the Airy-0 location and orientation of Mars at the standard epoch. Thermal Emission Imaging System (THEMIS) IR image cubes of the Airy and Gale crater regions were tied to the global terrain grid using precision stereo photogrammetric image processing techniques. The Airy-0 location was determined to be about 0.001 degrees east of its predicted location using the currently defined International Astronomical Union (IAU) prime meridian location. Information on this new location and how it was derived will be provided to the NASA Mars Exploration Program Geodesy and Cartography Working Group for their assessment. This NASA group will make a recommendation to the IAU Working Group on Cartographic Coordinates and Rotational Elements to update the expression for the Mars spin axis direction, spin rate, and prime meridian location. C1 [Duxbury, T. C.; Seregina, N. V.] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA. [Christensen, P.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Smith, D. E.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. [Neumann, G. A.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Kirk, R. L.; Archinal, B. A.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Caplinger, M. A.] Malin Space Sci Syst, San Diego, CA USA. [Albee, A. A.] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. [Seregina, N. V.] Moscow MV Lomonosov State Univ, Geol Fac, Dept Geocryol, Moscow, Russia. [Neukum, G.] Free Univ Berlin, Dept Planetary Sci & Remote Sensing, Berlin, Germany. RP Duxbury, TC (reprint author), George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA. EM tduxbury@gmu.edu RI Neumann, Gregory/I-5591-2013 OI Neumann, Gregory/0000-0003-0644-9944 FU NASA Science Mission Directorate Mars Odyssey Participating Scientist; Mars Express Participating Scientist; Mars Data Analysis Programs FX Appreciation is expressed to the MGS, ODY, and MEX flight operation teams and the MOLA, THEMIS, and HRSC science teams without whose efforts the data used in this article would not have been available. E. Wright and A. Maser of JPL configured the computer used for this analysis to use the NAIF SPICE toolkit and system of data kernels and the X-terminal image display tools. This work was supported by the NASA Science Mission Directorate 2001 Mars Odyssey Participating Scientist, the Mars Express Participating Scientist, and the Mars Data Analysis Programs. NR 23 TC 0 Z9 0 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC PY 2014 VL 119 IS 12 BP 2471 EP 2486 DI 10.1002/2014JE004678 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AZ8GJ UT WOS:000348453000004 ER PT J AU Glenar, DA Stubbs, TJ Hahn, JM Wang, YL AF Glenar, David A. Stubbs, Timothy J. Hahn, Joseph M. Wang, Yongli TI Search for a high-altitude lunar dust exosphere using Clementine navigational star tracker measurements SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE lunar exosphere; dust scattering ID ZODIACAL LIGHT; SPACE PROBES; BRIGHTNESS; MOON; CORONAGRAPH; ATMOSPHERE; SURFACES; MODEL AB During the 1994 Clementine lunar mapping mission, portions of 25 orbits were dedicated to a search for lunar horizon glow (LHG) using the spacecraft star tracker navigation cameras. Previous putative detections of LHG were believed to result from forward scattering of sunlight by exospheric dust grains with radii approximate to 0.1 mu m, observable above the limb from within the shadow of the Moon near orbital sunrise or sunset. We have examined star tracker image sequences from five Clementine orbits in which the limb occulted the Sun, and was at least partially shadowed from earthshine, minimizing the chance of stray light contamination. No LHG appears in the image data, or in any of the net brightness images, after subtraction of a reference zodiacal light model. However, some of the images display faint excess limb brightness that appears to be solar streamer structure. Therefore, we derive upper limits for the amount of dust in the lunar exosphere that could be hidden by these brightness fluctuations using a dust-scattering simulation code and simple exponential dust profiles defined by surface concentration n(0) and scale height H. Simulations using grains of radius 0.1 mu m show that fluctuations in the observed excess brightness can be matched by a dust exosphere with a vertical column abundance n(0)H of 5-30cm(-2) and overlying mass <10(-12)gcm(-2). These dust upper limit estimates are highly dependent on assumed grain size due to the rapid increase in per-grain brightness with grain radius. C1 [Glenar, David A.] Univ Maryland, Ctr Space Sci & Technol, Baltimore, MD 21201 USA. [Glenar, David A.; Stubbs, Timothy J.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Glenar, David A.; Stubbs, Timothy J.] NASA Ames Res Ctr, NASA Lunar Sci Inst, Moffett Field, CA USA. [Hahn, Joseph M.] Univ Texas Austin, Space Sci Inst, Austin, TX 78712 USA. [Wang, Yongli] Univ Maryland, Goddard Planetary & Heliophys Inst, Baltimore, MD 21201 USA. RP Glenar, DA (reprint author), Univ Maryland, Ctr Space Sci & Technol, Baltimore, MD 21201 USA. EM dglenar@umbc.edu RI Stubbs, Timothy/I-5139-2013 OI Stubbs, Timothy/0000-0002-5524-645X FU NASA/LASER [NNX09AO79G]; NASA Solar System Exploration Virtual Institute SSERVI/DREAM2 [NNX09AH61A] FX This work was funded by NASA/LASER grant NNX09AO79G and by the NASA Solar System Exploration Virtual Institute SSERVI/DREAM2, under grant NNX09AH61A. The SOHO/LASCO data used here are produced by a consortium of the Naval Research Laboratory (U.S.), Max-Planck-Institut fuer Aeronomie (Germany), Laboratoire d'Astronomie (France), and the University of Birmingham (UK) and are available online from the Naval Research Laboratory (http://lasco-www.nrl.navy.mil). We benefited from data made publicly available by the NASA/GSFC OMNIWeb and Satellite Situation Center websites (http://omniweb.gsfc.nasa.gov and http://sscweb.gsfc.nasa.gov), as well as the IAU Meteor Data Center (http://www.ta3.sk/IAUC22DB/MDC2007/). NR 50 TC 4 Z9 4 U1 1 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC PY 2014 VL 119 IS 12 BP 2548 EP 2567 DI 10.1002/2014JE004702 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AZ8GJ UT WOS:000348453000008 ER PT J AU Piskorz, D Elkins-Tanton, LT Smrekar, SE AF Piskorz, Danielle Elkins-Tanton, Linda T. Smrekar, Suzanne E. TI Coronae formation on Venus via extension and lithospheric instability SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Venus; coronae; rifts; volcanism; Rayleigh-Taylor instabilities ID EAST-AFRICAN; MANTLE PLUMES; MODEL; DELAMINATION; CONVECTION; EVOLUTION; BENEATH; ORIGIN; CRUST; CONSTRAINTS AB Over 500 quasi-circular volcano-tectonic features called coronae occur on Venus. They are believed to form via small-scale mantle upwellings, lithospheric instability, or a combination thereof. Coronae and rifts commonly occur together, including many coronae that lie outside of the fracture zone. However, the genetic link between the two has remained unclear. This paper proposes a mechanism for the formation of off-rift coronae due to the rifting process. We model the interaction of a rising mantle plume associated with a rift with a hypothetical preexisting layer of dense material in the lithosphere. We show that a rift and its associated off-rift coronae could be genetically linked by the process of development of secondary ringlike dripping instabilities initiating at the plume margins. We calculate the resulting surface topographies, melt volumes, and Bouguer gravity anomalies and compare them to observations. C1 [Piskorz, Danielle] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Elkins-Tanton, Linda T.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Smrekar, Suzanne E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Piskorz, D (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM dpiskorz@gps.caltech.edu NR 61 TC 1 Z9 1 U1 0 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC PY 2014 VL 119 IS 12 BP 2568 EP 2582 DI 10.1002/2014JE004636 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AZ8GJ UT WOS:000348453000009 ER PT J AU Eriksson, D MacMillan, DS Gipson, JM AF Eriksson, David MacMillan, D. S. Gipson, John M. TI Tropospheric delay ray tracing applied in VLBI analysis SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE troposphere ray tracing ID MAPPING FUNCTIONS; INTERFEROMETRY; ATMOSPHERE AB Tropospheric delay modeling error continues to be one of the largest sources of error in VLBI (very long baseline interferometry) analysis. For standard operational solutions, we use the VMF1 elevation-dependent mapping functions derived from European Centre for Medium-Range Weather Forecasts data. These mapping functions assume that tropospheric delay at a site is azimuthally symmetric. As this assumption is not true, we have instead determined the ray trace delay along the signal path through the troposphere for each VLBI quasar observation. We determined the troposphere refractivity fields from the pressure, temperature, specific humidity, and geopotential height fields of the NASA Goddard Space Flight Center Goddard Earth Observing System version 5 numerical weather model. When applied in VLBI analysis, baseline length repeatabilities were improved compared with using the VMF1 mapping function model for 72% of the baselines and site vertical repeatabilities were better for 11 of 13 sites during the 2 week CONT11 observing period in September 2011. When applied to a larger data set (2011-2013), we see a similar improvement in baseline length and also in site position repeatabilities for about two thirds of the stations in each of the site topocentric components. C1 [Eriksson, David] Cornell Univ, Ctr Appl Math, Ithaca, NY 14853 USA. [MacMillan, D. S.; Gipson, John M.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, NVI Inc, Greenbelt, MD 20771 USA. RP MacMillan, DS (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, NVI Inc, Greenbelt, MD 20771 USA. EM daniel.s.macmillan@nasa.gov OI Eriksson, David/0000-0002-3143-0922 FU NASA [NNG12HP00C] FX We thank the NASA Global Modeling and Assimilation Office (GMAO) for providing data from the numerical weather model GEOS 5.9.1 and the International VLBI Service for Geodesy and Astrometry (IVS) for providing VLBI data for our analysis. GMAO data are available at http://gmao.gsfc.nasa.gov/products/, and IVS data products can be accessed from http://ivscc.gsfc.nasa.gov/products-data/products.html. We acknowledge our support from NASA contract NNG12HP00C. We would also like to thank two anonymous reviewers for their helpful comments. NR 26 TC 1 Z9 1 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD DEC PY 2014 VL 119 IS 12 BP 9156 EP 9170 DI 10.1002/2014JB011552 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AZ8GC UT WOS:000348452200033 ER PT J AU Svec, L AF Svec, Leedjia TI To Engineer Diversity: Photons, Faces, and Phenomenology SO NAVAL ENGINEERS JOURNAL LA English DT Article C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Svec, L (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 30 TC 0 Z9 0 U1 1 U2 4 PU AMER SOC NAVAL ENG INC PI ALEXANDRIA PA 1452 DUKE STREET, ALEXANDRIA, VA 22314-3458 USA SN 0028-1425 EI 1559-3584 J9 NAV ENG J JI Nav. Eng. J. PD DEC PY 2014 VL 126 IS 4 BP 65 EP 72 PG 8 WC Engineering, Marine; Engineering, Civil; Oceanography SC Engineering; Oceanography GA AY7JC UT WOS:000347735700010 ER PT J AU Grudinin, IS Yu, N AF Grudinin, Ivan S. Yu, Nan TI Frequency combs from crystalline resonators: influence of cavity parameters on comb dynamics SO OPTICAL ENGINEERING LA English DT Article DE combs; crystalline; whispering; gallery; resonator; dispersion ID WHISPERING-GALLERY MODES; RAMAN-SCATTERING; MICRORESONATORS; GENERATION; DISPERSION; LASER AB We experimentally study the factors that influence the span in frequency combs derived from the crystalline whispering gallery mode resonators. We observe that cavity dispersion plays an important role in generation of combs by a cascaded four-wave mixing process. We observed combs from the resonators with anomalous dispersion and nearly zero dispersion at the pump wavelength. In addition, the comb generation efficiency is found to be affected by the crossing of modes of different families. The influence of Raman gain is discussed as well as the roles of the cavity diameter and pump power. (C) 2014 Society of Photo-Optical Instrumentation Engineers (SPIE) C1 [Grudinin, Ivan S.; Yu, Nan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Grudinin, IS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM grudinin@jpl.nasa.gov NR 39 TC 1 Z9 1 U1 9 U2 16 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 0091-3286 EI 1560-2303 J9 OPT ENG JI Opt. Eng. PD DEC PY 2014 VL 53 IS 12 AR 122609 DI 10.1117/1.OE.53.12.122609 PG 7 WC Optics SC Optics GA AY7EX UT WOS:000347725200041 ER PT J AU Ishikawa, SN Glesener, L Christe, S Ishibashi, K Brooks, DH Williams, DR Shimojo, M Sako, N Krucker, S AF Ishikawa, Shin-Nosuke Glesener, Lindsay Christe, Steven Ishibashi, Kazunori Brooks, David H. Williams, David R. Shimojo, Masumi Sako, Nobuharu Krucker, Saem TI Constraining hot plasma in a non-flaring solar active region with FOXSI hard X-ray observations SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE Sun: corona; Sun: X-rays, gamma rays; Sun: UV radiation ID ULTRAVIOLET IMAGING SPECTROMETER; 1ST IMAGES; HINODE; EMISSION; TELESCOPE; CORONA; CALIBRATION; RHESSI; XRT; IONIZATION AB We present new constraints on the high-temperature emission measure of a non-flaring solar active region using observations from the recently flown Focusing Optics X-ray Solar Imager (FOXSI) sounding rocket payload. FOXSI has performed the first focused hard X-ray (HXR) observation of the Sun in its first successful flight on 2012 November 2. Focusing optics, combined with small strip detectors, enable high-sensitivity observations with respect to previous indirect imagers. This capability, along with the sensitivity of the HXR regime to high-temperature emission, offers the potential to better characterize high-temperature plasma in the corona as predicted by nanoflare heating models. We present a joint analysis of the differential emission measure (DEM) of active region 11602 using coordinated observations by FOXSI, Hinode/XRT, and Hinode/EIS. The Hinode-derived DEM predicts significant emission measure between 1MK and 3MK, with a peak in the DEM predicted at 2.0-2.5MK. The combined XRT and EIS DEM also shows emission from a smaller population of plasma above 8MK. This is contradicted by FOXSI observations that significantly constrain emission above 8 MK. This suggests that the Hinode DEM analysis has larger uncertainties at higher temperatures and that > 8MK plasma above an emission measure of 3 x 10(44) cm(-3) is excluded in this active region. C1 [Ishikawa, Shin-Nosuke; Shimojo, Masumi; Sako, Nobuharu] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Glesener, Lindsay; Krucker, Saem] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christe, Steven] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ishibashi, Kazunori] Nagoya Univ, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Brooks, David H.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Williams, David R.] Univ Coll London, Mullard Space Sci Lab, Holmbury RH5 6NT, Surrey, England. [Krucker, Saem] Univ Appl Sci & Arts NorthWestern Switzerland, Sch Engn, Inst Technol 4D, CH-5210 Windisch, Switzerland. RP Ishikawa, SN (reprint author), Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. EM s.ishikawa@nao.ac.jp; glesener@ssl.berkeley.edu; steven.d.christe@nasa.gov; bish@u.phys.nagoya-u.ac.jp; dhbrooks@ssd5.nrl.navy.mil; d.r.williams@ucl.ac.uk; masumi.shimojo@nao.ac.jp; sako@solar.mtk.nao.ac.jp; krucker@ssl.berkeley.edu RI Williams, David/E-6676-2011; Shimojo, Masumi/J-2605-2016; OI Williams, David/0000-0001-9922-8117; Shimojo, Masumi/0000-0002-2350-3749; Christe, Steven/0000-0001-6127-795X FU NASA's LCAS program [NNX11AB75G]; Japan Society for the Promotion of Science; NASA GSRP fellowship [NNX09AM40H] FX FOXSI was funded by NASA's LCAS program, grant NNX11AB75G. We would like to thank Dr. Kyoung-Sun Lee for her help with the EIS DEM analysis. The work was supported through a Grant-in-Aid for JSPS Fellows from the Japan Society for the Promotion of Science. Work at UC Berkeley received support from NASA GSRP fellowship NNX09AM40H. Hinode is a Japanese mission developed and launched by ISAS/JAXA, collaborating with NAOJ as a domestic partner, NASA and STFC (UK) as international partners. Scientific operation of the Hinode mission is conducted by the Hinode science team organized at ISAS/JAXA. This team mainly consists of scientists from institutes in the partner countries. Support for the post-launch operation is provided by JAXA and NAOJ (Japan), STFC (UK), NASA, ESA, and NSC (Norway). NR 46 TC 5 Z9 5 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD DEC PY 2014 VL 66 SI 1 AR S15 DI 10.1093/pasj/psu090 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AZ9GG UT WOS:000348521000015 ER PT J AU Young, PR Muglach, K AF Young, Peter R. Muglach, Karin TI A coronal hole jet observed with Hinode and the Solar Dynamics Observatory SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE Sun: activity; Sun: corona; Sun: magnetic fields; Sun: UV radiation ID X-RAY JETS; BLOWOUT JET; ACTIVE-REGION; ATOMIC DATABASE; KINEMATICS; DICHOTOMY; SDO/AIA; CHIANTI; TWIST AB A small blowout jet was observed at the boundary of the south polar coronal hole on 2011 February 8 at around 21:00UT. Images from the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO) revealed an expanding loop rising from one footpoint of a compact, bipolar bright point. Magnetograms from the Helioseismic Magnetic Imager (HMI) on board SDO showed that the jet was triggered by the cancelation of a parasitic positive polarity feature near the negative pole of the bright point. The jet emission was present for 25 min and it extended 30Mm from the bright point. Spectra from the Extreme Ultraviolet Imaging Spectrometer on board Hinode yielded a temperature and density of 1.6 MK and 0.9-1.7x10(8) cm(-3) for the ejected plasma. Line-of-sight velocities reached up to 250 kms(-1) and were found to increase with height, suggesting plasma acceleration within the body of the jet. Evidence was found for twisting motions within the jet based on variations of the line-of-sight velocities across the jet width. The derived angular speed was in the range (9-12) x10(-3) rad s(-1), consistent with previous measurements from jets. The density of the bright point was 7.6x10(8) cm(-3), and the peak of the bright point's emission measure occurred at 1.3 MK, with no plasma above 3 MK. C1 [Young, Peter R.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Muglach, Karin] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Muglach, Karin] ARTEP Inc, Ellicott City, MD 21042 USA. RP Young, PR (reprint author), George Mason Univ, Coll Sci, 4400 Unversity Dr, Fairfax, VA 22030 USA. EM pyoung9@gmu.edu; kmuglach@gmx.de OI Young, Peter/0000-0001-9034-2925 FU National Science Foundation [AGS-1159353]; ISSI FX The authors acknowledge funding from National Science Foundation grant AGS-1159353, and we thank the referee for valuable comments. P.R.Y. thanks ISSI for financial support to attend the 2014 International Team Meeting "Understanding Solar Jets and their Role in Atmospheric Structure and Dynamics" (PI: N.-E. Raouafi), and he thanks the participants for useful discussions. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in co-operation with ESA and NSC (Norway). SDO is a mission for NASA's Living With a Star program, and data are provided courtesy of NASA/SDO and the AIA and HMI science teams. NR 22 TC 6 Z9 6 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD DEC PY 2014 VL 66 SI 1 AR S12 DI 10.1093/pasj/psu088 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AZ9GG UT WOS:000348521000012 ER PT J AU Yang, YM Meng, X Komjathy, A Verkholyadova, O Langley, RB Tsurutani, BT Mannucci, AJ AF Yang, Yu-Ming Meng, X. Komjathy, A. Verkholyadova, O. Langley, R. B. Tsurutani, B. T. Mannucci, A. J. TI Tohoku-Oki earthquake caused major ionospheric disturbances at 450km altitude over Alaska SO RADIO SCIENCE LA English DT Article DE coseismic ionospheric perturbations; atmospheric neutral density perturbations; remote sensing ID PLANETARY SEISMOLOGY; ELECTRON-CONTENT; MODEL; ATMOSPHERE; SYSTEM; GRACE; WAVES AB Ionospheric total electron content (TEC) and atmospheric density perturbations were derived from measurements made from instruments on board the Gravity Recovery and Climate Experiment (GRACE) spacecraft. At the time of the Tohoku-Oki earthquake on 11 March 2011, the twin spacecraft were orbiting at an altitude of similar to 450km over Alaska. Significant TEC fluctuations (up to 0.6total electron content unit (TECU; 1TECU=10(16)elm(-2)), atmospheric density perturbations (similar to 3.610(-14)kg/m(3)), and sudden changes in GRACE acceleration (similar to 410(-8)m/s(2)) were observed similar to 8min after the arrival of seismic and infrasound waves on the ground in Alaska, similar to 20min after the Tohoku-Oki main shock at 05:46:23 UTC. The results of the three-dimensional ionospheric-thermospheric modeling and infrasound ray-tracing simulations are consistent with the arrival time and physical characteristics of the disturbances at GRACE. This is the first time that ionospheric disturbances associated with an earthquake are clearly attributable to perturbations at such high altitudes. C1 [Yang, Yu-Ming; Meng, X.; Komjathy, A.; Verkholyadova, O.; Tsurutani, B. T.; Mannucci, A. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Komjathy, A.; Langley, R. B.] Univ New Brunswick, Dept Geodesy & Geomat Engn, Fredericton, NB, Canada. RP Yang, YM (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Oscar.Yang@jpl.nasa.gov RI Meng, Xing/A-1929-2016 FU National Aeronautics and Space Administration FX The authors would like to thank NASA Headquarters, the NASA ROSES 2011 GNSS Remote Sensing Science Team (NNH11ZDA001N-GNSS), and the NASA Postdoctoral Program administrated by Oak Ridge Associated Universities. Our research was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We acknowledge the NASA/GFZ GRACE project for the GRACE data products (distributed by JPL PODAAC (http://podaac.jpl.nasa.gov/gravity/grace)). NR 28 TC 6 Z9 7 U1 1 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0048-6604 EI 1944-799X J9 RADIO SCI JI Radio Sci. PD DEC PY 2014 VL 49 IS 12 BP 1206 EP 1213 DI 10.1002/2014RS005580 PG 8 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA CA0XU UT WOS:000348637600007 ER PT J AU Rosenfeld, D Andreae, MO Asmi, A Chin, M de Leeuw, G Donovan, DP Kahn, R Kinne, S Kivekas, N Kulmala, M Lau, W Schmidt, KS Suni, T Wagner, T Wild, M Quaas, J AF Rosenfeld, Daniel Andreae, Meinrat O. Asmi, Ari Chin, Mian de Leeuw, Gerrit Donovan, David P. Kahn, Ralph Kinne, Stefan Kivekas, Niku Kulmala, Markku Lau, William Schmidt, K. Sebastian Suni, Tanja Wagner, Thomas Wild, Martin Quaas, Johannes TI Global observations of aerosol-cloud-precipitation-climate interactions SO REVIEWS OF GEOPHYSICS LA English DT Review DE cloud aerosol interactions; remote sensing; climate change ID DEEP CONVECTIVE CLOUDS; ASIAN SUMMER MONSOON; CONDENSATION NUCLEI CONCENTRATION; MESOSCALE CELLULAR STRUCTURES; SPECTRAL-RESOLUTION LIDAR; DROPLET EFFECTIVE RADIUS; BOUNDARY-LAYER CLOUDS; BIOMASS BURNING SMOKE; MODIS SATELLITE DATA; OPTICAL DEPTH AB Cloud drop condensation nuclei (CCN) and ice nuclei (IN) particles determine to a large extent cloud microstructure and, consequently, cloud albedo and the dynamic response of clouds to aerosol-induced changes to precipitation. This can modify the reflected solar radiation and the thermal radiation emitted to space. Measurements of tropospheric CCN and IN over large areas have not been possible and can be only roughly approximated from satellite-sensor-based estimates of optical properties of aerosols. Our lack of ability to measure both CCN and cloud updrafts precludes disentangling the effects of meteorology from those of aerosols and represents the largest component in our uncertainty in anthropogenic climate forcing. Ways to improve the retrieval accuracy include multiangle and multipolarimetric passive measurements of the optical signal and multispectral lidar polarimetric measurements. Indirect methods include proxies of trace gases, as retrieved by hyperspectral sensors. Perhaps the most promising emerging direction is retrieving the CCN properties by simultaneously retrieving convective cloud drop number concentrations and updraft speeds, which amounts to using clouds as natural CCN chambers. These satellite observations have to be constrained by in situ observations of aerosol-cloud-precipitation-climate (ACPC) interactions, which in turn constrain a hierarchy of model simulations of ACPC. Since the essence of a general circulation model is an accurate quantification of the energy and mass fluxes in all forms between the surface, atmosphere and outer space, a route to progress is proposed here in the form of a series of box flux closure experiments in the various climate regimes. A roadmap is provided for quantifying the ACPC interactions and thereby reducing the uncertainty in anthropogenic climate forcing. C1 [Rosenfeld, Daniel] Hebrew Univ Jerusalem, Inst Earth Sci, IL-91905 Jerusalem, Israel. [Andreae, Meinrat O.] Max Planck Inst Chem, Biogeochem Dept, D-55128 Mainz, Germany. [Asmi, Ari; de Leeuw, Gerrit; Kulmala, Markku; Suni, Tanja] Univ Helsinki, Dept Phys, Helsinki, Finland. [Chin, Mian; Kahn, Ralph; Lau, William] NASA Goddard Space Flight Ctr, Earth Sci Div, Greenbelt, MD USA. [de Leeuw, Gerrit; Kivekas, Niku] Finnish Meteorol Inst, Atmospher Composit Res Unit, FIN-00101 Helsinki, Finland. [Donovan, David P.] Royal Netherlands Meteorol Inst KNMI, Ae De Bilt, Netherlands. [Kinne, Stefan] Max Planck Inst Meteorol, D-20146 Hamburg, Germany. [Kivekas, Niku] Lund Univ, Dept Phys, Div Nucl Phys, S-22362 Lund, Sweden. [Schmidt, K. Sebastian] Univ Colorado Boulder, Lab Atmospher & Space Phys, Boulder, CO USA. [Schmidt, K. Sebastian] Univ Colorado Boulder, Dept Atmospher & Ocean Sci, Boulder, CO USA. [Wagner, Thomas] Max Planck Inst Chem, Satellite Remote Sensing Grp, D-55128 Mainz, Germany. [Wild, Martin] Swiss Fed Inst Technol, Inst Atmospher & Climate Sci, Zurich, Switzerland. [Quaas, Johannes] Univ Leipzig, Inst Meteorol, D-04109 Leipzig, Germany. RP Rosenfeld, D (reprint author), Hebrew Univ Jerusalem, Inst Earth Sci, IL-91905 Jerusalem, Israel. EM daniel@huji.ac.il RI Wild, Martin/J-8977-2012; Rosenfeld, Daniel/F-6077-2016; Quaas, Johannes/I-2656-2013; Kulmala, Markku/I-7671-2016; SCHMIDT, KONRAD SEBASTIAN/C-1258-2013; Chin, Mian/J-8354-2012; Andreae, Meinrat/B-1068-2008 OI Rosenfeld, Daniel/0000-0002-0784-7656; Quaas, Johannes/0000-0001-7057-194X; Kulmala, Markku/0000-0003-3464-7825; SCHMIDT, KONRAD SEBASTIAN/0000-0003-3899-228X; Andreae, Meinrat/0000-0003-1968-7925 FU International Space Science Institute (ISSI); IGBP core project iLEAPS (Integrated Land-Ecosystem - Atmosphere Processes Study); IGBP core project IGAC (International Global Atmospheric Chemistry); aerosol Climate Change Initiative (CCI) project - European Space Agency (ESA), ESA Climate Change Initiative FX The authors gratefully acknowledge the financial and programmatic support provided by the International Space Science Institute (ISSI), the IGBP core projects iLEAPS (Integrated Land-Ecosystem - Atmosphere Processes Study) and IGAC (International Global Atmospheric Chemistry), and the aerosol Climate Change Initiative (CCI) project funded by the European Space Agency (ESA) as part of the ESA Climate Change Initiative. NR 374 TC 34 Z9 35 U1 27 U2 133 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 8755-1209 EI 1944-9208 J9 REV GEOPHYS JI Rev. Geophys. PD DEC PY 2014 VL 52 IS 4 BP 750 EP 808 DI 10.1002/2013RG000441 PG 59 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AZ8GA UT WOS:000348452000005 ER PT J AU Golombek, MP Warner, NH Ganti, V Lamb, MP Parker, TJ Fergason, RL Sullivan, R AF Golombek, M. P. Warner, N. H. Ganti, V. Lamb, M. P. Parker, T. J. Fergason, R. L. Sullivan, R. TI Small crater modification on Meridiani Planum and implications for erosion rates and climate change on Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; erosion; climate; crater modification; erosion rate ID SMALL IMPACT CRATERS; ROVER LANDING SITE; MARTIAN HIGHLANDS; DEPOSITS; DENUDATION; SEDIMENT; SLOPE; MORPHOMETRY; OPPORTUNITY; EVOLUTION AB A morphometric and morphologic catalog of similar to 100 small craters imaged by the Opportunity rover over the 33.5km traverse between Eagle and Endeavour craters on Meridiani Planum shows craters in six stages of degradation that range from fresh and blocky to eroded and shallow depressions ringed by planed off rim blocks. The age of each morphologic class from < 50-200ka to similar to 20Ma has been determined from the size-frequency distribution of craters in the catalog, the retention age of small craters on Meridiani Planum, and the age of the latest phase of ripple migration. The rate of degradation of the craters has been determined from crater depth, rim height, and ejecta removal over the class age. These rates show a rapid decrease from 1m/Myr for craters < 1Ma to similar to < 0.1m/Myr for craters 10-20Ma, which can be explained by topographic diffusion with modeled diffusivities of similar to 10(-6)m(2)/yr. In contrast to these relatively fast, short-term erosion rates, previously estimated average erosion rates on Mars over 100 Myr and 3 Gyr timescales from the Amazonian and Hesperian are of order < 0.01m/Myr, which is 3-4 orders of magnitude slower than typical terrestrial rates. Erosion rates during the Middle-Late Noachian averaged over similar to 250 Myr, and similar to 700 Myr intervals are around 1m/Myr, comparable to slow terrestrial erosion rates calculated over similar timescales. This argues for a wet climate before similar to 3Ga in which liquid water was the erosional agent, followed by a dry environment dominated by slow eolian erosion. C1 [Golombek, M. P.; Warner, N. H.; Parker, T. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Warner, N. H.] SUNY Coll Geneseo, Dept Geol Sci, Geneseo, NY USA. [Ganti, V.; Lamb, M. P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Fergason, R. L.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Sullivan, R.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Golombek, MP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM mgolombek@jpl.nasa.gov FU NASA [NNX13AM83G]; NSF NCED2 program FX Research described in this paper was carried out by the Mars Exploration Rover Project, Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. All data from the Opportunity rover and HiRISE are available from the NASA Planetary Data System. N. Warner was supported by the NASA Postdoctoral Program. M. Lamb was supported by NASA grant NNX13AM83G. V. Ganti was supported by NSF NCED2 program. We thank Brad Jolliff for help with the crater catalog, John Grant for data on Eagle, Endurance, Victoria, and Santa Maria craters, Jane Willenbring for discussions on timescale bias in erosion rates, C. Fassett, T. Platz, R. Anderson, and P. Geissler for reviews, and V. Carranza, C. Schwartz, and E. Bondi for help with the figures. NR 92 TC 13 Z9 13 U1 5 U2 19 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC PY 2014 VL 119 IS 12 BP 2522 EP 2547 DI 10.1002/2014JE004658 PG 26 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AZ8GJ UT WOS:000348453000007 ER PT J AU Ho, K de Weck, OL Hoffman, JA Shishko, R AF Ho, Koki de Weck, Olivier L. Hoffman, Jeffrey A. Shishko, Robert TI Dynamic modeling and optimization for space logistics using time-expanded networks SO ACTA ASTRONAUTICA LA English DT Article DE Space systems; Space logistics; Mars exploration; Network optimization; Time-expanded network ID ARCHITECTURES; PROPELLANT AB This research develops a dynamic logistics network formulation for lifecycle optimization of mission sequences as a system-level integrated method to find an optimal combination of technologies to be used at each stage of the campaign. This formulation can find the optimal transportation architecture considering its technology trades over time. The proposed methodologies are inspired by the ground logistics analysis techniques based on linear programming network optimization. Particularly, the time-expanded network and its extension are developed for dynamic space logistics network optimization trading the quality of the solution with the computational load. In this paper, the methodologies are applied to a human Mars exploration architecture design problem. The results reveal multiple dynamic system-level trades over time and give recommendation of the optimal strategy for the human Mars exploration architecture. The considered trades include those between In-Situ Resource Utilization (ISRU) and propulsion technologies as well as the orbit and depot location selections over time. This research serves as a precursor for eventual permanent settlement and colonization of other planets by humans and us becoming a multi-planet species. (C) 2014 IAA. Published by Elsevier Ltd. All rights reserved. C1 [Ho, Koki; de Weck, Olivier L.; Hoffman, Jeffrey A.] MIT, Cambridge, MA 02139 USA. [Shishko, Robert] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Ho, K (reprint author), MIT, Cambridge, MA 02139 USA. EM koki_ho@mit.edu; deweck@mit.edu; jhoffma1@mit.edu; robert.shishko@jpl.nasa.gov FU Funai Foundation for Information and Technology FX The first author, K. Ho, is grateful to Funai Foundation for Information and Technology for support for this research through a graduate student scholarship. NR 32 TC 4 Z9 4 U1 0 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD DEC PY 2014 VL 105 IS 2 BP 428 EP 443 DI 10.1016/j.actaastro.2014.10.026 PG 16 WC Engineering, Aerospace SC Engineering GA AY7WQ UT WOS:000347767100006 ER PT J AU Badavi, FF Nealy, JE AF Badavi, Francis F. Nealy, John E. TI A deterministic computational model for the two dimensional electron and photon transport SO ACTA ASTRONAUTICA LA English DT Article DE Electron photon transport; Space radiation; Cross section ID ORBIT AB A deterministic (non-statistical) two dimensional (2D) computational model describing the transport of electron and photon typical of space radiation environment in various shield media is described. The 2D formalism is casted into a code which is an extension of a previously developed one dimensional (1D) deterministic electron and photon transport code. The goal of both 10 and 2D codes is to satisfy engineering design applications (i.e. rapid analysis) while maintaining an accurate physics based representation of electron and photon transport in space environment. Both 10 and 20 transport codes have utilized established theoretical representations to describe the relevant collisional and radiative interactions and transport processes. In the 20 version, the shield material specifications are made more general as having the pertinent cross sections. In the 20 model, the specification of the computational field is in terms of a distance of traverse z along an axial direction as well as a variable distribution of deflection (i.e. polar) angles theta where -pi/2 0.15) for non-X-ray sources. More specifically, we obtain sigma(NMAD) = 0.024 with 2.7% outliers for sources brighter than R = 23 mag, sigma(NMAD) = 0.035 with 7.4% outliers for sources fainter than R = 23 mag, sigma(NMAD) = 0.026 with 3.9% outliers for sources having z < 1, and sigma(NMAD) = 0.034 with 9.0% outliers for sources having z > 1. Our Z(phot) quality shows an overall improvement over an earlier Z(phot) work that focused only on the central H-HDF-N area. We also classify each object as a star or galaxy through template spectral energy distribution fitting and complementary morphological parameterization, resulting in 4959 stars and 126,719 galaxies. Furthermore, we match our catalog with the 2 Ms Chandra Deep Field-North main X-ray catalog. For the 462 matched non-stellar X-ray sources (281 having Z(spec)), we improve their Z(phot) quality by adding three additional active galactic nucleus templates, achieving sigma(NMAD) = 0.035 and an outlier fraction of 12.5%. We make our catalog publicly available presenting both photometry and Z(phot), and provide guidance on how to make use of our catalog. C1 [Yang, G.; Xue, Y. Q.; Kong, X.; Wang, J. -X.; Yuan, Y. -F.; Zhou, H. Y.] Chinese Acad Sci, Univ Sci & Technol China, Key Lab Res Galaxies & Cosmol, Ctr Astrophys,Dept Astron, Hefei 230026, Anhui, Peoples R China. [Luo, B.; Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Luo, B.; Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, F. E.] Millennium Inst Astrophys, Santiago 7820436, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Cui, W.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Lehmer, B. D.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Lehmer, B. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wu, X. -B.] Peking Univ, Dept Astron, Beijing 100871, Peoples R China. [Wu, X. -B.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Yuan, F.] Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China. [Zhou, H. Y.] Polar Res Inst China, Shanghai 200136, Peoples R China. RP Yang, G (reprint author), Chinese Acad Sci, Univ Sci & Technol China, Key Lab Res Galaxies & Cosmol, Ctr Astrophys,Dept Astron, Hefei 230026, Anhui, Peoples R China. EM yg1991@mail.ustc.edu.cn; xuey@ustc.edu.cn OI Yang, Guang/0000-0001-8835-7722 FU Thousand Young Talents (QingNianQianRen) program [KJ2030220004]; 973 Program [2015CB857004]; USTC startup funding [ZC9850290195]; National Natural Science Foundation of China [NSFC-11473026, 11421303, 11243008]; Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences [XDB09000000]; Fund for Fostering Talents in Basic Science of the National Natural Science Foundation of China [NSFC-J1310021]; CXC grant [AR3-14015X]; NASA ADP grant [NNX10AC99G]; UK Science and Technology Facilities Council (STFC) [ST/I001573/I]; Leverhulme Trust; Basal-CATA [PFB-06/2007]; CONICYT-Chile; FONDECYT [1141218]; Gemini-CONICYT [32120003]; "EMBIGGEN" Anillo [ACT1101]; Millennium Institute of Astrophysics (MAS) - Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo [IC120009] FX We thank the referee for helpful feedback that improved this work. We thank Matthew Ashby for advice on the use of SEDS data, Ryan Keenan for providing the J- and H-band images, Wei-Hao Wang for providing information on the Ks-band image, and Masami Ouchi for providing the zoband image. We are grateful to Gustavo Bruzual for providing the newest version of GALAXEV, to Russ Laher for his novel APT software, to Roberto Assef for the Low Resolution Templates code, and to Gabriel Brammer for the EAzY code. We also thank Tinggui Wang for helpful discussions. G. Y. and Y. Q. X. acknowledge the financial support of the Thousand Young Talents (QingNianQianRen) program (KJ2030220004), the 973 Program (2015CB857004), the USTC startup funding (ZC9850290195), the National Natural Science Foundation of China (NSFC-11473026, 11421303, 11243008), the Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences (XDB09000000), and the Fund for Fostering Talents in Basic Science of the National Natural Science Foundation of China (NSFC-J1310021). W. N. B. and B. L. acknowledge support from the CXC grant AR3-14015X and the NASA ADP grant NNX10AC99G. D. M. A acknowledges support from the UK Science and Technology Facilities Council (STFC, grant ST/I001573/I) and the Leverhulme Trust. F. E. B. acknowledges support from Basal-CATA PFB-06/2007, CONICYT-Chile (FONDECYT 1141218, Gemini-CONICYT 32120003, "EMBIGGEN" Anillo ACT1101), and Project IC120009 "Millennium Institute of Astrophysics (MAS)" funded by the Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo. NR 51 TC 3 Z9 3 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD DEC PY 2014 VL 215 IS 2 AR 27 DI 10.1088/0067-0049/215/2/27 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AY4IX UT WOS:000347542500012 ER PT J AU Asano, T Taoka, M Yamauchi, Y Everroad, RC Seto, Y Isobe, T Kamo, M Chosa, N AF Asano, Tsunaki Taoka, Masato Yamauchi, Yoshio Everroad, R. Craig Seto, Yosuke Isobe, Toshiaki Kamo, Masaharu Chosa, Naoyuki TI Re-examination of a alpha-chymotrypsin-solubilized laccase in the pupal cuticle of the silkworm, Bombyx mori: Insights into the regulation system for laccase activation during the ecdysis process SO INSECT BIOCHEMISTRY AND MOLECULAR BIOLOGY LA English DT Article DE Laccase; Activation; Phylogenetic analysis ID DROSOPHILA-MELANOGASTER; ANOPHELES-GAMBIAE; CUTICULAR PHENOLOXIDASE; MULTICOPPER OXIDASE; TRIBOLIUM-CASTANEUM; TOBACCO HORNWORM; MANDUCA-SEXTA; PURIFICATION; EXPRESSION; PEPTIDES AB The laccase in the pupal cuticle of the silkworm, Bombyx mori, is thought to accumulate as an inactive precursor that can be activated stage-dependently. In this study we isolated an 81-kDa laccase from cuticular extract of B. mori that was prepared by digestion of the pupal cuticles with alpha-chymotrypsin. The mass spectrometric analysis of the purified protein indicates that this 81-kDa laccase is a product of the Bombyx laccase2 gene. The purified 81-kDa laccase (alpha-chymotrypsin-solubilized Bombyx laccase2: Bm-clac2) has an N-terminal sequence of RNPADS that corresponds to Arg(146) to Ser(151) of the deduced protein sequence of Bmlaccase2 cDNA, indicating that Bm-clac2 lacks the N-terminal part upstream from residue Arg(146). Bm-clac2 shows enzymatic activity, but its specific activity is increased around 17-fold after treatment with trypsin, which involves cleavage of peptide bonds at the C-terminal region. We also found that the activity of Bm-clac2 is increased in the presence of isopropanol. In previous reports, proteolytic processing has been hypothesized as a system for laccase activation in vivo, but the present result implies that this type of processing is not the only way to convert Bm-clac2 to the high-activity enzyme. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Asano, Tsunaki; Seto, Yosuke] Tokyo Metropolitan Univ, Dept Biol Sci, Hachioji, Tokyo 1920397, Japan. [Taoka, Masato; Yamauchi, Yoshio; Isobe, Toshiaki] Tokyo Metropolitan Univ, Dept Chem, Hachioji, Tokyo 1920397, Japan. [Everroad, R. Craig] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. [Kamo, Masaharu; Chosa, Naoyuki] Iwate Med Univ, Dept Biochem, Div Cellular Biosignal Sci, Yahaba, Iwate 0283694, Japan. RP Asano, T (reprint author), Tokyo Metropolitan Univ, Dept Biol Sci, Hachioji, Tokyo 1920397, Japan. EM asano-tsunaki@tmu.ac.jp RI Chosa, Naoyuki/G-5538-2014; OI Chosa, Naoyuki/0000-0002-5399-2061; Kamo, Masaharu/0000-0001-6791-8754; Taoka, Masato/0000-0001-5554-4951 FU Japanese Ministry of Education, Culture, Sports and Technology [16780038] FX We thank Dr. Hiroko Yamazaki for her valuable experience and advice on laccase experiments, Dr. Masaaki Ashida for encouragement and research suggestions, Dr. Masanori Ochiai for N-terminal sequencing, Mr.Kazuhiro Kusunoki for the help of experiments in early stage of this study, Dr. Toshiro Aigaki for advice, Dr. Michael Kanost, Dr. Maureen Gorman and Dr. Neal Dittmer for valuable discussion about MCOs including the laccase2 of insects. This work was supported by grant (16780038) from the Japanese Ministry of Education, Culture, Sports and Technology. NR 40 TC 2 Z9 2 U1 2 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0965-1748 EI 1879-0240 J9 INSECT BIOCHEM MOLEC JI Insect Biochem. Mol. Biol. PD DEC PY 2014 VL 55 BP 61 EP 69 DI 10.1016/j.ibmb.2014.10.004 PG 9 WC Biochemistry & Molecular Biology; Entomology SC Biochemistry & Molecular Biology; Entomology GA AY5HF UT WOS:000347602700008 PM 25460512 ER PT J AU Capece, AM Polk, JE Shepherd, JE AF Capece, Angela M. Polk, James E. Shepherd, Joseph E. TI X-ray photoelectron spectroscopy study of BaWO4 and Ba2CaWO6 SO JOURNAL OF ELECTRON SPECTROSCOPY AND RELATED PHENOMENA LA English DT Article DE XPS; Barium; Tungsten; Calcium; Tungstate ID NANORODS AB XPS reference spectra for Ba2CaWO6 and BaWO4 are presented, including high resolution spectra of the Ba 3d, W 4f, C 1s, Ca 2p, and O 1s lines. The peak locations and full widths at half maximum are also given. The binding energies of the Ba 3d and W 4f lines are 0.7 eV higher for BaWO4 than for Ba2CaWO6. The Ca 2p spectrum contains two sets of Ca 2p doublets that were attributed to Ba2CaWO6 and CaCO3. (C) 2014 Elsevier B.V. All rights reserved. C1 [Capece, Angela M.; Shepherd, Joseph E.] CALTECH, Pasadena, CA 91125 USA. [Polk, James E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Capece, AM (reprint author), Princeton Plasma Phys Lab, POB 451, Princeton, NJ 08543 USA. EM acapece@pppl.gov RI Shepherd, Joseph/B-5997-2014 OI Shepherd, Joseph/0000-0003-3181-9310 FU National Aeronautics and Space Administration FX The research described in this paper was carried out by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 11 TC 0 Z9 0 U1 1 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0368-2048 EI 1873-2526 J9 J ELECTRON SPECTROSC JI J. Electron Spectrosc. Relat. Phenom. PD DEC PY 2014 VL 197 BP 102 EP 105 DI 10.1016/j.elspec.2014.10.001 PG 4 WC Spectroscopy SC Spectroscopy GA AY7SS UT WOS:000347759800016 ER PT J AU Schiffbauer, JD Xiao, SH Cai, YP Wallace, AF Hua, H Hunter, J Xu, HF Peng, YB Kaufman, AJ AF Schiffbauer, James D. Xiao, Shuhai Cai, Yaoping Wallace, Adam F. Hua, Hong Hunter, Jerry Xu, Huifang Peng, Yongbo Kaufman, Alan J. TI A unifying model for Neoproterozoic-Palaeozoic exceptional fossil preservation through pyritization and carbonaceous compression SO NATURE COMMUNICATIONS LA English DT Article ID BURGESS SHALE-TYPE; BEECHERS TRILOBITE BED; SOFT-BODIED FOSSILS; SOUTHERN SHAANXI; GAOJIASHAN LAGERSTATTE; PYRITE FORMATION; ORGANIC-MATTER; HUNSRUCK SLATE; CLAY-MINERALS; IRON MINERALS AB Soft-tissue fossils capture exquisite biological detail and provide our clearest views onto the rise of animals across the Ediacaran-Cambrian transition. The processes contributing to fossilization of soft tissues, however, have long been a subject of debate. The Ediacaran Gaojiashan biota displays soft-tissue preservational styles ranging from pervasive pyritization to carbonaceous compression, and thus provides an excellent opportunity to dissect the relationships between these taphonomic pathways. Here geochemical analyses of the Gaojiashan fossil Conotubus hemiannulatus show that pyrite precipitation was fuelled by the degradation of labile tissues through bacterial sulfate reduction (BSR). Pyritization initiated with nucleation on recalcitrant tube walls, proceeded centripetally, decelerated with exhaustion of labile tissues and possibly continued beneath the BSR zone. We propose that pyritization and kerogenization are regulated principally by placement and duration of the decaying organism in different microbial zones of the sediment column, which hinge on post-burial sedimentation rate and/or microbial zone thickness. C1 [Schiffbauer, James D.] Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. [Xiao, Shuhai] Virginia Tech, Dept Geosci, Blacksburg, VA 24061 USA. [Cai, Yaoping; Hua, Hong] NW Univ Xian, Early Life Inst, State Key Lab Continental Dynam, Xian 710069, Peoples R China. [Cai, Yaoping; Hua, Hong] NW Univ Xian, Dept Geol, Xian 710069, Peoples R China. [Wallace, Adam F.] Univ Delaware, Dept Geol Sci, Newark, DE 19716 USA. [Hunter, Jerry] Virginia Tech, Inst Crit Technol & Appl Sci, Nanoscale Characterizat & Fabricat Lab, Blacksburg, VA 24061 USA. [Xu, Huifang] Univ Wisconsin, Dept Geosci, NASA, Astrobiol Inst, Madison, WI 53706 USA. [Peng, Yongbo] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA. [Kaufman, Alan J.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Kaufman, Alan J.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. RP Schiffbauer, JD (reprint author), Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. EM schiffbauerj@missouri.edu RI Xiao, Shuhai/A-2190-2009 OI Xiao, Shuhai/0000-0003-4655-2663 FU NASA Exobiology and Evolutionary Biology Program, NASA Astrobiology Institute [N07-5489]; National Science Foundation [EAR-0824890, EAR095800, EAR1124062]; Chinese Academy of Sciences, National Natural Science Foundation of China [41202006, 41030209, 41272011]; Chinese Ministry of Science and Technology, Virginia Tech Institute for Critical Technology and Applied Sciences; China Postdoctoral Science Foundation [2013M531410] FX This research was supported by funding through NASA Exobiology and Evolutionary Biology Program, NASA Astrobiology Institute (N07-5489), National Science Foundation (EAR-0824890, EAR095800, EAR1124062), Chinese Academy of Sciences, National Natural Science Foundation of China (41202006; 41030209; 41272011), Chinese Ministry of Science and Technology, Virginia Tech Institute for Critical Technology and Applied Sciences and China Postdoctoral Science Foundation (2013M531410). We would like to thank K.L. Shelton and J.W. Huntley for insightful discussion. NR 67 TC 19 Z9 19 U1 4 U2 27 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 DEC PY 2014 VL 5 AR 5754 DI 10.1038/ncomms6754 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AY5KT UT WOS:000347611700003 PM 25517864 ER PT J AU Zenitani, S Hesse, M Klimas, A Black, C Kuznetsova, M AF Zenitani, Seiji Hesse, Michael Klimas, Alex Black, Carrie Kuznetsova, Masha TI The inner structure of collisionless magnetic reconnection: The electron-frame dissipation measure and Hall fields (vol 18, 122108, 2011) SO PHYSICS OF PLASMAS LA English DT Correction C1 [Zenitani, Seiji; Hesse, Michael; Klimas, Alex; Black, Carrie; Kuznetsova, Masha] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Zenitani, S (reprint author), Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. EM seiji.zenitani@nao.ac.jp RI NASA MMS, Science Team/J-5393-2013 OI NASA MMS, Science Team/0000-0002-9504-5214 NR 2 TC 0 Z9 0 U1 0 U2 3 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD DEC PY 2014 VL 21 IS 12 AR 129906 DI 10.1063/1.4905516 PG 1 WC Physics, Fluids & Plasmas SC Physics GA AX8ME UT WOS:000347162700122 ER PT J AU Coustenis, A Atreya, S Castillo, J Coll, P Mueller-Wodarg, I Spilker, L AF Coustenis, A. Atreya, S. Castillo, J. Coll, P. Mueller-Wodarg, I. Spilker, L. TI Surfaces, atmospheres and magnetospheres of the outer planets and their satellites and ring systems: Part X Preface SO PLANETARY AND SPACE SCIENCE LA English DT Editorial Material C1 [Coustenis, A.] LESIA, Paris Meudon Observ, F-92195 Meudon, France. [Atreya, S.] Univ Michigan, Ann Arbor, MI 48109 USA. [Castillo, J.] JPLCaltech, Pasadena, CA USA. [Coll, P.] Univ Paris 07, LISA, CNRS, Paris Est Creteil, Creteil, France. [Mueller-Wodarg, I.] Univ London Imperial Coll Sci Technol & Med, London, England. [Spilker, L.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Coustenis, A (reprint author), LESIA, Paris Meudon Observ, F-92195 Meudon, France. EM athena.coustenis@obspm.fr NR 0 TC 0 Z9 0 U1 0 U2 1 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 DEC PY 2014 VL 104 SI SI BP 1 EP 2 DI 10.1016/j.pss.2014.11.002 PN A PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AY5AH UT WOS:000347585400001 ER PT J AU Mousis, O Fletcher, LN Lebreton, JP Wurz, P Cavaliee, T Coustenis, A Courtin, R Gautier, D Helled, R Irwin, PGJ Morse, AD Nettelmann, N Marty, B Rousselot, P Venot, O Atkinson, DH Waite, JH Reh, KR Simon, AA Atreya, S Andre, N Blanc, M Daglis, IA Fischer, G Geppertt, WD Guillot, T Hedman, MM Hueso, R Lellouch, E Lunine, JI Murray, CD O'Donoghue, J Rengel, M Sanchez-Lavega, A Schmider, FX Spiga, A Spilker, T Petit, JM Tiscareno, MS Ali-Dib, M Altwegg, K Bolton, SJ Bouquet, A Briois, C Fouchet, T Guerlet, S Kostiuk, T Lebleu, D Moreno, R Orton, GS Poncy, J AF Mousis, O. Fletcher, L. N. Lebreton, J. P. Wurz, P. Cavalie, T. Coustenis, A. Courtin, R. Gautier, D. Helled, R. Irwin, P. G. J. Morse, A. D. Nettelmann, N. Marty, B. Rousselot, P. Venot, O. Atkinson, D. H. Waite, J. H. Reh, K. R. Simon, A. A. Atreya, S. Andre, N. Blanc, M. Daglis, I. A. Fischer, G. Geppertt, W. D. Guillot, T. Hedman, M. M. Hueso, R. Lellouch, E. Lunine, J. I. Murray, C. D. O'Donoghue, J. Rengel, M. Sanchez-Lavega, A. Schmider, F. X. Spiga, A. Spilker, T. Petit, J. -M. Tiscareno, M. S. Ali-Dib, M. Altwegg, K. Bolton, S. J. Bouquet, A. Briois, C. Fouchet, T. Guerlet, S. Kostiuk, T. Lebleu, D. Moreno, R. Orton, G. S. Poncy, J. TI Scientific rationale for Saturn's in situ exploration SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Entry probe; Saturn atmosphere; Giant planet formation; Solar system formation; In situ measurements; Elemental and isotopic composition ID PROBE MASS-SPECTROMETER; ISO-SWS OBSERVATIONS; HELIUM INTERFEROMETER EXPERIMENT; DOPPLER WIND EXPERIMENT; GIANT PLANETS; JUPITERS ATMOSPHERE; CASSINI/CIRS OBSERVATIONS; SPATIAL-DISTRIBUTION; POLAR NEPHELOMETER; JOVIAN ATMOSPHERE AB Remote sensing observations meet some limitations when used to study the bulk atmospheric composition of the giant planets of our solar system. A remarkable example of the superiority of in situ probe measurements is illustrated by the exploration of Jupiter, where key measurements such as the determination of the noble gases' abundances and the precise measurement of the helium mixing ratio have only been made available through in situ measurements by the Galileo probe. This paper describes the main scientific goals to be addressed by the future in situ exploration of Saturn placing the Galileo probe exploration of Jupiter in a broader context and before the future probe exploration of the more remote ice giants. In situ exploration of Saturn's atmosphere addresses two broad themes that are discussed throughout this paper: first, the formation history of our solar system and second, the processes at play in planetary atmospheres. In this context, we detail the reasons why measurements of Saturn's bulk elemental and isotopic composition would place important constraints on the volatile reservoirs in the protosolar nebula. We also show that the in situ measurement of CO (or any other disequilibrium species that is depleted by reaction with water) in Saturn's upper troposphere may help constraining its bulk O/H ratio. We compare predictions of Jupiter and Saturn's bulk compositions from different formation scenarios, and highlight the key measurements required to distinguish competing theories to shed light on giant planet formation as a common process in planetary systems with potential applications to most extrasolar systems. In situ measurements of Saturn's stratospheric and tropospheric dynamics, chemistry and cloud-forming processes will provide access to phenomena unreachable to remote sensing studies. Different mission architectures are envisaged, which would benefit from strong international collaborations, all based on an entry probe that would descend through Saturn's stratosphere and troposphere under parachute down to a minimum of 10 bar of atmospheric pressure. We finally discuss the science payload required on a Saturn probe to match the measurement requirements. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Mousis, O.; Rousselot, P.; Petit, J. -M.; Ali-Dib, M.; Bouquet, A.] Univ Franche Comte, Inst UTINAM, CNRS INSU, Observ Sci Univ Besancon,UMR 6213, F-25030 Besancon, France. [Fletcher, L. N.; Irwin, P. G. J.] Univ Oxford, Clarendon Lab, Dept Phys, Oxford OX1 3PU, England. [Lebreton, J. P.; Briois, C.] Univ Orleans, CNRS, LPC2E, F-45071 Orleans 2, France. [Lebreton, J. P.; Coustenis, A.; Courtin, R.; Gautier, D.; Lellouch, E.; Fouchet, T.; Moreno, R.] Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris, F-92195 Meudon, France. [Wurz, P.; Altwegg, K.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Cavalie, T.; Rengel, M.] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany. [Helled, R.] Tel Aviv Univ, Dept Geophys Atmospher & Planetary Sci, IL-69978 Tel Aviv, Israel. [Morse, A. D.] Open Univ, Dept Phys, Milton Keynes MK7 6AA, Bucks, England. [Nettelmann, N.] Univ Rostock, Inst Phys, D-18051 Rostock, Germany. [Marty, B.] Nancy Univ, CNRS, CRPG, F-54501 Vandoeuvre Les Nancy, France. [Venot, O.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Leuven, Belgium. [Atkinson, D. H.] Univ Idaho, Dept Elect & Comp Engn, Moscow, ID 83844 USA. [Waite, J. H.; Bolton, S. J.; Bouquet, A.] Southwest Res Inst SwRI, San Antonio, TX 78228 USA. [Atkinson, D. H.; Reh, K. R.; Orton, G. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Simon, A. A.; Kostiuk, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Atreya, S.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Andre, N.; Blanc, M.] Univ Toulouse 3, CNRS, IRAP, UMR 5277, F-31028 Toulouse 4, France. [Daglis, I. A.] Univ Athens, Dept Phys, Athens 15784, Greece. [Fischer, G.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria. [Geppertt, W. D.] Stockholm Univ, Dept Phys, Astrobiol Ctr, AlbaNova, S-10691 Stockholm, Sweden. [Guillot, T.; Schmider, F. X.] Observ Cote Azur, Lab Lagrange, F-06304 Nice 4, France. [Hedman, M. M.] Univ Idaho, Dept Phys, Moscow, ID 83843 USA. [Hueso, R.; Sanchez-Lavega, A.] UPV, EHU, Dept Fis Aplicada 1, ETS Ingn, Bilbao 48013, Spain. [Hueso, R.; Sanchez-Lavega, A.] CSIC, Unidad Asociada Grp Ciencias Planetarias UPV EHU, Bilbao 48013, Spain. [Lunine, J. I.; Tiscareno, M. S.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Murray, C. D.] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England. [O'Donoghue, J.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Spiga, A.; Guerlet, S.] Univ Paris 06, Inst Pierre Simon Laplace, Lab Meteorol Dynam, Paris, France. [Spilker, T.] Solar Syst Sci & Explorat, Monrovia, CA USA. [Lebleu, D.; Poncy, J.] Thales Alenia Space, Cannes, France. RP Mousis, O (reprint author), Univ Franche Comte, Inst UTINAM, CNRS INSU, Observ Sci Univ Besancon,UMR 6213, F-25030 Besancon, France. EM olivier.mousis@obs-besancon.fr RI Daglis, Ioannis/L-6100-2013; Fletcher, Leigh/D-6093-2011; Fouchet, Thierry/C-6374-2017; Simon, Amy/C-8020-2012; Spiga, Aymeric/O-4858-2014 OI Daglis, Ioannis/0000-0002-0764-3442; Fletcher, Leigh/0000-0001-5834-9588; Fouchet, Thierry/0000-0001-9040-8285; Irwin, Patrick/0000-0002-6772-384X; Simon, Amy/0000-0003-4641-6186; Spiga, Aymeric/0000-0002-6776-6268 FU CNES; Royal Society Research Fellowship at the University of Oxford; Swiss National Science Foundation; KU Leuven IDO project [IDO/10/2013]; FWO; Spanish MICIIN [AYA2012-36666, PRICIT-S2009/ESP-1496]; Grupos Gobierno Vasco [IT765-13, UPV/EHU UFI11/55]; Austrian Science Fund FWF [P24325-N16] FX O.M. acknowledges support from CNES. L.N.F. was supported by a Royal Society Research Fellowship at the University of Oxford. P. W. acknowledges support from the Swiss National Science Foundation. O.V. acknowledges support from the KU Leuven IDO project IDO/10/2013 and from the FWO Postdoctoral Fellowship program. A.S.L. and R.H. were supported by the Spanish MICIIN project AYA2012-36666 with FEDER support, PRICIT-S2009/ESP-1496, Grupos Gobierno Vasco IT765-13 and UPV/EHU UFI11/55, G.F. acknowledges support from the Austrian Science Fund FWF via project P24325-N16. NR 163 TC 8 Z9 8 U1 0 U2 17 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD DEC PY 2014 VL 104 SI SI BP 29 EP 47 DI 10.1016/j.pss.2014.09.014 PN A PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AY5AH UT WOS:000347585400004 ER PT J AU Tobie, G Teanby, NA Coustenis, A Jaumann, R Raulin, E Schmidt, J Carrasco, N Coates, A Cordier, D De Kok, R Geppert, WD Lebreton, JP Lefevre, A Livengood, TA Mandt, KE Mitri, G Nimmo, F Nixon, CA Norman, L Pappalardo, RT Postberg, F Rodriguez, S SchuizeMakuch, D Soderblom, JM Solomonidou, A Stephan, K Stofan, ER Turtle, EP Wagner, RJ West, RA Westlake, JH AF Tobie, G. Teanby, N. A. Coustenis, A. Jaumann, R. Raulin, E. Schmidt, J. Carrasco, N. Coates, Aj. Cordier, D. De Kok, R. Geppert, W. D. Lebreton, J. -P. Lefevre, A. Livengood, T. A. Mandt, K. E. Mitri, G. Nimmo, F. Nixon, C. A. Norman, L. Pappalardo, R. T. Postberg, F. Rodriguez, S. SchuizeMakuch, D. Soderblom, J. M. Solomonidou, A. Stephan, K. Stofan, E. R. Turtle, E. P. Wagner, R. J. West, R. A. Westlake, J. H. TI Science goals and mission concept for the future exploration of Titan and Enceladus SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Titan; Enceladus; Atmosphere; Surface; Ocean; Interior; Missions ID CASSINI RADAR OBSERVATIONS; NEUTRAL MASS-SPECTROMETER; HUYGENS LANDING SITE; GEYSER-LIKE PLUMES; SATURNS E-RING; UPPER-ATMOSPHERE; SOUTH-POLE; POSSIBLE ORIGIN; ONTARIO LACUS; IN-SITU AB Saturn's moons, Titan and Enceladus, are two of the Solar System's most enigmatic bodies and are prime targets for future space exploration. Titan provides an analogue for many processes relevant to the Earth, more generally to outer Solar System bodies, and a growing host of newly discovered icy exoplanets. Processes represented include atmospheric dynamics, complex organic chemistry, meteorological cycles (with methane as a working fluid), astrobiology, surface liquids and lakes, geology, fluvial and aeolian erosion, and interactions with an external plasma environment. In addition, exploring Enceladus over multiple targeted flybys will give us a unique opportunity to further study the most active icy moon in our Solar System as revealed by Cassini and to analyse in situ its active plume with highly capable instrumentation addressing its complex chemistry and dynamics. Enceladus' plume likely represents the most accessible samples from an extra-terrestrial liquid water environment in the Solar system, which has far reaching implications for many areas of planetary and biological science. Titan with its massive atmosphere and Enceladus with its active plume are prime planetary objects in the Outer Solar System to perform in situ investigations. In the present paper, we describe the science goals and key measurements to be performed by a future exploration mission involving a Saturn-Titan orbiter and a Titan balloon, which was proposed to ESA in response to the call for definition of the science themes of the next Large-class mission in 2013. The mission scenario is built around three complementary science goals: (A) Titan as an Earth-like system; (B) Enceladus as an active cryovolcanic moon; and (C) Chemistry of Titan and Enceladus - clues for the origin of life. The proposed measurements would provide a step change in our understanding of planetary processes and evolution, with many orders of magnitude improvement in temporal, spatial, and chemical resolution over that which is possible with Cassini-Huygens. This mission concept builds upon the successes of Cassini-Huygens and takes advantage of previous mission heritage in both remote sensing and in situ measurement technologies. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Tobie, G.; Lefevre, A.; Mitri, G.] Univ Nantes, Lab Planetol & Geodynam Nantes, CNRS, UMR 6112, F-44322 Nantes, France. [Teanby, N. A.] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England. [Coustenis, A.; Solomonidou, A.] Univ Paris 06, Univ Paris 05, CNRS, LESIA Observ Paris, F-92195 Meudon, France. [Jaumann, R.; Stephan, K.; Wagner, R. J.] DLR, Inst Planetary Res, Berlin, Germany. [Raulin, E.] Univ Paris, CNRS, UMR 7583, Lab Interuniv Syst Atmospher,IPSL, F-94010 Creteil, France. [Schmidt, J.] Univ Potsdam, D-14469 Potsdam, Germany. [Carrasco, N.] Univ Versailles St Quentin, Univ Paris 06, CNRS, LATMOS, F-78280 Guyancourt, France. [Coates, Aj.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Cordier, D.] Univ Franche Comte, Inst UTINAM, CNRS INSU, UMR 6213,Observ Sri Univ THETA, F-25030 Besancon, France. [De Kok, R.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Geppert, W. D.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Lebreton, J. -P.] European Space Agcy, NL-2200 AG Noordwijk, Netherlands. [Livengood, T. A.; Nixon, C. A.; Stofan, E. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mandt, K. E.] SW Res Inst, Space & Sci Engn Div, San Antonio, TX 78238 USA. [Nimmo, F.] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Norman, L.] UCL, Dept Space & Climate Phys, Inst Origins, London WC1E 6BT, England. [Pappalardo, R. T.; West, R. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Postberg, F.] Heidelberg Univ, Inst Earth Sri, D-69120 Heidelberg, Germany. [Rodriguez, S.] Univ Paris 07, Lab AIM, CNRS, CPA,Ctr Orne IVIerisiers, F-91191 Gif Sur Yvette, France. [SchuizeMakuch, D.] Washington State Univ, Pullman, WA 99163 USA. [Soderblom, J. M.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Solomonidou, A.] Univ Athens, Dept Geol & Geoenvironm, Athens 15784, Greece. [Turtle, E. P.; Westlake, J. H.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA. RP Tobie, G (reprint author), Univ Nantes, Lab Planetol & Geodynam Nantes, CNRS, UMR 6112, F-44322 Nantes, France. EM gabriel.tobie@univ-nantes.fr; n.teanby@bristol.ac.uk RI Nixon, Conor/A-8531-2009; Coates, Andrew/C-2396-2008; Westlake, Joseph/G-2732-2015; Turtle, Elizabeth/K-8673-2012; Carrasco, Nathalie/D-2365-2012; Rodriguez, Sebastien/H-5902-2016; OI Nixon, Conor/0000-0001-9540-9121; Coates, Andrew/0000-0002-6185-3125; Westlake, Joseph/0000-0003-0472-8640; Turtle, Elizabeth/0000-0003-1423-5751; Carrasco, Nathalie/0000-0002-0596-6336; Rodriguez, Sebastien/0000-0003-1219-0641; Teanby, Nicholas/0000-0003-3108-5775; Mandt, Kathleen/0000-0001-8397-3315 FU European Research Council under the European Community's Seventh Framework Programme [259285]; UK Science and Technology Facilities Council; Leverhulme Trust; CNES FX The research leading to these results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013 Grant agreement no. 259285), UK Science and Technology Facilities Council, Leverhulme Trust and CNES. NR 179 TC 4 Z9 4 U1 8 U2 63 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 DEC PY 2014 VL 104 SI SI BP 59 EP 77 DI 10.1016/j.pss.2014.10.002 PN A PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AY5AH UT WOS:000347585400006 ER PT J AU Mitri, G Coustenis, A Fanchini, G Hayes, AG Less, L Khurana, K Lebreton, JP Lopes, RM Lorenz, RD Meriggiola, R Moriconi, ML Orosei, R Sotin, C Stofan, E Tobie, G Tokano, T Tosi, F AF Mitri, Giuseppe Coustenis, Athena Fanchini, Gilbert Hayes, Alex G. Less, Luciano Khurana, Krishan Lebreton, Jean-Pierre Lopes, Rosaly M. Lorenz, Ralph D. Meriggiola, Rachele Moriconi, Maria Luisa Orosei, Roberto Sotin, Christophe Stofan, Ellen Tobie, Gabriel Tokano, Tetsuya Tosi, Federico TI The exploration of Titan with an orbiter and a lake probe SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Titan ID CASSINI RADAR; METHANE CYCLE; HUYGENS PROBE; SURFACE; TOPOGRAPHY; ATMOSPHERE; ORIGIN; SHAPE; DUNES; FEATURES AB Fundamental questions involving the origin, evolution, and history of both Titan and the broader Saturnian system can be answered by exploring this satellite from an orbiter and also in situ. We present the science case for an exploration of Titan and one of its lakes from a dedicated orbiter and a lake probe. Observations from an orbit-platform can improve our understanding of Titan's geological processes, surface composition and atmospheric properties. Further, combined measurements of the gravity field, rotational dynamics and electromagnetic field can expand our understanding of the interior and evolution of Titan. An in situ exploration of Titan's lakes provides an unprecedented opportunity to understand the hydrocarbon cycle, investigate a natural laboratory for prebiotic chemistry and habitability potential, and study meteorological and marine processes in an exotic environment. We briefly discuss possible mission scenarios for a future exploration of Titan with an orbiter and a lake probe. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Mitri, Giuseppe] Univ Nantes, LPGNantes, UMR 6112, F-44322 Nantes, France. [Coustenis, Athena] Univ Paris Diderot, Univ Paris 06, CNRS, LESIA,Observ Paris, Meudon, France. [Fanchini, Gilbert] Smart Struct Solut Srl, Rome, Italy. [Hayes, Alex G.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Less, Luciano; Meriggiola, Rachele] Univ Roma La Sapienza, Dipartimento Ingn Meccan & Aerosp, I-00184 Rome, Italy. [Khurana, Krishan] Inst Geophys & Planetaiy Phys, Dept Earth & Space Sci, Los Angeles, CA USA. [Lebreton, Jean-Pierre] LPC2E CNRS, Paris, France. [Lebreton, Jean-Pierre] LESIA Obs, Paris, France. [Lopes, Rosaly M.; Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Lorenz, Ralph D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Moriconi, Maria Luisa] CNR, ISAC, Rome, Italy. [Orosei, Roberto] INAF, IRA, Bologna, Italy. [Stofan, Ellen] Proxemy Res, Rectortown, VA USA. [Tobie, Gabriel] CNRS, LPGNantes, UMR 6112, F-44322 Nantes, France. [Tokano, Tetsuya] Univ Cologne, Inst Geophys & Meteorol, Cologne, Germany. [Tosi, Federico] IAPS, Ist Nazl Astrofis INAF, Rome, Italy. RP Mitri, G (reprint author), Univ Nantes, LPGNantes, UMR 6112, 2 Rue Houssiniere, F-44322 Nantes, France. EM Giuseppe.Mitri@univ-nantes.fr RI moriconi, maria luisa/B-7201-2009; Lorenz, Ralph/B-8759-2016; Lopes, Rosaly/D-1608-2016; IESS, Luciano/F-4902-2011 OI Tosi, Federico/0000-0003-4002-2434; moriconi, maria luisa/0000-0003-2609-2620; Lorenz, Ralph/0000-0001-8528-4644; Lopes, Rosaly/0000-0002-7928-3167; IESS, Luciano/0000-0002-6230-5825 FU NASA FX The authors thank the Reviewer Jani Radebaugh for her constructive comments. Some of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 120 TC 5 Z9 5 U1 2 U2 24 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 DEC PY 2014 VL 104 SI SI BP 78 EP 92 DI 10.1016/j.pss.2014.07.009 PN A PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AY5AH UT WOS:000347585400007 ER PT J AU Masters, A Achilleos, N Agnor, CB Campagnola, S Charnoz, S Christophe, B Coates, AJ Fletcher, LN Jones, GH Lamy, L Marzari, F Nettelmann, N Ruiz, J Ambrosi, R Andre, N Bhardwaj, A Fortney, J Hansen, CJ Helled, R Moragas-Klostermeyer, G Orton, G Ray, L Reynaud, S Sergis, N Srama, R Volwerk, M AF Masters, A. Achilleos, N. Agnor, C. B. Campagnola, S. Charnoz, S. Christophe, B. Coates, A. J. Fletcher, L. N. Jones, G. H. Lamy, L. Marzari, F. Nettelmann, N. Ruiz, J. Ambrosi, R. Andre, N. Bhardwaj, A. Fortney, Jj. Hansen, C. J. Helled, R. Moragas-Klostermeyer, G. Orton, G. Ray, L. Reynaud, S. Sergis, N. Srama, R. Volwerk, M. TI Neptune and Triton: Essential pieces of the Solar System puzzle SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Neptune; Triton; Solar System exploration ID GIANT PLANETS; WAVE OBSERVATIONS; MAGNETIC-FIELDS; CLOUD STRUCTURE; DARK ENERGY; SURFACE AGE; RING ARCS; URANUS; DUST; SATELLITES AB The planet Neptune and its largest moon Triton hold the keys to major advances across multiple fields of Solar System science. The ice giant Neptune played a unique and important role in the process of Solar System formation, has the most meteorologically active atmosphere in the Solar System (despite its great distance from the Sun), and may be the best Solar System analogue of the dominant class of exoplanets detected to date. Neptune's moon Triton is very likely a captured Kuiper Belt object, holding the answers to questions about the icy dwarf planets that formed in the outer Solar System. Triton is geologically active, has a tenuous nitrogen atmosphere, and is predicted to have a subsurface ocean. However, our exploration of the Neptune system remains limited to a single spacecraft flyby, made by Voyager 2 in 1989. Here, we present the high-level science case for further exploration of this outermost planetary system, based on a white paper submitted to the European Space Agency (ESA) for the definition of the second and third large missions in the ESA Cosmic Vision Programme 2015-2025. We discuss all the major science themes that are relevant for further spacecraft exploration of the Neptune system, and identify key scientific questions in each area. We present an overview of the results of a European-led Neptune orbiter mission analysis. Such a mission has significant scope for international collaboration, and is essential to achieve our aim of understanding how the Solar System formed, and how it works today. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Masters, A.; Campagnola, S.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Achilleos, N.; Ray, L.] UCL, Dept Phys & Astron, Atmospher Phys Lab, London WC1E 6BT, England. [Achilleos, N.; Coates, A. J.; Jones, G. H.; Ray, L.] UCL Birkbeck, Ctr Planetary Sci, London WC1E 6BT, England. [Agnor, C. B.] Queen Mary Univ London, Sch Phys & Astron, Astron Unit, London E1 4NS, England. [Charnoz, S.] Univ Paris Diderot, CEA, CNRS, Lab AIM, F-91191 Gif Sur Yvette, France. [Charnoz, S.] Inst Univ France, F-75005 Paris, France. [Christophe, B.] Off Natl Etud & Rech Aerosp, French Aerosp Lab, F-92322 Chatillon, France. [Coates, A. J.; Jones, G. H.] Univ Coll London, Dept Space & Climate Phys, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Fletcher, L. N.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. [Lamy, L.] Univ Paris Diderot, Univ Pierre & Marie Curie, CNRS, LESIA,Obsenrv Paris, Meudon, France. [Marzari, F.] Univ Padua, Dipartimento Fis, I-35131 Padua, Italy. [Nettelmann, N.; Fortney, Jj.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Ruiz, J.] Univ Complutense Madrid, Fac Ciencias Geol, Dept Geodinam, Madrid 28040, Spain. [Ambrosi, R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Andre, N.] Univ Paul Sabatier Toulouse, CNRS, IRAP, Toulouse, France. [Bhardwaj, A.] Vikram Sarabhai Space Ctr, Space Phys Lab, Trivandrum 695022, Kerala, India. [Hansen, C. J.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Helled, R.] Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. [Moragas-Klostermeyer, G.; Srama, R.] Univ Stuttgart, Inst Raumfahrtsyst, D-70569 Stuttgart, Germany. [Orton, G.] CALTECH, Jet Prop Lab, MS 169237, Pasadena, CA 91109 USA. [Reynaud, S.] CNRS, UPMC, ENS, LKB, F-75252 Paris 05, France. [Sergis, N.] Acad Athens, Off Space Res & Technol, Athens 1527, Greece. [Volwerk, M.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria. RP Masters, A (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan. EM a.masters@stp.isas.jaxa.jp RI Ruiz, Javier/P-3975-2015; Sergis, Nick/A-9881-2015; Fletcher, Leigh/D-6093-2011; Reynaud, Serge/J-8061-2014; Coates, Andrew/C-2396-2008 OI Jones, Geraint/0000-0002-5859-1136; Ruiz, Javier/0000-0002-3937-8380; Achilleos, Nicholas/0000-0002-5886-3509; Bhardwaj, Anil/0000-0003-1693-453X; Fletcher, Leigh/0000-0001-5834-9588; Reynaud, Serge/0000-0002-1494-696X; Coates, Andrew/0000-0002-6185-3125 FU JAXA International Top Young Fellowship Programme; Royal Society Research Fellowship at the University of Oxford FX We are very grateful to more than 100 scientists around the world who supported the white paper on Neptune-Triton science that was submitted to ESA in May 2013 for the definition of the second and third large missions in the Cosmic Vision Programme 2015-2025. AM and SC acknowledge the support of the JAXA International Top Young Fellowship Programme. LNF was supported by a Royal Society Research Fellowship at the University of Oxford. NR 113 TC 4 Z9 4 U1 4 U2 33 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 DEC PY 2014 VL 104 SI SI BP 108 EP 121 DI 10.1016/j.pss.2014.05.008 PN A PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AY5AH UT WOS:000347585400009 ER PT J AU Arridge, CS Achilleos, N Agarwal, J Agnor, CB Ambrosi, R Andre, N Badman, SV Baines, K Banfield, D Barthelemy, M Bisi, MM Blum, J Bocanegra-Bahamon, T Bonfond, B Bracken, C Brandt, P Briand, C Briois, C Brooks, S Castillo-Rogez, J Cavalie, T Christophe, B Coates, AJ Collinson, G Cooper, JF Costa-Sitja, M Courtin, R Daglis, IA De Pater, I Desai, M Dirkx, D Dougherty, MK Ebert, RW Filacchione, G Fletcher, LN Fortney, J Gerth, I Grassi, D Grodent, D Grun, E Gustin, J Hedman, M Helled, R Henri, P Hess, S Hillier, JK Hofstadter, MH Holme, R Horanyi, M Hospodarsky, G Hsu, S Irwin, P Jackman, CM Karatekin, O Kempf, S Khalisi, E Konstantinidis, K Kruger, H Kurth, WS Labrianidis, C Lainey, V Lamy, LL Laneuville, M Lucchesi, D Luntzer, A MacArthur, J Maier, A Masters, A McKenna-Lawlor, S Melin, H Milillo, A Moragas-Klostermeyer, G Morschhauser, A Moses, JI Mousis, O Nettelmann, N Neubauer, FM Nordheim, T Noyelles, B Orton, GS Owens, M Peron, R Plainaki, C Postberg, F Rambaux, N Retherford, K Reynaud, S Roussos, E Russell, CT Rymer, A Sallantin, R Sanchez-Lavega, A Santolik, O Saur, J Sayanagi, K Schenk, P Schubert, J Sergis, N Sittler, EC Smith, A Spahn, F Srama, R Stallard, T Sterken, V Sternovsky, Z Tiscareno, M Tobie, G Tosi, F Trieloff, M Turrini, D Turtle, EP Vinatier, S Wilson, R Zarkat, P AF Arridge, C. S. Achilleos, N. Agarwal, J. Agnor, C. B. Ambrosi, R. Andre, N. Badman, S. V. Baines, K. Banfield, D. Barthelemy, M. Bisi, M. M. Blum, J. Bocanegra-Bahamon, T. Bonfond, B. . Bracken, C. Brandt, P. Briand, C. Briois, C. Brooks, S. Castillo-Rogez, J. Cavalie, T. Christophe, B. Coates, A. J. Collinson, G. Cooper, J. F. Costa-Sitja, M. Courtin, R. Daglis, I. A. De Pater, I. Desai, M. Dirkx, D. Dougherty, M. K. Ebert, R. W. Filacchione, G. Fletcher, L. N. Fortney, J. Gerth, I. Grassi, D. Grodent, D. Grun, E. Gustin, J. Hedman, M. Helled, R. Henri, P. Hess, S. Hillier, J. K. Hofstadter, M. H. Holme, R. Horanyi, M. Hospodarsky, G. Hsu, S. Irwin, P. Jackman, C. M. Karatekin, O. Kempf, S. Khalisi, E. Konstantinidis, K. Kruger, H. Kurth, W. S. Labrianidis, C. Lainey, V. Lamy, L. L. Laneuville, M. Lucchesi, D. Luntzer, A. MacArthur, J. Maier, A. Masters, A. McKenna-Lawlor, S. Melin, H. Milillo, A. Moragas-Klostermeyer, G. Morschhauser, A. Moses, J. I. Mousis, O. Nettelmann, N. Neubauer, F. M. Nordheim, T. Noyelles, B. Orton, G. S. Owens, M. Peron, R. Plainaki, C. Postberg, F. Rambaux, N. Retherford, K. Reynaud, S. Roussos, E. Russell, C. T. Rymer, Am. Sallantin, R. Sanchez-Lavega, A. Santolik, O. Saur, J. Sayanagi, Km. Schenk, P. Schubert, J. Sergis, N. Sittler, E. C. Smith, A. Spahn, F. Srama, R. Stallard, T. Sterken, V. Sternovsky, Z. Tiscareno, M. Tobie, G. Tosi, F. Trieloff, M. Turrini, D. Turtle, E. P. Vinatier, S. Wilson, R. Zarkat, P. TI The science case for an orbital mission to Uranus: Exploring the origins and evolution of ice giant planets SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Uranus; Magnetosphere; Atmosphere; Natural satellites; Rings; Planetary interior ID IRREGULAR SATELLITES SYCORAX; INNER URANIAN SATELLITES; MAGNETIC-FIELDS; SOLAR-SYSTEM; SUBSURFACE OCEANS; OUTER PLANETS; WATER ICE; E-RING; NEPTUNE; DYNAMICS AB Giant planets helped to shape the conditions we see in the Solar System today and they account for more than 99% of the mass of the Sun's planetary system. They can be subdivided into the Ice Giants (Uranus and Neptune) and the Gas Giants (Jupiter and Saturn), which differ from each other in a number of fundamental ways. Uranus, in particular is the most challenging to our understanding of planetary formation and evolution, with its large obliquity, low self-luminosity, highly asymmetrical internal field, and puzzling internal structure. Uranus also has a rich planetary system consisting of a system of inner natural satellites and complex ring system, five major natural icy satellites, a system of irregular moons with varied dynamical histories, and a highly asymmetrical magnetosphere. Voyager 2 is the only spacecraft to have explored Uranus, with a flyby in 1986, and no mission is currently planned to this enigmatic system. However, a mission to the uranian system would open a new window on the origin and evolution of the Solar System and would provide crucial information on a wide variety of physicochemical processes in our Solar System. These have clear implications for understanding exoplanetary systems. In this paper we describe the science case for an orbital mission to Uranus with an atmospheric entry probe to sample the composition and atmospheric physics in Uranus' atmosphere. The characteristics of such an orbiter and a strawman scientific payload are described and we discuss the technical challenges for such a mission. This paper is based on a white paper submitted to the European Space Agency's call for science themes for its large-class mission programme in 2013. (C) 2014 Published by Elsevier Ltd. C1 [Arridge, C. S.; Coates, A. J.; Nordheim, T.; Smith, A.] UCL, Mullard Space Sci Lab, London WC1E 6BT, England. [Arridge, C. S.; Achilleos, N.; Coates, A. J.; MacArthur, J.; Nordheim, T.] UCL Birkbeck, Ctr Planetary Sci, London, England. [Achilleos, N.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Agarwal, J.] European Space Agcy, ESTEC, F-75738 Paris 15, France. [Agnor, C. B.] Queen Mary Univ London, London, England. [Ambrosi, R.; Melin, H.] Univ Leicester, Space Res Ctr, Leicester LE1 7RH, Leics, England. [Andre, N.; Sallantin, R.] IRAP, Toulouse, France. [Badman, S. V.; Masters, A.] ISAS, JAXA, Sagamihara, Kanagawa, Japan. [Badman, S. V.] Univ Lancaster, Dept Phys, Lancaster LA1 4YW, England. [Baines, K.; Brooks, S.; Castillo-Rogez, J.; Hofstadter, M. H.; Orton, G. S.] NASA, Jet Prop Lab, Washington, DC USA. [Baines, K.] Univ Wisconsin, Madison, WI 53706 USA. [Banfield, D.; Tiscareno, M.] Cornell, Ithaca, NY USA. [Barthelemy, M.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. [Bisi, M. M.] STFC, Rutherford Appleton Lab, Chilton, England. [Blum, J.] Tech Univ, Braunschweig, Germany. [Bocanegra-Bahamon, T.; Dirkx, D.; Gerth, I.] Delft Univ Technol, NL-2600 AA Delft, Netherlands. [Bonfond, B. .; Grodent, D.; Gustin, J.] Univ Liege, B-4000 Liege, Belgium. [Bracken, C.] Natl Univ Ireland, Maynooth, Kildare, Ireland. [Brandt, P.; Rymer, Am.; Turtle, E. P.] Johns Hopkins Univ, Appl Phys Lab, Baltimore, MD 21218 USA. [Briand, C.; Courtin, R.; Lamy, L. L.; Vinatier, S.; Zarkat, P.] Observ Paris, LESIA, F-75014 Paris, France. [Briois, C.; Henri, P.] Univ Orleans, CNRS, LPC2E, Orleans, France. [Cavalie, T.; Kruger, H.; Roussos, E.] Max Planck Inst Solar Syst Res, Gottingen, Germany. [Christophe, B.] Off Natl Etud & Rech Aerosp, Chatillon, France. [Collinson, G.; Cooper, J. F.; Sittler, E. C.] NASA, Goddard Space Flight Ctr, Washington, DC USA. [Costa-Sitja, M.] European Space Agcy, ESAC, F-75738 Paris 15, France. [Daglis, I. A.] Univ Athens, Dept Phys, GR-10679 Athens, Greece. [De Pater, I.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Desai, M.; Ebert, R. W.; Retherford, K.] SW Res Inst, San Antonio, TX USA. [Dougherty, M. K.; Masters, A.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London, England. [Filacchione, G.; Grassi, D.; Lucchesi, D.; Milillo, A.; Peron, R.; Plainaki, C.; Tosi, F.; Turrini, D.] INAF IAPS, Ist Astrofts & Planetol Spaziali, Rome, Italy. [Fletcher, L. N.; Irwin, P.] Univ Oxford, Dept Phys, Oxford OX1 2JD, England. [Fortney, J.; Nettelmann, N.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Grun, E.; Sterken, V.] Max Planck Inst Nucl Phys, Heidelberg, Germany. [Grun, E.; Horanyi, M.; Hsu, S.; Kempf, S.; Sternovsky, Z.; Wilson, R.] Univ Colorado, LASP, Boulder, CO 80309 USA. [Hedman, M.] Univ Idaho, Moscow, ID 83843 USA. [Helled, R.] Tel Aviv Univ, IL-69978 Tel Aviv, Israel. [Hess, S.] LATMOS, Paris, France. [Hillier, J. K.; Trieloff, M.] Heidelberg Univ, D-69115 Heidelberg, Germany. [Holme, R.] Univ Liverpool, Liverpool L69 3BX, Merseyside, England. [Hospodarsky, G.; Kurth, W. S.] Univ Iowa, Ames, IA USA. [Jackman, C. M.] Univ Southampton, Dept Phys & Astron, Southampton SO9 5NH, Hants, England. [Karatekin, O.] Royal Observ Belgium, Brussels, Belgium. [Khalisi, E.; Moragas-Klostermeyer, G.; Postberg, F.; Srama, R.] Univ Stuttgart, Stuttgart, Germany. [Konstantinidis, K.] Univ Bundeswehr, Munich, Germany. [Labrianidis, C.] UTesat Spacecom GmbH, Backnang, Germany. [Lainey, V.; Rambaux, N.] Univ Lille 1, UPMC, CNRS, IMCCE Observ Paris,UMR 8028, F-75014 Paris, France. [Laneuville, M.] Inst Phys Globe Paris, F-75251 Paris, France. [Luntzer, A.] Univ Vienna, A-1010 Vienna, Austria. [Maier, A.] Austrian Acad Sci, Space Res Inst, A-1010 Vienna, Austria. [McKenna-Lawlor, S.] Natl Univ Ireland, Space Technol Ireland, Cork, Ireland. [Morschhauser, A.] DLR, Cologne, Germany. [Moses, J. I.] Space Sci Inst, Boulder, CO USA. [Mousis, O.] Observ Besancon, Besancon, France. [Neubauer, F. M.; Saur, J.] Univ Cologne, Cologne, Germany. [Noyelles, B.] Univ Namur, Namur, Belgium. [Owens, M.] Univ Reading, Reading RG6 2AH, Berks, England. [Rambaux, N.] Univ Paris 06, F-75252 Paris 05, France. [Reynaud, S.] CNRS, UMPC, Lab Kastler Brossel, F-75700 Paris, France. [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Sanchez-Lavega, A.] Univ Basque Country, Vizcaya, Spain. [Santolik, O.] Inst Atmospher Phys, Prague, Czech Republic. [Sayanagi, Km.] Hampton Univ, Dept Atmospher & Planetary Sci, Hampton, VA 23668 USA. [Schenk, P.] Univ Arizona, Lunar & Planetary Inst, Tucson, AZ 85721 USA. [Schubert, J.] Univ Calif Los Angeles, Dept Earth Sci, Los Angeles, CA 90024 USA. [Sergis, N.] Acad Athens, Off Space Res & Technol, Athens, Greece. [Spahn, F.] Univ Potsdam, Potsdam, Germany. [Stallard, T.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Tobie, G.] Univ Nantes, CNRS, LPG, Nantes, France. [Sterken, V.] Int Space Sci Inst, Bern, Switzerland. [Barthelemy, M.] CNRS, IPAG, F-38000 Grenoble, France. RP Arridge, CS (reprint author), UCL, Mullard Space Sci Lab, London WC1E 6BT, England. EM c.arridge@ucl.ac.uk RI Moses, Julianne/I-2151-2013; Sergis, Nick/A-9881-2015; Owens, Mathew/B-3006-2010; Laneuville, Matthieu/F-8523-2010; Arridge, Christopher/A-2894-2009; Fletcher, Leigh/D-6093-2011; Reynaud, Serge/J-8061-2014; M., Achim/J-4946-2015; Coates, Andrew/C-2396-2008; Noyelles, Benoit/Q-1767-2015; Daglis, Ioannis/L-6100-2013; Turtle, Elizabeth/K-8673-2012; Wilson, Rob/C-2689-2009; OI Moses, Julianne/0000-0002-8837-0035; Owens, Mathew/0000-0003-2061-2453; Laneuville, Matthieu/0000-0001-6022-0046; Arridge, Christopher/0000-0002-0431-6526; Fletcher, Leigh/0000-0001-5834-9588; Reynaud, Serge/0000-0002-1494-696X; M., Achim/0000-0001-7955-4441; Coates, Andrew/0000-0002-6185-3125; Noyelles, Benoit/0000-0003-4106-8741; Daglis, Ioannis/0000-0002-0764-3442; Turtle, Elizabeth/0000-0003-1423-5751; Wilson, Rob/0000-0001-9276-2368; Plainaki, Christina /0000-0003-1483-5052; KEMPF, SASCHA/0000-0001-5236-3004; Peron, Roberto/0000-0002-1774-5725; Achilleos, Nicholas/0000-0002-5886-3509; Jackman, Caitriona/0000-0003-0635-7361; Turrini, Diego/0000-0002-1923-7740; Milillo, Anna/0000-0002-0266-2556; Filacchione, Gianrico/0000-0001-9567-0055; Irwin, Patrick/0000-0002-6772-384X; Grassi, Davide/0000-0003-1653-3066; Hospodarsky, George/0000-0001-9200-9878; Roussos, Elias/0000-0002-5699-0678; Kurth, William/0000-0002-5471-6202; Tosi, Federico/0000-0003-4002-2434; Stallard, Tom/0000-0003-3990-670X; Banfield, Don/0000-0003-2664-0164 FU Royal Society University Research Fellowships FX CSA and LNF were supported by Royal Society University Research Fellowships. C.S.A. thanks O. Bedworth, B. Jacobson, and J.-P. Lebreton for useful discussions and comments on the manuscript. NR 151 TC 4 Z9 4 U1 4 U2 33 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 DEC PY 2014 VL 104 SI SI BP 122 EP 140 DI 10.1016/j.pss.2014.08.009 PN A PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AY5AH UT WOS:000347585400010 ER PT J AU Beichman, C Benneke, B Knutson, H Smith, R Lagage, PO Dressing, C Latham, D Lunine, J Birkmann, S Ferruit, P Giardino, G Kempton, E Carey, S Krick, J Deroo, PD Mandell, A Ressler, ME Shporer, A Swain, M Vasisht, G Ricker, G Bouwman, J Crossfield, I Greene, T Howell, S Christiansen, J Ciardi, D Clampin, M Greenhouse, M Sozzetti, A Goudfrooij, P Hines, D Keyes, T Lee, J McCullough, P Robberto, M Stansberry, J Valenti, J Rieke, M Rieke, G Fortney, J Bean, J Kreidberg, L Ehrenreich, D Deming, D Albert, L Doyon, R Sing, D AF Beichman, Charles Benneke, Bjoern Knutson, Heather Smith, Roger Lagage, Pierre-Olivier Dressing, Courtney Latham, David Lunine, Jonathan Birkmann, Stephan Ferruit, Pierre Giardino, Giovanna Kempton, Eliza Carey, Sean Krick, Jessica Deroo, Pieter D. Mandell, Avi Ressler, Michael E. Shporer, Avi Swain, Mark Vasisht, Gautam Ricker, George Bouwman, Jeroen Crossfield, Ian Greene, Tom Howell, Steve Christiansen, Jessie Ciardi, David Clampin, Mark Greenhouse, Matt Sozzetti, Alessandro Goudfrooij, Paul Hines, Dean Keyes, Tony Lee, Janice McCullough, Peter Robberto, Massimo Stansberry, John Valenti, Jeff Rieke, Marcia Rieke, George Fortney, Jonathan Bean, Jacob Kreidberg, Laura Ehrenreich, David Deming, Drake Albert, Loic Doyon, Rene Sing, David TI Observations of Transiting Exoplanets with the James Webb Space Telescope (JWST) SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID PLANET HD 189733B; EARTH-SIZED EXOPLANET; ALL-SKY SURVEY; SUPER-EARTH; SECONDARY ECLIPSE; TRANSMISSION SPECTRUM; GIANT PLANETS; M-DWARFS; THERMAL EMISSION; GJ 1214B AB This article summarizes a workshop held on March, 2014, on the potential of the James Webb Space Telescope (JWST) to revolutionize our knowledge of the physical properties of exoplanets through transit observations. JWSTs unique combination of high sensitivity and broad wavelength coverage will enable the accurate measurement of transits with high signal-to-noise ratio (S/N). Most importantly, JWST spectroscopy will investigate planetary atmospheres to determine atomic and molecular compositions, to probe vertical and horizontal structure, and to follow dynamical evolution, i.e., exoplanet weather. JWST will sample a diverse population of planets of varying masses and densities in a wide variety of environments characterized by a range of host star masses and metallicities, orbital semi-major axes, and eccentricities. A broad program of exoplanet science could C1 [Beichman, Charles] CALTECH, Jet Prop Lab, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Benneke, Bjoern; Knutson, Heather; Smith, Roger; Lagage, Pierre-Olivier] CALTECH, Pasadena, CA 91125 USA. [Lagage, Pierre-Olivier] CEA Saclay, F-91191 Gif Sur Yvette, France. [Dressing, Courtney; Latham, David] Harvard Univ, Ctr Astrophys, Cambridge, MA 02138 USA. [Lunine, Jonathan] Cornell Univ, Ithaca, NY 14853 USA. [Birkmann, Stephan; Ferruit, Pierre; Giardino, Giovanna] European Space Agcy, NL-2200 AG Noordwijk, Netherlands. [Kempton, Eliza] Grinnell Coll, Grinnell, IA 50112 USA. [Carey, Sean; Krick, Jessica] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Deroo, Pieter D.; Mandell, Avi; Ressler, Michael E.; Shporer, Avi; Swain, Mark; Vasisht, Gautam] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Ricker, George] MIT, Cambridge, MA 02139 USA. [Bouwman, Jeroen; Crossfield, Ian] Max Planck Inst Astrophys, D-69117 Heidelberg, Germany. [Greene, Tom; Howell, Steve] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Christiansen, Jessie; Ciardi, David] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Clampin, Mark; Greenhouse, Matt] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sozzetti, Alessandro] Osserv Astron Torino, I-10025 Pino Torinese, Italy. [Goudfrooij, Paul; Hines, Dean; Keyes, Tony; Lee, Janice; McCullough, Peter; Robberto, Massimo; Stansberry, John; Valenti, Jeff] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Rieke, Marcia; Rieke, George] Univ Arizona, Tucson, AZ 85721 USA. [Fortney, Jonathan] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Bean, Jacob; Kreidberg, Laura] Univ Chicago, Chicago, IL 60637 USA. [Ehrenreich, David] Univ Geneva, CH-1290 Versoix, Switzerland. [Deming, Drake] Univ Maryland, College Pk, MD 20742 USA. [Albert, Loic; Doyon, Rene] Univ Montreal, Montreal, PQ H3T 1J4, Canada. [Sing, David] Univ Exeter, Exeter EX4 1HS, Devon, England. RP Beichman, C (reprint author), CALTECH, Jet Prop Lab, NASA Exoplanet Sci Inst, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. OI Sing, David /0000-0001-6050-7645; Sozzetti, Alessandro/0000-0002-7504-365X; Ciardi, David/0000-0002-5741-3047; Ehrenreich, David/0000-0001-9704-5405 NR 89 TC 29 Z9 29 U1 1 U2 18 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD DEC PY 2014 VL 126 IS 946 BP 1134 EP 1173 DI 10.1086/679566 PG 40 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AY3BG UT WOS:000347458900006 ER PT J AU Jiang, J Hathaway, DH Cameron, RH Solanki, SK Gizon, L Upton, L AF Jiang, J. Hathaway, D. H. Cameron, R. H. Solanki, S. K. Gizon, L. Upton, L. TI Magnetic Flux Transport at the Solar Surface SO SPACE SCIENCE REVIEWS LA English DT Review DE Sun: magnetic fields; Sun: photosphere; Flux transport; Meridional flow; Differential rotation; Diffusion ID TIME-DISTANCE HELIOSEISMOLOGY; MICHELSON DOPPLER IMAGER; EVOLVING SYNOPTIC MAPS; SUNS MERIDIONAL FLOW; WHITE-LIGHT IMAGES; LARGE-SCALE; MOUNT-WILSON; DIFFERENTIAL ROTATION; CONVECTION ZONE; CYCLE 23 AB After emerging to the solar surface, the Sun's magnetic field displays a complex and intricate evolution. The evolution of the surface field is important for several reasons. One is that the surface field, and its dynamics, sets the boundary condition for the coronal and heliospheric magnetic fields. Another is that the surface evolution gives us insight into the dynamo process. In particular, it plays an essential role in the Babcock-Leighton model of the solar dynamo. Describing this evolution is the aim of the surface flux transport model. The model starts from the emergence of magnetic bipoles. Thereafter, the model is based on the induction equation and the fact that after emergence the magnetic field is observed to evolve as if it were purely radial. The induction equation then describes how the surface flows-differential rotation, meridional circulation, granular, supergranular flows, and active region inflows-determine the evolution of the field (now taken to be purely radial). In this paper, we review the modeling of the various processes that determine the evolution of the surface field. We restrict our attention to their role in the surface flux transport model. We also discuss the success of the model and some of the results that have been obtained using this model. C1 [Jiang, J.] Chinese Acad Sci, Key Lab Solar Act, Natl Astron Observ, Beijing 100012, Peoples R China. [Hathaway, D. H.] NASA MSFC, Huntsville, AL 35812 USA. [Cameron, R. H.; Solanki, S. K.; Gizon, L.] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany. [Solanki, S. K.] Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi Do, South Korea. [Gizon, L.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Upton, L.] Vanderbilt Univ, Nashville, TN 37235 USA. [Upton, L.] Univ Alabama, Huntsville, AL 35899 USA. RP Jiang, J (reprint author), Chinese Acad Sci, Key Lab Solar Act, Natl Astron Observ, Beijing 100012, Peoples R China. EM jiejiang@nao.cas.cn; david.hathaway@nasa.gov; cameron@mps.mpg.de; solanki@mps.mpg.de; gizon@mps.mpg.de; lar0009@uah.edu FU National Natural Science Foundations of China [11173033, 11221063, 2011CB811401]; Knowledge Innovation Program of the CAS [KJCX2-EW-T07]; BK21 plus program through the National Research Foundation (NRF) - Ministry of Education of Korea; DFG [SFB 963]; Astrophysical Flow Instabilities and Turbulence [A18/1]; EU FX We are grateful to the referee for helpful comments on the paper. We acknowledge the support from ISSI Bern, for our participation in the workshop on the solar activity cycle: physical causes and consequences. J.J. acknowledges the financial support by the National Natural Science Foundations of China (11173033, 11221063, 2011CB811401) and the Knowledge Innovation Program of the CAS (KJCX2-EW-T07). S.K.S. acknowledges the partial support for this work by the BK21 plus program through the National Research Foundation (NRF) funded by the Ministry of Education of Korea. L.G. acknowledges support from DFG SFB 963 Astrophysical Flow Instabilities and Turbulence (Project A18/1) and from EU FP7 Collaborative Project Exploitation of Space Data for Innovative Helio-and Asteroseismology (SPACEINN). NR 170 TC 17 Z9 18 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD DEC PY 2014 VL 186 IS 1-4 BP 491 EP 523 DI 10.1007/s11214-014-0083-1 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AY2HO UT WOS:000347409800017 ER PT J AU Kim, B Lu, YJ Kim, T Han, JW Meyyappan, M Li, J AF Kim, Beomseok Lu, Yijiang Kim, Taemin Han, Jin-Woo Meyyappan, M. Li, Jing TI Carbon Nanotube Coated Paper Sensor for Damage Diagnosis SO ACS NANO LA English DT Article DE carbon nanotube; paper sensor; structural diagnosis; electrical resistance tomography ID ELECTRICAL-IMPEDANCE TOMOGRAPHY; CELLULOSE PAPER; IMPACT DAMAGE; STRAIN; DELAMINATION AB A carbon nanotube coated paper sensor has been developed for the detection of damages in structural components. Electrical resistance tomography is used to measure changes in electrical potential at various locations induced by applying a small electrical current to the sample. The spatial locations and magnitudes of multiple damages are predicted accurately with a sensitivity of 73 ppm in sensing area. The detection limit of the sensor is estimated to be 29 ppm in sensing area, which is at least 30 times better in sensitivity than previous results (0.1-0.65%) in the literature. C1 [Kim, Beomseok; Lu, Yijiang] ELORET Corp, Moffett Field, CA 94035 USA. [Kim, Taemin] SGT Inc, Moffett Field, CA 94035 USA. [Han, Jin-Woo] NASA, Ames Res Ctr, USRA, Moffett Field, CA 94035 USA. RP Kim, B (reprint author), ELORET Corp, Moffett Field, CA 94035 USA. EM beomseok.kim@nasa.gov FU Nanotechnology Thematic Project in NASA's Game Changing Development Program FX This work was supported by the Nanotechnology Thematic Project in NASA's Game Changing Development Program. NR 24 TC 5 Z9 5 U1 3 U2 25 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1936-0851 EI 1936-086X J9 ACS NANO JI ACS Nano PD DEC PY 2014 VL 8 IS 12 BP 12092 EP 12097 DI 10.1021/nn5037653 PG 6 WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Chemistry; Science & Technology - Other Topics; Materials Science GA AX8CL UT WOS:000347138000022 PM 25402864 ER PT J AU Anderson, RL Lo, MW AF Anderson, Rodney L. Lo, Martin W. TI Spatial approaches to moons from resonance relative to invariant manifolds SO ACTA ASTRONAUTICA LA English DT Article DE Spatial approach; Resonance; Dynamical systems; Invariant manifolds ID RESTRICTED 3-BODY PROBLEM; DYNAMICAL-SYSTEMS ANALYSIS; TRAJECTORY DESIGN; ORBITS; CAPTURE; COMETS; CONNECTIONS; MECHANICS; TRANSFERS; FLYBYS AB In this study, the final approach to a moon or other body from resonance is explored and compared to the invariant manifolds of unstable periodic orbits. It is shown that the stable manifolds of planar Lyapunov orbits can act as a guide for the periods or resonances that are required for the final approach in both the planar and spatial problems. Previously developed techniques for the planar problem are expanded for use with resonances and used for comparison with trajectories approaching a moon from these resonances. A similar technique is then used for exploring the relationship of invariant manifolds to approach trajectories in the spatial problem. It is shown that the invariant manifolds of unstable periodic orbits provide insight into the trajectory design, and they can be used as a guide to the more direct approach trajectories. (C) 2014 IAA. Published by Elsevier Ltd. All rights reserved. C1 [Anderson, Rodney L.; Lo, Martin W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Anderson, RL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-121, Pasadena, CA 91109 USA. EM rodney.l.anderson@jpl.nasa.gov; martin.w.lo@jpl.nasa.gov OI Anderson, Rodney/0000-0001-5336-2775 FU National Aeronautics and Space Administration FX The authors would like to thank Jon Sims and Damon Landau for their helpful comments and careful reviews of this paper. The research presented in this paper has been carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 63 TC 4 Z9 4 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD DEC PY 2014 VL 105 IS 1 BP 355 EP 372 DI 10.1016/j.actaastro.2014.09.015 PG 18 WC Engineering, Aerospace SC Engineering GA AX6GP UT WOS:000347021400036 ER PT J AU Jin, B Kim, J Pi, DH Kim, HS Meyyappan, M Lee, JS AF Jin, Bo Kim, Jungsik Pi, Dong-Hai Kim, Hyoung Seop Meyyappan, M. Lee, Jeong-Soo TI Role of an encapsulating layer for reducing resistance drift in phase change random access memory SO AIP ADVANCES LA English DT Article ID FILMS; GE2SB2TE5; BEHAVIOR AB Phase change random access memory (PCRAM) devices exhibit a steady increase in resistance in the amorphous phase upon aging and this resistance drift phenomenon directly affects the device reliability. A stress relaxation model is used here to study the effect of a device encapsulating layer material in addressing the resistance drift phenomenon in PCRAM. The resistance drift can be increased or decreased depending on the biaxial moduli of the phase change material (Y-PCM) and the encapsulating layer material (Y-ELM) according to the stress relationship between them in the drift regime. The proposed model suggests that the resistance drift can be effectively reduced by selecting a proper material as an encapsulating layer. Moreover, our model explains that reducing the size of the phase change material (PCM) while fully reset and reducing the amorphous/crystalline ratio in PCM help to improve the resistance drift, and thus opens an avenue for highly reliable multilevel PCRAM applications. (C) 2014 Author(s). All article content, except where otherwise noted, is licensed under a Creative Commons Attribution 3.0 Unported License. C1 [Jin, Bo; Kim, Jungsik; Lee, Jeong-Soo] Pohang Univ Sci & Technol POSTECH, Div IT Convergence Engn, Pohang 790784, South Korea. [Pi, Dong-Hai; Kim, Hyoung Seop] Pohang Univ Sci & Technol POSTECH, Dept Mat Sci & Engn, Pohang 790784, South Korea. [Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Meyyappan, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM m.meyyappan@nasa.gov; ljs6951@postech.ac.kr RI Kim, Hyoung Seop/C-2166-2009; OI Kim, Hyoung Seop/0000-0002-3155-583X; Jin, Bo/0000-0003-4407-1954 FU National Research Foundation (NRF) [2012R1A2A2A02010 432]; center for advanced soft electronics under the global frontier research program of the Ministry of Education, Science, and Technology (MEST), Korea [2011-0031638]; POSTECH; Samsung Electronics Co. Ltd. FX This work was supported by National Research Foundation (NRF) (No. 2012R1A2A2A02010 432); by a grant (Code No. 2011-0031638) from the center for advanced soft electronics under the global frontier research program of the Ministry of Education, Science, and Technology (MEST), Korea; by Semiconductor Industry Collaborative Project between POSTECH and Samsung Electronics Co. Ltd. NR 30 TC 0 Z9 0 U1 0 U2 16 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 2158-3226 J9 AIP ADV JI AIP Adv. PD DEC PY 2014 VL 4 IS 12 DI 10.1063/1.4905451 PG 9 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied SC Science & Technology - Other Topics; Materials Science; Physics GA AX8PC UT WOS:000347170100086 ER PT J AU Jones, MO Kimball, JS Nemani, RR AF Jones, Matthew O. Kimball, John S. Nemani, Ramakrishna R. TI Asynchronous Amazon forest canopy phenology indicates adaptation to both water and light availability SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE vegetation optical depth; AMSR-E; amazon; phenology; seasonality; tropical forests ID RAIN-FOREST; CLIMATE-CHANGE; VEGETATION DYNAMICS; CARBON BALANCE; DROUGHT STRESS; VARIABILITY; SENSITIVITY; INDEXES; STORAGE; FLUXES AB Amazon forests represent nearly half of all tropical vegetation biomass and, through photosynthesis and respiration, annually process more than twice the amount of estimated carbon (CO2) from fossil fuel emissions. Yet the seasonality of Amazon canopy cover, and the extent to which seasonal fluctuations in water availability and photosynthetically available radiation influence these processes, is still poorly understood. Implementing six remotely sensed data sets spanning nine years (2003-2011), with reported field and flux tower data, we show that southern equatorial Amazon forests exhibit a distinctive seasonal signal. Seasonal timing of water availability, canopy biomass growth and net leaf flush are asynchronous in regions with short dry seasons and become more synchronous across a west-to-east longitudinal moisture gradient of increasing dry season. Forest cover is responsive to seasonal disparities in both water and solar radiation availability, temporally adjusting net leaf flush to maximize use of these generally abundant resources, while reducing drought susceptibility. An accurate characterization of this asynchronous behavior allows for improved understanding of canopy phenology across contiguous tropical forests and their sensitivity to climate variability and drought. C1 [Jones, Matthew O.; Kimball, John S.] Univ Montana, Flathead Lake Biol Stn, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA. [Nemani, Ramakrishna R.] NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA. RP Jones, MO (reprint author), Univ Montana, NTSG, DHC 021,32 Campus, Missoula, MT 59812 USA. EM matt.jones@ntsg.umt.edu FU NASA MEaSUREs program; NASA [NNX11AD46G] FX We thank the flux tower Principal Investigators, S Wofsy, V Kirchhoff, Goulden, da Rocha, M Waterloo, A Manzi, and L Sa of the Large Scale Biosphere-Atmosphere Experiment in Amazonia (LBA) for making their data freely available and Alexei Lyapustin for creating the MODIS MAIAC data. We also thank Saleska, da Rocha, Restrepo-Coupe, Huete, A Nobre, P Artaxo, and Y Shimabukuro for creating the publicly available LBA flux tower integrated database, Dr Cory Cleveland for his valuable input, and the anonymous reviewers for their valuable input and suggestions which improved this manuscript. The GRACE land data (available at http://grace.jpl.nasa.gov) processing algorithms were provided by Sean Swenson, and supported by the NASA MEaSUREs program. This work was performed at the University of Montana, and the Ames Research Center with funding provided by the NASA Science of Terra and Aqua program (NNX11AD46G). NR 60 TC 12 Z9 12 U1 4 U2 30 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-9326 J9 ENVIRON RES LETT JI Environ. Res. Lett. PD DEC PY 2014 VL 9 IS 12 AR 124021 DI 10.1088/1748-9326/9/12/124021 PG 10 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AY2ZP UT WOS:000347454800022 ER PT J AU Mezuman, K Price, C Galanti, E AF Mezuman, Keren Price, Colin Galanti, Eli TI On the spatial and temporal distribution of global thunderstorm cells SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE thunderstorms; lightning; global electric circuit; very low frequency; World Wide Lightning Location ID LIGHTNING LOCATION NETWORK; OPTICAL TRANSIENT DETECTOR; ELECTRIC-CIRCUIT; PERFORMANCE ASSESSMENT; ATMOSPHERIC ELECTRICITY; DETECTION EFFICIENCY; SCHUMANN RESONANCE; WWLLN; WEATHER; SENSOR AB Estimates of global thunderstorm activity have been made predominately by direct measurements of lightning discharges around the globe, either by optical measurements from satellites, or using ground-based radio antennas. In this paper we propose a new methodology in which thunderstorm clusters are constructed based on the lightning strokes detected by the World Wide Lightning Location Network (WWLLN) in the very low frequency range. We find that even with low lightning detection efficiency on a global scale, the spatial and temporal distribution of global thunderstorm cells is well reproduced. This is validated by comparing the global diurnal variations of the thunderstorm cells, and the currents produced by these storms, with the well-known Carnegie Curve, which represents the mean diurnal variability of the global atmospheric electric circuit, driven by thunderstorm activity. While the Carnegie Curve agrees well with our diurnal thunderstorm cluster variations, there is little agreement between the Carnegie Curve and the diurnal variation in the number of lightning strokes detected by the WWLLN. When multiplying the number of clusters we detect by the mean thunderstorm conduction current for land and ocean thunderstorms (Mach et al 2011 J. Geophys. Res. 116 D05201) we get a total average current of about 760 A. Our results show that thunderstorms alone explain more than 90% in the variability of the global electric circuit. However, while it has been previously shown that 90% of the global lightning occurs over continental landmasses, we show that around 50% of the thunderstorms are over the oceans, and from 00-09UTC there are more thunderstorm cells globally over the oceans than over the continents. Since the detection efficiency of the WWLLN system has increased over time, we estimate that the lower bound of the mean number of global thunderstorm cells in 2012 was around 1050 per hour, varying from around 840 at 03UTC to 1150 storms at 19UTC. C1 [Mezuman, Keren] Columbia Univ, New York, NY 10027 USA. [Mezuman, Keren] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Mezuman, Keren; Price, Colin; Galanti, Eli] Tel Aviv Univ, IL-69978 Tel Aviv, Israel. RP Mezuman, K (reprint author), Columbia Univ, New York, NY 10027 USA. EM cprice@flash.tau.ac.il NR 55 TC 4 Z9 4 U1 3 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-9326 J9 ENVIRON RES LETT JI Environ. Res. Lett. PD DEC PY 2014 VL 9 IS 12 AR 124023 DI 10.1088/1748-9326/9/12/124023 PG 9 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AY2ZP UT WOS:000347454800024 ER PT J AU Finley, AO Banerjee, S Weiskittel, AR Babcock, C Cook, BD AF Finley, Andrew O. Banerjee, Sudipto Weiskittel, Aaron R. Babcock, Chad Cook, Bruce D. TI Dynamic spatial regression models for space-varying forest stand tables SO ENVIRONMETRICS LA English DT Article DE Gaussian spatial process; MCMC; forestry; dynamic model ID LASER SCANNER DATA; DIAMETER DISTRIBUTIONS; TREE DIAMETER; WEIBULL DISTRIBUTION; FINITE MIXTURE; AGED STANDS; PARAMETERS; RECOVERY; COMPLEX; GROWTH AB Many forest management planning decisions are based on information about the number of trees by species and diameter per unit area. This information is commonly summarized in a stand table, where a stand is defined as a group of forest trees of sufficiently uniform species composition, age, condition, or productivity to be considered a homogeneous unit for planning purposes. Typically, information used to construct stand tables is gleaned from observed subsets of the forest selected using a probability-based sampling design. Such sampling campaigns are expensive, and hence, only a small number of sample units are typically observed. This data paucity means that stand tables can only be estimated for relatively large areal units. Contemporary forest management planning and spatially explicit ecosystem models require stand table input at higher spatial resolution than can be affordably provided using traditional approaches. We propose a dynamic multivariate Poisson spatial regression model that accommodates both spatial correlation between observed diameter distributions and also correlation between tree counts across diameter classes within each location. To improve fit and prediction at unobserved locations, diameter specific intensities can be estimated using auxiliary data such as management history or remotely sensed information. The proposed model is used to analyze a diverse forest inventory dataset collected on the United States Forest Service Penobscot Experimental Forest in Bradley, Maine. Results demonstrate that explicitly modeling the residual spatial structure via a multivariate Gaussian process and incorporating information about forest structure from Light Detection and Ranging (LiDAR) covariates improve model fit and can provide high spatial resolution stand table maps with associated estimates of uncertainty. Copyright (c) 2014 John Wiley & Sons, Ltd. C1 [Finley, Andrew O.] Michigan State Univ, Dept Geog, E Lansing, MI 48824 USA. [Banerjee, Sudipto] Univ Calif Los Angeles, Dept Biostat, Los Angeles, CA USA. [Weiskittel, Aaron R.] Univ Maine, Sch Forest Resources, Orono, ME USA. [Babcock, Chad] Univ Washington, Sch Environm & Forest Sci, Seattle, WA 98195 USA. [Cook, Bruce D.] Natl Aeronaut & Space Adm, Biospher Sci Lab, Greenbelt, MD USA. [Finley, Andrew O.] Michigan State Univ, Dept Forestry, E Lansing, MI 48824 USA. RP Finley, AO (reprint author), Michigan State Univ, Dept Forestry, E Lansing, MI 48824 USA. EM finleya@msu.edu FU National Science Foundation [DMS-1106609, EF-1137309, EF-1241874, EF-1253225]; NASA FX This work was supported by National Science Foundation grants DMS-1106609, EF-1137309, EF-1241874, and EF-1253225, as well as NASA Carbon Monitoring System grants. NR 46 TC 2 Z9 2 U1 1 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1180-4009 EI 1099-095X J9 ENVIRONMETRICS JI Environmetrics PD DEC PY 2014 VL 25 IS 8 SI SI BP 596 EP 609 DI 10.1002/env.2322 PG 14 WC Environmental Sciences; Mathematics, Interdisciplinary Applications; Statistics & Probability SC Environmental Sciences & Ecology; Mathematics GA AX4NI UT WOS:000346908700005 ER PT J AU Johnston, AH Swimm, RT Thorboum, DO Adell, PC Rax, BG AF Johnston, A. H. Swimm, R. T. Thorboum, D. O. Adell, P. C. Rax, B. G. TI Field Dependence of Charge Yield in Silicon Dioxide SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 51st Annual IEEE International Nuclearand Space Radiation Effects Conference (NSREC) CY JUL 14-18, 2014 CL Paris, FRANCE SP IEEE DE Ionization; radiation effects; semiconductor device modeling ID ENERGY X-RAY; MOS DEVICES; CO-60; HOLE; SIO2; RECOMBINATION; IRRADIATIONS; TRANSISTORS; CAPACITORS; INSULATORS AB New experimental results for the yield of electron-hole pairs in at low temperature are inconsistent with the Onsager theory of recombination. A revised model is developed to account for this, taking boundary conditions into effect. The model predicts a strong thickness dependence for yield under low-field conditions that is important at lower temperatures. New definitions for charge yield are proposed that distinguish between the initial escape probability and the net yield after charge transport, along with revised interpretations of older work on charge yield. C1 [Johnston, A. H.] JK Associates LLC, Coupeville, WA 98239 USA. [Swimm, R. T.] ManTech, Montrose, CA 91020 USA. [Thorboum, D. O.; Adell, P. C.; Rax, B. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Johnston, AH (reprint author), JK Associates LLC, Coupeville, WA 98239 USA. EM JohnstonAH25@gmail.com; Ran-dall.T.Swimm@jpl.nasa.gov; Dennis.O.Thorbourn@jpl.nasa.gov; Philippe.C.Adell@jpl.nasa.gov; Bernard.G.Rax@jp1.nasa.gov FU Jet Propulsion Laboratory, California Institute of Technology, under National Aeronautics and Space Administration (NASA) FX This work was supported by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). NR 27 TC 4 Z9 4 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2014 VL 61 IS 6 BP 2818 EP 2825 DI 10.1109/TNS.2014.2367512 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA AX1RO UT WOS:000346724100004 ER PT J AU Scheick, L AF Scheick, Leif TI Determination of Single-Event Effect Application Requirements for Enhancement Mode Gallium Nitride HEMTs for Use in Power Distribution Circuits SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 51st Annual IEEE International Nuclearand Space Radiation Effects Conference (NSREC) CY JUL 14-18, 2014 CL Paris, FRANCE SP IEEE DE Buck regulator; gallium nitride; single-event effects ID PROTON RADIATION-DAMAGE; LOW-TEMPERATURE; TRANSISTORS; FILMS AB Characterization of destructive single-event effects in enhancement mode gallium nitride high electron mobility transistors is presented as related to the optimal application of and operating conditions for power management circuits. A mechanism for the phenomenon is also presented. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Scheick, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM leif.z.scheick@jpl.nasa.gov NR 18 TC 6 Z9 6 U1 1 U2 8 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2014 VL 61 IS 6 BP 2881 EP 2888 DI 10.1109/TNS.2014.2365545 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA AX1RO UT WOS:000346724100013 ER PT J AU Pellish, JA Marshall, PW Rodbell, KP Gordon, MS LaBel, KA Schwank, JR Dodds, NA Castaneda, CM Berg, MD Kim, HS Phan, AM Seidleck, CM AF Pellish, Jonathan A. Marshall, Paul W. Rodbell, Kenneth P. Gordon, Michael S. LaBel, Kenneth A. Schwank, James R. Dodds, Nathaniel A. Castaneda, Carlos M. Berg, Melanie D. Kim, Hak S. Phan, Anthony M. Seidleck, Christina M. TI Criticality of Low-Energy Protons in Single-Event Effects Testing of Highly-Scaled Technologies SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 51st Annual IEEE International Nuclearand Space Radiation Effects Conference (NSREC) CY JUL 14-18, 2014 CL Paris, FRANCE SP IEEE DE Alpha particle radiation effects; proton radiation effects; radiation hardness assurance testing; silicon-on-insulator technology; single-event upset ID NM SOI SRAM; UPSETS AB We report low-energy proton and low-energy alpha particle SEE data on a 32 nm SOI CMOS SRAM that demonstrates the criticality of using low-energy protons for SEE testing of highly-scaled technologies. Low-energy protons produced a significantly higher fraction of multi-bit upsets relative to single-bit upsets when compared to similar alpha particle data. This difference highlights the importance of performing hardness assurance testing with protons that include energy distribution components below 2 MeV. The importance of low-energy protons to system-level single-event performance is based on the technology under investigation as well as the target radiation environment. C1 [Pellish, Jonathan A.; LaBel, Kenneth A.; Berg, Melanie D.; Kim, Hak S.; Phan, Anthony M.; Seidleck, Christina M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Marshall, Paul W.] NASA Consultant, Brookneal, VA 24528 USA. [Rodbell, Kenneth P.; Gordon, Michael S.] IBM TJ Watson Res Ctr, Yorktown Hts, NY 10598 USA. [Schwank, James R.; Dodds, Nathaniel A.] Sandia Natl Labs, Albuquerque, NM 87185 USA. [Castaneda, Carlos M.] Univ Calif Davis, Crocker Nucl Lab, Davis, CA 95616 USA. RP Pellish, JA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM jonathan.pellish@nasa.gov FU NASA Electronic Parts and Packaging program; Defense Threat Reduction Agency Radiation Hardened Microelectronics program; National Reconnaissance Office FX This work was supported in part by the NASA Electronic Parts and Packaging program, the Defense Threat Reduction Agency Radiation Hardened Microelectronics program, and the National Reconnaissance Office. NR 18 TC 8 Z9 8 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2014 VL 61 IS 6 BP 2896 EP 2903 DI 10.1109/TNS.2014.2369171 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA AX1RO UT WOS:000346724100015 ER PT J AU Dodds, NA Schwank, JR Shaneyfelt, MR Dodd, PE Doyle, BL Trinczek, M Blackmore, EW Rodbell, KP Gordon, MS Reed, RA Pellish, JA Label, KA Marshall, PW Swanson, SE Vizkelethy, G Van Deusen, S Sexton, FW Martinez, MJ AF Dodds, N. A. Schwank, J. R. Shaneyfelt, M. R. Dodd, P. E. Doyle, B. L. Trinczek, M. Blackmore, E. W. Rodbell, K. P. Gordon, M. S. Reed, R. A. Pellish, J. A. Label, K. A. Marshall, P. W. Swanson, S. E. Vizkelethy, G. Van Deusen, S. Sexton, F. W. Martinez, M. J. TI Hardness Assurance for Proton Direct Ionization-Induced SEEs Using a High-Energy Proton Beam SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 51st Annual IEEE International Nuclearand Space Radiation Effects Conference (NSREC) CY JUL 14-18, 2014 CL Paris, FRANCE SP IEEE DE Energy straggle; error rate prediction; low energy protons; proton direct ionization (PDI); single-event effects (SEEs) ID SINGLE-EVENT-UPSETS; NM SOI SRAM; PREDICTIONS AB The low-energy proton energy spectra of all shielded space environments have the same shape. This shape is easily reproduced in the laboratory by degrading a high-energy proton beam, producing a high-fidelity test environment. We use this test environment to dramatically simplify rate prediction for proton direct ionization effects, allowing the work to be done at high-energy proton facilities, on encapsulated parts, without knowledge of the IC design, and with little or no computer simulations required. Proton direct ionization (PDI) is predicted to significantly contribute to the total error rate under the conditions investigated. Scaling effects are discussed using data from 65-nm, 45-nm, and 32-nm SOI SRAMs. These data also show that grazing-angle protons will dominate the PDI-induced error rate due to their higher effective LET, so PDI hardness assurance methods must account for angular effects to be conservative. We show that this angular dependence can be exploited to quickly assess whether an IC is susceptible to PDI. C1 [Dodds, N. A.; Schwank, J. R.; Shaneyfelt, M. R.; Dodd, P. E.; Doyle, B. L.; Swanson, S. E.; Vizkelethy, G.; Van Deusen, S.; Sexton, F. W.; Martinez, M. J.] Sandia Natl Labs, Albuquerque, NM 87123 USA. [Trinczek, M.; Blackmore, E. W.] TRIUMF, Vancouver, BC V6T 2A3, Canada. [Rodbell, K. P.; Gordon, M. S.] IBM TJ Watson Res Ctr, Yorktown Hts, NY 10598 USA. [Reed, R. A.] Vanderbilt Univ, Nashville, TN 37203 USA. [Pellish, J. A.; Label, K. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Marshall, P. W.] NASA, Brookneal, VA 24528 USA. RP Dodds, NA (reprint author), Sandia Natl Labs, Albuquerque, NM 87123 USA. EM nadodds@sandia.gov FU Defense Threat Reduction Agency [DTRA100277008]; TRIUMF - National Research Council of Canada; Laboratory Directed Research and Development program at Sandia National Laboratories; United States Department of Energy [DE-AC04-94AL85000] FX This work was supported by the Defense Threat Reduction Agency under contract DTRA100277008, by TRIUMF, which receives funding via a contribution agreement through the National Research Council of Canada, and by the Laboratory Directed Research and Development program at Sandia National Laboratories, a multi-program laboratory operated by Sandia Corporation, a Lockheed Martin Company, for the United States Department of Energy, under contract DE-AC04-94AL85000. NR 22 TC 10 Z9 10 U1 0 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2014 VL 61 IS 6 BP 2904 EP 2914 DI 10.1109/TNS.2014.2364953 PN 1 PG 11 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA AX1RO UT WOS:000346724100016 ER PT J AU Dhombres, S Michez, A Boch, J Saigne, F Beauvivre, S Kraehenbuehl, D Vaille, JR Adell, PC Lorfevre, E Ecoffet, R Roig, F AF Dhombres, S. Michez, A. Boch, J. Saigne, F. Beauvivre, S. Kraehenbuehl, D. Vaille, J. -R. Adell, P. C. Lorfevre, E. Ecoffet, R. Roig, F. TI Study of a Thermal Annealing Approach for Very High Total Dose Environments SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 51st Annual IEEE International Nuclearand Space Radiation Effects Conference (NSREC) CY JUL 14-18, 2014 CL Paris, FRANCE SP IEEE DE Active pixel sensor (APS); CMOS active pixel sensor; extending lifetime; MOS devices; total dose effects ID PREDICTION; DEVICES; TRAPS AB Total dose effect remains one challenging issue for electronics systems intended to space applications. For high total dose missions, like Jupiter missions, or for scientific instruments for which functionality and precision must be guaranteed, dose effect is one of the main drawbacks. So, new solutions must be found in order to ensure the reliability of the mission. In this paper, an analysis of a thermal annealing approach is done. This approach consists of applying isothermal annealing cycles to a device such that its electrical characteristics can be regenerated after being degraded by total ionizing dose. The analysis is based on experimental results obtained on Power MOSFET and CMOS APS imager. The impact of electric field during annealing is also investigated. It is shown that thermal annealing can be applied to electronic devices in order to extend their lifetime. C1 [Dhombres, S.; Michez, A.; Boch, J.; Saigne, F.; Vaille, J. -R.; Roig, F.] Univ Montpellier, F-34000 Montpellier, France. [Dhombres, S.; Michez, A.; Boch, J.; Saigne, F.; Vaille, J. -R.; Roig, F.] CNRS, F-34000 Montpellier, France. [Dhombres, S.; Beauvivre, S.; Kraehenbuehl, D.] Systheia, F-34000 Montpellier, France. [Adell, P. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lorfevre, E.; Ecoffet, R.] Ctr Natl Etud Spatiales, F-31401 Toulouse, France. RP Dhombres, S (reprint author), Univ Montpellier, F-34000 Montpellier, France. EM dhombres@ies.univ-montp2.fr; michez@ies.univ-montp2.fr; jerome.boch@ies.univ-montp2.fr; saigne@ies.univ-montp2.fr; stephane.beauvivre@systheia.com; daniel.kraehenbuehl@sys-theia.com; vaille@ies.univ-montp2.fr; philippe.c.adell@jpl.nasa.gov; ericlorfevre@cnes.fr; robert.ecoffet@cnes.fr; roig@ies.univ-montp2.fr NR 16 TC 1 Z9 1 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2014 VL 61 IS 6 BP 2923 EP 2929 DI 10.1109/TNS.2014.2365875 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA AX1RO UT WOS:000346724100018 ER PT J AU Roche, NJH Buchner, SP Foster, CC King, MP Dodds, NA Warner, JH Mc Morrow, D Decker, T O'Neill, PM Reddell, BD Nguyen, KV Samsel, IK Hooten, NC Bennett, WG Reed, RA AF Roche, N. J-H. Buchner, S. P. Foster, C. C. King, M. P. Dodds, N. A. Warner, J. H. Mc Morrow, D. Decker, T. O'Neill, P. M. Reddell, B. D. Nguyen, K. V. Samsel, I. K. Hooten, N. C. Bennett, W. G. Reed, R. A. TI Validation of the Variable Depth Bragg Peak Method for Single-Event Latchup Testing Using Ion Beam Characterization SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 51st Annual IEEE International Nuclearand Space Radiation Effects Conference (NSREC) CY JUL 14-18, 2014 CL Paris, FRANCE SP IEEE DE Bragg peak; heavy ions; pulse height analysis; single event latchup AB The Variable Depth Bragg Peak method has been investigated for single event latchup testing by comparing latchup cross sections for heavy ions at low and high energies and by pulse height analysis. Results show that, unlike for an SOI device previously tested, where the charge collection depth is very small (70 nm), the comparison is not straightforward for latchup because of the large charge collection volumes involved. The variation in LET with depth for lower-energy ions greatly affects the comparison, but, if a charge collection depth of 50 mu m is assumed and the LET is averaged over that distance, the comparison improves significantly. C1 [Roche, N. J-H.] George Washington Univ, Washington, DC 20073 USA. [Buchner, S. P.; Warner, J. H.; Mc Morrow, D.] Naval Res Lab, Washington, DC 20375 USA. [Foster, C. C.] Foster Consulting Serv LLC, University Pl, WA 98466 USA. [King, M. P.; Dodds, N. A.; Samsel, I. K.; Hooten, N. C.; Bennett, W. G.; Reed, R. A.] Vanderbilt Univ, Nashville, TN 37212 USA. [Decker, T.] Analog Devices Inc, Greensboro, NC 27409 USA. [O'Neill, P. M.; Reddell, B. D.] NASA, JSC, Houston, TX 77058 USA. [Nguyen, K. V.] Jacobs Technol, Houston, TX 77258 USA. RP Roche, NJH (reprint author), George Washington Univ, Washington, DC 20073 USA. EM Nicolas.roche.ctr.fr@nrl.navy.mil; fosterchc@nventure.com; decker@analog.com; kyson.v.nguyen@nasa.gov NR 9 TC 2 Z9 2 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2014 VL 61 IS 6 BP 3061 EP 3067 DI 10.1109/TNS.2014.2367593 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA AX1RO UT WOS:000346724100039 ER PT J AU Chen, DK Kim, H Phan, A Wilcox, E LaBel, K Buchner, S Khachatrian, A Roche, N AF Chen, Dakai Kim, Hak Phan, Anthony Wilcox, Edward LaBel, Kenneth Buchner, Stephen Khachatrian, Ani Roche, Nicolas TI Single-Event Effect Performance of a Commercial Embedded ReRAM SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 51st Annual IEEE International Nuclearand Space Radiation Effects Conference (NSREC) CY JUL 14-18, 2014 CL Paris, FRANCE SP IEEE DE Heavy ion testing; lasers; non-volatile memory; radiation effects in ICs; single-event effect (SEE) ID HEAVY-ION IRRADIATION; ELECTRICAL CHARACTERISTICS; NONVOLATILE MEMORY; IMPACT; CELLS AB We show the single-event effect characteristics of a production-level embedded resistive memory. The resistive memory under investigation is a reduction-oxidation random access memory embedded inside a microcontroller. The memory structure consists of Ir top electrode, Ta-2 O5-6/TaOx metal-oxide, and TaN bottom electrode. The radiation testing focused on the resistive memory array and peripheral circuits, while other portions of the microcontroller were shielded against the ion beam. We found that the resistive memory array is hardened against heavy ion and pulsed-laser-induced bit upsets. However, the microcontroller is susceptible to single-event functional interrupts due to single-event upsets in the resistive memory peripheral control circuits, which comprise of CMOS elements. Furthermore, the resistive memory architecture is not susceptible to functional failures during write, which is problematic for flash memories due to radiation-induced charge pump degradation. C1 [Chen, Dakai; LaBel, Kenneth] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kim, Hak; Phan, Anthony; Wilcox, Edward] ASRC Space & Def, Seabrook, MD 20706 USA. [Buchner, Stephen; Khachatrian, Ani; Roche, Nicolas] Naval Res Lab, Washington, DC 20375 USA. RP Chen, DK (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM dakai.chen-1@nasa.gov; hak.s.kim@nasa.gov; stephen.buchner@nrl.navy.mil FU NASA Electronic Parts and Packaging (NEPP) Program; Defense Threat Reduction Agency (DTRA) under IACRO [DTRA10027-8002] FX This work was supported in part by the NASA Electronic Parts and Packaging (NEPP) Program and the Defense Threat Reduction Agency (DTRA) under IACRO DTRA10027-8002 to NASA. NR 24 TC 7 Z9 7 U1 3 U2 14 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2014 VL 61 IS 6 BP 3088 EP 3094 DI 10.1109/TNS.2014.2361488 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA AX1RO UT WOS:000346724100043 ER PT J AU Xapsos, MA Stauffer, C Jordan, T Poivey, C Haskins, DN Lum, G Pergosky, AM Smith, DC LaBel, KA AF Xapsos, M. A. Stauffer, C. Jordan, T. Poivey, C. Haskins, D. N. Lum, G. Pergosky, A. M. Smith, D. C. LaBel, K. A. TI How Long Can the Hubble Space Telescope Operate Reliably?-A Total Dose Perspective SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 51st Annual IEEE International Nuclearand Space Radiation Effects Conference (NSREC) CY JUL 14-18, 2014 CL Paris, FRANCE SP IEEE DE Hubble Space Telescope (HST); radiation shielding; radiation transport; total ionizing dose; van Allen belts ID RADIATION AB The Hubble Space Telescope has been at the forefront of discoveries in the field of astronomy for more than 20 years. It was the first telescope designed to be serviced in space and the last such servicing mission occurred in May 2009. The question of how much longer this valuable resource can continue to return science data remains. In this paper a detailed analysis of the total dose exposure of electronic parts at the box level is performed using solid angle sectoring/3-dimensional ray trace and Monte Carlo radiation transport simulations. Results are related to parts that have been proposed as possible total dose concerns. The spacecraft subsystem that appears to be at the greatest risk for total dose failure is identified. This is discussed with perspective on the overall lifetime of the spacecraft. C1 [Xapsos, M. A.; Haskins, D. N.; LaBel, K. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Stauffer, C.] AS&D Inc, Greenbelt, MD 20770 USA. [Jordan, T.] EMP Consultants, Gaithersburg, MD 20878 USA. [Poivey, C.] ESA ESTEC, NL-2200 AG Noordwijk, Netherlands. [Lum, G.] Lockheed Martin Space Syst Co, Sunnyvale, CA 94088 USA. [Pergosky, A. M.; Smith, D. C.] Lockheed Martin Informat Syst & Global Serv, Greenbelt, MD 20770 USA. RP Xapsos, MA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Michael.A.Xapsos@nasa.gov FU Hubble Space Telescope Program FX This work is supported by the Hubble Space Telescope Program. NR 18 TC 0 Z9 0 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2014 VL 61 IS 6 BP 3356 EP 3362 DI 10.1109/TNS.2014.2360827 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA AX1RO UT WOS:000346724100077 ER PT J AU Hajra, R Echer, E Tsurutani, BT Gonzalez, WD AF Hajra, Rajkumar Echer, Ezequiel Tsurutani, Bruce T. Gonzalez, Walter D. TI Superposed epoch analyses of HILDCAAs and their interplanetary drivers: Solar cycle and seasonal dependences SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE HILDCAAs; High-speed streams; CIRs; Solar cycle phases ID COROTATING INTERACTION REGIONS; HELIOSPHERIC CURRENT SHEET; CORONAL MASS EJECTIONS; GEOMAGNETIC-ACTIVITY; HIGH-INTENSITY; LONG-DURATION; ELECTRON ACCELERATION; SEMIANNUAL VARIATION; MAGNETIC-FIELD; WIND STREAMS AB We study the solar cycle and seasonal dependences of high-intensity, long-duration, continuous AE activity (HILDCAA) events and associated solar wind/interplanetary external drivers for similar to 31/2 solar cycle period, from 1975 to 2011. 99 HILDCAAs which had simultaneous solar wind/interplanetary data are considered in the present analyses. The peak occurrence frequency of HILDCAAs was found to be in the descending phase of the solar cycle. These events had the strongest time-integrated AE intensities and were coincident with peak occurrences of high-speed solar wind streams. The event initiations were statistically coincident with high-to-slow speed stream interactions, compressions in the solar wind plasma and interplanetary magnetic field (IMF). The latter were corotating interaction regions (CIRs). The signatures of related CIRs were most prominent for the events occurring during the descending and solar minimum phases of the solar cycles. For these events, the solar wind speed increased by similar to 41% and similar to 57% across the CIRs, respectively. There was weak or no stream-stream interaction or CIR structure during the ascending and solar maximum phases. HILDCAAs occurring during spring and fall seasons were found to occur preferentially in negative and positive IMF sector regions (toward and away from the Sun), respectively. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Hajra, Rajkumar; Echer, Ezequiel; Gonzalez, Walter D.] INPE, BR-12227010 Sao Jose Dos Campos, SP, Brazil. [Tsurutani, Bruce T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hajra, R (reprint author), INPE, Av Dos Astronautas 1758, BR-12227010 Sao Jose Dos Campos, SP, Brazil. EM rajkumarhajra@yahoo.co.in RI Hajra, Rajkumar/C-1246-2011; OI Hajra, Rajkumar/0000-0003-0447-1531 FU Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) through post-doctoral research fellowship at INPE; Brazilian CNPq agency [301233/2011-0]; NASA; Jet Propulsion Laboratory, California Institute of Technology FX We wish to thank the two referees for their insightful and helpful comments. The work of RH. is financially supported by Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) through post-doctoral research fellowship at INPE. E.E. would like to thank to the Brazilian CNPq (301233/2011-0) agency for financial support. Portions of this research were performed at the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. NR 59 TC 6 Z9 6 U1 0 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD DEC PY 2014 VL 121 BP 24 EP 31 DI 10.1016/j.jastp.2014.09.012 PN A PG 8 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AX6GY UT WOS:000347022200003 ER PT J AU Liou, K Wu, CC Dryer, M Wu, ST Rich, N Plunkett, S Simpson, L Fry, CD Schenk, K AF Liou, Kan Wu, Chin-Chun Dryer, Murray Wu, Shi-Tsan Rich, Nathan Plunkett, Simon Simpson, Lynn Fry, Craig D. Schenk, Kevin TI Global simulation of extremely fast coronal mass ejection on 23 July 2012 SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Coronal mass ejection; MHD simulation; CME-driven shock ID SOLAR-WIND; INTERPLANETARY SPACE; GEOMAGNETIC STORMS; SHOCK-WAVES; BOW SHOCK; TIME; ARRIVAL; MODEL; EARTH; ACCELERATION AB The July 23, 2012 CME was an extremely fast backside event, reaching similar to 1 AU (STEREO-A) within 20 h as compared to similar to 3-6 days for typical CME events. Here, we present results from a simulation study of the CME and its driven shock using a combined kinematic and magnetohydrodynamic (MHD) simulation model, H3DMHD. In general, the model results match well with in situ measurements in the arrival time of the CME-driven shock and the total magnetic field strength, assuming an initial CME speed of 3100 km/s. Based on extrapolation of an empirical model, the fast CME and its large magnetic field (I vertical bar B vertical bar similar to 120 nT) are capable of producing an extremely large geomagnetic storm (Dst similar to - 545 nT), comparable to the well-known Halloween storm in 2003, if the CME had made a direct impact to the Earth. We investigated the effect of the adiabatic index (gamma). It is found that the shock tends to arrive slightly later for a smaller gamma value, and gamma=5/3 provides the best agreement for the shock arrival time. We also demonstrate that the strength (the Mach number) of the CME-driven fast-mode shock is not the largest at the "nose" of the CME. This is mainly due to the manifestation of fast-mode wave speed upstream of the shock. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Liou, Kan] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Wu, Chin-Chun; Rich, Nathan; Plunkett, Simon; Simpson, Lynn] US Navy, Res Lab, Washington, DC 20375 USA. [Dryer, Murray] NOAA, Space Weather Predict Ctr Ret, Boulder, CO 80305 USA. [Wu, Shi-Tsan] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Fry, Craig D.] Explorat Phys Int Inc, Huntsville, AL 35806 USA. [Schenk, Kevin] NASA, GSFC, Greenbelt, MD USA. RP Liou, K (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM kan.liou@jhuapl.edu RI Liou, Kan/C-2089-2016 OI Liou, Kan/0000-0001-5277-7688 FU NSF [AGS-0964396, AGS1153323]; APL's Janney grant; ONR 6.1 program FX We are grateful to the Reviewers for their constructive comments on the paper. We acknowledge the use of solar EUV disk and coronagraph images from the STEREO/SECCHI instrument (R.A. Howard, PI), solar wind plasma data from STEREO/PLASTIC Investigation (A.B. Galvin, PI), and magnetic field data from STEREO/IMPACT (J. Luhmann, PI). The SECCHI data used here are produced by an international consortium of the Naval Research Laboratory, Lockheed Martin Solar and Astrophysics Laboratory, and NASA Goddard Space Flight Center (USA), Rutherford Appleton Laboratory and University of Birmingham (UK), Max-Planck-Institut fur Sonnensystemforschung (Germany), Centre Spatiale de Liege (Belgium), Institut d'Optique Theorique et Appliquee and Institut d'Astrophysique Spatiale (France). The work at JHUAPL was supported partially by NSF Grant AGS-0964396. KL acknowledges support from APL's Janney grant for preparation of the manuscript. The work at NRL was supported by ONR 6.1 program. The work of S.-T. Wu is supported by NSF Grant AGS1153323 to UAH. NR 54 TC 11 Z9 11 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD DEC PY 2014 VL 121 BP 32 EP 41 DI 10.1016/j.jastp.2014.09.013 PN A PG 10 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AX6GY UT WOS:000347022200004 ER PT J AU Zhang, XL Mao, M Berg, MJ Sun, WB AF Zhang, Xiaolin Mao, Mao Berg, Matthew J. Sun, Wenbo TI Insight into wintertime aerosol characteristics over Beijing SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Aerosol; Microphysical and optical properties; Haze episode; Beijing urban area ID NORTH CHINA PLAIN; SINGLE-SCATTERING PROPERTIES; SOOT-CONTAINING AEROSOLS; PEARL RIVER-DELTA; OPTICAL-PROPERTIES; RADIATIVE-TRANSFER; LIGHT-ABSORPTION; SPECTRAL RELATIONSHIPS; BOUNDARY-LAYER; URBAN AREA AB Aerosol particle pollution in northern China has crucial impact on regional and global climate. The monthly mean aerosol optical depth (ACID) at 550 nm in the northern China had its minimum in winter. Surface measurements of aerosol microphysical and optical properties over the Beijing urban area from December 3, 2011 to January 1, 2012 are presented here. The aim of this study was to evaluate wintertime aerosol characteristics, which were impacted by wind and relative humidity. The following mean values were observed: scattering coefficient (293 +/- 283 Mm(-1), 1 Mm(-1)=10(-6) m(-1)), absorption coefficient (136 +/- 125 Mm(-1)), backscattering ratio (0.15 +/- 0.02), single scattering albedo (0.65 +/- 0.08), at 550 nm, and scattering Angstrom exponent (2.01 +/- 0.22), with mean relative humidity of (47 +/- 24)%. Wintertime values of scattering and absorption coefficients had wind dependence, showing that high values occurred with calm winds while the dilution effect of strong winds was obtained for wind speed larger than 4 m s(-1). Based on air mass backward trajectories, wintertime haze episodes in Beijing were induced by local-pollution emissions, whereas clear periods were dominated by air masses from clean, continental, northwestern areas. Our study indicates that the main challenge to improve wintertime air quality in Beijing is to control local emissions of particulate pollution. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Zhang, Xiaolin; Mao, Mao] Nanjing Univ Informat Sci & Technol, Sch Atmospher Phys, Nanjing 210044, Jiangsu, Peoples R China. [Zhang, Xiaolin] Univ Chinese Acad Sci, Beijing 100039, Peoples R China. [Zhang, Xiaolin; Berg, Matthew J.] Mississippi State Univ, Mississippi State, MS 39762 USA. [Sun, Wenbo] Sci Syst & Applicat Inc, Hampton, VA 23666 USA. [Sun, Wenbo] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Mao, M (reprint author), Nanjing Univ Informat Sci & Technol, Sch Atmospher Phys, Nanjing 210044, Jiangsu, Peoples R China. EM mcszlx@gmail.com RI Xiongfei, Zhao/G-7690-2015 FU National Natural Science Foundation of China (NSFC) [21406189]; Startup Foundation for Introducing Talent of NUIST [S8113073001]; China Scholarship FX This work was supported by the National Natural Science Foundation of China (NSFC) under Grant no. 21406189 and the Startup Foundation for Introducing Talent of NUIST under Grant no. S8113073001. This work was also funded by the China Scholarship. The Analysis and visualizations used in this study were produced with the Giovanni online data system, developed and maintained by the NASA Goddard Earth Sciences (GES) Data and Information Services Center (DISC). The authors gratefully acknowledge the NOAA Air Resources Laboratory (ARL) for the provision of the HYSPLIT transport and dispersion model and/or READY website (http://www.ready.noaa.gov) used in this publication. NR 64 TC 3 Z9 3 U1 0 U2 30 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD DEC PY 2014 VL 121 BP 63 EP 71 DI 10.1016/j.jastp.2014.09.017 PN A PG 9 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AX6GY UT WOS:000347022200008 ER PT J AU Hartwig, J Darr, S AF Hartwig, Jason Darr, Samuel TI Analytical model for steady flow through a finite channel with one porous wall with arbitrary variable suction or injection SO PHYSICS OF FLUIDS LA English DT Article ID DIRECT NUMERICAL-SIMULATION; PARTICLE IMAGE VELOCIMETRY; LAMINAR BOUNDARY-LAYER; REYNOLDS-STRESS MODEL; MASS-TRANSFER; LIQUID-HYDROGEN; PERMEABLE WALL; ULTRAFILTRATION PERFORMANCE; MEMBRANE FILTRATION; 3-DIMENSIONAL FLOW AB This paper presents an exact solution of two-dimensional laminar flow through a finite length channel with one porous wall. It improves upon previous solutions by (1) satisfying the no-slip boundary condition at the channel dead end, (2) adding a turbulent term to the porous wall boundary condition, (3) allowing for arbitrary variable suction or injection across the porous wall, and (4) model validation against new cryogenic liquid hydrogen and oxygen experimental data. Of particular interest in the current work is the modeling of cryogenic propellant flow through a porous liquid acquisition device (LAD) screen and channel inside a propellant tank. First, a detailed review of the literature is presented for previously attempted solutions to channel flow with one porous wall. Next, the governing equations, boundary conditions, and model assumptions are used to derive the analytical flow solution and present general model results for pressure and velocity fields within the channel. Then, the model solution is compared with horizontal LAD channel flow data in liquid oxygen as well as vertical LAD channel flow data in an inverted outflow configuration in liquid hydrogen. Model results are used to update the static cryogenic bubble point pressure model with a dynamic bubble point term which factors in enhanced convection and cooling at the screen during propellant outflow. Convective heat transfer at the LAD screen during outflow is also quantified by comparing model and data. The new analytical flow solution with the dynamic bubble point model is shown to compare well with available cryogenic experimental data. (C) 2014 AIP Publishing LLC. C1 [Hartwig, Jason] NASA Glenn Res Ctr, Propuls & Propellants Branch, Cleveland, OH 44135 USA. [Darr, Samuel] Univ Florida, Gainesville, FL 32611 USA. RP Hartwig, J (reprint author), NASA Glenn Res Ctr, Propuls & Propellants Branch, Cleveland, OH 44135 USA. EM Jason.W.Hartwig@nasa.gov NR 109 TC 3 Z9 3 U1 2 U2 20 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1070-6631 EI 1089-7666 J9 PHYS FLUIDS JI Phys. Fluids PD DEC PY 2014 VL 26 IS 12 AR 123603 DI 10.1063/1.4904739 PG 24 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA AX8LS UT WOS:000347161600034 ER PT J AU Hooker, SB Morrow, JH Booth, CR AF Hooker, Stanford B. Morrow, John H. Booth, Charles R. TI OCULLAR Next-Generation Research: Ocean Color at Night Hybridnamic Multitectors Use the Moon for Ocean Color Research SO SEA TECHNOLOGY LA English DT Article C1 [Hooker, Stanford B.] NASA, Washington, DC 20546 USA. [Morrow, John H.] Univ So Calif, Los Angeles, CA 90089 USA. [Booth, Charles R.] Scripps Inst Oceanog, San Diego, CA USA. RP Hooker, SB (reprint author), NASA, Washington, DC 20546 USA. FU GSFC IRAD program [NNG13HA84P, NNG13HF62P] FX The authors gratefully acknowledge the many essential engineering contributions to the OCULLAR project made by Randall Lind, director of manufacturing and engineering at Biospherical Instruments Inc. (San Diego, California). The project was funded by the GSFC IRAD program under contract numbers NNG13HA84P and NNG13HF62P. NR 0 TC 0 Z9 0 U1 1 U2 2 PU COMPASS PUBLICATIONS, INC PI ARLINGTON PA 1501 WILSON BLVD., STE 1001, ARLINGTON, VA 22209-2403 USA SN 0093-3651 J9 SEA TECHNOL JI Sea Technol. PD DEC PY 2014 VL 55 IS 12 BP 15 EP + PG 4 WC Engineering, Ocean SC Engineering GA AX5EC UT WOS:000346948700003 ER PT J AU Neigh, CSR Bolton, DK Williams, JJ Diabate, M AF Neigh, Christopher S. R. Bolton, Douglas K. Williams, Jennifer J. Diabate, Mouhamad TI Evaluating an Automated Approach for Monitoring Forest Disturbances in the Pacific Northwest from Logging, Fire and Insect Outbreaks with Landsat Time Series Data SO FORESTS LA English DT Article DE Pacific Northwest; Landsat; AVHRR; disturbance; time series; NDVI; logging; insect; fire; GIMMS ID MOUNTAIN PINE-BEETLE; ACCURACY ASSESSMENT; TREE MORTALITY; WESTERN OREGON; UNITED-STATES; BARK BEETLE; SAMPLING DESIGNS; SATELLITE DATA; CARBON BUDGET; BURN SEVERITY AB Forests are the largest aboveground sink for atmospheric carbon (C), and understanding how they change through time is critical to reduce our C-cycle uncertainties. We investigated a strong decline in Normalized Difference Vegetation Index (NDVI) from 1982 to 1991 in Pacific Northwest forests, observed with the National Ocean and Atmospheric Administration's (NOAA) series of Advanced Very High Resolution Radiometers (AVHRRs). To understand the causal factors of this decline, we evaluated an automated classification method developed for Landsat time series stacks (LTSS) to map forest change. This method included: (1) multiple disturbance index thresholds; and (2) a spectral trajectory-based image analysis with multiple confidence thresholds. We produced 48 maps and verified their accuracy with air photos, monitoring trends in burn severity data and insect aerial detection survey data. Area-based accuracy estimates for change in forest cover resulted in producer's and user's accuracies of 0.21 +/- 0.06 to 0.38 +/- 0.05 for insect disturbance, 0.23 +/- 0.07 to 1 +/- 0 for burned area and 0.74 +/- 0.03 to 0.76 +/- 0.03 for logging. We believe that accuracy was low for insect disturbance because air photo reference data were temporally sparse, hence missing some outbreaks, and the annual anniversary time step is not dense enough to track defoliation and progressive stand mortality. Producer's and user's accuracy for burned area was low due to the temporally abrupt nature of fire and harvest with a similar response of spectral indices between the disturbance index and normalized burn ratio. We conclude that the spectral trajectory approach also captures multi-year stress that could be caused by climate, acid deposition, pathogens, partial harvest, thinning, etc. Our study focused on understanding the transferability of previously successful methods to new ecosystems and found that this automated method does not perform with the same accuracy in Pacific Northwest forests. Using a robust accuracy assessment, we demonstrate the difficulty of transferring change attribution methods to other ecosystems, which has implications for the development of automated detection/attribution approaches. Widespread disturbance was found within AVHRR-negative anomalies, but identifying causal factors in LTSS with adequate mapping accuracy for fire and insects proved to be elusive. Our results provide a background framework for future studies to improve methods for the accuracy assessment of automated LTSS classifications. C1 [Neigh, Christopher S. R.] NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bolton, Douglas K.] Univ British Columbia, Dept Forest Resources Management, Vancouver, BC V6T 1Z4, Canada. [Williams, Jennifer J.] Royal Bot Gardens, Richmond TW9 3AE, Surrey, England. [Diabate, Mouhamad] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. RP Neigh, CSR (reprint author), NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Code 618, Greenbelt, MD 20771 USA. EM christopher.s.neigh@nasa.gov; doug.k.bolton@alumni.ubc.ca; jenjwilliams@gmail.com; mdiabate@gmail.com RI Neigh, Christopher/D-4700-2012 OI Neigh, Christopher/0000-0002-5322-6340 FU NASA's Terrestrial Ecology program [NNH08ZDA001N-TE] FX This study was made possible by NASA's Terrestrial Ecology program under Grant NNH08ZDA001N-TE. We would like to thank Compton Tucker for suggestions that improved the quality of the manuscript. We would also like to thank the three anonymous reviewers that provided comments that enhanced the content and structure of this manuscript. NR 88 TC 1 Z9 1 U1 2 U2 40 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 1999-4907 J9 FORESTS JI Forests PD DEC PY 2014 VL 5 IS 12 BP 3169 EP 3198 DI 10.3390/f5123169 PG 30 WC Forestry SC Forestry GA AX2TT UT WOS:000346798100013 ER PT J AU Juarez, PD Matthews-Juarez, P Hood, DB Im, W Levine, RS Kilbourne, BJ Langston, MA Al-Hamdan, MZ Crosson, WL Estes, MG Estes, SM Agboto, VK Robinson, P Wilson, S Lichtveld, MY AF Juarez, Paul D. Matthews-Juarez, Patricia Hood, Darryl B. Im, Wansoo Levine, Robert S. Kilbourne, Barbara J. Langston, Michael A. Al-Hamdan, Mohammad Z. Crosson, William L. Estes, Maurice G. Estes, Sue M. Agboto, Vincent K. Robinson, Paul Wilson, Sacoby Lichtveld, Maureen Y. TI The Public Health Exposome: A Population-Based, Exposure Science Approach to Health Disparities Research SO INTERNATIONAL JOURNAL OF ENVIRONMENTAL RESEARCH AND PUBLIC HEALTH LA English DT Article DE exposome; public health; health disparities; trans-disciplinary; exposure science; social-ecological; combinatorial analysis; CBPR; geographical information systems; PPGIS ID BLACK-WHITE DISPARITIES; ENVIRONMENTAL JUSTICE; PARTICIPATORY RESEARCH; UNITED-STATES; TELOMERE LENGTH; LOS-ANGELES; AIR TOXICS; FRAMEWORK; COMMUNITY; EPIDEMIOLOGY AB The lack of progress in reducing health disparities suggests that new approaches are needed if we are to achieve meaningful, equitable, and lasting reductions. Current scientific paradigms do not adequately capture the complexity of the relationships between environment, personal health and population level disparities. The public health exposome is presented as a universal exposure tracking framework for integrating complex relationships between exogenous and endogenous exposures across the lifespan from conception to death. It uses a social-ecological framework that builds on the exposome paradigm for conceptualizing how exogenous exposures "get under the skin". The public health exposome approach has led our team to develop a taxonomy and bioinformatics infrastructure to integrate health outcomes data with thousands of sources of exogenous exposure, organized in four broad domains: natural, built, social, and policy environments. With the input of a transdisciplinary team, we have borrowed and applied the methods, tools and terms from various disciplines to measure the effects of environmental exposures on personal and population health outcomes and disparities, many of which may not manifest until many years later. As is customary with a paradigm shift, this approach has far reaching implications for research methods and design, analytics, community engagement strategies, and research training. C1 [Juarez, Paul D.; Matthews-Juarez, Patricia] Univ Tennessee, Ctr Hlth Sci, Res Ctr Hlth Dispar Equ & Exposome, Memphis, TN 38105 USA. [Hood, Darryl B.] Ohio State Univ, Dept Environm Hlth Sci, Coll Publ Hlth, Columbus, OH 43210 USA. [Im, Wansoo] Vertices Inc, New Brunswick, NJ 08901 USA. [Levine, Robert S.; Agboto, Vincent K.] Meharry Med Coll, Dept Family & Community Med, Nashville, TN 37208 USA. [Kilbourne, Barbara J.] Tennessee State Univ, Dept Sociol, Nashville, TN 37209 USA. [Langston, Michael A.] Univ Tennessee, Dept Elect Engn & Comp Sci, Knoxville, TN 37996 USA. [Al-Hamdan, Mohammad Z.; Crosson, William L.; Estes, Sue M.] NASA, Natl Space Sci & Technol Ctr, Univ Space Res Assoc, Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Estes, Maurice G.] Univ Alabama, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. [Robinson, Paul] Charles R Drew Univ Med & Sci, Dept Ophthalmol, Los Angeles, CA 90059 USA. [Wilson, Sacoby] Univ Maryland, Sch Publ Hlth, Maryland Inst Appl Environm Hlth, College Pk, MD 20742 USA. [Lichtveld, Maureen Y.] Tulane Univ, Dept Global Environm Hlth Sci, Sch Publ Hlth & Trop Med, New Orleans, LA 70112 USA. RP Juarez, PD (reprint author), Univ Tennessee, Ctr Hlth Sci, Res Ctr Hlth Dispar Equ & Exposome, 66 N Pauline, Memphis, TN 38105 USA. EM pjuarez@uthsc.edu; pmatthe3@uthsc.edu; hood.188@osu.edu; wansooim@gmail.com; rlevine@mmc.edu; bkilbourne@tnstate.edu; langston@eecs.utk.edu; mohammad.alhamdan@nasa.gov; bill.crosson@nasa.gov; maury.estes@nsstc.uah.edu; sue.m.estes@nasa.gov; vagboto@mmc.edu; paulrobinson@cdrewu.edu; swilson2@umd.edu; mlichtve@tulane.edu FU Environmental Protection Agency [3P20MD000516-07S1]; National Center on Minority Health and Health Disparities FX We wish to thank Katy Kilbourne, Vicente Samaniego, Tyler Skelton, and Charlotte Woods, for their tireless efforts and dedicated support in preparing and managing data and generating maps. "Funding for this article was made possible (in part) by 3P20MD000516-07S1 by a grant received from the Environmental Protection Agency and the National Center on Minority Health and Health Disparities. The views expressed in written conference materials or publications and by speakers and moderators do not necessarily reflect the official policies of the Department of Health and Human Services; nor does mention by trade names, commercial practices, or organizations imply endorsement by the U.S. Government". NR 88 TC 9 Z9 9 U1 7 U2 46 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 1660-4601 J9 INT J ENV RES PUB HE JI Int. J. Environ. Res. Public Health PD DEC PY 2014 VL 11 IS 12 BP 12866 EP 12895 DI 10.3390/ijerph111212866 PG 30 WC Environmental Sciences; Public, Environmental & Occupational Health SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health GA AX2TJ UT WOS:000346797100050 PM 25514145 ER PT J AU Montanaro, M Levy, R Markham, B AF Montanaro, Matthew Levy, Raviv Markham, Brian TI On-Orbit Radiometric Performance of the Landsat 8 Thermal Infrared Sensor SO REMOTE SENSING LA English DT Article DE Landsat; TIRS; performance; noise; stability AB The Thermal Infrared Sensor (TIRS) requirements for noise, stability, and uniformity were designed to ensure the radiometric integrity of the data products. Since the launch of Landsat 8 in February 2013, many of these evaluations have been based on routine measurements of the onboard calibration sources, which include a variable-temperature blackbody and a deep space view port. The noise equivalent change in temperature (NEdT) of TIRS data is approximately 0.05 K @ 300 K in both bands, exceeding requirements by about a factor of 8 and Landsat 7 ETM+ performance by a factor of 3. Coherent noise is not readily apparent in TIRS data. No apparent change in the detector linearization has been observed. The radiometric stability of the TIRS instrument over the period between radiometric calibrations (about 40 min) is less than one count of dark current and the variation in terms of radiance is less than 0.015 W/m(2)/sr/mu m (or 0.13 K) at 300 K, easily meeting the short term stability requirements. Long term stability analysis has indicated a degradation of about 0.2% or less per year. The operational calibration is only updated using the biases taken every orbit, due to the fundamental stability of the instrument. By combining the data from two active detector rows per band, 100% detector operability is maintained for the instrument. No trends in the noise, operability, or short term radiometric stability are apparent over the mission life. The uniformity performance is more difficult to evaluate as scene-varying banding artifacts have been observed in Earth imagery. Analyses have shown that stray light is affecting the recorded signal from the Earth and inducing the banding depending on the content of the surrounding Earth surface. As the stray light effects are stronger in the longer wavelength TIRS band11 (12.0 mu m), the uniformity is better in the shorter wavelength band10 (10.9 mu m). Both bands have exceptional noise and stability performance and band10 has generally adequate uniformity performance and should currently be used in preference to band11. The product uniformity will improve with the stray light corrections being developed. C1 [Montanaro, Matthew] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA. [Levy, Raviv] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. [Markham, Brian] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Montanaro, M (reprint author), NASA, Goddard Space Flight Ctr, Sigma Space Corp, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM matthew.montanaro@nasa.gov; raviv.levy-1@nasa.gov; brian.l.markham@nasa.gov FU NASA [NNG09HP18C] FX The work presented here was funded under NASA contract NNG09HP18C. NR 11 TC 10 Z9 11 U1 0 U2 12 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD DEC PY 2014 VL 6 IS 12 BP 11753 EP 11769 DI 10.3390/rs61211753 PG 17 WC Remote Sensing SC Remote Sensing GA AX2ST UT WOS:000346795300005 ER PT J AU Markham, B Barsi, J Kvaran, G Ong, L Kaita, E Biggar, S Czapla-Myers, J Mishra, N Helder, D AF Markham, Brian Barsi, Julia Kvaran, Geir Ong, Lawrence Kaita, Edward Biggar, Stuart Czapla-Myers, Jeffrey Mishra, Nischal Helder, Dennis TI Landsat-8 Operational Land Imager Radiometric Calibration and Stability SO REMOTE SENSING LA English DT Article DE Landsat; radiometry; calibration ID SPECTRAL IRRADIANCE; ORBIT AB The Landsat-8 Operational Land Imager (OLI) was radiometrically calibrated prior to launch in terms of spectral radiance, using an integrating sphere source traceable to National Institute of Standards and Technology (NIST) standards of spectral irradiance. It was calibrated on-orbit in terms of reflectance using diffusers characterized prior to launch using NIST traceable standards. The radiance calibration was performed with an uncertainty of similar to 3%; the reflectance calibration to an uncertainty of similar to 2%. On-orbit, multiple calibration techniques indicate that the sensor has been stable to better than 0.3% to date, with the exception of the shortest wavelength band, which has degraded about 1.0%. A transfer to orbit experiment conducted using the OLI's heliostat-illuminated diffuser suggests that some bands increased in sensitivity on transition to orbit by as much as 5%, with an uncertainty of similar to 2.5%. On-orbit comparisons to other instruments and vicarious calibration techniques show the radiance (without a transfer to orbit adjustment), and reflectance calibrations generally agree with other instruments and ground measurements to within the uncertainties. Calibration coefficients are provided with the data products to convert to either radiance or reflectance units. C1 [Markham, Brian] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Barsi, Julia; Ong, Lawrence; Kaita, Edward] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. [Kvaran, Geir] Ball Aerosp & Technol Corp, Boulder, CO 80301 USA. [Biggar, Stuart; Czapla-Myers, Jeffrey] Univ Arizona, Coll Opt Sci, Remote Sensing Grp, Tucson, AZ 85721 USA. [Mishra, Nischal; Helder, Dennis] S Dakota State Univ, Coll Engn, Brookings, SD 57007 USA. RP Markham, B (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA. EM Brian.L.Markham@nasa.gov; Julia.A.Barsi@nasa.gov; gkvaran@ball.com; Lawrence.Ong@nasa.gov; Edward.Kaita-1@nasa.gov; biggar@optics.arizona.edu; jscm@optics.arizona.edu; Nischal.Mishra@sdstate.edu; Dennis.Helder@sdstate.edu OI Czapla-Myers, Jeffrey/0000-0003-4804-5358 FU NASA [NNG07HW18C, NNG09HP18C] FX Ball Aerospace's work and the University of Arizona's BRDF characterizations were performed under NASA Contract NNG07HW18C.; Science Systems and Applications work was performed under NASA contract NNG09HP18C. NR 26 TC 24 Z9 26 U1 0 U2 14 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD DEC PY 2014 VL 6 IS 12 BP 12275 EP 12308 DI 10.3390/rs61212275 PG 34 WC Remote Sensing SC Remote Sensing GA AX2ST UT WOS:000346795300028 ER PT J AU Sedano, F Kempeneers, P Hurtt, G AF Sedano, Fernando Kempeneers, Pieter Hurtt, George TI A Kalman Filter-Based Method to Generate Continuous Time Series of Medium-Resolution NDVI Images SO REMOTE SENSING LA English DT Article DE Kalman filter; Landsat; MODIS; time series; data fusion; filtering; smoothing; monitoring; uncertainty ID LANDSAT SURFACE REFLECTANCE; BOREAL FOREST COVER; ETM PLUS DATA; VEGETATION DYNAMICS; MULTITEMPORAL MODIS; LEAF-AREA; DATA SET; PRODUCTS; FUSION; MODEL AB A data assimilation method to produce complete temporal sequences of synthetic medium-resolution images is presented. The method implements a Kalman filter recursive algorithm that integrates medium and moderate resolution imagery. To demonstrate the approach, time series of 30-m spatial resolution NDVI images at 16-day time steps were generated using Landsat NDVI images and MODIS NDVI products at four sites with different ecosystems and land cover-land use dynamics. The results show that the time series of synthetic NDVI images captured seasonal land surface dynamics and maintained the spatial structure of the landscape at higher spatial resolution. The time series of synthetic medium-resolution NDVI images were validated within a Monte Carlo simulation framework. Normalized residuals decreased as the number of available observations increased, ranging from 0.2 to below 0.1. Residuals were also significantly lower for time series of synthetic NDVI images generated at combined recursion (smoothing) than individually at forward and backward recursions (filtering). Conversely, the uncertainties of the synthetic images also decreased when the number of available observations increased and combined recursions were implemented. C1 [Sedano, Fernando; Hurtt, George] Univ Maryland, Dept Geog Sci, College Pk, MD 20740 USA. [Sedano, Fernando] NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA. [Kempeneers, Pieter] Vlaamse Instelling Technol Onderzoek, B-2400 Mol, Belgium. RP Sedano, F (reprint author), Univ Maryland, Dept Geog Sci, 2181 LeFrak Hall, College Pk, MD 20740 USA. EM fsedano@umd.edu; kempenep@gmail.com; gchurtt@umd.edu FU Joint Global Carbon Cycle Center FX This work was performed with the support of the Joint Global Carbon Cycle Center. We thank Giuseppe Amatulli and Nicholas Clinton for their comments on the early version of the manuscript, which substantially improved the manuscript. NR 79 TC 6 Z9 6 U1 2 U2 14 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD DEC PY 2014 VL 6 IS 12 BP 12381 EP 12408 DI 10.3390/rs61212381 PG 28 WC Remote Sensing SC Remote Sensing GA AX2ST UT WOS:000346795300032 ER PT J AU Lee, S Chiang, KF Xiong, XX Sun, CB Anderson, S AF Lee, Shihyan Chiang, Kwofu Xiong, Xiaoxiong Sun, Chengbo Anderson, Samuel TI The S-NPP VIIRS Day-Night Band On-Orbit Calibration/Characterization and Current State of SDR Products SO REMOTE SENSING LA English DT Article DE remote sensing; nighttime lights; day-night band; Vis/NIR; VIIRS; on-orbit calibration; Solar Diffuser; stray light; noise; SNR AB The launch of VIIRS on-board the Suomi-National Polar-orbiting Partnership (S-NPP) on 28 October 2011, marked the beginning of the next chapter on nighttime lights observation started by the Defense Meteorological Satellite Program's (DMSP) OLS sensor more than two decades ago. The VIIRS observes the nighttime lights on Earth through its day-night band (DNB), a panchromatic channel covering the wavelengths from 500 nm to 900 nm. Compared to its predecessors, the VIIRS DNB has a much improved spatial/temporal resolution, radiometric sensitivity and, more importantly, continuous calibration using on-board calibrators (OBCs). In this paper, we describe the current state of the NASA calibration and characterization methodology used in supporting mission data quality assurance and producing consistent mission-wide sensor data records (SDRs) through NASA's Land Product Evaluation and Analysis Tool Element (Land PEATE). The NASA calibration method utilizes the OBCs to determine gains, offset drift and sign-to-noise ratio (SNR) over the entire mission. In gain determination, the time-dependent relative spectral response (RSR) is used to correct the optical throughput change over time. A deep space view acquired during an S-NPP pitch maneuver is used to compute the airglow free dark offset for DNB's high gain stage. The DNB stray light is estimated each month from new-moon dark Earth surface observations to remove the excessive stray light over the day-night terminators. As the VIIRS DNB on-orbit calibration is the first of its kind, the evolution of the calibration methodology is evident when the S-NPP VIIRS's official calibrations are compared with our latest mission-wide reprocessing. In the future, the DNB calibration methodology is likely to continue evolving, and the mission-wide reprocessing is a key to providing consistently calibrated DNB SDRs for the user community. In the meantime, the NASA Land PEATE provides an alternative source to obtain mission-wide DNB SDR products that are calibrated based on the latest NASA DNB calibration methodology. C1 [Lee, Shihyan] Earth Resource Technol Inc, Laurel, MD 20707 USA. [Chiang, Kwofu; Sun, Chengbo; Anderson, Samuel] Sigma Space Corp, Lanham, MD 20706 USA. [Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20661 USA. RP Lee, S (reprint author), Earth Resource Technol Inc, 14401 Sweitzer Lane, Laurel, MD 20707 USA. EM shihyanlee@yahoo.com; Vincent.Chiang@ssaihq.com; Xiaoxiong.Xiong.1@gsfc.nasa.gov; Chengbo.Sun@ssaihq.com; Samuel.Anderson@ssaihq.com NR 20 TC 9 Z9 9 U1 1 U2 14 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD DEC PY 2014 VL 6 IS 12 BP 12427 EP 12446 DI 10.3390/rs61212427 PG 20 WC Remote Sensing SC Remote Sensing GA AX2ST UT WOS:000346795300034 ER PT J AU Mishra, N Haque, MO Leigh, L Aaron, D Helder, D Markham, B AF Mishra, Nischal Haque, Md Obaidul Leigh, Larry Aaron, David Helder, Dennis Markham, Brian TI Radiometric Cross Calibration of Landsat 8 Operational Land Imager (OLI) and Landsat 7 Enhanced Thematic Mapper Plus (ETM plus ) SO REMOTE SENSING LA English DT Article DE Operational Land Imager (OLI); Landsat; ETM; PICS; cross-calibration; Spectral Band Adjustment Factor (SBAF) ID OPTICAL SATELLITE SENSORS; DATA CONTINUITY MISSION; DESERT SITES; ABSOLUTE CALIBRATION; INTERCALIBRATION; PERFORMANCE; STABILITY; HYPERION; TARGETS; IMPACT AB This study evaluates the radiometric consistency between Landsat-8 Operational Land Imager (OLI) and Landsat 7 Enhanced Thematic Mapper Plus (ETM+) using cross calibration techniques. Two approaches are used, one based on cross calibration between the two sensors using simultaneous image pairs, acquired during an underfly event on 29-30 March 2013. The other approach is based on using time series of image statistics acquired by these two sensors over the Libya 4 pseudo invariant calibration site (PICS) (+28.55 degrees N, + 23.39 degrees E). Analyses from these approaches show that the reflectance calibration of OLI is generally within +/- 3% of the ETM+ radiance calibration for all the reflective bands from visible to short wave infrared regions when the ChKur solar spectrum is used to convert the ETM+ radiance to reflectance. Similar results are obtained comparing the OLI radiance calibration directly with the ETM+ radiance calibration and the results in these two different physical units (radiance and reflectance) agree to within +/- 2% for all the analogous bands. These results will also be useful to tie all the Landsat heritage sensors from Landsat 1 MultiSpectral Scanner (MSS) through Landsat-8 OLI to a consistent radiometric scale. C1 [Mishra, Nischal; Leigh, Larry; Aaron, David; Helder, Dennis] S Dakota State Univ, Engn Off Res, Brookings, SD 57007 USA. [Haque, Md Obaidul] SGT Inc, Sioux Falls, SD 57198 USA. [Markham, Brian] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. RP Mishra, N (reprint author), S Dakota State Univ, Engn Off Res, Brookings, SD 57007 USA. EM Nischal.Mishra@sdstate.edu; ohaque@usgs.gov; Larry.Leigh@sdstate.edu; David.Aaron@sdstate.edu; Dennis.Helder@sdstate.edu; Brian.L.Markham@nasa.gov FU NASA from Landsat Project Science Office [NNX09AH23A]; USGS EROS [G08AC00031]; USGS [G10PC00044] FX The authors would like to thank the Landsat Calibration/Validation Team at the USGS EROS Data Center and NASA Goddard Space Flight Center for their advice and feedback on this project. We are also grateful to the reviewers and editors for their valuable comments and insights in the article. This work was supported by NASA grant NNX09AH23A from the Landsat Project Science Office, by USGS EROS grant G08AC00031 and under USGS contract #G10PC00044. NR 30 TC 21 Z9 21 U1 6 U2 26 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD DEC PY 2014 VL 6 IS 12 BP 12619 EP 12638 DI 10.3390/rs61212619 PG 20 WC Remote Sensing SC Remote Sensing GA AX2ST UT WOS:000346795300043 ER PT J AU Duignan, PJ Van Bressem, MF Baker, JD Barbieri, M Colegrove, KM De Guise, S de Swart, RL Di Guardo, G Dobson, A Duprex, WP Early, G Fauquier, D Goldstein, T Goodman, SJ Grenfell, B Groch, KR Gulland, F Hall, A Jensen, BA Lamy, K Matassa, K Mazzariol, S Morris, SE Nielsen, O Rotstein, D Rowles, TK Saliki, JT Siebert, U Waltzek, T Wellehan, JFX AF Duignan, Padraig J. Van Bressem, Marie-Francoise Baker, Jason D. Barbieri, Michelle Colegrove, Kathleen M. De Guise, Sylvain de Swart, Rik L. Di Guardo, Giovanni Dobson, Andrew Duprex, W. Paul Early, Greg Fauquier, Deborah Goldstein, Tracey Goodman, Simon J. Grenfell, Bryan Groch, Katia R. Gulland, Frances Hall, Ailsa Jensen, Brenda A. Lamy, Karina Matassa, Keith Mazzariol, Sandro Morris, Sinead E. Nielsen, Ole Rotstein, David Rowles, Teresa K. Saliki, Jeremy T. Siebert, Ursula Waltzek, Thomas Wellehan, James F. X. TI Phocine Distemper Virus: Current Knowledge and Future Directions SO VIRUSES-BASEL LA English DT Review DE Morbillivirus; pinnipeds; sea otter; CD150/SLAM; phylogeny; pathology; epidemiology; immunity; vaccine ID EUROPEAN HARBOR SEALS; OTTERS ENHYDRA-LUTRIS; SCOTTISH GREY SEALS; HAWAIIAN MONK SEAL; CANINE-DISTEMPER; MEASLES-VIRUS; HALICHOERUS-GRYPUS; MORBILLIVIRUS INFECTION; MASS MORTALITY; CETACEAN MORBILLIVIRUS AB Phocine distemper virus (PDV) was first recognized in 1988 following a massive epidemic in harbor and grey seals in north-western Europe. Since then, the epidemiology of infection in North Atlantic and Arctic pinnipeds has been investigated. In the western North Atlantic endemic infection in harp and grey seals predates the European epidemic, with relatively small, localized mortality events occurring primarily in harbor seals. By contrast, PDV seems not to have become established in European harbor seals following the 1988 epidemic and a second event of similar magnitude and extent occurred in 2002. PDV is a distinct species within the Morbillivirus genus with minor sequence variation between outbreaks over time. There is now mounting evidence of PDV-like viruses in the North Pacific/Western Arctic with serological and molecular evidence of infection in pinnipeds and sea otters. However, despite the absence of associated mortality in the region, there is concern that the virus may infect the large Pacific harbor seal and northern elephant seal populations or the endangered Hawaiian monk seals. Here, we review the current state of knowledge on PDV with particular focus on developments in diagnostics, pathogenesis, immune response, vaccine development, phylogenetics and modeling over the past 20 years. C1 [Duignan, Padraig J.; Lamy, Karina] Univ Calgary, Dept Ecosyst & Publ Hlth, Calgary, AB T2N 4Z6, Canada. [Van Bressem, Marie-Francoise] Peruvian Ctr Cetacean Res CEPEC, Cetacean Conservat Med Grp CMED, Lima 20, Peru. [Baker, Jason D.; Barbieri, Michelle] NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96818 USA. [Barbieri, Michelle; Gulland, Frances] Marine Mammal Ctr, Sausalito, CA 94965 USA. [Colegrove, Kathleen M.] Univ Illinois, Coll Vet Med, Zool Pathol Program, Maywood, IL 60153 USA. [De Guise, Sylvain] Univ Connecticut, Dept Pathobiol & Vet Sci, Storrs, CT 06269 USA. [De Guise, Sylvain] Univ Connecticut, Connecticut Sea Grant Coll Program, Storrs, CT 06269 USA. [de Swart, Rik L.] Erasmus MC, Dept Virosci, NL-3015 CN Rotterdam, Netherlands. [Di Guardo, Giovanni] Univ Teramo, Fac Vet Med, I-64100 Teramo, Italy. [Dobson, Andrew; Grenfell, Bryan; Morris, Sinead E.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Duprex, W. Paul] Boston Univ, Sch Med, Dept Microbiol, Boston, MA 02118 USA. [Early, Greg] Integrated Stat, Woods Hole, MA 02543 USA. [Fauquier, Deborah; Rowles, Teresa K.] NOAA, Natl Marine Fisheries Serv, Marine Mammal Hlth & Stranding Response Program, Silver Spring, MD 20910 USA. [Goldstein, Tracey] Univ Calif Davis, Sch Vet Med, Hlth Inst 1, Davis, CA 95616 USA. [Goodman, Simon J.] Univ Leeds, Sch Biol, Leeds LS2 9JT, W Yorkshire, England. [Grenfell, Bryan] NIH, Fogarty Int Ctr, Bethesda, MD 20892 USA. [Groch, Katia R.] Univ Sao Paulo, Sch Vet Med & Anim Sci, Dept Pathol, BR-05508270 Sao Paulo, Brazil. [Gulland, Frances] Marine Mammal Commiss, Bethesda, MD 20814 USA. [Hall, Ailsa] Univ St Andrews, Scottish Oceans Inst, Sea Mammal Res Unit, St Andrews KY16 8LB, Fife, Scotland. [Jensen, Brenda A.] Hawaii Pacific Univ, Dept Nat Sci, Kaneohe, HI 96744 USA. [Matassa, Keith] Pacific Marine Mammal Ctr, Laguna Beach, CA 92651 USA. [Mazzariol, Sandro] Univ Padua, Dept Comparat Biomed & Food Sci, I-35020 Legnaro Padua, Italy. [Nielsen, Ole] Dept Fisheries & Oceans Canada, Winnipeg, MB R3T 2N6, Canada. [Rotstein, David] Marine Mammal Pathol Serv, Olney, MD 20832 USA. [Saliki, Jeremy T.] Univ Georgia, Coll Vet Med, Athens Vet Diagnost Lab, Athens, GA 30602 USA. [Siebert, Ursula] Univ Vet Med, Inst Terr & Aquat Wildlife Res, D-30173 Hannover, Germany. [Waltzek, Thomas] Univ Florida, Coll Vet Med, Dept Infect Dis & Pathol, Gainesville, FL 32611 USA. [Wellehan, James F. X.] Univ Florida, Coll Vet Med, Dept Small Anim Clin Sci, Gainesville, FL 32610 USA. RP Duignan, PJ (reprint author), Univ Calgary, Dept Ecosyst & Publ Hlth, Calgary, AB T2N 4Z6, Canada. EM ppjduign@ucalgary.ca; mfb.cmed@gmail.com; Jason.Baker@noaa.gov; michelle.barbieri@noaa.gov; katie.colegrove@gmail.com; sylvain.deguise@uconn.edu; r.deswart@erasmusmc.nl; gdiguardo@unite.it; dobson@princeton.edu; pduprex@bu.edu; greg.early@yahoo.com; deborah.fauquier@noaa.gov; tgoldstein@ucdavis.edu; s.j.goodman@leeds.ac.uk; grenfell@princeton.edu; katia.groch@gmail.com; gullandf@tmmc.org; ajh7@st-andrews.ac.uk; bjensen@hpu.edu; klamy@gmail.com; kmatassa@pacificmmc.org; sandro.mazzariol@unipd.it; semorris@princeton.edu; ole.nielsen@dfo-mpo.gc.ca; drdrot@gmail.com; teri.rowles@noaa.gov; jsaliki@uga.edu; ursula.siebert@tiho-hannover.de; tomwaltzek@gmail.com; wellehanj@ufl.edu OI Mazzariol, Sandro/0000-0002-4756-1871; De Swart, Rik/0000-0003-3599-8969 FU RAPIDD program of the Science and Technology Directorate, Department of Homeland Security; Fogarty International Center, National Institutes of Health FX This review is the product of an international marine mammal morbillivirus workshop held at Princeton University, USA, in August 2014 and funded by the RAPIDD program of the Science and Technology Directorate, Department of Homeland Security and the Fogarty International Center, National Institutes of Health. NR 228 TC 7 Z9 7 U1 4 U2 50 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 1999-4915 J9 VIRUSES-BASEL JI Viruses-Basel PD DEC PY 2014 VL 6 IS 12 BP 5093 EP 5134 DI 10.3390/v6125093 PG 42 WC Virology SC Virology GA AX3JA UT WOS:000346834500015 PM 25533658 ER PT J AU Klein, KL Masson, S Bouratzis, C Grechnev, V Hillaris, A Preka-Papadema, P AF Klein, K. -L. Masson, S. Bouratzis, C. Grechnev, V. Hillaris, A. Preka-Papadema, P. TI The relativistic solar particle event of 2005 January 20: origin of delayed particle acceleration SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE acceleration of particles; Sun: radio radiation; solar-terrestrial relations; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: particle emission ID CORONAL MASS EJECTION; GAMMA-RAY FLARE; ENERGETIC PARTICLES; RADIO-BURSTS; MAGNETIC RECONNECTION; JUNE 15; EMISSION; APRIL; CME; PROTONS AB Context. The highest energies of solar energetic nucleons detected in space or through gamma-ray emission in the solar atmosphere are in the GeV range. Where and how the particles are accelerated is still controversial. Aims. We search for observational information on the location and nature of the acceleration region(s) by comparing the timing of relativistic protons detected on Earth and radiative signatures in the solar atmosphere during the particularly well-observed 2005 Jan. 20 event. Methods. This investigation focusses on the post-impulsive flare phase, where a second peak was observed in the relativistic proton time profile by neutron monitors. This time profile is compared in detail with UV imaging and radio spectrography over a broad frequency band from the low corona to interplanetary space. Results. It is shown that the late relativistic proton release to interplanetary space was accompanied by a distinct new episode of energy release and electron acceleration in the corona traced by the radio emission and by brightenings of UV kernels. These signatures are interpreted in terms of magnetic restructuring in the corona after the coronal mass ejection passage. Conclusions. We attribute the delayed relativistic proton acceleration to magnetic reconnection and possibly to turbulence in large-scale coronal loops. While Type II radio emission was observed in the high corona, no evidence of a temporal relationship with the relativistic proton acceleration was found. C1 [Klein, K. -L.; Masson, S.] Univ Paris 6 & 7, LESIA UMR 8109, Observ Paris, Observ Meudon,CNRS, F-92195 Meudon, France. [Masson, S.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. [Masson, S.] Catholic Univ Amer, Washington, DC 20064 USA. [Bouratzis, C.; Hillaris, A.; Preka-Papadema, P.] Univ Athens, Sect Astrophys Astron & Mech, Dept Phys, Athens 15783, Greece. [Grechnev, V.] Inst Solar Terr Phys SB RAS, Irkutsk 664033, Russia. RP Klein, KL (reprint author), Univ Paris 6 & 7, LESIA UMR 8109, Observ Paris, Observ Meudon,CNRS, F-92195 Meudon, France. EM ludwig.klein@obspm.fr; sophie.masson@nasa.gov; kbouratz@phys.uoa.gr; grechnev@iszf.irk.ru FU University of Athens Research Center (ELKE/EKPA); French Polar Institute (IPEV); French space agency (CNES) FX The authors are grateful to the Nobeyama Radio Observatory, the CORONAS gamma-ray team, the worldwide network of neutron monitors, and the RSTN network for providing data. K.L.K. acknowledges helpful discussions with J. Bieber, R. Butikofer, P. Evenson, E. Fluckiger, D. Lario, V. Petrosian, J. Ryan, and K. Shibasaki, and the kind hospitality of the solar radio astronomy group of the University of Athens and the space research group of the National Observatory of Athens. The referee and the language editor are thanked for most helpful comments on the manuscript. This work was supported in part by the University of Athens Research Center (ELKE/EKPA), by the French Polar Institute (IPEV) and the French space agency (CNES). NR 70 TC 4 Z9 4 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2014 VL 572 AR A4 DI 10.1051/0004-6361/201423783 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AW2ET UT WOS:000346101700056 ER PT J AU Lopez, A Tercero, B Kisiel, Z Daly, AM Bermudez, C Calcutt, H Marcelino, N Viti, S Drouin, BJ Medvedev, IR Neese, CF Pszczolkowski, L Alonso, JL Cernicharo, J AF Lopez, A. Tercero, B. Kisiel, Z. Daly, A. M. Bermudez, C. Calcutt, H. Marcelino, N. Viti, S. Drouin, B. J. Medvedev, I. R. Neese, C. F. Pszczolkowski, L. Alonso, J. L. Cernicharo, J. TI Laboratory characterization and astrophysical detection of vibrationally excited states of vinyl cyanide in Orion-KL SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: abundances; ISM: molecules; stars: formation; line: identification; methods: laboratory: molecular; radio lines: ISM ID STAR-FORMING REGIONS; MILLIMETER-WAVE SPECTRUM; MOLECULAR LINE SURVEY; CENTRIFUGAL-DISTORTION CONSTANTS; ROTATION-INVERSION SPECTRUM; GRAIN-SURFACE-CHEMISTRY; ELECTRIC-DIPOLE MOMENTS; 1ST ISM DETECTION; ETHYL-CYANIDE; HYPERFINE-STRUCTURE AB Context. We perform a laboratory characterization in the 18-1893 GHz range and astronomical detection between 80-280 GHz in Orion-KL with IRAM-30 m of CH2CHCN (vinyl cyanide) in its ground and vibrationally excited states. Aims. Our aim is to improve the understanding of rotational spectra of vibrationally excited vinyl cyanide with new laboratory data and analysis. The laboratory results allow searching for these excited state transitions in the Orion-KL line survey. Furthermore, rotational lines of CH2CHCN contribute to the understanding of the physical and chemical properties of the cloud. Methods. Laboratory measurements of CH2CHCN made on several different frequency-modulated spectrometers were combined into a single broadband 50-1900 GHz spectrum and its assignment was confirmed by Stark modulation spectra recorded in the 18-40 GHz region and by ab-initio anharmonic force field calculations. For analyzing the emission lines of vinyl cyanide detected in Orion-KL we used the excitation and radiative transfer code (MADEX) at LTE conditions. Results. Detailed characterization of laboratory spectra of CH2CHCN in nine different excited vibrational states: v(11) = 1, v(15) = 1, v(11) = 2, v(10) = 1 double left right arrow (v(11) = 1, v(15) = 1), v(11) = 3/v(15) = 2/v(14) = 1, (v(11) = 1, v(10) = 1) double left right arrow (v(11) = 2, v(15) = 1), v(9) = 1, (v(11) = 1, v(15) = 2) double left right arrow (v(10) = 1, v(15) = 1) double left right arrow (v(11) = 1, v(14) = 1), and v(11) = 4 are determined, as well as the detection of transitions in the v(11) = 2 and v(11) = 3 states for the first time in Orion-KL and of those in the v(10) = 1 double left right arrow (v(11) = 1, v(15) = 1) dyad of states for the first time in space. The rotational transitions of the ground state of this molecule emerge from four cloud components of hot core nature, which trace the physical and chemical conditions of high mass star forming regions in the Orion-KL Nebula. The lowest energy vibrationally excited states of vinyl cyanide, such as v(11) = 1 (at 328.5 K), v(15) = 1 (at 478.6 K), v(11) = 2 (at 657.8 K), the v(10) = 1 double left right arrow (v(11) = 1, v(15) = 1) dyad (at 806.4/809.9 K), and v(11) = 3 (at 987.9 K), are populated under warm and dense conditions, so they probe the hottest parts of the Orion-KL source. The vibrational temperatures derived for the v(11) = 1, v(11) = 2, and v(15) = 1 states are 252 +/- 76 K, 242 +/- 121 K, and 227 +/- 68K, respectively; all of them are close to the mean kinetic temperature of the hot core component (210 K). The total column density of CH2CHCN in the ground state is (3.0 +/- 0.9) x 10(15) cm(-2). We report the detection of methyl isocyanide (CH3NC) for the first time in Orion-KL and a tentative detection of vinyl isocyanide (CH2CHNC). We also give column density ratios between the cyanide and isocyanide isomers, obtaining a N(CH3NC)/N(CH3CN) ratio of 0.002. Conclusions. Laboratory characterization of many previously unassigned vibrationally excited states of vinyl cyanide ranging from microwave to THz frequencies allowed us to detect these molecular species in Orion-KL. Column density, rotational and vibrational temperatures for CH2CHCN in their ground and excited states, and the isotopologues have been constrained by means of a sample of more than 1000 lines in this survey. C1 [Lopez, A.; Tercero, B.; Cernicharo, J.] Ctr Astrobiol CSIC INTA, Dept Astrofis Mol, Madrid 28850, Spain. [Kisiel, Z.; Pszczolkowski, L.] Polish Acad Sci, Inst Phys, PL-02668 Warsaw, Poland. [Daly, A. M.; Drouin, B. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Daly, A. M.; Bermudez, C.; Alonso, J. L.] Univ Valladolid, Unidad Asociada CSIC, GEM, Lab Espect & Bioespect, E-47011 Valladolid, Spain. [Calcutt, H.; Viti, S.] UCL, Dept Phys & Astron, London WC1E 6B, England. [Marcelino, N.] NRAO, Charlottesville, VA 22902 USA. [Medvedev, I. R.] Wright State Univ, Dayton, OH 45435 USA. [Neese, C. F.] Ohio State Univ, Columbus, OH 43210 USA. RP Lopez, A (reprint author), Ctr Astrobiol CSIC INTA, Dept Astrofis Mol, Ctra Ajalvir Km 4, Madrid 28850, Spain. EM lopezja@cab.inta-csic.es RI Kisiel, Zbigniew/K-8798-2016; Pszczolkowski, Lech/S-3018-2016; OI Kisiel, Zbigniew/0000-0002-2570-3154; Calcutt, Hannah/0000-0003-3393-294X FU INTA-CSIC; Spanish MINECO; Junta de Castilla y Leon from grants the CONSOLIDER program "ASTROMOL" [CSD2009-00038, AYA2009-07304, AYA2012-32032, CTQ2010-19008, VA175U13]; Spanish MINECO for the FPI grant [BES-2011-047695]; Polish National Science Centre [DEC/2011/02/A/ST2/00298]; National Aeronautics and Space Administration FX We thank the anonymous referee who provided comments that improved this manuscript. We thank INTA-CSIC, and the Spanish MINECO and Junta de Castilla y Leon for funding support from grants the CONSOLIDER program "ASTROMOL" CSD2009-00038, AYA2009-07304, AYA2012-32032, CTQ2010-19008 and VA175U13. C.B. thanks also the Spanish MINECO for the FPI grant (BES-2011-047695). The IFPAN authors acknowledge a grant from the Polish National Science Centre, decision number DEC/2011/02/A/ST2/00298. Portions of this research were carried out at the Jet Propulsion Laboratory, California Institute of technology, under contract with the National Aeronautics and Space Administration. NR 141 TC 16 Z9 16 U1 2 U2 20 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2014 VL 572 AR A44 DI 10.1051/0004-6361/201423622 PG 39 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AW2ET UT WOS:000346101700061 ER PT J AU Rimola, A Taquet, V Ugliengo, P Balucani, N Ceccarelli, C AF Rimola, Albert Taquet, Vianney Ugliengo, Piero Balucani, Nadia Ceccarelli, Cecilia TI Combined quantum chemical and modeling study of CO hydrogenation on water ice SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: clouds; ISM: molecules; ISM: abundances ID LASER-INDUCED FLUORESCENCE; H2O-CO ICE; CARBON-MONOXIDE; GRAIN MANTLES; CH3O (X)OVER-TILDE(2)E; DENSITY FUNCTIONALS; VIBRATIONAL-SPECTRA; BARRIER HEIGHTS; RATE CONSTANTS; HARTREE-FOCK AB Context. Successive hydrogenation reactions of CO on interstellar icy grain surfaces are considered one of the most efficient mechanisms in interstellar environments for the formation of H2CO and CH3OH, two of the simplest organic molecules detected in space. In the past years, several experimental and theoretical works have been focused on these reactions, providing relevant information both at the macroscopic and atomic scale. However, several questions still remain open, such as the exact role played by water in these processes, a crucial aspect because water is the dominant constituent of the ice mantles around dust grain cores. Aims. We here present a quantum chemical description of the successive H additions to CO both in the gas phase and on the surfaces of several water clusters. Methods. The hydrogenation steps were calculated by means of accurate quantum chemical methods and structural cluster models consisting of 3, 18, and 32 water molecules. Results. Our main result is that the interaction of CO and H2CO with the water cluster surfaces through H-bonds with the O atoms increases the C-O polarization, thus weakening the C-O bond. Consequently, the C atoms are more prone to receiving H atoms, which in turn lowers the energy barriers for the H additions compared to the gas-phase processes. The calculated energy barriers and transition frequencies associated with the reaction coordinate were adopted as input parameters in our numerical model of the surface chemistry (GRAINOBLE) to simulate the distribution of the H2CO and CH3OH ice abundances (with respect to water). Our GRAINOBLE results based on the energy barriers and transition frequencies for the reactions on the 32 water molecule cluster compare well with the observed abundances in low-mass protostars and dark cores. C1 [Rimola, Albert] Univ Autonoma Barcelona, Dept Quim, Bellaterra 08193, Cerdanyola Del, Spain. [Taquet, Vianney] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20770 USA. [Taquet, Vianney] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20770 USA. [Ugliengo, Piero] Univ Turin, Dipartimento Chim, I-10125 Turin, Italy. [Ugliengo, Piero] Univ Turin, NIS Ctr Nanostruct Interfaces & Surfaces, I-10125 Turin, Italy. [Balucani, Nadia] Univ Perugia, Dipartimento Chim Biol & Biotecnol, I-06123 Perugia, Italy. [Ceccarelli, Cecilia] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. [Ceccarelli, Cecilia] IPAG, CNRS, F-38000 Grenoble, France. RP Rimola, A (reprint author), Univ Autonoma Barcelona, Dept Quim, Bellaterra 08193, Cerdanyola Del, Spain. EM Albert.Rimola@uab.cat RI ugliengo, piero/H-6373-2015; Rimola, Albert/K-1813-2014; Balucani, Nadia/B-8211-2011 OI ugliengo, piero/0000-0001-8886-9832; Rimola, Albert/0000-0002-9637-4554; Balucani, Nadia/0000-0001-5121-5683 FU MINECO [CTQ2011-24847/BQU, CTQ2013-40347-ERC]; MINECO of the Spanish Government; Progetti di Ricerca di Ateneo-Compagnia di San Paolo-Linea 1A, progetto [ORTO11RRT5]; French agency ANR, project FORCOMS [ANR-08-BLAN-0225] FX A. R. is indebted to MINECO of the Spanish Government for a Juan de la Cierva contract. Financial support from MINECO (projects CTQ2011-24847/BQU and CTQ2013-40347-ERC) and the use of the Catalonia Supercomputer Centre (CESCA) are gratefully acknowledged. PU acknowledge Progetti di Ricerca di Ateneo-Compagnia di San Paolo-2011-Linea 1A, progetto ORTO11RRT5 for funding. C.C. and V.T. acknowledge the funding by the French agency ANR, project FORCOMS ANR-08-BLAN-0225. NR 67 TC 5 Z9 5 U1 4 U2 24 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2014 VL 572 AR A70 DI 10.1051/0004-6361/201424046 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AW2ET UT WOS:000346101700090 ER PT J AU Spoto, F Milani, A Farnocchia, D Chesley, SR Micheli, M Valsecchi, GB Perna, D Hainaut, O AF Spoto, Federica Milani, Andrea Farnocchia, Davide Chesley, Steven R. Micheli, Marco Valsecchi, Giovanni B. Perna, Davide Hainaut, Olivier TI Nongravitational perturbations and virtual impactors: the case of asteroid (410777) 2009 FD SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE minor planets, asteroids: individual: 2009 FD; celestial mechanics ID NEAR-EARTH ASTEROIDS; MAGNITUDE AB Asteroid (410777) 2009 FD could hit Earth between 2185 and 2196. The long term propagation to the possible impacts and the intervening planetary encounters make 2009 FD one of the most challenging asteroids in terms of hazard assessment. To compute accurate impact probabilities we model the Yarkovsky effect by using the available physical characterization of 2009 FD and general properties of the near Earth asteroid population. We perform the hazard assessment with two independent methods: the first method is a generalization of the standard impact monitoring algorithms in use by NEODyS and Sentry, while the second one is based on a Monte Carlo approach. Both methods generate orbital samples in a seven-dimensional space that includes orbital elements and the parameter characterizing the Yarkovsky effect. The highest impact probability is 2.7 x 10(-3) for an impact during the 2185 Earth encounter. Impacts after 2185 corresponding to resonant returns are possible, the most relevant being in 2190 with a probability of 3 x 10(-4). Both numerical methods can be used in the future to handle similar cases. The structure of resonant returns and the list of the possible keyholes on the target plane of the scattering encounter in 2185 can be predicted by an analytic theory. C1 [Spoto, Federica; Milani, Andrea] Univ Pisa, Dept Math, I-56126 Pisa, Italy. [Farnocchia, Davide; Chesley, Steven R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Micheli, Marco] ESA NEO Coordinat Ctr, I-00044118 Rome, Italy. [Micheli, Marco; Valsecchi, Giovanni B.] IAPS INAF, I-00133 Rome, Italy. [Valsecchi, Giovanni B.] IFAC CNR, Florence, Italy. [Perna, Davide] Univ Paris Diderot, UPMC, CNRS, LESIA Observ Paris, F-92195 Meudon, France. [Hainaut, Olivier] European So Observ, D-85748 Munich, Germany. RP Spoto, F (reprint author), Univ Pisa, Dept Math, I-56126 Pisa, Italy. EM spoto@mail.dm.unipi.it OI Valsecchi, Giovanni/0000-0002-2915-1465; Micheli, Marco/0000-0001-7895-8209 NR 21 TC 3 Z9 3 U1 1 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2014 VL 572 AR A100 DI 10.1051/0004-6361/201424743 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AW2ET UT WOS:000346101700003 ER PT J AU Velusamy, T Langer, WD AF Velusamy, T. Langer, W. D. TI Origin and z-distribution of Galactic diffuse [C II] emission SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: structure; Galaxy: structure ID INTERSTELLAR-MEDIUM; MILKY-WAY; H I; LINE EMISSION; MOLECULAR GAS; PLANE SURVEY; PHYSICAL CONDITIONS; COOLING LINES; RING SURVEY; DARK GAS AB Context. The [CII] emission is an important probe of star formation in the Galaxy and in external galaxies. The GOT C+ survey and its follow up observations of spectrally resolved 1.9 THz [C II] emission using Herschel HIFI provides the data needed to quantify the Galactic interstellar [CII] gas components as tracers of star formation. Aims. We determine the source of the diffuse [CII] emission by studying its spatial (radial and vertical) distributions by separating and evaluating the fractions of [C II] and CO emissions in the Galactic ISM gas components. Methods. We used the HIFI [C II] Galactic survey (GOT C+), along with ancillary HI, (CO)-C-12, (CO)-C-13, and (CO)-O-18 data toward 354 lines of sight, and several HIFI [C II] and [C I] position-velocity maps. We quantified the emission in each spectral line profile by evaluating the intensities in 3 kms(-1) wide velocity bins, "spaxels". Using the detection of [CII] with CO or [C I], we separated the dense and diffuse gas components. We derived 2D Galactic disk maps using the spaxel velocities for kinematic distances. We separated the warm and cold H-2 gases by comparing CO emissions with and without associated [CII]. Results. We find evidence of widespread diffuse [C II] emission with a z-scale distribution larger than that for the total [C II] or CO. The diffuse [C II] emission consists of (i) diffuse molecular (CO-faint) H-2 clouds and (ii) diffuse H I clouds and/or WIM. In the inner Galaxy we find a lack of [C II] detections in a majority (similar to 62%) of Hi spaxels and show that the diffuse component primarily comes from the WIM (similar to 21%) and that the Hi gas is not a major contributor to the diffuse component (similar to 6%). The warm-H-2 radial profile shows an excess in the range 4 to 7 kpc, consistent with enhanced star formation there. Conclusions. We derive, for the first time, the 2D [C II] spatial distribution in the plane and the z-distributions of the individual [C II] gas component. From the GOT C+ detections we estimate the fractional [C II] emission tracing (i) H-2 gas in dense and diffuse molecular clouds as similar to 48% and similar to 14%, respectively, (ii) in the Hi gas similar to 18%, and (iii) in the WIM similar to 21%. Including non-detections from Hi increases the [C II] in Hi to similar to 27%. The z-scale distributions FWHM from smallest to largest are [C II] sources with CO, similar to 130 pc, (CO-faint) diffuse H-2 gas, similar to 200 pc, and the diffuse Hi and WIM, similar to 330 pc. When combined with [C II], CO observations probe the warm-H-2 gas, tracing star formation. C1 [Velusamy, T.; Langer, W. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Velusamy, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Thangasamy.Velusamy@jpl.nasa.gov FU National Aeronautics and Space Administration FX We thank the referee Dr. Jay Lockman for a careful reading of the manuscript and for constructive comments and suggestions. We thank the staffs of the ESA Herschel Science Centre and NASA Herschel Science Center, and the HIFI, Instrument Control Centre (ICC) for their help with the data reduction routines. This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 56 TC 12 Z9 12 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2014 VL 572 AR A45 DI 10.1051/0004-6361/201424350 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AW2ET UT WOS:000346101700062 ER PT J AU Leising, AW Schroeder, ID Bograd, SJ Bjorkstedt, EP Field, J Sakuma, K Abell, J Robertson, RR Tyburczy, J Peterson, WT Brodeur, R Barcelo, C Auth, TD Daly, EA Campbell, GS Hildebrand, JA Suryan, RM Gladics, AJ Horton, CA Kahru, M Manzano-Sarabia, M McClatchie, S Weber, ED Watson, W Santora, JA Sydeman, WJ Melin, SR Delong, RL Largier, J Kim, SY Chavez, FP Golightly, RT Schneider, SR Warzybok, P Bradley, R Jahncke, J Fisher, J Peterson, J AF Leising, Andrew W. Schroeder, Isaac D. Bograd, Steven J. Bjorkstedt, Eric P. Field, John Sakuma, Keith Abell, Jeffrey Robertson, Roxanne R. Tyburczy, Joe Peterson, William T. Brodeur, Ric Barcelo, Caren Auth, Toby D. Daly, Elizabeth A. Campbell, Gregory S. Hildebrand, John A. Suryan, Robert M. Gladics, Amanda J. Horton, Cheryl A. Kahru, Mati Manzano-Sarabia, Marlenne McClatchie, Sam Weber, Edward D. Watson, William Santora, Jarrod A. Sydeman, William J. Melin, Sharon R. Delong, Robert L. Largier, John Kim, Sung Yong Chavez, Francisco P. Golightly, Richard T. Schneider, Stephanie R. Warzybok, Pete Bradley, Russel Jahncke, Jaime Fisher, Jennifer Peterson, Jay TI STATE OF THE CALIFORNIA CURRENT 2013-14: EL NINO LOOMING SO CALIFORNIA COOPERATIVE OCEANIC FISHERIES INVESTIGATIONS REPORTS LA English DT Article ID PELAGIC JUVENILE ROCKFISH; CURRENT SYSTEM; SOUTHERN CALIFORNIA; OCEANOGRAPHIC CONDITIONS; NORTHEAST PACIFIC; VARIABILITY; ANOMALIES; COMMUNITY; OREGON; COAST AB In 2013, the California current was dominated by strong coastal upwelling and high productivity. Indices of total cumulative upwelling for particular coastal locations reached some of the highest values on record. Chlorophyll a levels were high throughout spring and summer. Catches of upwelling-related fish species were also high. After a moderate drop in upwelling during fall 2013, the California current system underwent a major change in phase. Three major basin-scale indicators, the PDO, the NPGO, and the ENSO-MEI, all changed phase at some point during the winter of 2013/14. The PDO changed to positive values, indicative of warmer waters in the North Pacific; the NPGO to negative values, indicative of lower productivity along the coast; and the MEI to positive values, indicative of an oncoming El Nino. Whereas the majority of the California Current system appears to have transitioned to an El Nino state by August 2014, based on decreases in upwelling and chlorophyll a concentration, and increases in SST, there still remained pockets of moderate upwelling, cold water, and high chlorophyll a biomass at various central coast locations, unlike patterns seen during the more major El Ninos (e.g., the 97-98 event). Catches of rockfish, market squid, euphausiids, and juvenile sanddab remained high along the central coast, whereas catches of sardine and anchovy were low throughout the CCS. 2014 appears to be heading towards a moderate El Nino state, with some remaining patchy regions of upwelling-driven productivity along the coast. Superimposed on this pattern, three major regions have experienced possibly non-El Nino-related warming since winter: the Bering Sea, the Gulf of Alaska, and offshore of southern California. It is unclear how this warming may interact with the predicted El Nino, but the result will likely be reduced growth or reproduction for many key fisheries species. C1 [Leising, Andrew W.; Schroeder, Isaac D.; Bograd, Steven J.] Natl Marine Fisheries Serv, Div Environm Res, Monterey, CA 93940 USA. [Bjorkstedt, Eric P.; Field, John; Sakuma, Keith] Natl Marine Fisheries Serv, Fisheries Ecol Div, Santa Cruz, CA 95060 USA. [Abell, Jeffrey] Humboldt State Univ, Dept Oceanog, Arcata, CA 95521 USA. [Robertson, Roxanne R.] Humboldt State Univ, CIMEC, Arcata, CA USA. [Tyburczy, Joe] Calif Sea Grant, Eureka, CA USA. [Peterson, William T.; Brodeur, Ric] Oregon State Univ, Hatfield Marine Sci Ctr, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. [Barcelo, Caren] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA. [Auth, Toby D.] Oregon State Univ, Hatfield Marine Sci Ctr, Pacific States Marine Fisheries Commiss, Newport, OR 97365 USA. [Daly, Elizabeth A.] Oregon State Univ, Hatfield Marine Sci Ctr, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA. [Campbell, Gregory S.; Hildebrand, John A.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Suryan, Robert M.; Gladics, Amanda J.; Horton, Cheryl A.] Oregon State Univ, Hatfield Marine Sci Ctr, Dept Fisheries & Wildlife, Newport, OR 97365 USA. [Kahru, Mati; Manzano-Sarabia, Marlenne] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92121 USA. [Manzano-Sarabia, Marlenne] Univ Autonoma Sinaloa, Fac Ciencias Mar, Mazatlan, Sinaloa, Mexico. [McClatchie, Sam; Weber, Edward D.; Watson, William] Southwest Fisheries Sci Ctr, NMFS, La Jolla, CA 92037 USA. [Santora, Jarrod A.; Sydeman, William J.] Farallon Inst Adv Ecosyst Res, Petaluma, CA 94952 USA. [Melin, Sharon R.; Delong, Robert L.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Natl Marine Mammal Lab, Seattle, WA 98115 USA. [Largier, John] Univ Calif Davis, Bodega Marine Lab, Bodega Bay, CA 94923 USA. [Kim, Sung Yong] Korea Adv Inst Sci & Technol, Div Ocean Syst Engn, Taejon 305701, South Korea. [Chavez, Francisco P.] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. [Golightly, Richard T.; Schneider, Stephanie R.] Humboldt State Univ, Dept Wildlife, Arcata, CA 95521 USA. [Warzybok, Pete; Bradley, Russel; Jahncke, Jaime] Point Blue Conservat Sci, Petaluma, CA 94954 USA. [Warzybok, Pete; Bradley, Russel; Jahncke, Jaime] PRBO, Petaluma, CA 94954 USA. [Fisher, Jennifer; Peterson, Jay] Oregon State Univ, Cooperat Inst Marine Resources Studies, Hatfield Sci Ctr, Newport, OR 97365 USA. RP Leising, AW (reprint author), Natl Marine Fisheries Serv, Div Environm Res, 99 Pacific St,Suite 255A, Monterey, CA 93940 USA. RI Kim, Sung Yong/B-9852-2009 OI Kim, Sung Yong/0000-0003-1962-8992 FU NOAA's Fisheries and the Environment (FATE) program; NOAA's Stock Assessment Improvement Plan (SAIP); Fisheries and the Environment (FATE) programs; Bonneville Power Administration (BPA); NASA Ocean Biology and Biogeochemistry Program [NNX-09AT01G]; National Science Foundation [OCE-1026607]; National Marine Fisheries Service FX Andrew W. Leising was partially funded through NOAA's Fisheries and the Environment (FATE) program. Ichthyoplankton collections off the Oregon coast were supported in part by NOAA's Stock Assessment Improvement Plan (SAIP) and Fisheries and the Environment (FATE) programs, as well as from a grant through the Bonneville Power Administration (BPA). Financial support was provided by the NASA Ocean Biology and Biogeochemistry Program Grants NNX-09AT01G (M. K.), National Science Foundation (Grant OCE-1026607 to the CCE LTER Program). Satellite data were provided by the NASA Ocean Color Processing Group and ESA MERIS team. We thank the CalCOFI and CCE-LTER programs, NOAA SWFSC survey, Monterey Bay Aquarium Research Institute and Pacific Coastal Ocean Observing System for in situ data. R. DeLong, J. Harris, J. Laake, A. Orr and many field assistants participated in the data collection and summaries. Funding was provided by the National Marine Fisheries Service. Research was conducted under NMFS Permit 16087 issued to the National Marine Mammal Laboratory. NR 48 TC 7 Z9 8 U1 2 U2 38 PU SCRIPPS INST OCEANOGRAPHY PI LA JOLLA PA A-003, LA JOLLA, CA 92093 USA SN 0575-3317 J9 CAL COOP OCEAN FISH JI Calif. Coop. Ocean. Fish. Invest. Rep. PD DEC PY 2014 VL 55 BP 51 EP 87 PG 37 WC Fisheries SC Fisheries GA AW3NB UT WOS:000346192400004 ER PT J AU Stinton, A Ciannelli, L Reese, DC Wakefield, WW AF Stinton, Amy Ciannelli, Lorenzo Reese, Douglas C. Wakefield, W. Waldo TI USING IN SITU VIDEO ANALYSIS TO ASSESS JUVENILE FLATFISH BEHAVIOR ALONG THE OREGON CENTRAL COAST SO CALIFORNIA COOPERATIVE OCEANIC FISHERIES INVESTIGATIONS REPORTS LA English DT Article ID NORTHERN CALIFORNIA CURRENT; ESTUARINE FOOD-WEB; TROPHIC INTERACTIONS; HYPOXIA; FLOUNDER; OXYGEN; RESPONSES; ECOSYSTEM; PACIFIC; SUMMER AB We examined the feasibility of using a video beam trawl system to assess behavioral responses of juvenile flatfishes in relation to co-occurring habitat features, most notably dissolved oxygen (DO) concentrations. Sixteen samples were collected along a cross shelf transect in the central Oregon coast during summer 2008. We found that juvenile fish reaction duration, defined as the time in seconds from first reaction to capture, decreased with decreased DO. However, other variables such as bottom water temperature, fish size, and fish species composition by site are potentially confounding factors of the analysis. The dominant flatfish species shifted from English sole (Parophyrs vetulus) to Pacific sanddab (Citharichthys sordidus) with increased depth. Escape behavior varied from "burying" in the shallows, to "hovering" at mid-depth stations, and "running" at the deepest site. Collectively, our results suggest that the video beam trawl effectively monitor behavioral metrics and community composition of nearshore flatfish assemblages. C1 [Stinton, Amy] Bell Aquaculture, Albany, IN 47373 USA. [Ciannelli, Lorenzo] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA. [Reese, Douglas C.] Oregon State Univ, Dept Fisheries & Wildlife, Corvallis, OR 97331 USA. [Wakefield, W. Waldo] NW Fisheries Sci Ctr, Fishery Resource Anal & Monitoring Div, Natl Marine Fisheries Serv, Newport, OR 97365 USA. RP Stinton, A (reprint author), Bell Aquaculture, 11550 East Gregory Rd, Albany, IN 47373 USA. EM amy.stinton@bellaquaculture.com; lciannel@coas.oregonstate.edu FU Oregon Sea Grant [NA06OAR4170010]; National Oceanic and Atmospheric Administration's National Sea Grant College Program [R/ECO-23]; U.S. Department of Commerce; DOD Assure; NSF FX This research was sponsored by Oregon Sea Grant under award number NA06OAR4170010, project number R/ECO-23 from the National Oceanic and Atmospheric Administration's National Sea Grant College Program, U.S. Department of Commerce, and by appropriations made by the Oregon State Legislature. The statements, findings, conclusions, and recommendations are those of the authors and do not necessarily reflect the views of these funders. Amy Stinton was funded through the DOD Assure, and NSF. Special thanks goes to three anonymous reviewers for their insightful comments and to Angela Johnson, Natalie Ehrlich, Chris Toole, Cathleen Vestfals, Jason Phillips, Matthew Yergey and Bobby Ireland for intellectual and field support. Cathleen Vestfals and Lorey Stinton developed Figure 1. NR 36 TC 0 Z9 0 U1 1 U2 8 PU SCRIPPS INST OCEANOGRAPHY PI LA JOLLA PA A-003, LA JOLLA, CA 92093 USA SN 0575-3317 J9 CAL COOP OCEAN FISH JI Calif. Coop. Ocean. Fish. Invest. Rep. PD DEC PY 2014 VL 55 BP 158 EP 168 PG 11 WC Fisheries SC Fisheries GA AW3NB UT WOS:000346192400011 ER PT J AU Iguchi, T Matsui, T Tao, WK Khain, AP Phillips, VTJ Kidd, C L'Ecuyer, T Braun, SA Hou, A AF Iguchi, Takamichi Matsui, Toshihisa Tao, Wei-Kuo Khain, Alexander P. Phillips, Vaughan T. J. Kidd, Chris L'Ecuyer, Tristan Braun, Scott A. Hou, Arthur TI WRF-SBM Simulations of Melting-Layer Structure in Mixed-Phase Precipitation Events Observed during LPVEx SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID ATMOSPHERIC ICE PARTICLES; RADAR OBSERVATIONS; RAINFALL MEASUREMENTS; WIND-TUNNEL; PART I; MODEL; MICROPHYSICS; CLOUDS; BACKSCATTERING; DISDROMETERS AB Two mixed-phase precipitation events were observed on 21 September and 20 October 2010 over the southern part of Finland during the Light Precipitation Validation Experiment (LPVEx). These events have been simulated using the Weather Research and Forecasting Model coupled with spectral bin microphysics (WRF-SBM). The detailed ice-melting scheme with prognosis of the liquid water fraction during melting enables explicit simulation of microphysical properties in the melting layer. First, the simulations have been compared with C-band 3D radar measurements for the purpose of evaluating the overall profiles of cloud and precipitation. The simulation has some artificial convective patterns and errors in the forecast displacement of the precipitation system. The overall overestimation of reflectivity is consistent with a bias toward the range characterized by large-diameter droplets in the surface drop size distribution. Second, the structure of the melting bands has been evaluated against vertically pointing K-band radar measurements. A peak in reflectivity and a gradual change in Doppler velocity are observed and similarly simulated in the common temperature range from approximately 0 degrees to 3 degrees C. The effectiveness of the time-dependent melting scheme has been justified by intercomparison with a corresponding simulation using an instantaneous melting scheme. A weakness of the new melting scheme is that melting particles having high liquid water fractions on the order of 80%-90% cannot be simulated. This situation may cause underestimation of radar reflectivity in the melting layer because of the assumptions of melting-particle structure used to calculate the scattering properties. C1 [Iguchi, Takamichi; Matsui, Toshihisa; Kidd, Chris] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Iguchi, Takamichi; Matsui, Toshihisa; Tao, Wei-Kuo; Kidd, Chris; Braun, Scott A.; Hou, Arthur] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. [Khain, Alexander P.] Hebrew Univ Jerusalem, Inst Earth Sci, Dept Atmospher Sci, IL-91904 Jerusalem, Israel. [Phillips, Vaughan T. J.] Lund Univ, Dept Phys Geog & Ecosyst Sci, Lund, Sweden. [L'Ecuyer, Tristan] Univ Wisconsin, Dept Atmospher & Ocean Sci, Madison, WI USA. RP Iguchi, T (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 612, Greenbelt, MD 20771 USA. EM takamichi.iguchi@nasa.gov RI L'Ecuyer, Tristan/E-5607-2012; Measurement, Global/C-4698-2015 OI L'Ecuyer, Tristan/0000-0002-7584-4836; FU NASA GPM Ground Validation program FX This study was supported by the NASA GPM Ground Validation program (Dr. Mathew R. Schwaller). The sounding data at the Jokioinen site were kindly provided by the Department of Atmospheric Science of the College of Engineering at the University of Wyoming. The authors thank the two anonymous reviewers for their comments in improving the manuscript. This paper is dedicated to the memory of Arthur Y. Hou. NR 49 TC 4 Z9 4 U1 3 U2 12 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD DEC PY 2014 VL 53 IS 12 BP 2710 EP 2731 DI 10.1175/JAMC-D-13-0334.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AW4YU UT WOS:000346284300006 ER PT J AU Rutan, DA Smith, GL Wong, TM AF Rutan, David A. Smith, G. Louis Wong, Takmeng TI Diurnal Variations of Albedo Retrieved from Earth Radiation Budget Experiment Measurements SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID OUTGOING LONGWAVE RADIATION; ENERGY SYSTEM CERES; EXPERIMENT ERBE; CLOUD COVER; CYCLE; VARIABILITY; BALANCE AB Five years of measurements from the Earth Radiation Budget Satellite (ERBS) have been analyzed to define the diurnal cycle of albedo from 55 degrees N to 55 degrees S. The ERBS precesses through all local times every 72 days so as to provide data regarding the diurnal cycles for Earth radiation. Albedo together with insolation at the top of the atmosphere is used to compute the heating of the Earth-atmosphere system; thus its diurnal cycle is important in the energetics of the climate system. A principal component (PC) analysis of the diurnal variation of top-of-atmosphere albedo using these data is presented. The analysis is done separately for ocean and land because of the marked differences of cloud behavior over ocean and over land. For ocean, 90%-92% of the variance in the diurnal cycle is described by a single component; for land, the first PC accounts for 83%-89% of the variance. Some of the variation is due to the increase of albedo with increasing solar zenith angle, which is taken into account in the ERBS data processing by a directional model, and some is due to the diurnal cycle of cloudiness. The second PC describes 2%-4% of the variance for ocean and 5% for land, and it is primarily due to variations of cloudiness throughout the day, which are asymmetric about noon. These terms show the response of the atmosphere to the cycle of solar heating. The third PC for ocean is a two-peaked curve, and the associated map shows high values in cloudy regions. C1 [Rutan, David A.; Smith, G. Louis] Sci Syst Applicat Inc, Hampton, VA USA. [Wong, Takmeng] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23665 USA. RP Smith, GL (reprint author), Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. EM george.l.smith@nasa.gov FU NASA Science Mission Directorate through Langley Research Center to Science Systems and Applications, Inc. FX The authors gratefully acknowledge support by the CERES program from the NASA Science Mission Directorate through Langley Research Center to Science Systems and Applications, Inc. They also acknowledge the Atmospheric Sciences Data Center of Langley Research Center for access to the ERBE dataset. These data are available at http://eosweb.larc.nasa.gov. NR 26 TC 2 Z9 2 U1 0 U2 6 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD DEC PY 2014 VL 53 IS 12 BP 2747 EP 2760 DI 10.1175/JAMC-D-13-0119.1 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AW4YU UT WOS:000346284300008 ER PT J AU Behrangi, A Andreadis, K Fisher, JB Turk, FJ Granger, S Painter, T Das, N AF Behrangi, Ali Andreadis, Konstantinos Fisher, Joshua B. Turk, F. Joseph Granger, Stephanie Painter, Thomas Das, Narendra TI Satellite-Based Precipitation Estimation and Its Application for Streamflow Prediction over Mountainous Western US Basins SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID CONTERMINOUS UNITED-STATES; HYDROLOGICALLY BASED DATASET; CLOUD CLASSIFICATION-SYSTEM; LAND-SURFACE FLUXES; ATMOSPHERIC RIVERS; PASSIVE-MICROWAVE; CLIMATE-CHANGE; RAINFALL; MODEL; RESOLUTION AB Recognizing the importance and challenges inherent to the remote sensing of precipitation in mountainous areas, this study investigates the performance of the commonly used satellite-based high-resolution precipitation products (HRPPs) over several basins in the mountainous western United States. Five HRPPs [Tropical Rainfall Measuring Mission 3B42 and 3B42-RT algorithms, the Climate Prediction Center morphing technique (CMORPH), Precipitation Estimation from Remotely Sensed Imagery Using Artificial Neural Networks (PERSIANN), and the PERSIANN Cloud Classification System (PERSIANN-CCS)] are analyzed in the present work using ground gauge, gauge-adjusted radar, and CloudSat precipitation products. Using ground observation of precipitation and streamflow, the skill of HRPPs and the resulting streamflow simulations from the Variable Infiltration Capacity hydrological model are cross-compared. HRPPs often capture major precipitation events but seldom capture the observed magnitude of precipitation over the studied region and period (2003-09). Bias adjustment is found to be effective in enhancing the HRPPs and resulting streamflow simulations. However, if not bias adjusted using gauges, errors are typically large as in the lower-level precipitation inputs to HRPPs. The results using collocated Advanced Microwave Scanning Radiometer for Earth Observing System (AMSR-E) and CloudSat precipitation data show that missing data, often over frozen land, and limitations in retrieving precipitation from systems that lack frozen hydrometeors contribute to the observed microwave-based precipitation errors transferred to HRPPs. Over frozen land, precipitation retrievals from infrared sensors and microwave sounders show some skill in capturing the observed precipitation climatology maps. However, infrared techniques often show poor detection skill, and microwave sounding in dry atmosphere remains challenging. By recognizing the sources of precipitation error and in light of the operation of the Global Precipitation Measurement mission, further opportunity for enhancing the current status of precipitation retrievals and the hydrology of cold and mountainous regions becomes available. C1 [Behrangi, Ali; Andreadis, Konstantinos; Fisher, Joshua B.; Turk, F. Joseph; Granger, Stephanie; Painter, Thomas; Das, Narendra] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Behrangi, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 233-304, Pasadena, CA 91109 USA. EM ali.behrangi@jpl.nasa.gov RI Painter, Thomas/B-7806-2016; OI Fisher, Joshua/0000-0003-4734-9085 FU JPL Research and Technology Development investment (RHEAS); NASA New (Early Career) Investigator Program in Earth Science [NNH13ZDA001N-NIP]; NASA Weather [NNH13ZDA001N-WEATHER]; National Aeronautics and Space Administration FX Funding for this research came from a JPL Research and Technology Development investment (RHEAS). This study was also supported by the NASA New (Early Career) Investigator Program in Earth Science (NNH13ZDA001N-NIP) and NASA Weather (NNH13ZDA001N-WEATHER) awards. The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Government sponsorship is acknowledged. NR 73 TC 6 Z9 6 U1 0 U2 20 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD DEC PY 2014 VL 53 IS 12 BP 2823 EP 2842 DI 10.1175/JAMC-D-14-0056.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AW4YU UT WOS:000346284300013 ER PT J AU Coutens, A Vastel, C Hincelin, U Herbst, E Lis, DC Chavarria, L Gerin, M van der Tak, FFS Persson, CM Goldsmith, PF Caux, E AF Coutens, A. Vastel, C. Hincelin, U. Herbst, E. Lis, D. C. Chavarria, L. Gerin, M. van der Tak, F. F. S. Persson, C. M. Goldsmith, P. F. Caux, E. TI Water deuterium fractionation in the high-mass star-forming region G34.26+0.15 based on Herschel/HIFI data SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE astrochemistry; ISM: abundances; ISM: individual objects: G34.26+0.15; ISM: molecules ID H-II-REGIONS; DENSE INTERSTELLAR CLOUDS; PROTOSTAR IRAS 16293-2422; HYPERCOMPACT HII-REGIONS; MOLECULAR LINE EMISSION; GRAIN CHEMICAL-MODELS; DEUTERATED WATER; ROTATIONAL-EXCITATION; PHYSICAL-PROPERTIES; ORGANIC-MOLECULES AB Understanding water deuterium fractionation is important for constraining the mechanisms of water formation in interstellar clouds. Observations of HDO and (H2O)-O-18 transitions were carried out towards the high-mass star-forming region G34.26+0.15 with the Heterodyne Instrument for the Far-Infrared (HIFI) instrument onboard the Herschel Space Observatory, as well as with ground-based single-dish telescopes. 10 HDO lines and three (H2O)-O-18 lines covering a broad range of upper energy levels (22-204 K) were detected. We used a non-local thermal equilibrium 1D analysis to determine the HDO/H2O ratio as a function of radius in the envelope. Models with different water abundance distributions were considered in order to reproduce the observed line profiles. The HDO/H2O ratio is found to be lower in the hot core (similar to 3.5 x 10(-4)-7.5 x 10(-4)) than in the colder envelope (similar to 1.0 x 10(-3)-2.2 x 10(-3)). This is the first time that a radial variation of the HDO/H2O ratio has been found to occur in a high-mass source. The chemical evolution of this source was modelled as a function of its radius and the observations are relatively well reproduced. The comparison between the chemical model and the observations leads to an age of similar to 10(5) yr after the infrared dark cloud stage. C1 [Coutens, A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Coutens, A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Vastel, C.; Caux, E.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse, France. [Vastel, C.; Caux, E.] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France. [Hincelin, U.; Herbst, E.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Lis, D. C.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Lis, D. C.] Univ Paris 06, Sorbonne Univ, CNRS, Observ Paris,UMR 8112,LERMA, F-75014 Paris, France. [Chavarria, L.] Univ Chile, CONICYT, Santiago, Chile. [Gerin, M.] UPMC, Ecole Normale Super, Observ Paris, LERMA LRA,UMR CNRS 8112, F-75231 Paris 05, France. [Gerin, M.] UCP, F-75231 Paris 05, France. [van der Tak, F. F. S.] SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [van der Tak, F. F. S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Persson, C. M.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden. [Goldsmith, P. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Coutens, A (reprint author), Univ Copenhagen, Niels Bohr Inst, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. EM acoutens@nbi.dk RI Coutens, Audrey/M-4533-2014; Goldsmith, Paul/H-3159-2016 OI Coutens, Audrey/0000-0003-1805-3920; FU Swedish National Space Board; NASA through JPL/Caltech; INSU/CNRS (France); MPG (Germany); IGN (Spain) FX The authors are grateful to the anonymous referee for useful and pertinent comments and suggestions. They thank K. Furuya and Y. Aikawa for providing the initial chemical network of deuterated species and N. Flagey for providing the reduced HIFI data of H218O. They would also like to thank M. Hajigholi for fruitful discussions regarding the source modelling. AC and CV thank PCMI for support of the Herschel HIFI project on deuterated water. CMP acknowledges generous support from the Swedish National Space Board. Support for this work was also provided by NASA through an award issued by JPL/Caltech.; This work is based on observations carried out with the HIFI instrument onboard the Herschel Space Observatory, the Institut de RadioAstronomie Millimetrique (IRAM) 30-m Telescope, and the Caltech Submillimeter Telescope (CSO). Herschel is an ESA space observatory with science instruments provided by Europeanled principal investigator consortia and with important participation from NASA. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada, and the USA under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France, and the USA. Consortium members are: Canada: CSA, U. Waterloo; France: IRAP (formerly CESR), LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland: NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA); Sweden: Chalmers University of Technology - MC2, RSS and GARD, Onsala Space Observatory, Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). The CSO is operated by the California Institute of Technology under cooperative agreement with the National Science Foundation (AST-0838261). NR 118 TC 11 Z9 11 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 1 PY 2014 VL 445 IS 2 BP 1299 EP 1313 DI 10.1093/mnras/stu1816 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AX5IJ UT WOS:000346959400019 ER PT J AU Bernardini, F de Martino, D Mukai, K Falanga, M AF Bernardini, F. de Martino, D. Mukai, K. Falanga, M. TI Swift J2218.4+1925: a new hard-X-ray-selected polar observed with XMM-Newton SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE novae, cataclysmic variables; white dwarfs; X-rays: individual: Swift J2218.4+1925 ID CATACLYSMIC VARIABLES; OPTICAL SPECTROSCOPY; INTEGRAL OBJECTS; WHITE-DWARF; INTERMEDIATE POLARS; LUMINOSITY FUNCTION; ECLIPSING POLAR; AM-HERCULIS; IDENTIFICATION; TELESCOPE AB Swift J2218.4+1925, a hard-X-ray source detected by Swift Burst Alert Telescope (BAT), has been proposed as a candidate magnetic cataclysmic variable of the polar type from optical spectroscopy. Using XMM-Newton we perform detailed timing and spectral analysis with simultaneous X-ray (0.3-10 keV) and optical B-band data. We complement the spectral study with archival hard-X-ray (14-70 keV) spectra collected by Swift BAT as well as with optical, near and mid-infrared photometry from Sloan Digital Sky Survey, Two-Micron All Sky Survey and Wide-field Infrared Survey Explorer archive, respectively. A strong periodic X-ray signal at 2.16 h, fully consistent with the recently determined spectroscopic orbital period, adds Swift J2218.4+1925 to the small group of hard-X-ray polars and locates it at the low edge of the orbital period gap. The X-ray pulse profile shows the typical bright and faint phases seen in polars, that last similar to 70 and similar to 30 per cent of the orbit, respectively. A pronounced dip centred on the bright phase is also detected. It is stronger at lower energies and is mainly produced by photoelectric absorption. A binary inclination i similar to 40 degrees-50 degrees and a magnetic colatitude beta similar to 55 degrees-64 degrees are estimated. The source appears to accrete over a large area similar to 24 degrees wide. A multitemperature optically thin emission with complex absorption well describes the broad-band (0.3-70 keV) spectrum, with no signs of a soft X-ray blackbody component. The spectral shape strongly varies with the source rotation reaching plasma temperatures up to 55 keV, hardening at the dip and being softer during the faint phase (similar to 7 keV). We also find the first indication of an absorption edge due to a warm absorber in a polar. Indication of overabundance of neon is found in the Reflection Grating Spectrometer (RGS) spectra. The UV to mid-IR spectral energy distribution reveals an excess in the near and mid-IR, likely due to low cyclotron harmonics. We further estimate a white dwarf mass of 0.97 M-circle dot and a distance of 230-250 pc. C1 [Bernardini, F.] Wayne State Univ, Detroit, MI 48201 USA. [Bernardini, F.; de Martino, D.] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy. [Mukai, K.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Mukai, K.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Mukai, K.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Falanga, M.] ISSI, CH-3012 Bern, Switzerland. [Falanga, M.] Int Space Sci Inst Beijing, Beijing 100190, Peoples R China. RP Bernardini, F (reprint author), Wayne State Univ, 666 W Hancock St, Detroit, MI 48201 USA. EM bernardini@wayne.edu OI Bernardini, Federico/0000-0001-5326-2010; de Martino, Domitilla/0000-0002-5069-4202 FU ESA Member States; Swift, a National Aeronautics and Space Administration (NASA) science mission; NASA; 2MASS, a joint project of the University of Massachusetts; Infrared Processing and Analysis Center (IPAC)/Caltech; NSF; SDSS; INFN; ASI [ASI-INAF I/037/12/0] FX This work is based on observations obtained with XMM-Newton an ESA science mission with instruments and contributions directly funded by ESA Member States; with Swift, a National Aeronautics and Space Administration (NASA) science mission with Italian participation. This publication also makes use of data products from the WISE, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the NASA; the 2MASS, a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center (IPAC)/Caltech, funded by NASA and the NSF; and the SDSS.; FB acknowledge the Galileo Galilei Institute for Theoretical Physics for the hospitality and the INFN for partial support during the completion of this work, and thank Dr Giorgio Lanzuisi for his precious suggestions concerning Monte Carlo simulations. DdM and FB acknowledge financial support by ASI under contract ASI-INAF I/037/12/0. NR 50 TC 3 Z9 3 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 DEC 1 PY 2014 VL 445 IS 2 BP 1403 EP 1411 DI 10.1093/mnras/stu1819 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AX5IJ UT WOS:000346959400028 ER PT J AU Pon, A Johnstone, D Kaufman, MJ Caselli, P Plume, R AF Pon, Andy Johnstone, Doug Kaufman, Michael J. Caselli, Paola Plume, Rene TI Mid-J CO observations of Perseus B1-East 5: evidence for turbulent dissipation via low-velocity shocks SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE shock waves; turbulence; stars: formation; ISM: clouds; ISM: individual objects: Perseus B1-East; photodissociation region (PDR) ID PHOTON-DOMINATED REGIONS; GIANT MOLECULAR CLOUDS; INFRARED DARK CLOUD; STAR-FORMATION; PHOTODISSOCIATION REGIONS; MAGNETOHYDRODYNAMIC TURBULENCE; LARGE-SCALE; PDR CODE; EMISSION; DUST AB Giant molecular clouds contain supersonic turbulence and magnetohydrodynamic simulations predict that this turbulence should decay rapidly. Such turbulent dissipation has the potential to create a warm (T similar to 100 K) gas component within a molecular cloud. We present observations of the CO J = 5-4 and 6-5 transitions, taken with the Herschel Space Observatory, towards the Perseus B1-East 5 region. We combine these new observations with archival measurements of lower rotational transitions and fit photodissociation region models to the data. We show that Perseus B1-E5 has an anomalously large CO J = 6-5 integrated intensity, consistent with a warm gas component existing within the region. This excess emission is consistent with predictions for shock heating due to the dissipation of turbulence in low-velocity shocks with the shocks having a volume filling factor of 0.15 per cent. We find that B1-E has a turbulent energy dissipation rate of 3.5 x 10(32) erg s(-1) and a dissipation time-scale that is only a factor of 3 larger than the flow crossing time-scale. C1 [Pon, Andy; Caselli, Paola] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Pon, Andy; Caselli, Paola] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Johnstone, Doug] Joint Astron Ctr, Hilo, HI 96720 USA. [Johnstone, Doug] NRC Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, Doug] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. [Kaufman, Michael J.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Kaufman, Michael J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Plume, Rene] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. RP Pon, A (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. EM andyrpon@gmail.com FU Natural Sciences and Engineering Research Council (NSERC) Discovery Grant; European Research Council (ERC) [PALs 320620]; UK Science and Technology Funding Council FX DJ acknowledges support from a Natural Sciences and Engineering Research Council (NSERC) Discovery Grant. This research has made use of the Smithsonian Astrophysical Observatory (SAO) / National Aeronautics and Space Administration's (NASA's) Astrophysics Data System (ADS). PC acknowledges the financial support of the European Research Council (ERC; project PALs 320620) and of successive rolling grants awarded by the UK Science and Technology Funding Council. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada, and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France, and the United States. Consortium members are as follows. Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronmico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA); Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. This research has made use of the astro-ph archive. Some spectral line data were taken from the Spectral Line Atlas of Interstellar Molecules (SLAIM, available at http://www.splatalogue.net; F. J. Lovas, private communication; Remijan et al. 2007). Herschel is an European Space Agency (ESA) space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. NR 62 TC 10 Z9 10 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 DEC 1 PY 2014 VL 445 IS 2 BP 1508 EP 1520 DI 10.1093/mnras/stu1856 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AX5IJ UT WOS:000346959400036 ER PT J AU Bennet, ED Potts, HE Teodoro, LFA Diver, DA AF Bennet, Euan D. Potts, Hugh E. Teodoro, Luis F. A. Diver, Declan A. TI Electron acceleration by magnetic collapse during decoupling SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE magnetic fields; cosmology: theory ID FIELDS; UNIVERSE AB This paper identifies the non-equilibrium evolution of magnetic field structures at the onset of large-scale recombination of an inhomogeneously ionized plasma. The context for this is the Universe during the epoch of recombination. The electromagnetic treatment of this phase transition can produce energetic electrons scattered throughout the Universe, localized near the edges of magnetic domains. This is confirmed by a numerical simulation in which a magnetic domain is modelled as a uniform field region produced by a thin surrounding current sheet. Conduction currents sustaining the magnetic structure are removed as the charges comprising them combine into neutrals. The induced electric field accompanying the magnetic collapse is able to accelerate ambient stationary electrons (that is, electrons not participating in the current sheet) to energies of up to order 10keV. This is consistent with theoretical predictions. The localized electron acceleration leads to local imbalances of charge which has implications for charge separation in the early Universe. C1 [Bennet, Euan D.; Potts, Hugh E.; Diver, Declan A.] Univ Glasgow, Sch Phys & Astron, SUPA, Glasgow G12 8QQ, Lanark, Scotland. [Teodoro, Luis F. A.] NASA, Ames Res Ctr, BAER Inst, Moffett Field, CA 94935 USA. RP Bennet, ED (reprint author), Univ Glasgow, Sch Phys & Astron, SUPA, Glasgow G12 8QQ, Lanark, Scotland. EM Euan.Bennet@glasgow.ac.uk RI Diver, Declan/E-6672-2010 OI Diver, Declan/0000-0001-6478-6020 FU University of Glasgow scholarship; STFC [ST/I001808/1] FX EDB gratefully acknowledges support from a University of Glasgow scholarship. Additionally, the authors would like to recognize support from STFC via grant number ST/I001808/1. The authors are grateful to the referee for constructive comments which helped to improve the clarity of the paper. NR 17 TC 0 Z9 0 U1 1 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 DEC 1 PY 2014 VL 445 IS 2 BP 1521 EP 1525 DI 10.1093/mnras/stu1857 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AX5IJ UT WOS:000346959400037 ER PT J AU Lazio, J Deutsch, L AF Lazio, Joseph Deutsch, Les TI The Deep Space Network at 50 SO PHYSICS TODAY LA English DT Article C1 [Lazio, Joseph; Deutsch, Les] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Lazio, J (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 4 TC 0 Z9 0 U1 1 U2 5 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0031-9228 EI 1945-0699 J9 PHYS TODAY JI Phys. Today PD DEC PY 2014 VL 67 IS 12 BP 31 EP 37 PG 7 WC Physics, Multidisciplinary SC Physics GA AW9SB UT WOS:000346596300016 ER PT J AU Russell, CT Elphic, RC AF Russell, C. T. Elphic, R. C. TI The Lunar Atmosphere and Dust Environment Explorer Mission Foreword SO SPACE SCIENCE REVIEWS LA English DT Editorial Material C1 [Russell, C. T.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. [Elphic, R. C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Russell, CT (reprint author), Univ Calif Los Angeles, Los Angeles, CA 90095 USA. EM ctrussel@igpp.ucla.edu NR 0 TC 0 Z9 0 U1 0 U2 5 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD DEC PY 2014 VL 185 IS 1-4 BP 1 EP 2 DI 10.1007/s11214-014-0120-0 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AW4GU UT WOS:000346240100001 ER PT J AU Elphic, RC Delory, GT Hine, BP Mahaffy, PR Horanyi, M Colaprete, A Benna, M Noble, SK AF Elphic, R. C. Delory, G. T. Hine, Butler P. Mahaffy, P. R. Horanyi, M. Colaprete, A. Benna, M. Noble, S. K. CA LADEE Sci Team TI The Lunar Atmosphere and Dust Environment Explorer Mission SO SPACE SCIENCE REVIEWS LA English DT Review DE LADEE; Moon; Exosphere; Dust ID LEONID METEOR-SHOWER; UPPER LIMITS; SODIUM TAIL; MOON; EXOSPHERE; SURFACE; ENHANCEMENT; DISCOVERY; LRO/LAMP; ORBITER AB The Lunar Atmosphere and Dust Environment Explorer (LADEE) mission was designed to address long-standing scientific questions about the Moon's environment, including the assessment of the composition of the lunar atmosphere, and characterization of the lunar dust environment at low orbital altitudes. LADEE was derived from the Modular Common Spacecraft Bus design that was developed at NASA Ames Research Center; it used modularized subassemblies and existing commercial spaceflight hardware to reduce cost. LADEE was launched on the very first Minotaur V, and was also the first deep space mission launched from Wallops Flight Facility in Virginia. LADEE was equipped with two in situ instruments and a remote sensing instrument to address the atmosphere and dust measurement requirements. LADEE also carried the first deep-space optical communications demonstration, the Lunar Laser Communications Demonstration. LADEE was launched in early September, 2013, took science data for over 140 days in low lunar orbit, and impacted the surface on April 18, 2014. C1 [Elphic, R. C.; Delory, G. T.; Hine, Butler P.; Colaprete, A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Mahaffy, P. R.; Benna, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Horanyi, M.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. [Noble, S. K.] NASA Headquarters, Washington, DC 20546 USA. RP Elphic, RC (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM richard.c.elphic@nasa.gov RI Benna, Mehdi/F-3489-2012 NR 32 TC 20 Z9 20 U1 0 U2 18 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD DEC PY 2014 VL 185 IS 1-4 BP 3 EP 25 DI 10.1007/s11214-014-0113-z PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AW4GU UT WOS:000346240100002 ER PT J AU Mahaffy, PR Hodges, RR Benna, M King, T Arvey, R Barciniak, M Bendt, M Carigan, D Errigo, T Harpold, DN Holmes, V Johnson, CS Kellogg, J Kimvilakani, P Lefavor, M Hengemihle, J Jaeger, F Lyness, E Maurer, J Nguyen, D Nolan, TJ Noreiga, F Noriega, M Patel, K Prats, B Quinones, O Raaen, E Tan, F Weidner, E Woronowicz, M Gundersen, C Battel, S Block, BP Arnett, K Miller, R Cooper, C Edmonson, C AF Mahaffy, Paul R. Hodges, R. Richard Benna, Mehdi King, Todd Arvey, Robert Barciniak, Michael Bendt, Mirl Carigan, Daniel Errigo, Therese Harpold, Daniel N. Holmes, Vincent Johnson, Christopher S. Kellogg, James Kimvilakani, Patrick Lefavor, Matthew Hengemihle, Jerome Jaeger, Ferzan Lyness, Eric Maurer, John Nguyen, Daniel Nolan, Thomas J. Noreiga, Felix Noriega, Marvin Patel, Kiran Prats, Benito Quinones, Omar Raaen, Eric Tan, Florence Weidner, Edwin Woronowicz, Michael Gundersen, Cynthia Battel, Steven Block, Bruce P. Arnett, Ken Miller, Ryan Cooper, Curt Edmonson, Charles TI The Neutral Mass Spectrometer on the Lunar Atmosphere and Dust Environment Explorer Mission SO SPACE SCIENCE REVIEWS LA English DT Review DE Moon, lunar volatiles; Mass spectrometry; Noble gases; Argon; Helium ID LATERAL TRANSPORT; EXOSPHERES; ION AB The Neutral Mass Spectrometer (NMS) of the Lunar Atmosphere and Dust Environment Explorer (LADEE) Mission is designed to measure the composition and variability of the tenuous lunar atmosphere. The NMS complements two other instruments on the LADEE spacecraft designed to secure spectroscopic measurements of lunar composition and in situ measurement of lunar dust over the course of a 100-day mission in order to sample multiple lunation periods. The NMS utilizes a dual ion source designed to measure both surface reactive and inert species and a quadrupole analyzer. The NMS is expected to secure time resolved measurements of helium and argon and determine abundance or upper limits for many other species either sputtered or thermally evolved from the lunar surface. C1 [Mahaffy, Paul R.; Benna, Mehdi; King, Todd; Arvey, Robert; Barciniak, Michael; Bendt, Mirl; Carigan, Daniel; Errigo, Therese; Harpold, Daniel N.; Holmes, Vincent; Johnson, Christopher S.; Kellogg, James; Kimvilakani, Patrick; Lefavor, Matthew; Hengemihle, Jerome; Jaeger, Ferzan; Lyness, Eric; Maurer, John; Nguyen, Daniel; Nolan, Thomas J.; Noreiga, Felix; Noriega, Marvin; Patel, Kiran; Prats, Benito; Quinones, Omar; Raaen, Eric; Tan, Florence; Weidner, Edwin; Woronowicz, Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hodges, R. Richard] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. [Gundersen, Cynthia] AMU Engn, Miami, FL 33156 USA. [Battel, Steven] Battel Engn, Scottsdale, AZ 85253 USA. [Block, Bruce P.; Arnett, Ken; Miller, Ryan; Cooper, Curt; Edmonson, Charles] Univ Michigan, Space Phys Res Lab, Ann Arbor, MI 48109 USA. RP Mahaffy, PR (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM Paul.R.Mahaffy@nasa.gov RI Benna, Mehdi/F-3489-2012 FU Science Mission Directorate of the National Aeronautics and Space Administration FX The NMS development was funded by the Science Mission Directorate of the National Aeronautics and Space Administration. NR 24 TC 34 Z9 35 U1 0 U2 5 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD DEC PY 2014 VL 185 IS 1-4 BP 27 EP 61 DI 10.1007/s11214-014-0043-9 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AW4GU UT WOS:000346240100003 ER PT J AU Suselj, K Hogan, TF Teixeira, J AF Suselj, Kay Hogan, Timothy F. Teixeira, Joao TI Implementation of a Stochastic Eddy-Diffusivity/Mass-Flux Parameterization into the Navy Global Environmental Model SO WEATHER AND FORECASTING LA English DT Article DE Boundary layer; Convective parameterization; Parameterization; Stochastic models; Subgrid-scale processes ID SHALLOW CUMULUS CONVECTION; BOUNDARY-LAYER CLOUDS; PDF-BASED MODEL; UNIFIED PARAMETERIZATION; TURBULENCE CLOSURE; MOIST CONVECTION; PART II; SINGLE-COLUMN; TRANSPORT; PARAMETRIZATION AB A unified boundary layer and shallow convection parameterization based on a stochastic eddy-diffusivity/mass-flux (EDMF) approach is implemented and tested in the Navy Global Environmental Model (NAVGEM). The primary goals of this work are to improve the representation of convectively driven boundary layers and the coupling between the boundary layer and cumulus regions. Within the EDMF framework the subgrid vertical fluxes are calculated as a sum of an eddy-diffusivity part, which in the current implementation is based on the approach developed by Louis in the late 1970s, and a stochastic mass-flux parameterization. The mass-flux parameterization is a model for both dry and moist convective thermals. Dry thermals, which represent surface-forced coherent structures in a flow, provide countergradient mixing in the boundary layer and, if conditions permit, are the roots for moist thermals. Moist thermals represent shallow convective clouds. The new parameterization implemented in a single-column model (SCM) version of NAVGEM is shown to be able to realistically simulate a variety of dry and moist convective cases. The NAVGEM SCM results are validated against large-eddy-simulation results. The skill of NAVGEM as a global weather forecasting model is considerably improved with the new EDMF parameterization. The EDMF parameterization became part of the operational NAVGEM in November 2013. C1 [Suselj, Kay; Teixeira, Joao] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hogan, Timothy F.] Naval Res Lab, Marine Meteorol Div, Monterey, CA USA. RP Suselj, K (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM kay.suselj@jpl.nasa.gov FU Office of Naval Research [N0001411IP20087, N0001411IP20069, N0001413WX20163]; National Aeronautics and Space Administration FX We acknowledge the support provided by the Office of Naval Research, Marine Meteorology Program, under Awards N0001411IP20087, N0001411IP20069, and N0001413WX20163. This work was partially carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We thank the editor and two anonymous reviewers for their constructive comments, which helped us to improve the manuscript. NR 43 TC 6 Z9 6 U1 5 U2 20 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0882-8156 EI 1520-0434 J9 WEATHER FORECAST JI Weather Forecast. PD DEC PY 2014 VL 29 IS 6 BP 1374 EP 1390 DI 10.1175/WAF-D-14-00043.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AW5ZG UT WOS:000346348800008 ER PT J AU Dahlgren, RP Johnston, MJS Vanderbilt, VC Nakaba, RN AF Dahlgren, Robert P. Johnston, Malcolm J. S. Vanderbilt, Vern C. Nakaba, Rebecca N. TI Comparison of the Stress-Stimulated Current of Dry and Fluid-Saturated Gabbro Samples SO BULLETIN OF THE SEISMOLOGICAL SOCIETY OF AMERICA LA English DT Article ID SAN-ANDREAS FAULT; ELECTRICAL-RESISTIVITY; CREEPING SEGMENT; IGNEOUS ROCKS; GENERATION; ELECTRODES; SLIP AB We investigate charge generation as a function of stress in fine-grained gabbro for both nominally dry samples and samples fully saturated with electrically conductive brine fluids similar to those observed in active earthquake fault zones. These experiments address a number of proposed and reported electrical precursory and coseismic phenomena associated with earthquakes. Compressive load was applied to one end of the sample in repetitive cycles using a pair of precision steel platens driven by a large hydraulic press. The samples were tested by cycling between constant low stress and constant high stress values with a 200-s periodicity. Net charge transport between the stressed and unstressed sample ends was monitored with a picoammeter. For the nominally dry samples, stress-stimulated current (SSC) transients on the order of 50-400 pA peak-to-peak were observed with a decay time constant similar to 10 s during stress loading and unloading. Under constant compressive loads of similar to 22 MPa, small negative polarity SSC of similar to 15 pA magnitude was observed as an offset from the baseline current at low load (5 MPa) conditions. For the fluid-saturated samples, neither transients nor SSCs were observed as a function of stress when the load was cycled, an observation that is consistent with more rapid internal self-discharge due to higher electrical conductivity of the sample. Because the Earth's crust is fluid saturated, observation of significant electrical charge buildup is not expected during the observed slow stress accumulation prior to earthquakes or during any slow precursory stress release that may occur in the region of earthquake nucleation. However, observation of coseismic charge generation due to electrokinetic, triboelectric, and other processes may occur during earthquake stress drops, surface rupture, and seismic-wave arrivals from dynamic rupture. C1 [Dahlgren, Robert P.] NASA, Ames Res Ctr, CSUMB, Moffett Field, CA 94035 USA. [Johnston, Malcolm J. S.] US Geol Survey, Menlo Pk, CA 94025 USA. [Vanderbilt, Vern C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Nakaba, Rebecca N.] Wesleyan Univ, Van Vleck Observ, Middletown, CT 06457 USA. RP Dahlgren, RP (reprint author), NASA, Ames Res Ctr, CSUMB, Mail Stop 245-4, Moffett Field, CA 94035 USA. FU NASA [NNX08AG81G]; Search for Extraterrestrial Intelligence (SETI) Institute and Bennington College; San Jose State University and the SETI Institute FX We gratefully acknowledge the contributions of F. Freund who developed (beginning in 2002) the ST1 setup and then demonstrated it to our team at the beginning of this research, assisted in the development of the improved ST2 setup (Dahlgren, Johnston, Freund, Nakaba, and Vanderbilt, 2012), and participated in the collection of all data reported here (Dahlgren, Johnston, Freund, Nakaba, Jahoda, et al., 2012; Dahlgren, Vanderbilt, et al., 2012). The authors would like to thank the National Science Foundation Research Experiences for Undergraduates program, the NASA Engineering Evaluation Laboratory (Lynn Hofland and Jerry Wang), and the U.S. Geological Survey (USGS) Rock Mechanics Laboratory (David Lockner). The authors thank the two anonymous BSSA reviewers, peer reviewers at NASA Ames Research Center (Christine Scofield and Vincent Ambrosia), and the USGS (Dave Lockner and Nick Beeler) for helpful suggestions that improved the manuscript. This research was supported in part by the NASA Earth Surface and Interior program through a grant with F. Freund as the principal investigator (NNX08AG81G). Rebecca N. Nakaba received support from the Search for Extraterrestrial Intelligence (SETI) Institute and Bennington College and Robert P. Dahlgren received support from San Jose State University and the SETI Institute. NR 42 TC 5 Z9 5 U1 0 U2 5 PU SEISMOLOGICAL SOC AMER PI ALBANY PA 400 EVELYN AVE, SUITE 201, ALBANY, CA 94706-1375 USA SN 0037-1106 EI 1943-3573 J9 B SEISMOL SOC AM JI Bull. Seismol. Soc. Amer. PD DEC PY 2014 VL 104 IS 6 BP 2662 EP 2672 DI 10.1785/0120140144 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AW2RP UT WOS:000346136800003 ER PT J AU Bhawar, RL Jiang, JH Su, H Schwartz, MJ AF Bhawar, Rohini L. Jiang, Jonathan H. Su, Hui Schwartz, Michael J. TI Variation of upper tropospheric clouds and water vapour over the Indian Ocean SO INTERNATIONAL JOURNAL OF CLIMATOLOGY LA English DT Article DE clouds; variability; Indian Ocean ID TROPICAL DEEP CONVECTION; SEA-SURFACE TEMPERATURE; EL-NINO; CIRRUS CLOUDS; DIPOLE MODE; CLIMATE; FEEDBACK; ENSO; TELECONNECTION; VARIABILITY AB The objective of this paper is to understand the response of upper tropospheric (UT) clouds and water vapour (H2O) to sea surface temperature (SST) changes over the Indian Ocean. UT ice water content (IWC) and H2O observed by Aura Microwave Limb Sounder (MLS) show dominant dipole mode variability over the Indian Ocean. This is characterized by the oscillating differences between the western and eastern Indian Ocean (WIO and EIO) with greater amplitude in September, October and November (SON) as compared with other seasons. We denote X = X_WIO - X_EIO, with X being H2O and IWC at three UT levels (215, 147 and 100 hPa) or SST, following the documented definition for Indian Ocean Dipole (IOD). We find a strong positive correlation between IWC at the three UT levels and SST, and a relatively weak positive correlation between IWC and Nino 3.4 SST, suggesting that the UT clouds over the Indian Ocean are largely controlled by the local thermally driven circulation, while teleconnection to El Nino and Southern Oscillation (ENSO) plays a secondary role. The change per degree of SST for IWC in SON is 5.5 mg m(-3) C-1 at 215 hPa, 1.6 mg m(-3) C-1 at 147 hPa and 0.13 mg m(-3) C-1 at 100 hPa (i.e. 96% C-1, 87% C-1 and 46% C-1 increase at 215, 147 and 100 hPa, respectively). We find 36% C-1 increase in H2O at 215 hPa with increasing SST, associated with a sharp contrast in convective strength (indicated by IWC) over the Indian Ocean region. On the other hand, H2O at 100 hPa decreases with increasing SST because cold temperature is observed above convective clouds and 100 hPa H2O is largely controlled by temperature. The Nino 3.4 SST has a relatively weak positive (negative) correlation with H2O at 215 hPa (100 hPa). C1 [Bhawar, Rohini L.; Jiang, Jonathan H.; Su, Hui; Schwartz, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Bhawar, Rohini L.] Univ Pune, Dept Atmospher & Space Sci, Pune 411007, Maharashtra, India. RP Bhawar, RL (reprint author), Univ Pune, Dept Atmospher & Space Sci, Pune 411007, Maharashtra, India. EM rohinibhawar@gmail.com RI Schwartz, Michael/F-5172-2016 OI Schwartz, Michael/0000-0001-6169-5094 NR 45 TC 1 Z9 1 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0899-8418 EI 1097-0088 J9 INT J CLIMATOL JI Int. J. Climatol. PD DEC PY 2014 VL 34 IS 15 BP 3840 EP 3848 DI 10.1002/joc.3942 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AW0PX UT WOS:000345996500002 ER PT J AU Neena, JM Jiang, XN Waliser, D Lee, JY Wang, B AF Neena, J. M. Jiang, Xianan Waliser, Duane Lee, June-Yi Wang, Bin TI Eastern Pacific Intraseasonal Variability: A Predictability Perspective SO JOURNAL OF CLIMATE LA English DT Article ID MADDEN-JULIAN OSCILLATION; NORTH-AMERICAN-MONSOON; ASIAN SUMMER MONSOON; BOREAL SUMMER; FORECAST SYSTEM; POTENTIAL PREDICTABILITY; MIDSUMMER DROUGHT; PRINCIPAL MODES; GLOBAL TROPICS; MJO PREDICTION AB The eastern Pacific (EPAC) warm pool is a region of strong intraseasonal variability (ISV) during boreal summer. While the EPAC ISV is known to have large-scale impacts that shape the weather and climate in the region (e.g., tropical cyclones and local monsoon), simulating the EPAC ISV is still a great challenge for present-day global weather and climate models. In the present study, the predictive skill and predictability of the EPAC ISV are explored in eight coupled model hindcasts from the Intraseasonal Variability Hindcast Experiment (ISVHE). Relative to the prediction skill for the boreal winter Madden-Julian oscillation (MJO) in the ISVHE (similar to 15-25 days), the skill for the EPAC ISV is considerably lower in most models, with an average skill around 10 days. On the other hand, while the MJO exhibits a predictability of 35-45 days, the predictability estimate for the EPAC ISV is 20-30 days. The prediction skill was found to be higher when the hindcasts were initialized from the convective phase of the EPAC ISV as opposed to the subsidence phase. Higher prediction skill was also found to be associated with active MJO initial conditions over the western Pacific (evident in four out of eight models), signaling the importance of exploring the dynamic link between the MJO and the EPAC ISV. The results illustrate the possibility and need for improving dynamical prediction systems to facilitate more accurate and longer-lead predictions of the EPAC ISV and associated weather and short-term climate variability. C1 [Neena, J. M.; Jiang, Xianan; Waliser, Duane] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. [Neena, J. M.; Waliser, Duane] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lee, June-Yi; Wang, Bin] Univ Hawaii Manoa, Int Pacific Res Ctr, Honolulu, HI 96822 USA. [Lee, June-Yi; Wang, Bin] Univ Hawaii Manoa, Dept Meteorol, Honolulu, HI 96822 USA. [Lee, June-Yi] Pusan Natl Univ, Inst Environm Studies, Pusan, South Korea. RP Neena, JM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 233-300, Pasadena, CA 91109 USA. EM neena.j.mani@jpl.nasa.gov FU NOAA's Climate Program Office CTB Program [GC10287a]; MAPP Program [NA12OAR4310075]; Office of Naval Research [ONRBAA12-001]; NSF Climate and Large-Scale Dynamics Program [AGS-1221013, AGS-1228302]; National Aeronautics and Space Administration FX The authors thank all the participating members of ISVHE project for the dataset. This work was supported by NOAA's Climate Program Office CTB Program under Grant GC10287a and MAPP Program under Grant NA12OAR4310075, the Office of Naval Research under Project ONRBAA12-001, and NSF Climate and Large-Scale Dynamics Program under Awards AGS-1221013 and AGS-1228302. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 51 TC 6 Z9 7 U1 0 U2 17 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD DEC PY 2014 VL 27 IS 23 BP 8869 EP 8883 DI 10.1175/JCLI-D-14-00336.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AW1NC UT WOS:000346055100017 ER PT J AU Kalmus, P Lebsock, M Teixeira, J AF Kalmus, Peter Lebsock, Matthew Teixeira, Joao TI Observational Boundary Layer Energy and Water Budgets of the Stratocumulus-to-Cumulus Transition SO JOURNAL OF CLIMATE LA English DT Article ID LARGE-EDDY SIMULATIONS; MARINE STRATOCUMULUS; NUMERICAL SIMULATIONS; PACIFIC STRATOCUMULUS; STRATIFORM CLOUDS; DIURNAL CYCLE; SIMPLE-MODEL; PRECIPITATION; ENTRAINMENT; REANALYSIS AB The authors estimate summer mean boundary layer water and energy budgets along a northeast Pacific transect from 35 degrees to 15 degrees N, which includes the transition from marine stratocumulus to trade cumulus clouds. Observational data is used from three A-Train satellites, Aqua, CloudSat, and the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO); data derived from GPS signals intercepted by microsatellites of the Constellation Observing System for Meteorology, Ionosphere, and Climate (COSMIC); and the container-ship-based Marine Atmospheric Radiation Measurement Program (ARM) Global Energy and Water Cycle Experiment Cloud System Study/Working Group on Numerical Experimentation (GCSS/WGNE) Pacific Cross-Section Intercomparison (GPCI) Investigation of Clouds (MAGIC) campaign. These are unique satellite and shipborne observations providing the first global-scale observations of light precipitation, new vertically resolved radiation budget products derived from the active sensors, and well-sampled radiosonde data near the transect. In addition to the observations, the European Centre for Medium-Range Weather Forecasts (ECMWF) Interim Re-Analysis (ERA-Interim) fields are utilized to estimate the budgets. Both budgets approach within 3W m(-2) averaged along the transect, although uncertainty estimates from the study are much larger than this residual. A mean entrainment rate along the transect of 3.4(-1.1)(+1.2) mm s(-1) is also estimated. A gradual transition is observed in the climatological mean from the stratocumulus regime to the cumulus regime characterized by an increase in boundary layer height, latent heat flux, rain, and the horizontal advection of dry air and a decrease in entrainment of warm dry air. C1 [Kalmus, Peter; Lebsock, Matthew; Teixeira, Joao] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kalmus, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM peter.m.kalmus@jpl.nasa.gov FU National Aeronautics and Space Administration FX The research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We also acknowledge the NASA MEaSUREs program. Data were obtained from the Atmospheric Radiation Measurement Program (ARM) sponsored by the U.S. Department of Energy, Office of Science, Office of Biological and Environmental Research, Climate and Environmental Sciences Division. Data were obtained from the NASA CloudSat project. NCEP-2 data were provided by the NOAA/OAR/ESRL/PSD, Boulder, Colorado. We thank Chi Ao for providing COSMIC data and Mike Reynolds for providing MAGIC surface flux data. We are grateful for helpful suggestions from three anonymous referees. NR 47 TC 3 Z9 3 U1 2 U2 12 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD DEC PY 2014 VL 27 IS 24 BP 9155 EP 9170 DI 10.1175/JCLI-D-14-00242.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AW1NK UT WOS:000346055900010 ER PT J AU Horn, M Walsh, K Zhao, M Camargo, SJ Scoccimarro, E Murakami, H Wang, H Ballinger, A Kumar, A Shaevitz, DA Jonas, JA Oouchi, K AF Horn, Michael Walsh, Kevin Zhao, Ming Camargo, Suzana J. Scoccimarro, Enrico Murakami, Hiroyuki Wang, Hui Ballinger, Andrew Kumar, Arun Shaevitz, Daniel A. Jonas, Jeffrey A. Oouchi, Kazuyoshi TI Tracking Scheme Dependence of Simulated Tropical Cyclone Response to Idealized Climate Simulations SO JOURNAL OF CLIMATE LA English DT Article ID RESOLUTION; MODELS; ARCHIVE AB Future tropical cyclone activity is a topic of great scientific and societal interest. In the absence of a climate theory of tropical cyclogenesis, general circulation models are the primary tool available for investigating the issue. However, the identification of tropical cyclones in model data at moderate resolution is complex, and numerous schemes have been developed for their detection. The influence of different tracking schemes on detected tropical cyclone activity and responses in the Hurricane Working Group experiments is examined herein. These are idealized atmospheric general circulation model experiments aimed at determining and distinguishing the effects of increased sea surface temperature and other increased CO2 effects on tropical cyclone activity. Two tracking schemes are applied to these data and the tracks provided by each modeling group are analyzed. The results herein indicate moderate agreement between the different tracking methods, with some models and experiments showing better agreement across schemes than others. When comparing responses between experiments, it is found that much of the disagreement between schemes is due to differences in duration, wind speed, and formation-latitude thresholds. After homogenization in these thresholds, agreement between different tracking methods is improved. However, much disagreement remains, accountable for by more fundamental differences between the tracking schemes. The results indicate that sensitivity testing and selection of objective thresholds are the key factors in obtaining meaningful, reproducible results when tracking tropical cyclones in climate model data at these resolutions, but that more fundamental differences between tracking methods can also have a significant impact on the responses in activity detected. C1 [Horn, Michael; Walsh, Kevin] Univ Melbourne, Sch Earth Sci, Melbourne, Vic, Australia. [Zhao, Ming] NOAA GFDL, Princeton, NJ USA. [Camargo, Suzana J.; Shaevitz, Daniel A.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Scoccimarro, Enrico; Jonas, Jeffrey A.] Ist Nazl Geofis & Vulcanol, Bologna, Italy. [Scoccimarro, Enrico; Jonas, Jeffrey A.] Centro Euro Mediterraneo Cambiamenti Climat, Bologna, Italy. [Murakami, Hiroyuki] IPRC MRI, Tsukuba, Ibaraki, Japan. [Wang, Hui; Kumar, Arun] NOAA NWS NCEP Climate Predict Ctr, College Pk, MD USA. [Ballinger, Andrew] Princeton Univ, Program Atmospher & Ocean Sci, Princeton, NJ 08544 USA. Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. Columbia Univ, Ctr Climate Syst Res, New York, NY USA. NASA Goddard Inst Space Studies, New York, NY USA. [Oouchi, Kazuyoshi] Japan Agcy Marine Earth Sci & Technol, Yokohama, Kanagawa, Japan. RP Horn, M (reprint author), Univ Melbourne, Sch Earth Sci, Corner Swanston & Elgin St, Parkville, Vic 3010, Australia. EM mjhorn@student.unimelb.edu.au RI Camargo, Suzana/C-6106-2009; Murakami, Hiroyuki/L-5745-2015; Zhao, Ming/C-6928-2014 OI Camargo, Suzana/0000-0002-0802-5160; Walsh, Kevin/0000-0002-1860-510X; FU NSF [AGS 1143959]; NASA [NNX09AK34G]; Italian Ministry of Education, University and Research; Italian Ministry of Environment, Land and Sea FX The authors thank the U.S. Climate Variability and Predictability Program, the Australian Research Council Centre of Excellence for Climate System Science, and their respective institutions for supporting this work. Suzana Camargo, Dan Shaevitz, and Kevin Walsh are supported by NSF Grant AGS 1143959. Suzana Camargo is supported by NASA Grant NNX09AK34G. Enrico Scoccimarro acknowledges support from the Italian Ministry of Education, University and Research and the Italian Ministry of Environment, Land and Sea under the GEMINA project. Thanks also to Sally Lavender of CSIRO for help with plotting software. We acknowledge also the support provided by Naomi Henderson, who compiled the HWG model output archive. NR 23 TC 21 Z9 21 U1 1 U2 10 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD DEC PY 2014 VL 27 IS 24 BP 9197 EP 9213 DI 10.1175/JCLI-D-14-00200.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AW1NK UT WOS:000346055900012 ER PT J AU Koster, RD Chang, YH Schubert, SD AF Koster, Randal D. Chang, Yehui Schubert, Siegfried D. TI A Mechanism for Land-Atmosphere Feedback Involving Planetary Wave Structures SO JOURNAL OF CLIMATE LA English DT Article ID SOIL-MOISTURE; PRECIPITATION; CLIMATE; VARIABILITY; PERFORMANCE; PROJECT; HEAT AB While the ability of land surface conditions to influence the atmosphere has been demonstrated in various modeling and observational studies, the precise mechanisms by which land-atmosphere feedback occurs are still largely unknown: particularly the mechanisms that allow land moisture state in one region to affect atmospheric conditions in another. Such remote impacts are examined here in the context of atmospheric general circulation model (AGCM) simulations, leading to the identification of one potential mechanism: the phase locking and amplification of a planetary wave through the imposition of a spatial pattern of soil moisture at the land surface. This mechanism, shown here to be relevant in the AGCM, apparently also operates in nature, as suggested by supporting evidence found in reanalysis data. C1 [Koster, Randal D.; Chang, Yehui; Schubert, Siegfried D.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Chang, Yehui] Morgan State Univ, Baltimore, MD 21239 USA. RP Koster, RD (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA. EM randal.d.koster@nasa.gov RI Koster, Randal/F-5881-2012 OI Koster, Randal/0000-0001-6418-6383 FU NOAA; NASA Energy and Water Cycle Study (NEWS) program FX Support for this project was provided by the NOAA Modeling, Analysis, Predictions and Projections (MAPP) program; the NASA Energy and Water Cycle Study (NEWS) program; and the NASA Modeling, Analysis, and Prediction Program. We thank Sarith Mahanama, Greg Walker, and Hailan Wang for help with dataset logistics. NR 30 TC 7 Z9 7 U1 3 U2 16 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD DEC PY 2014 VL 27 IS 24 BP 9290 EP 9301 DI 10.1175/JCLI-D-14-00315.1 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AW1NK UT WOS:000346055900017 ER PT J AU Parkinson, CL AF Parkinson, Claire L. TI Global Sea Ice Coverage from Satellite Data: Annual Cycle and 35-Yr Trends SO JOURNAL OF CLIMATE LA English DT Article ID VARIABILITY; DECLINE; RECORD AB Well-established satellite-derived Arctic and Antarctic sea ice extents are combined to create the global picture of sea ice extents and their changes over the 35-yr period 1979-2013. Results yield a global annual sea ice cycle more in line with the high-amplitude Antarctic annual cycle than the lower-amplitude Arctic annual cycle but trends more in line with the high-magnitude negative Arctic trends than the lower-magnitude positive Antarctic trends. Globally, monthly sea ice extent reaches a minimum in February and a maximum generally in October or November. All 12 months show negative trends over the 35-yr period, with the largest magnitude monthly trend being the September trend, at -68 200 +/- 10 500 km(2) yr(-1) (-2.62% +/- 0.40% decade(-1)), and the yearly average trend being -35 000 +/- 5900km(2) yr(-1) (21.47% +/- 0.25% decade(-1)). C1 [Parkinson, Claire L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Parkinson, CL (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Code 615, Greenbelt, MD 20771 USA. EM claire.l.parkinson@nasa.gov FU NASA FX The author thanks Nick DiGirolamo of Science Systems and Applications, Inc., for his help in the generation of the figures, John E. Walsh for his help as the journal editor in charge of the paper, anonymous reviewers for their constructive comments, and the NASA Cryospheric Sciences Program for funding the work. NR 38 TC 11 Z9 12 U1 4 U2 42 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD DEC PY 2014 VL 27 IS 24 BP 9377 EP 9382 DI 10.1175/JCLI-D-14-00605.1 PG 6 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AW1NK UT WOS:000346055900023 ER PT J AU Kumar, SV Harrison, KW Peters-Lidard, CD Santanello, JA Kirschbaum, D AF Kumar, Sujay V. Harrison, Kenneth W. Peters-Lidard, Christa D. Santanello, Joseph A., Jr. Kirschbaum, Dalia TI Assessing the Impact of L-Band Observations on Drought and Flood Risk Estimation: A Decision-Theoretic Approach in an OSSE Environment SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Soil moisture; Satellite observations; Data assimilation; Land surface model ID SYSTEM SIMULATION EXPERIMENT; SOIL-MOISTURE OBSERVATIONS; DATA ASSIMILATION; UNITED-STATES; PROBABILISTIC FORECASTS; BRIGHTNESS TEMPERATURE; CLIMATE PREDICTABILITY; MICROWAVE EMISSION; ENSEMBLE FORECASTS; BAYESIAN-APPROACH AB Observing system simulation experiments (OSSEs) are often conducted to evaluate the worth of existing data and data yet to be collected from proposed new missions. As missions increasingly require a broader Earth systems focus, it is important that the OSSEs capture the potential benefits of the observations on end-use applications. Toward this end, the results from the OSSEs must also be evaluated with a suite of metrics that capture the value, uncertainty, and information content of the observations while factoring in both science and societal impacts. This article presents a soil moisture OSSE that employs simulated L-band measurements and assesses its utility toward improving drought and flood risk estimates using the NASA Land Information System (LIS). A decision-theory-based analysis is conducted to assess the economic utility of the observations toward improving these applications. The results suggest that the improvements in surface soil moisture, root-zone soil moisture, and total runoff fields obtained through the assimilation of L-band measurements are effective in providing improvements in the drought and flood risk assessments as well. The decision-theory analysis not only demonstrates the economic utility of observations but also shows that the use of probabilistic information from the model simulations is more beneficial compared to the use of corresponding deterministic estimates. The experiment also demonstrates the value of a comprehensive modeling environment such as LIS for conducting end-to-end OSSEs by linking satellite observations, physical models, data assimilation algorithms, and end-use application models in a single integrated framework. C1 [Kumar, Sujay V.] Sci Applicat Int Corp, Greenbelt, MD USA. [Kumar, Sujay V.; Harrison, Kenneth W.; Peters-Lidard, Christa D.; Santanello, Joseph A., Jr.; Kirschbaum, Dalia] NASA GSFC, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Harrison, Kenneth W.] Earth Syst Sci Interdisciplinary Ctr, College Pk, MD USA. RP Kumar, SV (reprint author), NASA GSFC, Hydrol Sci Lab, Code 617, Greenbelt, MD 20771 USA. EM sujay.v.kumar@nasa.gov RI Kumar, Sujay/B-8142-2015; Santanello, Joseph/D-4438-2012; Peters-Lidard, Christa/E-1429-2012 OI Santanello, Joseph/0000-0002-0807-6590; Peters-Lidard, Christa/0000-0003-1255-2876 FU NASA Earth Science Technology Office (ESTO) [AIST-11-0013] FX We gratefully acknowledge the financial support from the NASA Earth Science Technology Office (ESTO) [Advanced Information Systems Technology (AIST) program Award AIST-11-0013]. Computing was supported by the resources at the NASA Center for Climate Simulation (NCCS). The NLDAS-2 forcing data used in this effort were acquired as part of the activities of NASA's Science Mission Directorate and are archived and distributed by the Goddard Earth Sciences (GES) Data and Information Services Center (DISC). We are grateful to Dr. Gabrielle De Lannoy for assistance with the radiative transfer modeling components of this work. NR 73 TC 7 Z9 7 U1 5 U2 20 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD DEC PY 2014 VL 15 IS 6 BP 2140 EP 2156 DI 10.1175/JHM-D-13-0204.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AU9FZ UT WOS:000345898400003 ER PT J AU Getirana, ACV Boone, A Peugeot, C AF Getirana, Augusto C. V. Boone, Aaron Peugeot, Christophe TI Evaluating LSM-Based Water Budgets over a West African Basin Assisted with a River Routing Scheme SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Africa; Hydrologic models; Land surface model; Model evaluation; performance; Parameterization ID DONGA CATCHMENT BENIN; LAND-SURFACE; HYDROLOGICAL PROCESSES; EVAPOTRANSPIRATION ALGORITHM; AMAZON BASIN; MODEL; PARAMETERIZATION; PROJECT; SCALE; REPRESENTATION AB Within the framework of the African Monsoon Multidisciplinary Analysis (AMMA) Land Surface Model Intercomparison Project phase 2 (ALMIP-2), this study evaluates the water balance simulated by the Interactions between Soil, Biosphere, and Atmosphere (ISBA) over the upper Oueme River basin, in Benin, using a mesoscale river routing scheme (RRS). The RRS is based on the nonlinear Muskingum-Cunge method coupled with two linear reservoirs that simulate the time delay of both surface runoff and base flow that are produced by land surface models. On the basis of the evidence of a deep water-table recharge in that region, a reservoir representing the deep-water infiltration (DWI) is introduced. The hydrological processes of the basin are simulated for the 2005-08 AMMA field campaign period during which rainfall and streamflow data were intensively collected over the study area. Optimal RRS parameter sets were determined for three optimization experiments that were performed using daily streamflow at five gauges within the basin. Results demonstrate that the RRS simulates streamflow at all gauges with relative errors varying from -20% to 3% and Nash-Sutcliffe coefficients varying from 0.62 to 0.90. DWI varies from 24% to 67% of the base flow as a function of the subbasin. The relatively simple reservoir DWI approach is quite robust, and further improvements would likely necessitate more complex solutions (e.g., considering seasonality and soil type in ISBA); thus, such modifications are recommended for future studies. Although the evaluation shows that the simulated streamflows are generally satisfactory, further field investigations are necessary to confirm some of the model assumptions. C1 [Getirana, Augusto C. V.; Boone, Aaron] Meteo France, CNRM GAME, Toulouse, France. [Peugeot, Christophe] Hydrosciences, Montpellier, France. RP Getirana, ACV (reprint author), NASA Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM augusto.getirana@nasa.gov RI Getirana, Augusto/G-4630-2011 FU African Monsoon Multidisciplinary Analysis (AMMA) project FX A.C.V. Getirana was funded by EUMETSAT in the framework of the LSA SAF activities. This work is supported by the African Monsoon Multidisciplinary Analysis (AMMA) project. Based on a French initiative, AMMAwas built by an international scientific group and has been funded by a large number of agencies in France, the United Kingdom, the United States, and Africa. The ALMIP-2 project is supported by AMMA, IRD (French overseas research institute), and INSU/CNRS (EC2CO/CYTRIX programme) French agencies. Observed data were obtained in the framework of the AMMA-CATCH Observatory (www. amma-catch. org) and with the contribution of the scientific and technical teams in Benin (IRD and Direction Generale de l'Eau, Cotonou). In particular, acknowledgements are due to Arnaud Zannou for providing streamflow data. NR 49 TC 3 Z9 3 U1 2 U2 14 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD DEC PY 2014 VL 15 IS 6 BP 2331 EP 2346 DI 10.1175/JHM-D-14-0012.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AU9FZ UT WOS:000345898400014 ER PT J AU Kumar, SV Peters-Lidard, CD Mocko, D Reichle, R Liu, YQ Arsenault, KR Xia, YL Ek, M Riggs, G Livneh, B Cosh, M AF Kumar, Sujay V. Peters-Lidard, Christa D. Mocko, David Reichle, Rolf Liu, Yuqiong Arsenault, Kristi R. Xia, Youlong Ek, Michael Riggs, George Livneh, Ben Cosh, Michael TI Assimilation of Remotely Sensed Soil Moisture and Snow Depth Retrievals for Drought Estimation SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Streamflow; Drought; Snow; Soil moisture; Data assimilation ID LAND DATA ASSIMILATION; PASSIVE MICROWAVE OBSERVATIONS; ENSEMBLE KALMAN FILTER; SURFACE MODEL; UNITED-STATES; WATER EQUIVALENT; RIVER-BASIN; STREAMFLOW FORECASTS; INFORMATION-SYSTEM; NATIONAL CENTERS AB The accurate knowledge of soil moisture and snow conditions is important for the skillful characterization of agricultural and hydrologic droughts, which are defined as deficits of soil moisture and streamflow, respectively. This article examines the influence of remotely sensed soil moisture and snow depth retrievals toward improving estimates of drought through data assimilation. Soil moisture and snow depth retrievals from a variety of sensors (primarily passive microwave based) are assimilated separately into the Noah land surface model for the period of 1979-2011 over the continental United States, in the North American Land Data Assimilation System (NLDAS) configuration. Overall, the assimilation of soil moisture and snow datasets was found to provide marginal improvements over the open-loop configuration. Though the improvements in soil moisture fields through soil moisture data assimilation were barely at the statistically significant levels, these small improvements were found to translate into subsequent small improvements in simulated streamflow. The assimilation of snow depth datasets were found to generally improve the snow fields, but these improvements did not always translate to corresponding improvements in streamflow, including some notable degradations observed in the western United States. A quantitative examination of the percentage drought area from root-zone soil moisture and streamflow percentiles was conducted against the U.S. Drought Monitor data. The results suggest that soil moisture assimilation provides improvements at short time scales, both in the magnitude and representation of the spatial patterns of drought estimates, whereas the impact of snow data assimilation was marginal and often disadvantageous. C1 [Kumar, Sujay V.; Mocko, David; Arsenault, Kristi R.] Sci Applicat Int Corp, Mclean, VA 22102 USA. [Kumar, Sujay V.; Peters-Lidard, Christa D.; Mocko, David; Liu, Yuqiong; Arsenault, Kristi R.] NASA GSFC, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Mocko, David; Reichle, Rolf] NASA Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Liu, Yuqiong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Xia, Youlong] IM Syst Grp Inc, College Pk, MD USA. [Xia, Youlong; Ek, Michael] NOAA NCEP Environm Modeling Ctr, College Pk, MD USA. [Riggs, George] Sci Syst & Applicat Inc, Lanham, MD USA. [Riggs, George] NASA Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA. [Livneh, Ben] Univ Colorado, NOAA, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Cosh, Michael] ARS, Hydrol & Remote Sensing Lab, USDA, Mclean, VA USA. RP Kumar, SV (reprint author), NASA GSFC, Hydrol Sci Lab, Code 617, Greenbelt, MD 20771 USA. EM sujay.v.kumar@nasa.gov RI Cosh, MIchael/A-8858-2015; Kumar, Sujay/B-8142-2015; Reichle, Rolf/E-1419-2012; Livneh, Ben/I-2939-2015; Peters-Lidard, Christa/E-1429-2012; OI Cosh, MIchael/0000-0003-4776-1918; Peters-Lidard, Christa/0000-0003-1255-2876; LIVNEH, BEN/0000-0001-5445-2473 FU NASA Science Mission Directorate's Earth Science Division through the National Climate Assessment (NCA) project FX Funding for this work was provided by the NASA Science Mission Directorate's Earth Science Division through the National Climate Assessment (NCA) project. Computing was supported by the resources at the NASA Center for Climate Simulation. The NLDAS-2 forcing data used in this effort were acquired as part of the activities of NASA's Science Mission Directorate and are archived and distributed by the Goddard Earth Sciences (GES) Data and Information Services Center (DISC). Part of the funding for this effort was provided by NOAA's Climate Program Office MAPP program. Rolf Reichle was supported by the NASA program on the Science of Terra and Aqua. We are grateful to Dr. Gabrielle De Lannoy for the assistance with the reprocessed and quality-controlled SCAN soil moisture dataset and to Drs. Dorothy Hall and James Foster for their help with the development of snow depth retrieval products. NR 113 TC 22 Z9 23 U1 4 U2 36 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD DEC PY 2014 VL 15 IS 6 BP 2446 EP 2469 DI 10.1175/JHM-D-13-0132.1 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AU9FZ UT WOS:000345898400020 ER PT J AU Getirana, ACV Dutra, E Guimberteau, M Kam, JH Li, HY Decharme, B Zhang, ZQ Ducharne, A Boone, A Balsamo, G Rodell, M Toure, AM Xue, YK Peters-Lidard, CD Kumar, SV Arsenault, K Drapeau, G Leung, LR Ronchail, J Sheffield, J AF Getirana, Augusto C. V. Dutra, Emanuel Guimberteau, Matthieu Kam, Jonghun Li, Hong-Yi Decharme, Bertrand Zhang, Zhengqiu Ducharne, Agnes Boone, Aaron Balsamo, Gianpaolo Rodell, Matthew Toure, Ally M. Xue, Yongkang Peters-Lidard, Christa D. Kumar, Sujay V. Arsenault, Kristi Drapeau, Guillaume Leung, L. Ruby Ronchail, Josyane Sheffield, Justin TI Water Balance in the Amazon Basin from a Land Surface Model Ensemble SO JOURNAL OF HYDROMETEOROLOGY LA English DT Article DE Amazon region; Runoff; Hydrologic models; Land surface model ID RUNOFF ROUTING MODEL; RIVER-BASIN; PARAMETERIZATION SCHEME; HYDRAULIC CONDUCTIVITY; HYDROLOGICAL CYCLE; BIOSPHERE MODEL; SOIL HYDROLOGY; ECMWF MODEL; RAIN-FOREST; CLIMATE AB Despite recent advances in land surface modeling and remote sensing, estimates of the global water budget are still fairly uncertain. This study aims to evaluate the water budget of the Amazon basin based on several state-of-the-art land surface model (LSM) outputs. Water budget variables (terrestrial water storage TWS, evapotranspiration ET, surface runoff R, and base flow B) are evaluated at the basin scale using both remote sensing and in situ data. Meteorological forcings at a 3-hourly time step and 1 degrees spatial resolution were used to run 14 LSMs. Precipitation datasets that have been rescaled to match monthly Global Precipitation Climatology Project (GPCP) and Global Precipitation Climatology Centre (GPCC) datasets and the daily Hydrologie du Bassin de l'Amazone (HYBAM) dataset were used to perform three experiments. The Hydrological Modeling and Analysis Platform (HyMAP) river routing scheme was forced with R and B and simulated discharges are compared against observations at 165 gauges. Simulated ET and TWS are compared against FLUXNET and MOD16A2 evapotranspiration datasets and Gravity Recovery and Climate Experiment (GRACE) TWS estimates in two subcatchments of main tributaries (Madeira and Negro Rivers). At the basin scale, simulated ET ranges from 2.39 to 3.26 mm day(-1) and a low spatial correlation between ET and precipitation indicates that evapotranspiration does not depend on water availability over most of the basin. Results also show that other simulated water budget components vary significantly as a function of both the LSM and precipitation dataset, but simulated TWS generally agrees with GRACE estimates at the basin scale. The best water budget simulations resulted from experiments using HYBAM, mostly explained by a denser rainfall gauge network and the rescaling at a finer temporal scale. C1 [Getirana, Augusto C. V.; Rodell, Matthew; Toure, Ally M.; Peters-Lidard, Christa D.; Kumar, Sujay V.; Arsenault, Kristi] NASA Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20009 USA. [Dutra, Emanuel; Balsamo, Gianpaolo] ECMWF, Reading, Berks, England. [Guimberteau, Matthieu; Ducharne, Agnes] Inst Pierre Simon Laplace CNRS, Paris, France. [Kam, Jonghun; Sheffield, Justin] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. [Li, Hong-Yi; Leung, L. Ruby] Pacific NW Natl Lab, Richland, WA 99352 USA. [Decharme, Bertrand; Boone, Aaron] Meteo France, CNRM GAME, Toulouse, France. [Zhang, Zhengqiu; Xue, Yongkang] Univ Calif Los Angeles, Los Angeles, CA USA. [Zhang, Zhengqiu] Chinese Acad Meteorol Sci, Beijing, Peoples R China. [Ducharne, Agnes] CNRS Univ Pierre & Marie Curie, UMR METIS, Paris, France. [Drapeau, Guillaume] Univ Paris Diderot, PRODIG, Paris, France. [Ronchail, Josyane] Univ Paris Diderot, Univ Sorbonne Paris Cite, Paris, France. [Ronchail, Josyane] Univ Paris 06, Sorbonne, CNRS IRD MNHN, LOCEAN, Paris, France. RP Getirana, ACV (reprint author), NASA Goddard Space Flight Ctr, Hydrol Sci Lab, 8800 Greenbelt Rd, Greenbelt, MD 20009 USA. EM augusto.getirana@nasa.gov RI Kam, Jonghun/G-3550-2012; Balsamo, Gianpaolo/I-3362-2013; Kumar, Sujay/B-8142-2015; Li, Hong-Yi/C-9143-2014; Peters-Lidard, Christa/E-1429-2012; Dutra, Emanuel/A-3774-2010; Rodell, Matthew/E-4946-2012; Getirana, Augusto/G-4630-2011 OI Kam, Jonghun/0000-0002-7967-7705; Balsamo, Gianpaolo/0000-0002-1745-3634; Li, Hong-Yi/0000-0001-5690-3610; Peters-Lidard, Christa/0000-0003-1255-2876; Dutra, Emanuel/0000-0002-0643-2643; Guimberteau, Matthieu/0000-0001-8582-6087; Rodell, Matthew/0000-0003-0106-7437; FU DOE by Battelle Memorial Institute [DE-AC05-76RLO1830] FX A. Getirana was funded by the NASA Postdoctoral Program (NPP) managed by Oak Ridge Associated Universities (ORAU). E. Dutra was financially supported by the FP7 EU project EartH2Observe, and M. Guimberteau was supported by the EU-FP7 AMAZALERT project. H.-Y. Li acknowledges the support by the Office of Science of the U.S. Department of Energy as part of the Regional and Global Climate Modeling program. The Pacific Northwest National Laboratory is operated for the DOE by Battelle Memorial Institute under Contract DE-AC05-76RLO1830. The study benefited from data made available by Agencia Nacional de Aguas (ANA). We thank M. Jung for providing the gridded FLUXNET dataset. NR 103 TC 11 Z9 11 U1 5 U2 37 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1525-755X EI 1525-7541 J9 J HYDROMETEOROL JI J. Hydrometeorol. PD DEC PY 2014 VL 15 IS 6 BP 2586 EP 2614 DI 10.1175/JHM-D-14-0068.1 PG 29 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AU9FZ UT WOS:000345898400027 ER PT J AU Matheou, G Chung, D AF Matheou, Georgios Chung, Daniel TI Large-Eddy Simulation of Stratified Turbulence. Part II: Application of the Stretched-Vortex Model to the Atmospheric Boundary Layer SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID SHALLOW CUMULUS CONVECTION; NOCTURNAL MARINE STRATOCUMULUS; DIRECT NUMERICAL-SIMULATION; SUBGRID-STRESS MODEL; TOPPED MIXED LAYERS; NONPRECIPITATING STRATOCUMULUS; CLOUDS; PARAMETERIZATION; ENTRAINMENT; RESOLUTION AB The buoyancy-adjusted stretched-vortex subgrid-scale (SGS) model is assessed for a number of large-eddy simulations (LESs) corresponding to diverse atmospheric boundary layer conditions. The cases considered are free convection, a moderately stable boundary layer [first Global Energy and Water Exchanges (GEWEX) Atmospheric Boundary Layer Study (GABLS)] case, shallow cumulus [Barbados Oceanographic and Meteorological Experiment (BOMEX)], shallow precipitating cumulus [Rain in Cumulus over the Ocean (RICO)] and nocturnal stratocumulus [Second Dynamics and Chemistry of the Marine Stratocumulus (DYCOMS-II) field study RF01]. An identical LES setup, including advection discretization and SGS model parameters, is used for all cases, which is a stringent test on the ability of LES to accurately capture diverse conditions without any flow-adjustable parameters. The LES predictions agree well with observations and previously reported model results. A grid-resolution convergence study is carried out, and for all cases the mean profiles exhibit good grid-resolution independence, even for resolutions that are typically considered coarse. Second-order statistics, for example, variances, converge at finer resolutions compared to domain means. The simulations show that 90% of the turbulent kinetic energy (at each level) must be resolved to obtain sufficiently converged mean profiles. This empirical convergence criterion can be used as a guide in designing future LES runs. C1 [Matheou, Georgios] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chung, Daniel] Univ Melbourne, Dept Mech Engn, Melbourne, Vic, Australia. RP Matheou, G (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM georgios.matheou@jpl.nasa.gov RI Chung, Daniel/F-4468-2016 OI Chung, Daniel/0000-0003-3732-364X FU Office of Naval Research, Marine Meteorology Program [N0001411IP20087, N0001411IP20069]; NASA MAP Program; NOAA/CPO MAPP Program; National Aeronautics and Space Administration FX We would like to acknowledge discussions with J. Teixeira (JPL) and P. Dimotakis (Caltech). We thank B. Stevens (Max Planck Institute for Meteorology) for making the UCLALES code available and for his assistance. We acknowledge M. Inoue (JPL) for contributions to the present LES code. The 3D radiative transfer calculations were performed by A. Davis and Z. Qu (JPL). Computational resources supporting this work were provided by the JPL Office of the Chief Information Officer and the NASA High-End Computing (HEC) Program through the NASA Advanced Super-computing (NAS) Division at Ames Research Center. We acknowledge the support provided by the Office of Naval Research, Marine Meteorology Program under Awards N0001411IP20087 and N0001411IP20069, the NASA MAP Program, and the NOAA/CPO MAPP Program. This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 83 TC 8 Z9 8 U1 0 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 DEC PY 2014 VL 71 IS 12 BP 45 EP 66 DI 10.1175/JAS-D-13-0306.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AU9BF UT WOS:000345886100004 ER PT J AU Newman, PA Nash, ER Roscoe, H AF Newman, Paul A. Nash, Eric R. Roscoe, Howard TI Reply to "Comments on 'The Unusual Southern Hemisphere Winter of 2002" SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Letter ID NCAR REANALYSIS DATA; VORTEX SPLIT; TEMPERATURE; ANTARCTICA; TRENDS C1 [Newman, Paul A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nash, Eric R.] Sci Syst & Applicat Inc, Lanham, MD USA. [Roscoe, Howard] British Antarctic Survey, Cambridge CB3 0ET, England. RP Newman, PA (reprint author), NASA, Goddard Space Flight Ctr, Code 610, Greenbelt, MD 20771 USA. EM paul.a.newman@nasa.gov NR 15 TC 0 Z9 0 U1 2 U2 3 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 DEC PY 2014 VL 71 IS 12 BP 312 EP 315 DI 10.1175/JAS-D-14-0227.1 PG 4 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AU9BF UT WOS:000345886100020 ER PT J AU Balla, RJ AF Balla, R. Jeffrey TI Iodine Cordes Bands Thermometry in a Mach 10 Wake SO AIAA JOURNAL LA English DT Article ID DENSITY-MEASUREMENTS; AIR C1 NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23681 USA. RP Balla, RJ (reprint author), NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, MS 493, Hampton, VA 23681 USA. EM robert.j.balla@nasa.gov NR 7 TC 0 Z9 0 U1 1 U2 1 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD DEC PY 2014 VL 52 IS 12 BP 2901 EP 2903 DI 10.2514/1.J053305 PG 3 WC Engineering, Aerospace SC Engineering GA AU8NG UT WOS:000345852500023 ER PT J AU Summons, RE Sessions, AL Allwood, AC Barton, HA Beaty, DW Blakkolb, B Canham, J Clark, BC Dworkin, JP Lin, Y Mathies, R Milkovich, SM Steele, A AF Summons, R. E. Sessions, A. L. Allwood, A. C. Barton, H. A. Beaty, D. W. Blakkolb, B. Canham, J. Clark, B. C. Dworkin, J. P. Lin, Y. Mathies, R. Milkovich, S. M. Steele, A. CA 2014 Organic Contamination Panel TI Planning Considerations Related to the Organic Contamination of Martian Samples and Implications for the Mars 2020 Rover SO ASTROBIOLOGY LA English DT News Item ID POLYCYCLIC AROMATIC-HYDROCARBONS; SCIENCE ANALYSIS GROUP; AMINO-ACIDS; WESTERN-AUSTRALIA; ADVENTITIOUS CARBON; MASS-SPECTROMETRY; PILBARA CRATON; TERRESTRIAL CONTAMINATION; ISOTOPIC COMPOSITIONS; METEORITE AB Table of Contents 1. Executive Summary 2. Introduction 2.1. Introduction to the Mars 2020 OCP 2.1.1. Mars and the potential for habitability 2.1.2. Charge to the OCP 2.1.3. Introduction to the proposed Mars 2020 Mission 2.1.4. Definition of "organic contamination" 2.1.5. A note about units 2.2. Previous work on organic contamination control of acquired samples 2.3. Key concepts 2.3.1. Terrestrial microbial life forms (alive or dead) as sources of organic molecular contaminants 2.3.2. Analytical method limits of detection and contamination limits 2.3.3. Not all contaminants are equal 2.3.4. Contamination control versus contamination knowledge 2.4. Science and PP objectives both drive need for organic analyses 3. Sample-Based Investigations and Measurements 3.1. Need for early survey measurements 3.2. Potential analytical methods for returned samples 3.3. Survey versus targeted analytical methods 3.4. Survey analytical methods 4. Sample-Based Contaminants of Concern 4.1. General considerations 4.1.1. Selection criteria for choosing contaminants of concern 4.1.2. S/N threshold for acceptable contamination 4.1.3. Limits for TOC, individual molecules, or particles 4.1.4. Alive versus dead microbial contamination 4.1.5. The possibility of reproduction of Earth-sourced microbial contaminants in sealed sample tubes 4.2. Considerations related to specific contaminants 4.2.1. Which contaminants? 4.2.1.1. Tier-I contaminants 4.2.2. Allowable levels of contamination 4.2.2.1. What analyte concentrations do we expect? 4.2.2.2. What concentrations can we measure? 4.2.2.3. What level of cleanliness can we achieve? 4.2.3. Conclusions for specific compound levels 4.3. Considerations related to TOC 4.3.1. Allowable levels of contamination 4.3.1.1. What analyte concentrations do we expect? 4.3.1.2. What concentrations can we measure? 4.3.1.3. What level of cleanliness can we achieve? 4.3.1.3.1. Contamination pathways 4.3.1.4. Contamination transfer from sample-contacting surfaces 4.3.2. Conclusions for TOC levels 4.4. Considerations related to particulate organic matter 4.4.1. Introduction 4.4.2. Analytical approaches to measuring particulates on Earth 4.4.3. Limits on organic particulates 4.4.4. Conclusions and recommendations for particulates 4.5. Implementation 4.5.1. Strategy for implementing contaminant requirements 5. Strategies for Recognizing and Characterizing Organic Contamination 5.1. Introduction 5.2. Witness plates 5.3. Blanks and blank standards 5.4. Archive of organic and trace biological materials 5.5. Spatially resolved measurements on returned samples 6. Discussion and Proposals for Future Work 6.1. The case for cleaner 6.2. Summary and conclusions 6.3. Topics for future work Acknowledgments References A. Appendices and Supporting Files A.3. Appendix 3: Definitions of terms A.4. Appendix 4: Summary of instruments and measurements available as of 2014 for investigating organic molecules in rock and soil samples A.4.1. Notes regarding detection limits and capability of surface spectroscopic techniques C1 [Summons, R. E.] MIT, Cambridge, MA 02139 USA. [Sessions, A. L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91109 USA. [Allwood, A. C.] CALTECH, Pasadena, CA 91109 USA. [Beaty, D. W.] CALTECH, Mars Explorat Directorate, Pasadena, CA 91109 USA. [Blakkolb, B.; Lin, Y.; Milkovich, S. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Barton, H. A.] Univ Akron, Dept Biol, Akron, OH 44325 USA. [Canham, J.] ATK, Washington, DC USA. [Clark, B. C.] Space Sci Inst, Boulder, CO USA. [Dworkin, J. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mathies, R.] Univ Calif Berkeley, Dept Chem, Berkeley, CA 94720 USA. [Steele, A.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. RP Beaty, DW (reprint author), CALTECH, Jet Prop Lab, Mars Explorat Directorate, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM rsummons@mit.edu; als@gps.caltech.edu; David.W.Beaty@jpl.nasa.gov RI Dworkin, Jason/C-9417-2012; Sessions, Alex/C-2752-2008 OI Dworkin, Jason/0000-0002-3961-8997; Sessions, Alex/0000-0001-6120-2763 NR 156 TC 3 Z9 3 U1 5 U2 27 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD DEC 1 PY 2014 VL 14 IS 12 BP 969 EP 1027 DI 10.1089/ast.2014.1244 PG 59 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AW5SW UT WOS:000346335100001 PM 25495496 ER PT J AU Johnson, MS Yates, EL Iraci, LT Loewenstein, M Tadic, JM Wecht, KJ Jeong, S Fischer, ML AF Johnson, Matthew S. Yates, Emma L. Iraci, Laura T. Loewenstein, Max Tadic, Jovan M. Wecht, Kevin J. Jeong, Seongeun Fischer, Marc L. TI Analyzing source apportioned methane in northern California during Discover-AQ-CA using airborne measurements and model simulations SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Methane; Source apportionment; Emission inventory; Livestock emissions ID ATMOSPHERIC METHANE; ANTHROPOGENIC EMISSIONS; AIRCRAFT AB This study analyzes source apportioned methane (CH4) emissions and atmospheric mixing ratios in northern California during the Discover-AQ-CA field campaign using airborne measurement data and model simulations. Source apportioned CH4 emissions from the Emissions Database for Global Atmospheric Research (EDGAR) version 4.2 were applied in the 3-D chemical transport model GEOS-Chem and analyzed using airborne measurements taken as part of the Alpha Jet Atmospheric eXperiment over the San Francisco Bay Area (SFBA) and northern San Joaquin Valley (SJV). During the time period of the Discover-AQ-CA field campaign EDGAR inventory CH4 emissions were similar to 5.30 Gg day(-1) (Gg = 1.0 x 10(9) g) (equating to similar to 1.90 x 10(3) Gg yr(-1)) for all of California. According to EDGAR, the SFBA and northern SJV region contributes similar to 30% of total CH4 emissions from California. Source apportionment analysis during this study shows that CH4 mixing ratios over this area of northern California are largely influenced by global emissions from wetlands and local/global emissions from gas and oil production and distribution, waste treatment processes, and livestock management. Model simulations, using EDGAR emissions, suggest that the model under-estimates CH4 mixing ratios in northern California (average normalized mean bias (NMB) = -5.2% and linear regression slope = 0.20). The largest negative biases in the model were calculated on days when large amounts of CH4 were measured over local emission sources and atmospheric CH4 mixing ratios reached values >2.5 parts per million. Sensitivity emission studies conducted during this research suggest that local emissions of CH4 from livestock management processes are likely the primary source of the negative model bias. These results indicate that a variety, and larger quantity, of measurement data needs to be obtained and additional research is necessary to better quantify source apportioned CH4 emissions in California. Published by Elsevier Ltd. C1 [Johnson, Matthew S.; Yates, Emma L.; Iraci, Laura T.; Loewenstein, Max; Tadic, Jovan M.] NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA. [Wecht, Kevin J.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Jeong, Seongeun; Fischer, Marc L.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Dept Global Ecol, Berkeley, CA 94720 USA. [Tadic, Jovan M.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA USA. RP Johnson, MS (reprint author), NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA. EM matthew.s.johnson@nasa.gov RI Tadic, Jovan/P-3677-2016; OI Tadic, Jovan/0000-0003-4655-5063 FU NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at NASA Ames Research Center; University of California; California Energy Commission; California Air Resources Board [DE-AC02-05CH11231]; NASA's Earth Science Division at Ames Research Center; H211 L. L. C. FX The authors gratefully recognize the support and partnership of H211 L. L. C., with particular thanks to K. Ambrose, R. Simone, B. Quiambao, J. Lee, and R. Fisher. Technical contributions from W. Gore, A. Trias, M. Roby, E. Quigley, R. Walker, R. Belme, L Sharma, and B. Pierce made this project possible. Matthew Johnson would also like to thank D. Jacob and the Harvard University Atmospheric Chemistry Modeling Group for providing the base model GEOS-Chem used during our research. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at NASA Ames Research Center. Further thanks are due to D. Kokron for assisting in the installation of GEOS-Chem on NAS. Effort by LBNL was supported by the University of California, the California Energy Commission, and the California Air Resources Board under contract number DE-AC02-05CH11231. All the authors express gratitude to the support from NASA's Earth Science Division at Ames Research Center. Finally, the views, opinions, and findings contained in this report are those of the authors and should not be construed as an official NASA or United States Government position, policy, or decision. NR 30 TC 3 Z9 3 U1 1 U2 14 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD DEC PY 2014 VL 99 BP 248 EP 256 DI 10.1016/j.atmosenv.2014.09.068 PG 9 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AU7TS UT WOS:000345804400027 ER PT J AU Jing, P Lu, ZF Xing, J Streets, DG Tan, Q O'Brien, T Kamberos, J AF Jing, Ping Lu, Zifeng Xing, Jia Streets, David G. Tan, Qian O'Brien, Timothy Kamberos, Joseph TI Response of the summertime ground-level ozone trend in the Chicago area to emission controls and temperature changes, 2005-2013 SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Ozone trend; Temperature dependence of ozone; NOx and VOC emission control; Chicago ID UNITED-STATES; MONITORING INSTRUMENT; NOX EMISSIONS; URBAN AREAS; POWER-PLANTS; MEXICO-CITY; METEOROLOGY; RETRIEVALS; STRATEGIES; INDUSTRIAL AB Despite strenuous efforts to reduce the emissions of ozone precursors such as nitrogen oxides (NOx), concentrations of ground-level ozone (O-3) still often exceed the National Ambient Air Quality Standard in U.S. cities in summertime, including Chicago. Furthermore, studies have projected a future increase in O-3 formation due to global climate change. This study examines the response of summertime O-3 to emission controls and temperature change in the Chicago area from 2005 to 2013 by employing observations of O-3, O-3 precursors, and meteorological variables. We find that meteorology explains about 53% of the O-3 variance in Chicago. O-3 mixing ratios over Chicago are found to show no clear decline over the 2005-2013 period. The summertime ground-level O-3 trend consists of a decrease of 0.08 ppb/year between 2005 and 2009 and an increase of 1.49 ppb/year between 2009 and 2013. Emissions of NOx and concentrations of NO2 have been decreasing steadily from 2005 to 2013 in the Chicago area. Concentrations of volatile organic compounds (VOCs) in Chicago, however, have more than doubled since 2009, even though emission inventories suggest that VOC emissions have decreased. We believe that O-3 production in Chicago became more sensitive to VOCs starting in 2008/2009 and may have switched from being NOx-limited to VOC-limited. The warmer climate since 2008 has also contributed to the increasing ozone trend in the Chicago area. Increased attention should be paid to improving the quantification of VOC sources, enhancing the monitoring of reactive VOC concentrations, and designing VOC mitigation measures. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Jing, Ping; Kamberos, Joseph] Loyola Univ, Inst Environm Sustainabil, Chicago, IL 60660 USA. [Lu, Zifeng; Streets, David G.] Argonne Natl Lab, Decis & Informat Sci Div, Argonne, IL 60439 USA. [Xing, Jia] US EPA, Res Triangle Pk, NC 27711 USA. [Tan, Qian] NASA, Goddard Earth Sci Technol & Res GESTAR Studies &, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [O'Brien, Timothy] Loyola Univ, Dept Math & Stat, Chicago, IL 60660 USA. RP Jing, P (reprint author), Loyola Univ, Inst Environm Sustainabil, Chicago, IL 60660 USA. EM pjing@luc.edu RI xing, jia/O-1784-2014 FU Loyola University Chicago Summer Research Stipends FX This work was funded by the Loyola University Chicago Summer Research Stipends. We thank Gao Chen from NASA's Langley Research Center for helpful comments. NR 37 TC 5 Z9 5 U1 7 U2 39 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD DEC PY 2014 VL 99 BP 630 EP 640 DI 10.1016/j.atmosenv.2014.10.035 PG 11 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AU7TS UT WOS:000345804400066 ER PT J AU Barr, YR AF Barr, Yael R. TI Lumbar Puncture During Spaceflight: Operational Considerations, Constraints, Concerns, and Limitations SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Review DE astronauts; microgravity; intracranial pressure ID PSEUDOTUMOR CEREBRI; SURGICAL SKILLS; MICROGRAVITY; ULTRASOUND; SPACE; RISK; COMPLICATIONS; ASTRONAUTS; PRESSURE; GRAVITY AB Lumbar puncture (LP) is a commonly performed low-risk procedure terrestrially, used diagnostically for evaluation of cerebrospinal fluid (CSF) pressure as well as for collection of CSF for analysis. NASA is investigating noninvasive means for measurement of intracranial pressure (ICP) to assess the potential contribution of elevated intracranial pressures to recently reported changes in astronauts' visual acuity and eye anatomy, known collectively as the Visual Impairment/Intracranial Pressure risk. However, many of these noninvasive technologies are still under development, have limited clinical validation, are several years away from being ready for in-flight use, or only provide qualitative rather than quantitative ICP values. Therefore, performance of in-flight LPs, as part of crewmember evaluation, has also been considered by NASA. This manuscript summarizes the unique operational considerations, constraints, concerns, and limitations of using traditional LP as an adjunct or as an alternative to noninvasive ICP measurements during spaceflight. C1 [Barr, Yael R.] Univ Texas Med Branch, Galveston, TX 77555 USA. [Barr, Yael R.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Barr, YR (reprint author), 2101 NASA Pkwy,SK 37A, Houston, TX 77058 USA. EM yael.barr-1@nasa.gov FU NASA FX The author would like to thank Ms. Rachel Brady and Drs. Sharmi Watkins, Douglas Hamilton, Eric Kerstman, William Tarver, Emanuel Tanne, Michael Barratt, Peter Norsk, and Christian Otto for their review of this manuscript. This study was sponsored by NASA. NR 42 TC 2 Z9 2 U1 1 U2 3 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 EI 1943-4448 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD DEC PY 2014 VL 85 IS 12 BP 1209 EP 1213 DI 10.3357/ASEM.3674.2014 PG 5 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA AU8BA UT WOS:000345820500007 PM 25479263 ER PT J AU Zwart, SR Launius, RD Coen, GK Morgan, JLL Charles, JB Smith, SM AF Zwart, Sara R. Launius, Ryan D. Coen, Geoffrey K. Morgan, Jennifer L. L. Charles, John B. Smith, Scott M. TI Body Mass Changes During Long-Duration Spaceflight Response SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Letter C1 [Zwart, Sara R.] Univ Space Res Assoc, Houston, TX 77058 USA. [Launius, Ryan D.] Jacobs Technol Inc, Houston, TX USA. [Coen, Geoffrey K.] Lockheed Martin, Houston, TX USA. [Morgan, Jennifer L. L.] Oak Ridge Associated Univ, NASA, Houston, TX USA. [Charles, John B.; Smith, Scott M.] NASA, Johnson Space Ctr, Houston, TX USA. RP Zwart, SR (reprint author), Univ Space Res Assoc, Houston, TX 77058 USA. NR 4 TC 0 Z9 0 U1 0 U2 1 PU AEROSPACE MEDICAL ASSOC PI ALEXANDRIA PA 320 S HENRY ST, ALEXANDRIA, VA 22314-3579 USA SN 0095-6562 EI 1943-4448 J9 AVIAT SPACE ENVIR MD JI Aviat. Space Environ. Med. PD DEC PY 2014 VL 85 IS 12 BP 1229 EP 1230 PG 2 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA AU8BA UT WOS:000345820500012 PM 25479268 ER PT J AU Breier, JA Sheik, CS Gomez-Ibanez, D Sayre-McCord, RT Sanger, R Rauch, C Coleman, M Bennett, SA Cron, BR Li, M German, CR Toner, BM Dick, GJ AF Breier, J. A. Sheik, C. S. Gomez-Ibanez, D. Sayre-McCord, R. T. Sanger, R. Rauch, C. Coleman, M. Bennett, S. A. Cron, B. R. Li, M. German, C. R. Toner, B. M. Dick, G. J. TI A large volume particulate and water multi-sampler with in situ preservation for microbial and biogeochemical studies SO DEEP-SEA RESEARCH PART I-OCEANOGRAPHIC RESEARCH PAPERS LA English DT Article DE Deep-sea; Microbiology; Geochemistry; Hydrothermal vents; Instrumentation; Remotely operated vehicle ID SEA HYDROTHERMAL PLUME; EAST PACIFIC RISE; MID-CAYMAN RISE; FLUIDS; IRON; METHANOTROPHS; ENVIRONMENTS; POPULATIONS; DIVERSITY; PROCESSOR AB A new tool was developed for large volume sampling to facilitate marine microbiology and biogeochemical studies. It was developed for remotely operated vehicle and hydrocast deployments, and allows for rapid collection of multiple sample types from the water column and dynamic, variable environments such as rising hydrothermal plumes. It was used successfully during a cruise to the hydrothermal vent systems of the Mid-Cayman Rise. The Suspended Particulate Rosette V2 large volume multi-sampling system allows for the collection of 14 sample sets per deployment. Each sample set can include filtered material, whole (unfiltered) water, and filtrate. Suspended particulate can be collected on filters up to 142 mm in diameter and pore sizes down to 0.2 mu m. Filtration is typically at flowrates of 2 L min(-1) For particulate material, filtered volume is constrained only by sampling time and filter capacity, with all sample volumes recorded by digital flowmeter. The suspended particulate filter holders can be filled with preservative and sealed immediately after sample collection. Up to 2 L of whole water, filtrate, or a combination of the two, can be collected as part of each sample set. The system is constructed of plastics with titanium fasteners and nickel alloy spring loaded seals. There are no ferrous alloys in the sampling system. Individual sample lines are prefilled with filtered, deionized water prior to deployment and remain sealed unless a sample is actively being collected. This system is intended to facilitate studies concerning the relationship between marine microbiology and ocean biogeochemistry. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Breier, J. A.; Gomez-Ibanez, D.; Sayre-McCord, R. T.; Sanger, R.; German, C. R.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. [Sheik, C. S.; Li, M.; Dick, G. J.] Univ Michigan, Ann Arbor, MI 48109 USA. [Rauch, C.] Rauch Engn, Los Osos, CA 93402 USA. [Coleman, M.; Bennett, S. A.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Cron, B. R.; Toner, B. M.] Univ Minnesota Twin Cities, St Paul, MN 55108 USA. RP Breier, JA (reprint author), Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. EM jbreier@whoi.edu RI Toner, Brandy/N-7911-2016; OI Toner, Brandy/0000-0002-3681-3455; Sheik, Cody/0000-0003-0413-1924 FU Gordon and Betty Moore Foundation [GBMF2764, GBMF2609]; ROV Jason operations team; R/V Atlantis crew [AT18-16]; OASES science; National Science Foundation (NSF) [OCE-1061863]; National Aeronautics and Space Administration's (NASA) Astrobiology Science and Technology for Exploring Planets (ASTEP) program [NNX09AB75G]; NSF [OCE-1061881]; ASTEP grant [NNX09AB75G]; NSF grants [OCE-1061881]; Jet Propulsion Laboratory (jPL), California Institute of Technology; National Aeronautics and Space Administration (NASA); Director, Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy [DE-AC02-05CH11231] FX The SUPR-V2 was funded by the Gordon and Betty Moore Foundation through Grant GBMF2764 to J.B. This work was funded in part by the Gordon and Betty Moore Foundation Grant GBMF2609 to G.D. For field testing we would like to thank the ROV Jason operations team, the R/V Atlantis crew (AT18-16), and the OASES 2012 science party for assistance and support with all aspects of the cruise, which was supported jointly by grants to CRG from the National Science Foundation (NSF; OCE-1061863) and National Aeronautics and Space Administration's (NASA) Astrobiology Science and Technology for Exploring Planets (ASTEP) program (NNX09AB75G) and to M.C. from the NSF (OCE-1061881). The post-cruise contributions of S.A.B. and M.C. were supported through the same ASTEP grant (NNX09AB75G) and one of the NSF grants (OCE-1061881) and were carried out at the Jet Propulsion Laboratory (jPL), California Institute of Technology, under contract with the National Aeronautics and Space Administration (NASA). A portion of this research was conducted at beamline 5.3.2.2 of the Advanced Light Source (ALS) and we thank Kilcoyne for research support. The A.LS. is supported by the Director, Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy under Contract no. DE-AC02-05CH11231. We would like to thank the Microbial Systems Laboratory of the Host Microbiome Initiative of the University of Michigan for sequencing support. NR 48 TC 10 Z9 10 U1 4 U2 25 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0637 EI 1879-0119 J9 DEEP-SEA RES PT I JI Deep-Sea Res. Part I-Oceanogr. Res. Pap. PD DEC PY 2014 VL 94 BP 195 EP 206 DI 10.1016/j.dsr.2014.08.008 PG 12 WC Oceanography SC Oceanography GA AU8AW UT WOS:000345820100015 ER PT J AU Denney, E Pai, G AF Denney, Ewen Pai, Ganesh TI Automating the Assembly of Aviation Safety Cases SO IEEE TRANSACTIONS ON RELIABILITY LA English DT Article DE Safety cases; system safety; software safety; safety assurance; unmanned aircraft systems; formal methods ID SOFTWARE AB Safety cases are among the state of the art in safety management mechanisms, providing an explicit way to reason about system and software safety. The intent is to provide convincing, valid, comprehensive assurance that a system is acceptably safe for a given application in a defined operating environment, by creating an argument structure that links claims about safety to a body of evidence. However, their construction is a largely manual, and therefore a time consuming, error prone, and expensive process. We present a methodology for automatically assembling safety cases which are auto-generated from the application of a formal method to software, with manually created safety cases derived from system safety analysis. Our approach emphasizes the heterogeneity of safety-relevant information, and we show how diverse content can be integrated into a single argument structure. To illustrate our methodology, we have applied it to the Swift Unmanned Aircraft System (UAS) being developed at the NASA Ames Research Center. We present an end-to-end fragment of the resulting interim safety case comprising an aircraft-level argument manually constructed from the safety analysis of the Swift UAS, which is automatically assembled with an auto-generated lower-level argument produced from a formal proof of correctness of the safety-relevant properties of the software autopilot. C1 [Denney, Ewen; Pai, Ganesh] SGT Inc, NASA Ames Res Ctr, Moffett Field, CA 94035 USA. RP Denney, E (reprint author), SGT Inc, NASA Ames Res Ctr, Moffett Field, CA 94035 USA. EM ewen.denney@nasa.gov; ganesh.pai@nasa.gov RI Pai, Ganesh/G-4516-2013 OI Pai, Ganesh/0000-0002-9848-3754 FU Assurance of Flight Critical Systems (AFCS); NASA Aeronautics Research Mission Directorate (ARMD); NASA [NNA10DE83C] FX This work was supported in part by the Assurance of Flight Critical Systems (AFCS) element of the System-wide Safety Assurance Technologies (SSAT) project in the Aviation Safety Program of the NASA Aeronautics Research Mission Directorate (ARMD), and in part by NASA contract NNA10DE83C. Associate Editor: S. Shieh. NR 39 TC 1 Z9 1 U1 0 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9529 EI 1558-1721 J9 IEEE T RELIAB JI IEEE Trans. Reliab. PD DEC PY 2014 VL 63 IS 4 BP 830 EP 849 DI 10.1109/TR.2014.2335995 PG 20 WC Computer Science, Hardware & Architecture; Computer Science, Software Engineering; Engineering, Electrical & Electronic SC Computer Science; Engineering GA AU9IA UT WOS:000345904000002 ER PT J AU Emel'yanenko, VV Naroenkov, SA Jenniskens, P Popova, OP AF Emel'yanenko, Vacheslav V. Naroenkov, Sergey A. Jenniskens, Peter Popova, Olga P. TI The orbit and dynamical evolution of the Chelyabinsk object SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID ASTEROIDS; DESTRUCTION; CHONDRITE; METEORITE; AIRBURST; SUN AB The orbit of the Chelyabinsk object is calculated, applying the least-squares method directly to astrometric positions. The dynamical evolution of this object in the past is studied by integrating equations of motion for particles with orbits from the confidence region. It is found that the majority of the Chelyabinsk clones reach the near-Sun state. Sixty-seven percent of these objects have collisions with the Sun for 15 Myr in our numerical simulations. The distribution of minimum solar distances shows that the most probable time for the encounters of the Chelyabinsk object with the Sun lies in the interval from -0.8 Myr to -2 Myr. This is consistent with the estimate of a cosmic ray exposure age of 1.2 Myr (Popova et al. 2013). A parent body of the Chelyabinsk object should experience strong tidal and thermal effects at this time. The possible association of the Chelyabinsk object with 86039 (1999 NC43) and 2008 DJ is discussed. C1 [Emel'yanenko, Vacheslav V.; Naroenkov, Sergey A.] Russian Acad Sci, Inst Astron, Moscow 119017, Russia. [Jenniskens, Peter] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Jenniskens, Peter] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Popova, Olga P.] Russian Acad Sci, Inst Dynam Geospheres, Moscow 119334, Russia. RP Emel'yanenko, VV (reprint author), Russian Acad Sci, Inst Astron, 48 Pyatnitskaya, Moscow 119017, Russia. EM vvemel@inasan.ru RI Naroenkov, Sergey/I-5699-2013; Popova, Olga/K-1885-2012 NR 18 TC 3 Z9 3 U1 0 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD DEC PY 2014 VL 49 IS 12 BP 2169 EP 2174 DI 10.1111/maps.12382 PG 6 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AU7EE UT WOS:000345762800004 ER PT J AU Sippel, JA Zhang, FQ Weng, YH Tian, L Heymsfield, GM Braun, SA AF Sippel, Jason A. Zhang, Fuqing Weng, Yonghui Tian, Lin Heymsfield, Gerald M. Braun, Scott A. TI Ensemble Kalman Filter Assimilation of HIWRAP Observations of Hurricane Karl (2010) from the Unmanned Global Hawk Aircraft SO MONTHLY WEATHER REVIEW LA English DT Article ID SCALE DATA ASSIMILATION; AIRBORNE DOPPLER RADAR; MODEL; PARAMETERIZATION; CONVECTION; MESOSCALE AB This study utilizes an ensemble Kalman filter (EnKF) to assess the impact of assimilating observations of Hurricane Karl from the High-Altitude Imaging Wind and Rain Airborne Profiler (HIWRAP). HIWRAP is a new Doppler radar on board the NASA Global Hawk unmanned airborne system, which has the benefit of a 24-26-h flight duration, or about 2-3 times that of a conventional aircraft. The first HIWRAP observations were taken during NASA's Genesis and Rapid Intensification Processes (GRIP) experiment in 2010. Observations considered here are Doppler velocity (Vr) and Doppler-derived velocity-azimuth display (VAD) wind profiles (VWPs). Karl is the only hurricane to date for which HIWRAP data are available. Assimilation of either Vr or VWPs has a significant positive impact on the EnKF analyses and forecasts of Hurricane Karl. Analyses are able to accurately estimate Karl's observed location, maximum intensity, size, precipitation distribution, and vertical structure. In addition, forecasts initialized from the EnKF analyses are much more accurate than a forecast without assimilation. The forecasts initialized from VWP-assimilating analyses perform slightly better than those initialized from Vr-assimilating analyses, and the latter are less accurate than EnKF-initialized forecasts from a recent proof-of-concept study with simulated data. Likely causes for this discrepancy include the quality and coverage of the HIWRAP data collected from Karl and the presence of model error in this real-data situation. The advantages of assimilating VWP data likely include the ability to simultaneously constrain both components of the horizontal wind and to circumvent reliance upon vertical velocity error covariance. C1 [Sippel, Jason A.; Tian, Lin; Heymsfield, Gerald M.; Braun, Scott A.] NASA, GSFC, Atmospheres Lab, Greenbelt, MD 20771 USA. [Sippel, Jason A.; Tian, Lin] Morgan State Univ, Baltimore, MD 21239 USA. [Zhang, Fuqing; Weng, Yonghui] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA. RP Sippel, JA (reprint author), NASA, GSFC, Code 612, Greenbelt, MD 20771 USA. EM jason.sippel@nasa.gov RI Zhang, Fuqing/E-6522-2010 OI Zhang, Fuqing/0000-0003-4860-9985 FU NASA Hurricane Sciences Research Program; NASA's Earth Venture Program; NASA New Investigator Program FX The authors are thankful for discussions with Frank Marks, Stephen Guimond, and Altug Aksoy. This manuscript also benefited from comments from three anonymous reviewers and the editor, Dr. Jeffrey Anderson. Funding for this work came from the NASA Hurricane Sciences Research Program under Dr. Ramesh Kakar, the Hurricane and Severe Storm Sentinel Investigation under NASA's Earth Venture Program, and the NASA New Investigator Program. The simulations were conducted on NASA Center for Climate Simulation facilities. NR 25 TC 4 Z9 4 U1 6 U2 9 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 EI 1520-0493 J9 MON WEATHER REV JI Mon. Weather Rev. PD DEC PY 2014 VL 142 IS 12 BP 4559 EP 4580 DI 10.1175/MWR-D-14-00042.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AU8QE UT WOS:000345860400012 ER PT J AU Schindelegger, M Ray, RD AF Schindelegger, Michael Ray, Richard D. TI Surface Pressure Tide Climatologies Deduced from a Quality-Controlled Network of Barometric Observations SO MONTHLY WEATHER REVIEW LA English DT Article ID CONTINENTAL UNITED-STATES; LATENT-HEAT RELEASE; DIURNAL CYCLE; ATMOSPHERIC-PRESSURE; SEMIDIURNAL TIDES; MODEL; OSCILLATIONS; INTERPOLATION; SIMULATION; SYSTEM AB Global "ground truth'' knowledge of solar diurnal S-1 and semidiurnal S-2 surface pressure tides as furnished by barometric in situ observations represents a valuable standard for wide-ranging geophysical and meteorological applications. This study attempts to aid validations of the air pressure tide signature in current climate or atmospheric analysis models by developing a new global assembly of nearly 6900 mean annual S-1 and S-2 estimates on the basis of station and marine barometric reports from the International Surface Pressure Databank, version 2 (ISPDv2), for a principal time span of 1990-2010. Previously published tidal compilations have been limited by inadequate spatial coverage or by internal inconsistencies and outliers from suspect tidal analyses; here, these problems are mostly overcome through 1) automated data filtering under ISPDv2's quality-control framework and 2) a meticulously conducted visual inspection of station harmonic decompositions. The quality of the resulting compilation is sufficient to support global interpolation onto a reasonably fine mesh of 18 horizontal spacing. A multiquadric interpolation algorithm, with parameters fine-tuned by frequency and for land or ocean regions, is employed. Global charts of the gridded surface pressure climatologies are presented, and these are mapped to a wavenumber versus latitude spectrum for comparison with long-term means of S-1 and S-2 from four present-day atmospheric analysis systems. This cross verification, shown to be feasible even for the minor stationary modes of the tides, reveals a small but probably significant overestimation of up to 18% for peak semidiurnal amplitudes as predicted by global analysis models. C1 [Schindelegger, Michael] Vienna Univ Technol, Dept Geodesy & Geoinformat, A-1040 Vienna, Austria. [Ray, Richard D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Schindelegger, M (reprint author), Vienna Univ Technol, Dept Geodesy & Geoinformat, Gusshausstr 27-29, A-1040 Vienna, Austria. EM michael.schindelegger@tuwien.ac.at RI Schindelegger, Michael/C-7166-2016; Ray, Richard/D-1034-2012 OI Schindelegger, Michael/0000-0001-6250-7921; FU Austrian Science Fund (FWF) [I1479-N29]; U.S. National Aeronautics and Space Administration through GRACE project; U.S. National Aeronautics and Space Administration through Ocean Surface Topography project; U.S. Department of Energy, Office of Science Innovative and Novel Computational Impact on Theory and Experiment program; Office of Biological and Environmental Research; National Oceanic and Atmospheric Administration Climate Program Office FX We are indebted to Dr. Aiguo Dai for making his datasets freely available via his public website. Author M.S. thanks the Austrian Science Fund (FWF) for financial support within project I1479-N29. Author R.D.R. was supported by the U.S. National Aeronautics and Space Administration through the GRACE and Ocean Surface Topography projects. We greatly appreciate the meteorological data services supplied by the ECMWF and JMA, as well as NASA's GMAO, and we thank Thomas Cram of NCAR for his assistance in downloading the different ISPDv2 subsets. (Support for the ISPD is generally provided by the U.S. Department of Energy, Office of Science Innovative and Novel Computational Impact on Theory and Experiment program, and Office of Biological and Environmental Research, and by the National Oceanic and Atmospheric Administration Climate Program Office.) Comments from David Salstein and Harald Schuh are appreciated as well. NR 44 TC 4 Z9 4 U1 1 U2 12 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0027-0644 EI 1520-0493 J9 MON WEATHER REV JI Mon. Weather Rev. PD DEC PY 2014 VL 142 IS 12 BP 4872 EP 4889 DI 10.1175/MWR-D-14-00217.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AU8QE UT WOS:000345860400028 ER PT J AU Ford, M Becker, JM Merrifield, MA Song, YT AF Ford, Murray Becker, Janet M. Merrifield, Mark A. Song, Y. Tony TI Marshall Islands Fringing Reef and Atoll Lagoon Observations of the Tohoku Tsunami SO PURE AND APPLIED GEOPHYSICS LA English DT Article DE 2011 Tohoku tsunami; tide gauge records; Marshall Islands; coral reef; atoll ID INDIAN-OCEAN-TSUNAMI; 26 DECEMBER 2004; SUMATRA TSUNAMI; PACIFIC; FIELD AB The magnitude 9.0 Tohoku earthquake on 11 March 2011 generated a tsunami which caused significant impacts throughout the Pacific Ocean. A description of the tsunami within the lagoons and on the surrounding fringing reefs of two mid-ocean atoll islands is presented using bottom pressure observations from the Majuro and Kwajalein atolls in the Marshall Islands, supplemented by tide gauge data in the lagoons and by numerical model simulations in the deep ocean. Although the initial wave arrival was not captured by the pressure sensors, subsequent oscillations on the reef face resemble the deep ocean tsunami signal simulated by two numerical models, suggesting that the tsunami amplitudes over the atoll outer reefs are similar to that in deep water. In contrast, tsunami oscillations in the lagoon are more energetic and long lasting than observed on the reefs or modelled in the deep ocean. The tsunami energy in the Majuro lagoon exhibits persistent peaks in the 30 and 60 min period bands that suggest the excitation of closed and open basin normal modes, while energy in the Kwajalein lagoon spans a broader range of frequencies with weaker, multiple peaks than observed at Majuro, which may be associated with the tsunami behavior within the more irregular geometry of the Kwajalein lagoon. The propagation of the tsunami across the reef flats is shown to be tidally dependent, with amplitudes increasing/decreasing shoreward at high/low tide. The impact of the tsunami on the Marshall Islands was reduced due to the coincidence of peak wave amplitudes with low tide; however, the observed wave amplitudes, particularly in the atoll lagoon, would have led to inundation at different tidal phases. C1 [Ford, Murray] Univ Auckland, Sch Environm, Auckland 1142, New Zealand. [Becker, Janet M.] Univ Hawaii Manoa, Dept Geol & Geophys, Honolulu, HI 96822 USA. [Merrifield, Mark A.] Univ Hawaii Manoa, Dept Oceanog, Honolulu, HI 96822 USA. [Song, Y. Tony] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ford, M (reprint author), Univ Auckland, Sch Environm, Private Bag 92019, Auckland 1142, New Zealand. EM m.ford@auckland.ac.nz FU National Science Foundation [OCE-0927407] FX This study was supported by a grant from the National Science Foundation (OCE-0927407). DART buoy data were obtained from the NOAA National Data Buoy Center (http://www.ndbc.noaa.gov/dar.shtml), Kwajalein tide gauge data from the NOAA Center for Operational Oceanographic Products and Services (http://tidesandcurrents.noaa.gov), and Majuro tide gauge data from the National Tidal Centre, Australia. Comments by Alexander Rabinovich and two anonymous reviewers greatly improved the manuscript. We thank Rachel Tang for the MOST model data. Christopher Kontoes, Carly Fetherolf, and Derek Young were responsible for the Marshall Islands field observations. Hyang Yoon provided graphics and data processing support. NR 34 TC 1 Z9 1 U1 3 U2 14 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0033-4553 EI 1420-9136 J9 PURE APPL GEOPHYS JI Pure Appl. Geophys. PD DEC PY 2014 VL 171 IS 12 BP 3351 EP 3363 DI 10.1007/s00024-013-0757-8 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AU8KF UT WOS:000345844700011 ER PT J AU Wu, XL Walker, JP Das, NN Panciera, R Rudiger, C AF Wu, Xiaoling Walker, Jeffrey P. Das, Narendra N. Panciera, Rocco Ruediger, Christoph TI Evaluation of the SMAP brightness temperature downscaling algorithm using active-passive microwave observations SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Downscaling; Brightness temperature; Backscatter; Active-passive; SMAP; SMAPEx ID SOIL-MOISTURE RETRIEVAL; LAND DATA ASSIMILATION; L-BAND RADIOMETER; RADAR OBSERVATIONS; MISSION; FLUXES; SPACE AB The baseline radiometer brightness temperature (Tb) downscaling algorithm for NASA's Soil Moisture Active Passive (SMAP) mission, scheduled for launch in January 2015, is tested using an airborne simulation of the SMAP data stream. The algorithm synergistically uses 3 km Synthetic Aperture Radar (SAR) backscatter (sigma) to downscale a 36 km radiometer Tb to 9 km. While the algorithm has already been tested using experimental datasets from field campaigns in the USA, it is imperative that it is tested for a comprehensive range of land surface conditions (i.e. in different hydro-climatic regions) before global application. Consequently, this study evaluates the algorithm using data collected from the Soil Moisture Active Passive Experiments (SMAPEx) in south-eastern Australia, that closely simulate the SMAP data stream for a single SMAP radiometer pixel over a 3-week interval, with repeat coverage every 2-3 days. The results suggest that the average root-mean-square error (RMSE) in downscaled Tb is 3.1 K and 2.6 K for h- and v-polarizations respectively, when downscaled to 9 km resolution. This increases to 8.2 K and 6.6 K when applied at 1 km resolution. Downscaling over the relatively homogeneous grassland areas resulted in 2 K lower RMSE than for the heterogeneous cropping area. Overall, the downscaling error was around 2.4 K when applied at 9 km resolution for five of the nine days, which meets the 2.4 K error target of the SMAP mission. (C) 2014 Elsevier Inc. All rights reserved. C1 [Wu, Xiaoling; Walker, Jeffrey P.; Ruediger, Christoph] Monash Univ, Dept Civil Engn, Clayton, Vic 3800, Australia. [Das, Narendra N.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. [Panciera, Rocco] Univ Melbourne, Cooperat Res Ctr Spatial Informat, Melbourne, Vic 3053, Australia. RP Wu, XL (reprint author), Monash Univ, Dept Civil Engn, Room 156-Bldg 60,Clayton Campus, Clayton, Vic 3800, Australia. EM xiaoling.wu@monash.edu OI Rudiger, Christoph/0000-0003-4375-4446 FU Australian Research Council [DP0984586, LE0453434, LE0882509]; Monash University FX The SMAPEx field campaigns and related research development have been funded by the Australian Research Council Discovery (DP0984586) and Infrastructure (LE0453434 and LE0882509) grants. The authors acknowledge the collaboration of a large number of scientists from throughout Australia and around the world, and in particular key personnel from the SMAP team which provided significant contributions to the campaign's design and execution. The authors also acknowledge the scholarships awarded by Monash University to support Xiaoling Wu's PhD research. NR 23 TC 7 Z9 7 U1 5 U2 28 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD DEC PY 2014 VL 155 SI SI BP 210 EP 221 DI 10.1016/j.rse.2014.08.021 PG 12 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AU7TQ UT WOS:000345804200018 ER PT J AU Jagt, BJV Durand, MT Margulis, SA Kim, EJ Molotch, NP AF Jagt, Benjamin J. Vander Durand, Michael T. Margulis, Steven A. Kim, Edward J. Molotch, Noah P. TI The effect of spatial variability on the sensitivity of passive microwave measurements to snow water equivalent (vol 136, pg 163, 2013) SO REMOTE SENSING OF ENVIRONMENT LA English DT Correction C1 [Jagt, Benjamin J. Vander; Durand, Michael T.] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA. [Jagt, Benjamin J. Vander; Durand, Michael T.] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA. [Margulis, Steven A.] Univ Calif Los Angeles, Dept Civil & Environm Engn, Los Angeles, CA USA. [Kim, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Molotch, Noah P.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA. RP Jagt, BJV (reprint author), Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA. EM vander-jagt.1@osu.edu NR 1 TC 0 Z9 0 U1 1 U2 5 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD DEC PY 2014 VL 155 SI SI BP 378 EP 378 DI 10.1016/j.rse.2014.09.003 PG 1 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AU7TQ UT WOS:000345804200032 ER PT J AU Currie, T Muto, T Kudo, T Honda, M Brandt, TD Grady, C Fukagawa, M Burrows, A Janson, M Kuzuhara, M McElwain, MW Follette, K Hashimoto, J Henning, T Kandori, R Kusakabe, N Kwon, J Mede, K Morino, J Nishikawa, J Pyo, TS Serabyn, G Suenaga, T Takahashi, Y Wisniewski, J Tamura, M AF Currie, Thayne Muto, Takayuki Kudo, Tomoyuki Honda, Mitsuhiko Brandt, Timothy D. Grady, Carol Fukagawa, Misato Burrows, Adam Janson, Markus Kuzuhara, Masayuki McElwain, Michael W. Follette, Katherine Hashimoto, Jun Henning, Thomas Kandori, Ryo Kusakabe, Nobuhiko Kwon, Jungmi Mede, Kyle Morino, Jun-ichi Nishikawa, Jun Pyo, Tae-Soo Serabyn, Gene Suenaga, Takuya Takahashi, Yasuhiro Wisniewski, John Tamura, Motohide TI RECOVERY OF THE CANDIDATE PROTOPLANET HD 100546 b WITH GEMINI/NICI AND DETECTION OF ADDITIONAL (PLANET-INDUCED ?) DISK STRUCTURE AT SMALL SEPARATIONS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; stars: early-type; stars: individual (HD 100546) ID ORBITING HR 8799; HERBIG AE STARS; SUN-LIKE STAR; SPACE-TELESCOPE; CIRCUMSTELLAR DISK; TRANSITIONAL DISK; BETA-PICTORIS; COMPANION; DISCOVERY; CONFIRMATION AB We report the first independent, second epoch (re-) detection of a directly imaged protoplanet candidate. Using L' high-contrast imaging of HD 100546 taken with the Near-Infrared Coronagraph and Imager on Gemini South, we recover "HD 100546 b" with a position and brightness consistent with the original Very Large Telescope/NAos-COnica detection from Quanz et al., although data obtained after 2013 will be required to decisively demonstrate common proper motion. HD 100546 b may be spatially resolved, up to approximate to 12-13 AU in diameter, and is embedded in a finger of thermal IR-bright, polarized emission extending inward to at least 0 ''.3. Standard hot-start models imply a mass of approximate to 15 M-J. However, if HD 100546 b is newly formed or made visible by a circumplanetary disk, both of which are plausible, its mass is significantly lower (e.g., 1-7 M-J). Additionally, we discover a thermal IR-bright disk feature, possibly a spiral density wave, at roughly the same angular separation as HD 100546 b but 90 degrees. away. Our interpretation of this feature as a spiral arm is not decisive, but modeling analyses using spiral density wave theory implies a wave launching point exterior to approximate to 0 ''.45 embedded within the visible disk structure: plausibly evidence for a second, hitherto unseen, wide-separation planet. With one confirmed protoplanet candidate and evidence for one to two others, HD 100546 is an important evolutionary precursor to intermediate-mass stars with multiple super-Jovian planets at moderate/wide separations like HR 8799. C1 [Currie, Thayne; Kudo, Tomoyuki; Pyo, Tae-Soo] Subaru Telescope, NAOJ, Hilo, HI 96720 USA. [Muto, Takayuki] Kogashin Univ, Div Liberal Arts, Shinjuku Ku, Tokyo 1638677, Japan. [Honda, Mitsuhiko] Kanagawa Univ, Dept Math & Phys, Hiratsuka, Kanagawa 2591293, Japan. [Brandt, Timothy D.] Inst Adv Study, Dept Astrophys, Princeton, NJ 08540 USA. [Grady, Carol] Eureka Sci, Oakland, CA 96002 USA. [Fukagawa, Misato] Osaka Univ, Grad Sch Sci, Toyonaka, Osaka 5600043, Japan. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Janson, Markus] Stockholm Univ, SE-10691 Stockholm, Sweden. [Kuzuhara, Masayuki] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan. [McElwain, Michael W.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Follette, Katherine] Univ Arizona, Steward Observ, Dept Astron, Tucson, AZ 85721 USA. [Hashimoto, Jun; Wisniewski, John] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kandori, Ryo; Kusakabe, Nobuhiko; Morino, Jun-ichi; Nishikawa, Jun; Suenaga, Takuya; Takahashi, Yasuhiro; Tamura, Motohide] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Kwon, Jungmi; Mede, Kyle; Takahashi, Yasuhiro; Tamura, Motohide] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Serabyn, Gene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Currie, T (reprint author), Subaru Telescope, NAOJ, 650 N Aohoku Pl, Hilo, HI 96720 USA. EM currie@naoj.org NR 51 TC 32 Z9 32 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD DEC 1 PY 2014 VL 796 IS 2 AR L30 DI 10.1088/2041-8205/796/2/L30 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU3HP UT WOS:000345503400009 ER PT J AU de Foy, B Wilkins, JL Lu, ZF Streets, DG Duncan, BN AF de Foy, Benjamin Wilkins, Joseph L. Lu, Zifeng Streets, David G. Duncan, Bryan N. TI Model evaluation of methods for estimating surface emissions and chemical lifetimes from satellite data SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Emission inventory; Satellite retrieval; Chemical lifetime; Air quality model; Emissions estimation ID NOX EMISSIONS; POWER-PLANTS; NITROGEN-OXIDES; SPACE; RETRIEVALS; COLUMNS AB Column densities from satellite retrievals can provide valuable information for estimating emissions and chemical lifetimes objectively across the globe. To better understand the uncertainties associated with these estimates, we test four methods using simulated column densities from a point source: a box model approach, a 2D Gaussian fit, an Inverse Radius fit and an Exponentially-Modified Gaussian fit. The model results were simulated using the WRF and CAMx models for the year 2005, for a single point source outside Atlanta in Georgia, USA with specified emissions and three chemical scenarios: no chemical reactions, 12 h chemical lifetime and 1 h chemical lifetime. No other sources were included in the simulations. We find that the box model provides reliable estimates irrespective of plume speed and plume direction, if the plume speed and the chemical lifetime are known accurately. The 2D Gaussian fit was found to be sensitive to plume speed and direction, and requires omnidirectional dispersion in order to have a decent fit. However, the 2D Gaussian fit is only an approximate fit to the data, and the discrepancies mean that the results are dependent on the geographical domain used for the optimization. An Inverse Radius fit is introduced to correct this issue, which is found to provide improved emissions and lifetime estimates. The Exponentially-Modified Gaussian fit also gave improved estimates. It is however dependent on accurate plume rotation such that reported chemical lifetimes with this method could be significantly underestimated. (C) 2014 Elsevier Ltd. All rights reserved. C1 [de Foy, Benjamin; Wilkins, Joseph L.] St Louis Univ, Dept Earth & Atmospher Sci, St Louis, MO 63103 USA. [Lu, Zifeng; Streets, David G.] Argonne Natl Lab, Decis & Informat Sci Div, Argonne, IL 60439 USA. [Duncan, Bryan N.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA. RP de Foy, B (reprint author), St Louis Univ, Dept Earth & Atmospher Sci, St Louis, MO 63103 USA. EM bdefoy@slu.edu RI de Foy, Benjamin/A-9902-2010; Duncan, Bryan/A-5962-2011 OI de Foy, Benjamin/0000-0003-4150-9922; FU NASA [NNX11AJ63G] FX This research was funded by the NASA Air Quality Applied Sciences Team (AQAST) program, NASA grant #NNX11AJ63G, including funding for the AQAST Tiger Team "Relationships and trends among satellite NO2 columns, NOx emissions, and air quality in North America." We are grateful for valuable comments and discussion from the team members and the team leader and assistant leader, Daniel J. Jacob and Tracey Holloway. We are also grateful for detailed reviewer comments that improved the quality of the paper. NR 33 TC 9 Z9 9 U1 3 U2 22 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD DEC PY 2014 VL 98 BP 66 EP 77 DI 10.1016/j.atmosenv.2014.08.051 PG 12 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AU2WI UT WOS:000345475000009 ER PT J AU Kedia, S Ramachandran, S Holben, BN Tripathi, SN AF Kedia, Sumita Ramachandran, S. Holben, B. N. Tripathi, S. N. TI Quantification of aerosol type, and sources of aerosols over the Indo-Gangetic Plain SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Aerosol optical depth; Angstrom parameters; Single scattering albedo; Indo Gangetic plain; Fine mode fraction; Absorbing aerosol type; Organic carbon ID OPTICAL-PROPERTIES; ANGSTROM EXPONENT; NORTHERN INDIA; RAMAN-LIDAR; AERONET; BASIN; KANPUR; VARIABILITY; BIOMASS; DEPTH AB Differences and similarities in aerosol characteristics, for the first time, over two environmentally distinct locations in Indo-Gangetic plain (IGP) Kanpur (KPR) (urban location) and Gandhi College (GC) (rural site) are examined. Aerosol optical depths (AODs) exhibit pronounced seasonal variability with higher values during winter and premonsoon. Aerosol fine mode fraction (FMF) and Angstrom exponent (alpha) are higher over GC than KPR indicating relatively higher fine mode aerosol concentration over GC. Higher FMF over GC is attributed to local biomass burning activities. Analysis of AOD spectra revealed that aerosol size distribution is dominated by wide range of fine mode fractions or mixture of modes during winter and postmonsoon, while during premonsoon and monsoon coarse mode aerosols are more abundant. Single scattering albedo (SSA) is lower over GC than KPR. SSA spectra reveals the abundance of fine mode (coarse mode) absorbing (scattering) aerosols during winter and postmonsoon (premonsoon and monsoon). Spectral SSA features reveal that OC contribution to enhanced absorption is negligible. Analysis shows that absorbing aerosols can be classified as Mostly Black Carbon (BC), and Mixed BC and Dust over IGP. Mixed BC and dust is always higher over KPR, while Mostly BC is higher over GC throughout the year. The amount of long range transported dust exhibits a gradient between KPR (higher) and GC (lower). Results on seasonally varying aerosol types, and absorbing aerosol types and their gradients over an aerosol hotspot are important to tune models and to reduce the uncertainty in radiative and climate impact of aerosols. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Kedia, Sumita] Ctr Dev Adv Comp, Computat Earth Sci Grp, Pune 411007, Maharashtra, India. [Ramachandran, S.] Phys Res Lab, Space & Atmospher Sci Div, Ahmadabad 380009, Gujarat, India. [Holben, B. N.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Tripathi, S. N.] Indian Inst Technol, Dept Civil Engn, Kanpur 208016, Uttar Pradesh, India. RP Kedia, S (reprint author), Ctr Dev Adv Comp, Computat Earth Sci Grp, Pune 411007, Maharashtra, India. EM sumitag@cdac.in; ram@prl.res.in; brent.n.holben@nasa.gov; snt@iitk.ac.in RI Tripathi, Sachchida/J-4840-2016 FU National Academy of Sciences; USAID FX We thank Ramesh P. Singh for his efforts in establishing and maintaining the AERONET sun/sky radiometer at Kanpur the data of which are used in the present study. Temperature, relative humidity, and winds are obtained from NCEP Reanalysis data (http://www.cdc.noaa.gov). Rainfall data from TRMM (http://disc2.nascom.nasa.gov/Giovanni/tovas/) are downloaded from GESDISC. AERONET data for Kanpur and Gandhi College are downloaded from http://aeronet.gsfc.nasa.gov. Air back trajectory data are downloaded from https://ready.arl.noaa.gov/HYSPLIT.php. MODIS fire count data are obtained from http://disc.sci.gsfc.nasa.gov. Part of the work reported here was done by Sumita Kedia as a graduate student at Physical Research Laboratory, Ahmedabad. SNT is supported through a grant from National Academy of Sciences and USAID. NR 43 TC 15 Z9 15 U1 1 U2 15 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD DEC PY 2014 VL 98 BP 607 EP 619 DI 10.1016/j.atmosenv.2014.09.022 PG 13 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AU2WI UT WOS:000345475000065 ER PT J AU Srivastava, PK Han, DW Rico-Ramirez, MA Bray, M Islam, T Gupta, M Dai, Q AF Srivastava, Prashant K. Han, Dawei Rico-Ramirez, Miguel A. Bray, Michaela Islam, Tanvir Gupta, Manika Dai, Qiang TI Estimation of land surface temperature from atmospherically corrected LANDSAT TM image using 6S and NCEP global reanalysis product SO ENVIRONMENTAL EARTH SCIENCES LA English DT Article DE Precipitable water vapour; Agricultural landscape; Weather research and forecasting model (WRF); Land surface temperature (LST); 6S correction ID STRATOSPHERIC WATER-VAPOR; EMISSIVITY RETRIEVAL; PRECIPITABLE WATER; SATELLITE SIGNAL; SOLAR SPECTRUM; SMOS SATELLITE; AVHRR DATA; MODEL; VEGETATION; INDEX AB Water vapour is the most variable constituent in the atmosphere which is responsible for serious noise in the optical satellite images. This research is focused on the vertical distribution of water vapour and deducing its possible effects on the atmospheric correction process. The vertical distribution of precipitable water vapour, water vapour mixing ratio with geopotential height and pressure were estimated through the weather research and forecasting (WRF) model by downscaling the National Center for Environmental Prediction (NCEP) global reanalysis product. In addition, the most widely used LANDSAT TM satellite image has been used for this assessment. The WRF model was applied with three domains centred on a LANDSAT captured image over the area. The 6S atmospheric correction code was utilised for viewing the effect of precipitable water vapour on satellite image correction. The analysis was conducted on two pressure levels (1,000 and 100 hPa) representing the troposphere and stratosphere, respectively. The validation of the atmospheric correction has been performed by estimating the land surface temperature (LST) over the Walnut Creek region and its comparison with the Soil Moisture Experiments in 2002 (SMEX02) LST field validation datasets. The overall analyses indicate a higher accuracy of LST repossession with 100 hPa corrected image. C1 [Srivastava, Prashant K.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Srivastava, Prashant K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD USA. [Srivastava, Prashant K.; Han, Dawei; Rico-Ramirez, Miguel A.; Islam, Tanvir; Dai, Qiang] Univ Bristol, Dept Civil Engn, Bristol, Avon, England. [Bray, Michaela] Cardiff Univ, Hydroenvironm Ctr, Cardiff Sch Engn, Cardiff CF10 3AX, S Glam, Wales. [Islam, Tanvir] NOAA NESDIS Ctr Satellite Applicat & Res, College Pk, MD USA. [Islam, Tanvir] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA. [Gupta, Manika] Indian Inst Technol, Dept Civil Engn, Delhi, India. RP Srivastava, PK (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM prashant.k.srivastava@nasa.gov RI Islam, Tanvir/F-6922-2011; Rico-Ramirez, Miguel/H-3248-2014; OI Rico-Ramirez, Miguel/0000-0002-8885-4582; Islam, Tanvir/0000-0003-2429-3074 FU Commonwealth Scholarship Commission, United Kingdom; Ministry of Human Resource Development, Government of India FX The authors would like to thank the Commonwealth Scholarship Commission, United Kingdom and Ministry of Human Resource Development, Government of India for providing the necessary support and funding for this research. The authors are also thankful to SMEX team for all the validation data generated during the experiments and Computational and Information Systems Laboratory (CISL) at the National Center for Atmospheric Research (NCAR) for the NCEP data. The authors also acknowledge the Advanced Computing Research Centre at University of Bristol for providing the access to supercomputer facility (The Blue Crystal). The views expressed here are those of the authors solely and do not constitute a statement of policy, decision, or position on behalf of NOAA/NASA or the authors' affiliated institutions. NR 56 TC 8 Z9 8 U1 1 U2 16 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1866-6280 EI 1866-6299 J9 ENVIRON EARTH SCI JI Environ. Earth Sci. PD DEC PY 2014 VL 72 IS 12 SI SI BP 5183 EP 5196 DI 10.1007/s12665-014-3388-1 PG 14 WC Environmental Sciences; Geosciences, Multidisciplinary; Water Resources SC Environmental Sciences & Ecology; Geology; Water Resources GA AU1WB UT WOS:000345407000037 ER PT J AU Chabot, NL Ernst, CM Denevi, BW Nair, H Deutsch, AN Blewett, DT Murchie, SL Neumann, GA Mazarico, E Paige, DA Harmon, JK Head, JW Solomon, SC AF Chabot, Nancy L. Ernst, Carolyn M. Denevi, Brett W. Nair, Hari Deutsch, Ariel N. Blewett, David T. Murchie, Scott L. Neumann, Gregory A. Mazarico, Erwan Paige, David A. Harmon, John K. Head, James W. Solomon, Sean C. TI Images of surface volatiles in Mercury's polar craters acquired by the MESSENGER spacecraft SO GEOLOGY LA English DT Article ID ICE DEPOSITS; NORTH-POLE; LUNAR; STABILITY; REGION; WATER; MOON AB Images acquired by NASA's MESSENGER spacecraft have revealed the morphology of frozen volatiles in Mercury's permanently shadowed polar craters and provide insight into the mode of emplacement and evolution of the polar deposits. The images show extensive, spatially continuous regions with distinctive reflectance properties. A site within Prokofiev crater identified as containing widespread surface water ice exhibits a cratered texture that resembles the neighboring sunlit surface except for its uniformly higher reflectance, indicating that the surficial ice was emplaced after formation of the underlying craters. In areas where water ice is inferred to be present but covered by a thin layer of dark, organic-rich volatile material, regions with uniformly lower reflectance extend to the edges of the shadowed areas and terminate with sharp boundaries. The sharp boundaries indicate that the volatile deposits at Mercury's poles are geologically young, relative to the time scale for lateral mixing by impacts, and either are restored at the surface through an ongoing process or were delivered to the planet recently. C1 [Chabot, Nancy L.; Ernst, Carolyn M.; Denevi, Brett W.; Nair, Hari; Deutsch, Ariel N.; Blewett, David T.; Murchie, Scott L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Neumann, Gregory A.; Mazarico, Erwan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Paige, David A.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. [Harmon, John K.] Natl Astron & Ionosphere Ctr, Arecibo Observ, Arecibo, PR 00612 USA. [Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. RP Chabot, NL (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM Nancy.Chabot@jhuapl.edu RI Neumann, Gregory/I-5591-2013; Blewett, David/I-4904-2012; Ernst, Carolyn/I-4902-2012; Murchie, Scott/E-8030-2015; Chabot, Nancy/F-5384-2015; Denevi, Brett/I-6502-2012; Mazarico, Erwan/N-6034-2014 OI Neumann, Gregory/0000-0003-0644-9944; Blewett, David/0000-0002-9241-6358; Murchie, Scott/0000-0002-1616-8751; Chabot, Nancy/0000-0001-8628-3176; Denevi, Brett/0000-0001-7837-6663; Mazarico, Erwan/0000-0003-3456-427X FU NASA [NAS5-97271, NASW-00002]; MESSENGER Participating Scientist Program FX The MESSENGER project is supported by the NASA Discovery Program under contracts NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of Washington. Blewett and Paige are supported by the MESSENGER Participating Scientist Program. We thank P.O. Hayne, P. G. Lucey, and C. D. Neish for insightful reviews and J.B. Murphy for editorial handling. NR 26 TC 14 Z9 14 U1 0 U2 16 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 EI 1943-2682 J9 GEOLOGY JI Geology PD DEC PY 2014 VL 42 IS 12 BP 1051 EP 1054 DI 10.1130/G35916.1 PG 4 WC Geology SC Geology GA AU2IE UT WOS:000345440600007 ER PT J AU Ghent, RR Hayne, PO Bandfield, JL Campbell, BA Allen, CC Carter, LM Paige, DA AF Ghent, Rebecca R. Hayne, Paul O. Bandfield, Joshua L. Campbell, Bruce A. Allen, Carlton C. Carter, Lynn M. Paige, David A. TI Constraints on the recent rate of lunar ejecta breakdown and implications for crater ages SO GEOLOGY LA English DT Article ID MOON; ASTEROIDS; REGOLITH; SURFACE AB We present a new empirical constraint on the rate of breakdown of large ejecta blocks on the Moon based on observations from the Lunar Reconnaissance Orbiter (LRO) Diviner thermal radiometer. We find that the rockiness of fresh crater ejecta can be quantified using the Diviner-derived rock abundance data set, and we present a strong inverse correlation between the 95th percentile value of the ejecta rock abundance (RA(95/5)) and crater age. For nine craters with published model ages derived from crater counts on their continuous ejecta, RA(95/5) decreases with crater age, as (age [m.y.])(-0.46). This result implies shorter rock survival times than predicted based on downward extrapolation of 100 m crater size-frequency distributions, and represents a new empirical constraint on the rate of comminution of large rocks not previously analyzed experimentally or through direct observation. In addition, our result provides a new method for dating young lunar craters. C1 [Ghent, Rebecca R.] Univ Toronto, Dept Earth Sci, Toronto, ON M5S 3B1, Canada. [Ghent, Rebecca R.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Hayne, Paul O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bandfield, Joshua L.] Space Sci Inst, Boulder, CO 80301 USA. [Campbell, Bruce A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Allen, Carlton C.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Carter, Lynn M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Paige, David A.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. RP Ghent, RR (reprint author), Univ Toronto, Dept Earth Sci, 22 Russell St, Toronto, ON M5S 3B1, Canada. RI Carter, Lynn/D-2937-2012 FU National Science and Engineering Research Council of Canada; NASA FX This work was supported by a Discovery grant from the National Science and Engineering Research Council of Canada to Ghent, and by the NASA Lunar Reconnaissance Orbiter Participating Scientist program. We thank David Blewett and an anonymous reviewer for helpful comments. NR 25 TC 11 Z9 11 U1 2 U2 5 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 EI 1943-2682 J9 GEOLOGY JI Geology PD DEC PY 2014 VL 42 IS 12 BP 1059 EP 1062 DI 10.1130/G35926.1 PG 4 WC Geology SC Geology GA AU2IE UT WOS:000345440600009 ER PT J AU Williams, DA Yingst, RA Garry, WB AF Williams, David A. Yingst, R. Aileen Garry, W. Brent TI Introduction: The geologic mapping of Vesta SO ICARUS LA English DT Editorial Material DE Asteroid Vesta; Asteroids, surfaces; Geological processes ID HUBBLE-SPACE-TELESCOPE; ASTEROID 4 VESTA; FRAMING CAMERA IMAGES; CASSINI-ISS IMAGES; DAWN MISSION; SOLAR-SYSTEM; MAIN-BELT; PRIMORDIAL EXCITATION; DYNAMICAL EVOLUTION; CRATERING HISTORY AB The purpose of this paper is to introduce the Geologic Mapping of Vesta Special Issue/Section of Icarus, which includes several papers containing geologic maps of the surface of Vesta made to support data analysis conducted by the Dawn Science Team during the Vesta Encounter (July 2011-September 2012). In this paper we briefly discuss pre-Dawn knowledge of Vesta, provide the goals of our geologic mapping campaign, discuss the methodologies and materials used for geologic mapping, review the global geologic context of Vesta, discuss the challenges of mapping the geology of Vesta as a small airless body, and describe the content of the papers in this Special Issue/Section. We conclude with a discussion of lessons learned from our quadrangle-based mapping effort and provide recommendations for conducting mapping campaigns as part of planetary spacecraft nominal missions. (C) 2014 Elsevier Inc. All rights reserved. C1 [Williams, David A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. Planetary Sci Inst, Tucson, AZ 85719 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Williams, DA (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Box 871404, Tempe, AZ 85287 USA. EM david.williams@asu.edu NR 101 TC 18 Z9 18 U1 0 U2 7 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD DEC PY 2014 VL 244 SI SI BP 1 EP 12 DI 10.1016/j.icarus.2014.03.001 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU3UR UT WOS:000345539500001 ER PT J AU Blewett, DT Buczkowski, DL Ruesch, O Scully, JE O'Brien, DP Gaskell, R Roatsch, T Bowling, TJ Ermakov, A Hiesinger, H Williams, DA Raymond, CA Russell, CT AF Blewett, David T. Buczkowski, Debra L. Ruesch, Ottaviano Scully, Jennifer E. O'Brien, David P. Gaskell, Robert Roatsch, Thomas Bowling, Timothy J. Ermakov, Anton Hiesinger, Harald Williams, David A. Raymond, Carol A. Russell, Christopher T. TI Vesta's north pole quadrangle Av-1 (Albana): Geologic map and the nature of the south polar basin antipodes SO ICARUS LA English DT Article DE Asteroid Vesta; Geological processes; Impact processes ID ASTEROID 4 VESTA; FRAMING CAMERA IMAGES; IMPACT BASINS; FORMING IMPACTS; DARK MATERIAL; WATER ICE; DAWN; MERCURY; SPACE; SURFACE AB As part of systematic global mapping of Vesta using data returned by the Dawn spacecraft, we have produced a geologic map of the north pole quadrangle, Av-1 Albana. Extensive seasonal shadows were present in the north polar region at the time of the Dawn observations, limiting the ability to map morphological features and employ color or spectral data for determination of composition. The major recognizable units present include ancient cratered highlands and younger crater-related units (undivided ejecta, and mass-wasting material on crater floors). The antipode of Vesta's large southern impact basins, Rheasilvia and Veneneia, lie within or near the Av-1 quadrangle. Therefore it is of particular interest to search for evidence of features of the kind that are found at basin antipodes on other planetary bodies. Albedo markings known as lunar swirls are correlated with basin antipodes and the presence of crustal magnetic anomalies on the Moon, but lighting conditions preclude recognition of such albedo features in images of the antipode of Vesta's Rheasilvia basin. "Hilly and lineated terrain," found at the antipodes of large basins on the Moon and Mercury, is not present at the Rheasilvia or Veneneia antipodes. We have identified small-scale linear depressions that may be related to increased fracturing in the Rheasilvia and Veneneia antipodal areas, consistent with impact-induced stresses (Buczkowski, D. et al. [2012b]. Analysis of the large scale troughs on Vesta and correlation to a model of giant impact into a differentiated asteroid. Geol. Soc. of America Annual Meeting. Abstract 152-4; Bowling, T.J. et al. [2013]. J. Geophys. Res. - Planets, 118. http://dx.doi.org/10.1002/jgre.20123). The general high elevation of much of the north polar region could, in part, be a result of uplift caused by the Rheasilvia basin-forming impact, as predicted by numerical modeling (Bowling, T.J. et al. [2013]. J. Geophys. Res. - Planets, 118. http://dx.doi.org/10.1002/jgre.20123). However, stratigraphic and crater size-frequency distribution analysis indicate that the elevated terrain predates the two southern basins and hence is likely a remnant of the ancient vestan crust. The lack of large-scale morphological features at the basin antipodes can be attributed to weakened antipodal constructive interference of seismic waves caused by an oblique impact or by Vesta's non-spherical shape, or by attenuation of seismic waves because of the physical properties of Vesta's interior. A first-order analysis of the Dawn global digital elevation model for Vesta indicates that areas of permanent shadow are unlikely to be present in the vicinity of the north pole. (C) 2014 Elsevier Inc. All rights reserved. C1 [Blewett, David T.; Buczkowski, Debra L.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Planetary Explorat Grp, Laurel, MD 20723 USA. [Ruesch, Ottaviano; Hiesinger, Harald] Univ Munster, Inst Planetol, D-48149 Munster, Germany. [Scully, Jennifer E.; Russell, Christopher T.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. [O'Brien, David P.; Gaskell, Robert] Planetary Sci Inst, Tucson, AZ 85719 USA. [Roatsch, Thomas] DLR, Berlin, Germany. [Bowling, Timothy J.] Purdue Univ, W Lafayette, IN 47907 USA. [Ermakov, Anton] MIT, Cambridge, MA 02139 USA. [Williams, David A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Blewett, DT (reprint author), Johns Hopkins Univ, Appl Phys Lab, Dept Space, Planetary Explorat Grp, MS 200-W230,11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM david.blewett@jhuapl.edu RI Blewett, David/I-4904-2012; Buczkowski, Debra/I-7842-2015; OI Blewett, David/0000-0002-9241-6358; Buczkowski, Debra/0000-0002-4729-7804; Ermakov, Anton/0000-0002-7020-7061 FU NASA [NNX10AR57G] FX The authors thank the two anonymous reviewers for suggestions that helped us to improve this paper. We thank Carolyn Ernst (JHU-APL) for discussion of crater excavation depths. We are grateful to the Dawn flight, instrument, and science teams for their efforts that led to the successful mission at Vesta and the collection and processing of the data used in this study. The work of DTB and DLB was funded by NASA Dawn at Vesta Participating Scientist Program Grant Number NNX10AR57G (DTB, Principal Investigator). NR 76 TC 6 Z9 6 U1 0 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD DEC PY 2014 VL 244 SI SI BP 13 EP 22 DI 10.1016/j.icarus.2014.03.007 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU3UR UT WOS:000345539500002 ER PT J AU Scully, JEC Yin, A Russell, CT Buczkowski, DL Williams, DA Blewett, DT Ruesch, O Hiesinger, H Le Corre, L Mercer, C Yingst, RA Garry, WB Jaumann, R Roatsch, T Preusker, F Gaskell, RW Schroder, SE Ammannito, E Pieters, CM Raymond, CA AF Scully, Jennifer E. C. Yin, A. Russell, C. T. Buczkowski, D. L. Williams, D. A. Blewett, D. T. Ruesch, O. Hiesinger, H. Le Corre, L. Mercer, C. Yingst, R. A. Garry, W. B. Jaumann, R. Roatsch, T. Preusker, F. Gaskell, R. W. Schroeder, S. E. Ammannito, E. Pieters, C. M. Raymond, C. A. CA Dawn Sci Team TI Geomorphology and structural geology of Saturnalia Fossae and adjacent structures in the northern hemisphere of Vesta SO ICARUS LA English DT Article DE Asteroid Vesta; Asteroids, surfaces; Geological processes ID HUBBLE-SPACE-TELESCOPE; DAWN FRAMING CAMERA; ASTEROID 4 VESTA; DARK MATERIAL; IMAGES; HETEROGENEITY; REGOLITH; FAULTS AB Vesta is a unique, intermediate class of rocky body in the Solar System, between terrestrial planets and small asteroids, because of its size (average radius of similar to 263 km) and differentiation, with a crust, mantle and core. Vesta's low surface gravity (0.25 m/s(2)) has led to the continual absence of a protective atmosphere and consequently impact cratering and impact-related processes are prevalent. Previous work has shown that the formation of the Rh impact basin induced the equatorial Divalia Fossae, whereas the formation of the Veneneia impact basin induced the northern Saturnalia Fossae. Expanding upon this earlier work, we conducted photogeologic mapping of the Saturnalia Fossae, adjacent structures and geomorphic units in two of Vesta's northern quadrangles: Caparronia and Domitia. Our work indicates that impact processes created and/or modified all mapped structures and geomorphic units. The mapped units, ordered from oldest to youngest age based mainly on cross-cutting relationships, are: (1) Vestalia Terra unit, (2) cratered highlands unit, (3) Saturnalia Fossae trough unit, (4) Saturnalia Fossae cratered unit, (5) undifferentiated ejecta unit, (6) dark lobate unit, (7) dark crater ray unit and (8) lobate crater unit. The Saturnalia Fossae consist of five separate structures: Saturnalia Fossa A is the largest (maximum width of similar to 43 km) and is interpreted as a graben, whereas Saturnalia Fossa B-E are smaller (maximum width of similar to 15 km) and are interpreted as half grabens formed by synthetic faults. Smaller, second-order structures (maximum width of <1 km) are distinguished from the Saturnalia Fossae, a first-order structure, by the use of the general descriptive term 'adjacent structures', which encompasses minor ridges, grooves and crater chains. For classification purposes, the general descriptive term 'minor ridges' characterizes ridges that are not part of the Satumalia Fossae and are an order of magnitude smaller (maximum width of <1 km vs. maximum width of 43 km). Shear deformation resulting from the large-scale (diameter of <100 km) Rheasilvia impact is proposed to form minor ridges (similar to 2 km to similar to 25 km in length), which are interpreted as the surface expression of thrust faults, as well as grooves (similar to 3 km to similar to 25 km in length) and pit crater chains (similar to 1 km to similar to 25 km in length), which are interpreted as the surface expression of extension fractures and/or dilational normal faults. Secondary crater material, ejected from small-scale and medium-scale impacts (diameters of <100 km), are interpreted to form ejecta ray systems of grooves and crater chains by bouncing and scouring across the surface. Furthermore, seismic shaking, also resulting from small-scale and medium-scale impacts, is interpreted to form minor ridges because seismic shaking induces flow of regolith, which subsequently accumulates as minor ridges that are roughly parallel to the regional slope. In this work we expand upon the link between impact processes and structural features on Vesta by presenting findings of a photogeologic, structural mapping study which highlights how impact cratering and impact-related processes are expressed on this unique, intermediate Solar System body. (C) 2014 Elsevier Inc. All rights reserved. C1 [Scully, Jennifer E. C.; Yin, A.; Russell, C. T.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. [Buczkowski, D. L.; Blewett, D. T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Williams, D. A.; Mercer, C.] Arizona State Univ, Tempe, AZ 85004 USA. [Ruesch, O.; Hiesinger, H.] Univ Munster, Inst Planetol, D-48149 Munster, Germany. [Le Corre, L.; Yingst, R. A.; Gaskell, R. W.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Garry, W. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Jaumann, R.; Roatsch, T.; Preusker, F.; Schroeder, S. E.] German Aerosp Ctr DLR, D-12489 Berlin, Germany. [Ammannito, E.] Ist Nazl Astrofis INAF IFSI, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy. [Pieters, C. M.] Brown Univ, Providence, RI 02912 USA. [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Scully, JEC (reprint author), Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. EM jscully@ucla.edu RI Blewett, David/I-4904-2012; Schroder, Stefan/D-9709-2013; OI Blewett, David/0000-0002-9241-6358; Schroder, Stefan/0000-0003-0323-8324; Le Corre, Lucille/0000-0003-0349-7932 NR 53 TC 11 Z9 11 U1 0 U2 7 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD DEC PY 2014 VL 244 SI SI BP 23 EP 40 DI 10.1016/j.icarus.2014.01.013 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU3UR UT WOS:000345539500003 ER PT J AU Ruesch, O Hiesinger, H Blewett, DT Williams, DA Buczkowski, D Scully, J Yingst, RA Roatsch, T Preusker, F Jaumann, R Russell, CT Raymond, CA AF Ruesch, Ottaviano Hiesinger, Harald Blewett, David T. Williams, David A. Buczkowski, Debra Scully, Jennifer Yingst, R. Aileen Roatsch, Thomas Preusker, Frank Jaumann, Ralf Russell, Christopher T. Raymond, Carol A. TI Geologic map of the northern hemisphere of Vesta based on Dawn Framing Camera (FC) images SO ICARUS LA English DT Article DE Asteroid Vesta; Asteroids, surfaces; Geological processes ID ASTEROID 4 VESTA; INNER SOLAR-SYSTEM; DARK MATERIAL; 21 LUTETIA; 433 EROS; CRATER; PHOBOS; REGOLITH; FEATURES; MISSION AB The Dawn Framing Camera (FC) has imaged the northern hemisphere of the Asteroid (4) Vesta at high spatial resolution and coverage. This study represents the first investigation of the overall geology of the northern hemisphere (22-90 degrees N, quadrangles Av-1, 2, 3, 4 and 5) using these unique Dawn mission observations. We have compiled a morphologic map and performed crater size-frequency distribution (CSFD) measurements to date the geologic units. The hemisphere is characterized by a heavily cratered surface with a few highly subdued basins up to similar to 200 km in diameter. The most widespread unit is a plateau (cratered highland unit), similar to, although of lower elevation than the equatorial Vestalia Terra plateau. Large-scale troughs and ridges have regionally affected the surface. Between similar to 180 degrees E and similar to 270 degrees E, these tectonic features are well developed and related to the south pole Veneneia impact (Saturnalia Fossae trough unit), elsewhere on the hemisphere they are rare and subdued (Saturnalia Fossae cratered unit). In these pre-Rheasilvia units we observed an unexpectedly high frequency of impact craters up to similar to 10 km in diameter, whose formation could in part be related to the Rheasilvia basin-forming event. The Rheasilvia impact has potentially affected the northern hemisphere also with S-N small-scalelineations, but without covering it with an ejecta blanket. Post-Rheasilvia impact craters are small (<60 km in diameter) and show a wide range of degradation states due to impact gardening and mass wasting processes. Where fresh, they display an ejecta blanket, bright rays and slope movements on walls. In places, crater rims have dark material ejecta and some crater floors are covered by ponded material interpreted as impact melt. (C) 2014 Elsevier Inc. All rights reserved. C1 [Ruesch, Ottaviano; Hiesinger, Harald] Univ Munster, Inst Planetol, D-48149 Munster, Germany. [Blewett, David T.; Buczkowski, Debra] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Williams, David A.] Arizona State Univ, Tempe, AZ 85287 USA. [Scully, Jennifer; Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetaly Phys, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [Yingst, R. Aileen] Planetary Sci Inst, Tucson, AZ 85719 USA. [Roatsch, Thomas; Preusker, Frank; Jaumann, Ralf] German Aerosp Ctr DLR, Berlin, Germany. [Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ruesch, O (reprint author), Univ Munster, Inst Planetol, Wilhelm Klemm Str 10, D-48149 Munster, Germany. EM ottaviano.ruesch@uni-muenster.de RI Blewett, David/I-4904-2012 OI Blewett, David/0000-0002-9241-6358 FU German Aerospace Agency (DLR) [FKZ 50 OW 1102]; NASA [NNX10AR57G] FX We acknowledge the financial support of the German Aerospace Agency (DLR) (Grant FKZ 50 OW 1102). We also thank the NASA Dawn at Vesta Participating Scientists Program (Grant NNX10AR57G to D.T.B.), as well as DLR-PF and the Max Planck Institute for Solar System Research for the development and operation of the Framing Camera. We would like to thank Paul Helfenstein and an anonymous reviewer for their thorough review of the manuscript. NR 110 TC 18 Z9 18 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD DEC PY 2014 VL 244 SI SI BP 41 EP 59 DI 10.1016/j.icarus.2014.01.035 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU3UR UT WOS:000345539500004 ER PT J AU Schafer, M Nathues, A Williams, DA Mittlefehldt, DW Le Corre, L Buczkowski, DL Kneissl, T Thangjam, GS Hoffmann, M Schmedemann, N Schafer, T Scully, JEC Li, JY Reddy, V Garry, WB Krohn, K Yingst, RA Gaskell, RW Russell, CT AF Schaefer, Michael Nathues, Andreas Williams, David A. Mittlefehldt, David W. Le Corre, Lucille Buczkowski, Debra L. Kneissl, Thomas Thangjam, Guneshwar S. Hoffmann, Martin Schmedemann, Nico Schaefer, Tanja Scully, Jennifer E. C. Li, Jian-Yang Reddy, Vishnu Garry, W. Brent Krohn, Katrin Yingst, R. Aileen Gaskell, Robert W. Russell, Christopher T. TI Imprint of the Rheasilvia impact on Vesta - Geologic mapping of quadrangles Gegania and Lucaria SO ICARUS LA English DT Article DE Asteroid Vesta; Asteroids, surfaces; Geological processes; Impact processes; Tectonics ID DAWN; COLOR AB We produced two 1:250,000 scale geologic maps of the adjacent quadrangles Av-6 Gegania and Av-7 Lucaria, located in the equatorial region of (4) Vesta (0-144 degrees E, 22 S to 22 degrees N). The mapping is based on clear and color filter images of the Framing Camera (FC) onboard the Dawn spacecraft, which has captured the entire illuminated surface of Vesta with high spatial resolution (up to similar to 20 m/pixel), and on a digital terrain model derived from FC imagery. Besides the geologic mapping itself, a secondary purpose of this work is to investigate one of the most prominent morphological features on Vesta, namely the aggregation of several giant equatorial troughs termed the Divalia Fossae, most probably formed during the Rheasilvia impact near Vesta's south pole. The up to 465 km long and 22 km wide troughs show height differences of up to 5 km between adjacent troughs and ridges. Another imprint of the Rheasilvia impact is the >350 km long and similar to 250 km wide swath of ejecta crossing quadrangle Av-6 Gegania. This lobe shows a distinct appearance in FC color ratios and a high albedo in FC images, indicating a mineralogical similarity to material typically found within the Rheasilvia basin, in particular composed of diogenite-rich howardites. Almost the entire northern half of the mapping area shows the oldest surface, being dominated by upper crustal basaltic material. To the south, increasingly younger formations related to the Rheasilvia impact occur, either indicated by the troughs formed by Rheasilvia or by the Rheasilvia ejecta itself. Only medium sized impact craters with diameters less than 22 km occur within the two mapped quadrangles. Some of the craters exhibit ejecta blankets and/or distinctly dark or bright ejecta material in ejecta rays outside and exposures within the crater, and mass-wasting deposits down crater slopes, forming the youngest surfaces. (C) 2014 Elsevier Inc. All rights reserved. C1 [Schaefer, Michael; Nathues, Andreas; Thangjam, Guneshwar S.; Hoffmann, Martin; Schaefer, Tanja] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany. [Williams, David A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Mittlefehldt, David W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Le Corre, Lucille; Li, Jian-Yang; Reddy, Vishnu; Yingst, R. Aileen; Gaskell, Robert W.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Buczkowski, Debra L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Kneissl, Thomas; Schmedemann, Nico] Free Univ Berlin, Inst Geol Sci, D-12249 Berlin, Germany. [Scully, Jennifer E. C.; Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Garry, W. Brent] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krohn, Katrin] German Aerosp Ctr DLR, D-12489 Berlin, Germany. RP Schafer, M (reprint author), Max Planck Inst Solar Syst Res, Justus von Liebig Weg 3, D-37077 Gottingen, Germany. EM schaeferm@mps.mpg.de OI Reddy, Vishnu/0000-0002-7743-3491; Le Corre, Lucille/0000-0003-0349-7932 FU Max Planck Society (MPG, Germany); German Aerospace Center (DLR, Germany); Jet Propulsion Laboratory (NASA/JPL, USA) FX The authors would like to thank the Dawn Flight Operations team for a successful Vesta phase, and the MPS, DLR and IDA colleagues who designed, built and tested the Framing Cameras. The Dawn FC project is financially supported by Max Planck Society (MPG, Germany), German Aerospace Center (DLR, Germany), and Jet Propulsion Laboratory (NASA/JPL, USA). The data used in this paper are available from the website http://dawndata.igpp.ucla.edu/. NR 30 TC 8 Z9 8 U1 0 U2 7 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD DEC PY 2014 VL 244 SI SI BP 60 EP 73 DI 10.1016/j.icarus.2014.06.026 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU3UR UT WOS:000345539500005 ER PT J AU Williams, DA Denevi, BW Mittlefehldt, DW Mest, SC Schenk, PM Yingst, RA Buczkowski, DL Scully, JEC Garry, WB McCord, TB Combe, JP Jaumann, R Pieters, CM Nathues, A Le Corre, L Hoffmann, M Reddy, V Schafer, M Roatsch, T Preusker, F Marchi, S Kneissl, T Schmedemann, N Neukum, G Hiesinger, H De Sanctis, MC Ammannito, E Frigeri, A Prettyman, TH Russell, CT Raymond, CA AF Williams, David A. Denevi, Brett W. Mittlefehldt, David W. Mest, Scott C. Schenk, Paul M. Yingst, R. Aileen Buczkowski, Debra L. Scully, Jennifer E. C. Garry, W. Brent McCord, Thomas B. Combe, Jean-Phillipe Jaumann, Ralf Pieters, Carle M. Nathues, Andreas Le Corre, Lucille Hoffmann, Martin Reddy, Vishnu Schaefer, Michael Roatsch, Thomas Preusker, Frank Marchi, Simone Kneissl, Thomas Schmedemann, Nico Neukum, Gerhard Hiesinger, Harald De Sanctis, Maria Cristina Ammannito, Eleonora Frigeri, Alessandro Prettyman, Thomas H. Russell, Christopher T. Raymond, Carol A. CA Dawn Sci Team TI The geology of the Marcia quadrangle of asteroid Vesta: Assessing the effects of large, young craters SO ICARUS LA English DT Article DE Asteroid Vesta; Impact processes; Geological processes ID DARK MATERIAL; DAWN MISSION; HETEROGENEITY; MINERALOGY; VOLATILES; HISTORY; IMAGES; SHAPE AB We used Dawn spacecraft data to identify and delineate geological units and landforms in the Marcia quadrangle of Vesta as a means to assess the role of the large, relatively young impact craters Marcia (similar to 63 km diam.) and Calpurnia (similar to 53 km diam.) and their surrounding ejecta field on the local geology. We also investigated a local topographic high with a dark-rayed crater named Aricia Tholus, and the impact crater Octavia that is surrounded by a distinctive diffuse mantle. Crater counts and stratigraphic relations suggest that Marcia is the youngest large crater on Vesta, in which a putative impact melt on the crater floor ranges in age between similar to 40 and 60 Ma (depending upon choice of chronology system), and Marcia's ejecta blanket ranges in age between similar to 120 and 390 Ma (depending upon choice of chronology system). We interpret the geologic units in and around Marcia crater to mark a major vestan time-stratigraphic event, and that the Marcia Formation is one of the geologically youngest formations on Vesta. Marcia crater reveals pristine bright and dark material in its walls and smooth and pitted terrains on its floor. The smooth unit we interpret as evidence of flow of impact melts and (for the pitted terrain) release of volatiles during or after the impact process. The distinctive dark ejecta surrounding craters Marcia and Calpurnia is enriched in OH- or H-bearing phases and has a variable morphology, suggestive of a complex mixture of impact ejecta and impact melts including dark materials possibly derived from carbonaceous chondrite-rich material. Aricia Tholus, which was originally interpreted as a putative vestan volcanic edifice based on lower resolution observations, appears to be a fragment of an ancient impact basin rim topped by a dark-rayed impact crater. Octavia crater has a cratering model formation age of similar to 280-990 Ma based on counts of its ejecta field (depending upon choice of chronology system), and its ejects field is the second oldest unit in this quadrangle. The relatively young craters and their related ejecta materials in this quadrangle are in stark contrast to the surrounding heavily cratered units that are related to the billion years old or older Rheasilvia and Veneneia impact basins and Vesta's ancient crust preserved on Vestalia Terra. (C) 2014 Elsevier Inc. All rights reserved. C1 [Williams, David A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Denevi, Brett W.; Buczkowski, Debra L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Mittlefehldt, David W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Mest, Scott C.; Yingst, R. Aileen; Prettyman, Thomas H.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Schenk, Paul M.] LPI, Houston, TX 77058 USA. [Scully, Jennifer E. C.; Russell, Christopher T.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. [Garry, W. Brent] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McCord, Thomas B.; Combe, Jean-Phillipe] Bear Fight Ctr, Winthrope, WA 98862 USA. [Jaumann, Ralf; Roatsch, Thomas; Preusker, Frank] DLR, Berlin, Germany. [Pieters, Carle M.] Brown Univ, Providence, RI 02912 USA. [Nathues, Andreas; Le Corre, Lucille; Hoffmann, Martin; Reddy, Vishnu; Schaefer, Michael] Max Planck Inst, Katlenburg Lindau, Germany. [Marchi, Simone] NASA, Lunar Sci Inst, Boulder, CO 80302 USA. [Kneissl, Thomas; Schmedemann, Nico; Neukum, Gerhard] Free Univ Berlin, Berlin, Germany. [Hiesinger, Harald] Univ Munster, Inst Planetol, D-48149 Munster, Germany. [De Sanctis, Maria Cristina; Ammannito, Eleonora; Frigeri, Alessandro] Natl Inst Astrophys, Rome, Italy. [Raymond, Carol A.] CALTECH, NASA, JPL, Pasadena, CA 91109 USA. RP Williams, DA (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. EM david.williams@asu.edu RI Denevi, Brett/I-6502-2012; Frigeri, Alessandro/F-2151-2010; OI Denevi, Brett/0000-0001-7837-6663; Frigeri, Alessandro/0000-0002-9140-3977; De Sanctis, Maria Cristina/0000-0002-3463-4437; Reddy, Vishnu/0000-0002-7743-3491; Prettyman, Thomas/0000-0003-0072-2831; Le Corre, Lucille/0000-0003-0349-7932 FU NASA Dawn at Vesta Participating Scientists Program [NNX10AR24G]; Italian Space Agency (ASI) [I/004/12/0] FX The authors thank James Skinner, Wesley Patterson, and editor David Blewett for productive and helpful reviews. The authors also thank the NASA Dawn Science and Flight Teams at the Jet Propulsion Laboratory for their tireless work that enabled the successful Vesta encounter, and the instrument teams at the Max Planck Institute, the German Aerospace Center (DLR), the Italian National Institute of Astrophysics (INAF), and the Planetary Science Institute for collecting and processing the data that enabled this study. DAW was funded through Grant No. NNX10AR24G from the NASA Dawn at Vesta Participating Scientists Program. The VIR Team is funded by the Italian Space Agency (ASI) through Grant No. I/004/12/0. NR 37 TC 19 Z9 19 U1 1 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD DEC PY 2014 VL 244 SI SI BP 74 EP 88 DI 10.1016/j.icarus.2014.01.033 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU3UR UT WOS:000345539500006 ER PT J AU Buczkowski, DL Wyrick, DY Toplis, M Yingst, RA Williams, DA Garry, WB Mest, S Kneissl, T Scully, JEC Nathues, A De Sanctis, MC LeCorre, L Reddy, V Hoffmann, M Ammannito, E Frigeri, A Tosi, F Preusker, F Roatsch, T Raymond, CA Jaumann, R Pieters, CM Russell, CT AF Buczkowski, D. L. Wyrick, D. Y. Toplis, M. Yingst, R. A. Williams, D. A. Garry, W. B. Mest, S. Kneissl, T. Scully, J. E. C. Nathues, A. De Sanctis, M. C. LeCorre, L. Reddy, V. Hoffmann, M. Ammannito, E. Frigeri, A. Tosi, F. Preusker, F. Roatsch, T. Raymond, C. A. Jaumann, R. Pieters, C. M. Russell, C. T. TI The unique geomorphology and physical properties of the Vestalia Terra plateau SO ICARUS LA English DT Article DE Asteroid Vesta; Geological Processes; Tectonics; Volcanism; Impact Processes ID FRAMING CAMERA IMAGES; ASTEROID 4 VESTA; PARENT BODY; SURFACE-FEATURES; MARTIAN GULLIES; DAWN; PHOBOS; HETEROGENEITY; LANDSLIDES; DIOGENITES AB We produced a geologic map of the Av-9 Numisia quadrangle of asteroid Vesta using Dawn spacecraft data to serve as a tool to understand the geologic relations of surface features in this region. These features include the plateau Vestalia Terra, a hill named Brumalia Tholus, and an unusual "dark ribbon" material crossing the majority of the map area. Stratigraphic relations suggest that Vestalia Terra is one of the oldest features on Vesta, despite a model crater age date similar to that of much of the surface of the asteroid. Cornelia, Numisia and Drusilla craters reveal bright and dark material in their walls, and both Cornelia and Numisia have smooth and pitted terrains on their floors suggestive of the release of volatiles during or shortly after the impacts that formed these craters. Cornelia, Fabia and Teia craters have extensive bright ejecta lobes. While diogenitic material has been identified in association with the bright Teia and Fabia ejecta, hydroxyl has been detected in the dark material within Cornelia, Numisia and Drusilla. Three large pit crater chains appear in the map area, with an orientation similar to the equatorial troughs that cut the majority of Vesta. Analysis of these features has led to several interpretations of the geological history of the region. Vestalia Terra appears to be mechanically stronger than the rest of Vesta. Brumalia Tholus may be the surface representation of a dike-fed laccolith. The dark ribbon feature is proposed to represent a long-runout ejecta flow from Drusilla crater. (C) 2014 Published by Elsevier Inc. C1 [Buczkowski, D. L.] JHU APL, Laurel, MD 21045 USA. [Wyrick, D. Y.] SwRI, San Antonio, TX 78238 USA. [Toplis, M.] Univ Toulouse, Observ Midi Pyrenees, IRAP, F-31400 Toulouse, France. [Yingst, R. A.; Mest, S.] PSI, Tucson, AZ 85719 USA. [Williams, D. A.] ASU, Tempe, AZ 85004 USA. [Garry, W. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kneissl, T.; Ammannito, E.] Free Univ Berlin, Berlin, Germany. [Scully, J. E. C.; Russell, C. T.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. [Nathues, A.; LeCorre, L.; Reddy, V.; Hoffmann, M.] Max Planck Inst, Katlenburg Lindau, Germany. [De Sanctis, M. C.; Frigeri, A.; Tosi, F.] INAF IAPS, Rome, Italy. [Preusker, F.; Roatsch, T.; Jaumann, R.] DLR, Berlin, Germany. [Raymond, C. A.] CALTECH, JPL, Pasadena, CA 91109 USA. [Pieters, C. M.] Brown Univ, Providence, RI 02912 USA. RP Buczkowski, DL (reprint author), JHU APL, Laurel, MD 21045 USA. EM debra.buczkowski@jhuapl.edu RI Buczkowski, Debra/I-7842-2015; Frigeri, Alessandro/F-2151-2010; OI Buczkowski, Debra/0000-0002-4729-7804; Frigeri, Alessandro/0000-0002-9140-3977; De Sanctis, Maria Cristina/0000-0002-3463-4437; Reddy, Vishnu/0000-0002-7743-3491; Le Corre, Lucille/0000-0003-0349-7932; Tosi, Federico/0000-0003-4002-2434 FU Dawn at Vesta Participating Science Program [NNX10AR58G S06]; Dawn Instrument, Operations, and Science Teams FX The authors gratefully acknowledge the support of the Dawn Instrument, Operations, and Science Teams. This work was funded by the Dawn at Vesta Participating Science Program, Grant No. NNX10AR58G S06. 'The data used in this paper are available from the website http://dawndata.igpp.ucla.edu. We would also like to thank Brad Thomson and Amanda Nahm for their thoughtful and helpful reviews. NR 71 TC 16 Z9 16 U1 1 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD DEC PY 2014 VL 244 SI SI BP 89 EP 103 DI 10.1016/j.icarus.2014.03.035 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU3UR UT WOS:000345539500007 ER PT J AU Garry, WB Williams, DA Yingst, RA Mest, SC Buczkowski, DL Tosi, F Schafer, M Le Corre, L Reddy, V Jaumann, R Pieters, CM Russell, CT Raymond, CA AF Garry, W. Brent Williams, David A. Yingst, R. Aileen Mest, Scott C. Buczkowski, Debra L. Tosi, Federico Schaefer, Michael Le Corre, Lucille Reddy, Vishnu Jaumann, Ralf Pieters, Carle M. Russell, Christopher T. Raymond, Carol A. CA Dawn Sci Team TI Geologic mapping of ejecta deposits in Oppia Quadrangle, Asteroid (4) Vesta SO ICARUS LA English DT Article DE Asteroid Vesta; Asteroids, surfaces; Geological processes; Cratering ID NORTHERN-HEMISPHERE; CAMERA IMAGES; DAWN; IMPACT; CRATERS; MORPHOLOGY; OLIVINE; MISSION; SURFACE; CERES AB Oppia Quadrangle Av-10 (288-360 degrees E, +/- 22 degrees) is a junction of key geologic features that preserve a rough history of Asteroid (4) Vesta and serves as a case study of using geologic mapping to define a relative geologic timescale. Clear filter images, stereo-derived topography, slope maps, and multispectral color-ratio images from the Framing Camera on NASA's Dawn spacecraft served as basemaps to create a geologic map and investigate the spatial and temporal relationships of the local stratigraphy. Geologic mapping reveals the oldest map unit within Av-10 is the cratered highlands terrain which possibly represents original crustal material on Vesta that was then excavated by one or more impacts to form the basin Feralia Planitia. Saturnalia Fossae and Divalia Fossae ridge and trough terrains intersect the wall of Feralia Planitia indicating that this impact basin is older than both the Veneneia and Rheasilvia impact structures, representing Pre-Veneneian crustal material. Two of the youngest geologic features in Av-10 are Lepida (similar to 45 km diameter) and Oppia (similar to 40 km diameter) impact craters that formed on the northern and southern wall of Feralia Planitia and each cross-cuts a trough terrain. The ejecta blanket of Oppia is mapped as 'dark mantle' material because it appears dark orange in the Framing Camera 'Clementine-type' color-ratio image and has a diffuse, gradational contact distributed to the south across the rim of Rheasilvia. Mapping of surface material that appears light orange in color in the Framing Camera 'Clementine-type' color-ratio image as 'light mantle material' supports previous interpretations of an impact ejecta origin. Some light mantle deposits are easily traced to nearby source craters, but other deposits may represent distal ejecta deposits (emplaced >5 crater radii away) in a microgravity environment. Published by Elsevier Inc. C1 [Garry, W. Brent] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Williams, David A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Yingst, R. Aileen; Mest, Scott C.; Le Corre, Lucille; Reddy, Vishnu] Planetary Sci Inst, Tucson, AZ 85719 USA. [Buczkowski, Debra L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Tosi, Federico] Inst Space Astrophys & Planetol, I-00133 Rome, Italy. [Schaefer, Michael; Le Corre, Lucille; Reddy, Vishnu] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany. [Jaumann, Ralf] DLR, Berlin, Germany. [Pieters, Carle M.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Garry, WB (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Code 698, Greenbelt, MD 20771 USA. EM brent.garry@nasa.gov OI Reddy, Vishnu/0000-0002-7743-3491; Le Corre, Lucille/0000-0003-0349-7932; Tosi, Federico/0000-0003-4002-2434 FU Dawn at Vesta Participating Scientist Program [NNX10AR28G, NNX11AK16G] FX The authors would like to thank the Dawn flight, operations, and science teams at Jet Propulsion Laboratories, the instrument teams at the German Aerospace Center (DLR), the Italian National Institute for Astrophysics (INAF), Max Planck Institute, and the Planetary Science Institute. Thank you to Dr. J. Olaf Gustafson, an anonymous reviewer, and Guest Editor. Dr. David Blewett, for their thorough comments, edits, and suggestions. Support for W.B. Garry's research and writing of this manuscript was funded by the Dawn at Vesta Participating Scientist Program Grants NNX10AR28G (Smithsonian), NNX11AK16G (Planetary Science Institute), and award to NASA Goddard Space Flight Center. The data used in this paper are available from the website http://dawndata.igpp.ucla.edu. NR 55 TC 8 Z9 8 U1 0 U2 2 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 DEC PY 2014 VL 244 SI SI BP 104 EP 119 DI 10.1016/j.icarus.2014.08.046 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU3UR UT WOS:000345539500008 ER PT J AU Krohn, K Jaumann, R Otto, K Hoogenboom, T Wagner, R Buczkowski, DL Garry, B Williams, DA Yingst, RA Scully, J De Sanctis, MC Kneissl, T Schmedemann, N Kersten, E Stephan, K Matz, KD Pieters, CM Preusker, F Roatsch, T Schenk, P Russell, CT Raymond, CA AF Krohn, K. Jaumann, R. Otto, K. Hoogenboom, T. Wagner, R. Buczkowski, D. L. Garry, B. Williams, D. A. Yingst, R. A. Scully, J. De Sanctis, M. C. Kneissl, T. Schmedemann, N. Kersten, E. Stephan, K. Matz, K-D. Pieters, C. M. Preusker, F. Roatsch, T. Schenk, P. Russell, C. T. Raymond, C. A. TI Mass movement on Vesta at steep scarps and crater rims SO ICARUS LA English DT Article DE Asteroid Vesta; Asteroids, surfaces; Geological processes; Impact processes ID INDUCED SEISMIC ACTIVITY; FRAMING CAMERA IMAGES; MARTIAN GULLIES; SURFACE; DAWN; MORPHOLOGY; FEATURES AB The Quadrangles Av-11 and Av-12 on Vesta are located at the northern rim of the giant Rheasilvia south polar impact basin. The primary geologic units in Av-11 and Av-12 include material from the Rheasilvia impact basin formation, smooth material and different types of impact crater structures (such as bimodal craters, dark and bright crater ray material and dark ejecta material). Av-11 and Av-12 exhibit almost the full range of mass wasting features observed on Vesta, such as slump blocks, spur-and-gully morphologies and landslides within craters. Processes of collapse, slope instability and seismically triggered events force material to slump down crater walls or scarps and produce landslides or rotational slump blocks. The spur-and-gully morphology that is known to form on Mars is also observed on Vesta; however, on Vesta this morphology formed under dry conditions. (C) 2014 Elsevier Inc. All rights reserved. C1 [Krohn, K.; Jaumann, R.; Otto, K.; Wagner, R.; Kersten, E.; Stephan, K.; Matz, K-D.; Preusker, F.; Roatsch, T.] German Aerosp Ctr DLR, Inst Planetary Res, D-12489 Berlin, Germany. [Jaumann, R.; Kneissl, T.; Schmedemann, N.] Free Univ Berlin, Inst Geosci Planetol & Remote Sensing, D-12249 Berlin, Germany. [Hoogenboom, T.; Schenk, P.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Buczkowski, D. L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Garry, B.; Yingst, R. A.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Williams, D. A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Scully, J.; Russell, C. T.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [De Sanctis, M. C.] Natl Inst Astrophys, I-00133 Rome, Italy. [Pieters, C. M.] Brown Univ, Providence, RI 02912 USA. [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Krohn, K (reprint author), German Aerosp Ctr DLR, Inst Planetary Res, D-12489 Berlin, Germany. EM Katrin.Krohn@dlr.de OI De Sanctis, Maria Cristina/0000-0002-3463-4437 NR 39 TC 17 Z9 17 U1 3 U2 13 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 DEC PY 2014 VL 244 SI SI BP 120 EP 132 DI 10.1016/j.icarus.2014.03.013 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU3UR UT WOS:000345539500009 ER PT J AU Kneissl, T Schmedemann, N Reddy, V Williams, DA Walter, SHG Neesemann, A Michael, GG Jaumann, R Krohn, K Preusker, F Roatsch, T Le Corre, L Nathues, A Hoffmann, M Schafer, M Buczkowski, D Garry, WB Yingst, RA Mest, SC Russell, CT Raymond, CA AF Kneissl, T. Schmedemann, N. Reddy, V. Williams, D. A. Walter, S. H. G. Neesemann, A. Michael, G. G. Jaumann, R. Krohn, K. Preusker, F. Roatsch, T. Le Corre, L. Nathues, A. Hoffmann, M. Schaefer, M. Buczkowski, D. Garry, W. B. Yingst, R. A. Mest, S. C. Russell, C. T. Raymond, C. A. TI Morphology and formation ages of mid-sized post-Rheasilvia craters - Geology of quadrangle Tuccia, Vesta SO ICARUS LA English DT Article DE Asteroid Vesta; Asteroids, surfaces; Cratering; Geological processes; Impact processes ID CARBONACEOUS CHONDRITE CLASTS; ASTEROID 4 VESTA; DARK MATERIAL; DAWN MISSION; IMPACT; EJECTA; HETEROGENEITY; DEPOSITS; IMAGES; COLOR AB A variety of geologic landforms and features are observed within quadrangle Av-13 Tuccia in the southern hemisphere of Vesta. The quadrangle covers parts of the highland Vestalia Terra as well as the floors of the large Rheasilvia and Veneneia impact basins, which results in a substantial elevation difference of more than 40 km between the northern and the southern portions of the quadrangle. Measurements of crater size-frequency distributions within and surrounding the Rheasilvia basin indicate that gravity-driven mass wasting in the interior of the basin has been important, and that the basin has a more ancient formation age than would be expected from the crater density on the basin floor alone. Subsequent to its formation, Rheasilvia was superimposed by several mid-sized impact craters. The most prominent craters are Tuccia, Eusebia, Vibidia, Galeria, and Antonia, whose geology and formation ages are investigated in detail in this work. These impact structures provide a variety of morphologies indicating different sorts of subsequent impact-related or gravity-driven mass wasting processes. Understanding the geologic history of the relatively young craters in the Rheasilvia basin is important in order to understand the even more degraded craters in other regions of Vesta. (C) 2014 Elsevier Inc. All rights reserved. C1 [Kneissl, T.; Schmedemann, N.; Walter, S. H. G.; Neesemann, A.; Michael, G. G.] Free Univ Berlin, Inst Geol Sci, D-12249 Berlin, Germany. [Reddy, V.; Le Corre, L.; Nathues, A.; Hoffmann, M.; Schaefer, M.] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany. [Williams, D. A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Jaumann, R.; Krohn, K.; Preusker, F.; Roatsch, T.] German Aerosp Ctr DLR, D-12489 Berlin, Germany. [Buczkowski, D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Reddy, V.; Le Corre, L.; Garry, W. B.; Yingst, R. A.; Mest, S. C.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kneissl, T (reprint author), Free Univ Berlin, Inst Geol Sci Planetary Sci & Remote Sensing, Malteserstr 74-100, D-12249 Berlin, Germany. EM Thomas.Kneissl@fu-berlin.de OI Reddy, Vishnu/0000-0002-7743-3491; Le Corre, Lucille/0000-0003-0349-7932 FU Dawn Science, Instrument and Operations Teams; German Space Agency (DLR) [50 OW 1101] FX The authors acknowledge the support of the Dawn Science, Instrument and Operations Teams. This research has made use of the USGS Integrated Software for Imagers and Spectrometers (ISIS). We thank Michael Zanetti and an anonymous reviewer for the comments and suggestions, which helped improve the manuscript. This work was partly supported by the German Space Agency (DLR), Grant 50 OW 1101. NR 83 TC 11 Z9 11 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD DEC PY 2014 VL 244 SI SI BP 133 EP 157 DI 10.1016/j.icarus.2014.02.012 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU3UR UT WOS:000345539500010 ER PT J AU Williams, DA Jaumann, R McSween, HY Marchi, S Schmedemann, N Raymond, CA Russell, CT AF Williams, D. A. Jaumann, R. McSween, H. Y., Jr. Marchi, S. Schmedemann, N. Raymond, C. A. Russell, C. T. TI The chronostratigraphy of protoplanet Vesta SO ICARUS LA English DT Article DE Impact processes; Asteroid Vesta; Asteroids, surfaces; Geological processes ID BASALTIC ACHONDRITE; COLLISIONAL HISTORY; DARK MATERIAL; IMPACT MELT; METEORITES; DAWN; ORIGIN; EVOLUTION; REGOLITH; FAMILY AB In this paper we present a time-stratigraphic scheme and geologic time scale for the protoplanet Vesta, based on global geologic mapping and other analyses of NASA Dawn spacecraft data, complemented by insights gained from laboratory studies of howardite-eucrite-diogenite (HED) meteorites and geophysical modeling. On the basis of prominent impact structures and their associated deposits, we propose a time scale for Vesta that consists of four geologic time periods: Pre-Veneneian, Veneneian, Rheasilvian, and Marcian. The Pre-Veneneian Period covers the time from the formation of Vesta up to the Veneneia impact event, from 4.6 Ga to >2.1 Ga (using the asteroid flux-derived chronology system) or from 4.6 Ga to 3.7 Ga (under the lunar-derived chronology system). The Veneneian Period covers the time span between the Veneneia and Rheasilvia impact events, from >2.1 to 1 Ga (asteroid flux-derived chronology) or from 3.7 to 3.5 Ga (lunar-derived chronology), respectively. The Rheasilvian Period covers the time span between the Rheasilvia and Marcia impact events, and the Marcian Period covers the time between the Marcia impact event until the present. The age of the Marcia impact is still uncertain, but our current best estimates from crater counts of the ejecta blanket suggest an age between 120 and 390 Ma, depending upon choice of chronology system used. Regardless, the Marcia impact represents the youngest major geologic event on Vesta. Our proposed four-period geologic time scale for Vesta is, to a first order, comparable to those developed for other airless terrestrial bodies. (C) 2014 Elsevier Inc. All rights reserved. C1 [Williams, D. A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Jaumann, R.] DLR, Inst Planetary Res, Berlin, Germany. [Jaumann, R.; Schmedemann, N.] Free Univ Berlin, Inst Geowissensch, Berlin, Germany. [McSween, H. Y., Jr.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Marchi, S.] SW Res Inst, Solar Syst Explorat Res Virtual Inst, Boulder, CO 80302 USA. [Raymond, C. A.] CALTECH, NASA, JPL, Pasadena, CA 91109 USA. [Russell, C. T.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. RP Williams, DA (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Box 871404, Tempe, AZ 85287 USA. EM david.williams@asu.edu FU NASA Dawn at Vesta Participating Scientists Program [NNX10AR24G] FX We thank Paul K. Byrne and Nicholas Lang for helpful reviews. The authors also thank the NASA Dawn Science and Flight Teams at the Jet Propulsion Laboratory for their tireless work that enabled the successful Vesta encounter, and the instrument teams at the Max Planck Institute, the German Aerospace Center (DLR), the Italian National Institute of Astrophysics (INAF), and the Planetary Science Institute for collecting and processing the data that enabled this study. DAW was funded through grant number NNX10AR24G from the NASA Dawn at Vesta Participating Scientists Program. The data used in this paper are available from the website http://dawndata.igpp.ucla.edu. NR 73 TC 6 Z9 6 U1 1 U2 13 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 DEC PY 2014 VL 244 SI SI BP 158 EP 165 DI 10.1016/j.icarus.2014.06.027 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU3UR UT WOS:000345539500011 ER PT J AU Basu, C Caubel, JJ Kim, K Cheng, E Dhinakaran, A Agogino, AM Martin, RA AF Basu, Chandrayee Caubel, Julien J. Kim, Kyunam Cheng, Elizabeth Dhinakaran, Aparna Agogino, Alice M. Martin, Rodney A. TI Sensor-Based Predictive Modeling for Smart Lighting in Grid-Integrated Buildings SO IEEE SENSORS JOURNAL LA English DT Article DE Clustering; daylight harvesting; inverse model; support vector regression; wireless sensor network ID OPEN-PLAN OFFICES; ENERGY; ALGORITHMS; REGRESSION; SELECTION AB Studies show that if we retrofit all the lighting systems in the buildings of California with dimming ballasts, then it would be possible to obtain a 450 MW of regulation, 2.5 GW of nonspinning reserve, and 380 MW of contingency reserve from participation of lighting loads in the energy market. However, in order to guarantee participation, it will be important to monitor and model lighting demand and supply in buildings. To this end, wireless sensor and actuator networks have proven to bear a great potential for personalized intelligent lighting with reduced energy use at 50%-70%. Closed-loop control of these lighting systems relies upon instantaneous and dense sensing. Such systems can be expensive to install and commission. In this paper, we present a sensor-based intelligent lighting system for future grid-integrated buildings. The system is intended to guarantee participation of lighting loads in the energy market, based on predictive models of indoor light distribution, developed using sparse sensing. We deployed similar to 60% fewer sensors compared with state-of-art systems using one photosensor per luminaire. The sensor modules contained small solar panels that were powered by ambient light. Reduction in sensor deployments is achieved using piecewise linear predictive models of indoor light, discretized by clustering for sky conditions and sun positions. Day-ahead daylight is predicted from forecasts of temperature, humidity, and cloud cover. With two weeks of daylight and artificial light training data acquired at the sustainability base at NASA Ames, our model was able to predict the illuminance at seven monitored workstations with 80%-95% accuracy. Moreover, our support vector regression model was able to predict day-ahead daylight at similar to 92% accuracy. C1 [Basu, Chandrayee] Carnegie Mellon Univ, Pittsburgh, PA 15213 USA. [Caubel, Julien J.; Kim, Kyunam; Agogino, Alice M.] Univ Calif Berkeley, Dept Mech Engn, Berkeley, CA 94720 USA. [Cheng, Elizabeth] Univ Calif Berkeley, Dept Comp Sci & Appl Math, Berkeley, CA 94720 USA. [Dhinakaran, Aparna] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA. NASA, Ames Res Ctr, Mountain View, CA 94035 USA. RP Basu, C (reprint author), Carnegie Mellon Univ, Pittsburgh, PA 15213 USA. EM basu.chandrayee@gmail.com; jcaubel@berkeley.edu; knkim@berkeley.edu; elizabeth.y.cheng@gmail.com; aparnadhinak@gmail.com; agogino@berkeley.edu; rodney.martin@nasa.gov FU National Aeronautics and Space Administration, University of California at Berkeley, Berkeley, CA, USA; California Energy Commission FX This work was supported in part by the National Aeronautics and Space Administration, University of California at Berkeley, Berkeley, CA, USA, and in part by the California Energy Commission through the Energy Innovations Small Grant Program. The associate editor coordinating the review of this paper and approving it for publication was Dr. Ashish Pandharipande. NR 47 TC 5 Z9 5 U1 1 U2 28 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1530-437X EI 1558-1748 J9 IEEE SENS J JI IEEE Sens. J. PD DEC PY 2014 VL 14 IS 12 DI 10.1109/JSEN.2014.2352331 PG 14 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Physics, Applied SC Engineering; Instruments & Instrumentation; Physics GA AU5AM UT WOS:000345619500004 ER PT J AU Fathpour, N Blackmore, L Kuwata, Y Assad, C Wolf, MT Newman, C Elfes, A Reh, K AF Fathpour, Nanaz Blackmore, Lars Kuwata, Yoshiaki Assad, Christopher Wolf, Michael T. Newman, Claire Elfes, Alberto Reh, Kim TI Feasibility Studies on Guidance and Global Path Planning for Wind-Assisted Montgolfiere in Titan SO IEEE SYSTEMS JOURNAL LA English DT Article DE Decomposition algorithm; general purpose guidance algorithm; global reachability; graph search algorithm; loitering; Markov decision process; Montgolfiere; path planning; reachability maps; Titan; TitanWRF ID AUTONOMOUS UNDERWATER VEHICLES; GENERAL-CIRCULATION MODEL; SUPERROTATION; ATMOSPHERE; BALLOONS; COMPLEX; FIELDS; VENUS AB Recent studies have proposed the use of a hot-air (Montgolfiere) balloon for possible exploration of Titan, Mars, and Venus. One of NASA's Outer Planet Flagship mission concepts is the Titan Saturn System Mission, which would be a joint NASA-ESA partnership that plans to employ a Montgolfiere along with a lake lander and an orbiter. This Montgolfiere would circle Titan, investigating how Titan and Saturn operate as a system and determining how far prebiotic chemistry has developed. This paper provides a new method to analyze global path planning with balloons on Titan. The main objective of this study is to determine whether the balloon could reach a particular location of interest from a given initial position at its insertion point in the atmosphere using the wind fields on Titan. This study is the first comprehensive analysis and quantitative assessment of balloon guidance in Titan that proactively uses wind for global path planning. The paper will investigate and characterize the guidance and path-planning performance of Montgolfiere balloons in Titan's atmosphere for lower atmosphere and surface exploration in the presence of variable wind fields using the Titan Weather Research and Forecasting (TitanWRF) model. The study focuses on determining the altitude profile that a balloon could follow, using variable wind fields, in order to reach its target most quickly. Our results show that a simple unpropelled Montgolfiere without horizontal actuation would be able to reach a broad array of science targets within the constraints of the wind field. The study also indicates that even a small amount of horizontal thrust allows the balloon to reach any area of interest on Titan, in a fraction of the time needed by the unpropelled balloon. The results show that using the Titan wind field allows a balloon to significantly extend its scientific reach and that a Montgolfiere (unpropelled or propelled) is a highly desirable architecture that can significantly enhance the scientific return of a future Titan mission. C1 [Fathpour, Nanaz; Assad, Christopher; Wolf, Michael T.; Reh, Kim] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Blackmore, Lars; Kuwata, Yoshiaki] Space Explorat Technol, Hawthorne, CA 90250 USA. [Newman, Claire] Ashima Res, Pasadena, CA 91106 USA. [Elfes, Alberto] CSIRO, Pullenvale, Qld 4069, Australia. RP Fathpour, N (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Nanaz.Fathpour@jpl.nasa.gov RI Elfes, Alberto/E-2463-2011 OI Elfes, Alberto/0000-0003-2433-995X FU National Aeronautics and Space Administration FX This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 26 TC 0 Z9 0 U1 0 U2 12 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1932-8184 EI 1937-9234 J9 IEEE SYST J JI IEEE Syst. J. PD DEC PY 2014 VL 8 IS 4 BP 1112 EP 1125 DI 10.1109/JSYST.2013.2282700 PG 14 WC Computer Science, Information Systems; Engineering, Electrical & Electronic; Operations Research & Management Science; Telecommunications SC Computer Science; Engineering; Operations Research & Management Science; Telecommunications GA AU5AZ UT WOS:000345620800011 ER PT J AU Sudbrack, CK Hardy, MC AF Sudbrack, Chantal K. Hardy, Mark C. TI Long-Term Stability and Durability of High-Temperature Alloys SO JOM LA English DT Editorial Material C1 [Sudbrack, Chantal K.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Hardy, Mark C.] Rolls Royce PLC, Derby DE2 8BJ, England. RP Sudbrack, CK (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM chantal.k.sudbrack@nasa.gov; mark.hardy@rolls-royce.com NR 0 TC 0 Z9 0 U1 2 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1047-4838 EI 1543-1851 J9 JOM-US JI JOM PD DEC PY 2014 VL 66 IS 12 BP 2476 EP 2477 DI 10.1007/s11837-014-1191-9 PG 2 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering; Mineralogy; Mining & Mineral Processing SC Materials Science; Metallurgy & Metallurgical Engineering; Mineralogy; Mining & Mineral Processing GA AU1RF UT WOS:000345397200013 ER PT J AU Kalinoski, M Hirons, A Horodysky, A Brill, R AF Kalinoski, Mieka Hirons, Amy Horodysky, Andrij Brill, Richard TI Spectral sensitivity, luminous sensitivity, and temporal resolution of the visual systems in three sympatric temperate coastal shark species SO JOURNAL OF COMPARATIVE PHYSIOLOGY A-NEUROETHOLOGY SENSORY NEURAL AND BEHAVIORAL PHYSIOLOGY LA English DT Article DE Elasmobranch; Electroretinogram; Flicker fusion frequency; Temperature; Vision ID JUVENILE SANDBAR SHARKS; INHABITING CHESAPEAKE BAY; NORTHWEST ATLANTIC-OCEAN; MUSTELUS-CANIS; SMOOTH DOGFISH; DEEP-SEA; DINOFLAGELLATE LUMINESCENCE; MESOPELAGIC CRUSTACEANS; CARCHARHINUS-PLUMBEUS; SCYLIORHINUS-CANICULA AB We used electroretinography (ERG) to determine spectral and luminous sensitivities, and the temporal resolution (flicker fusion frequency, FFF) in three sympatric (but phylogenetically distant) coastal shark species: Carcharhinus plumbeus (sandbar shark), Mustelus canis (smooth dogfish), and Squalus acanthias (spiny dogfish). Spectral sensitivities were similar (range similar to 400-600 nm, peak sensitivity similar to 470 nm), with a high likelihood of rod/cone dichromacy enhancing contrast discrimination. Spiny dogfish were significantly less light sensitive than the other species, whereas their FFF was similar to 19 Hz at maximum intensities; a value equal to that of sandbar shark and significantly above that of smooth dogfish (similar to 9-12 Hz). This occurred even though experiments on spiny dogfish were conducted at 12 versus 25 A degrees C and 20 A degrees C for experiments on sandbar shark and smooth dogfish, respectively. Although spiny dogfish have a rod-dominated retina (rod:cone ratio 50:1), their visual system appears to have evolved for a relatively high temporal resolution (i.e., high FFF) through a short integration time, with the requisite concomitant reduction in luminous sensitivity. Our results suggest adaptive plasticity in the temporal resolution of elasmobranch visual systems which reflects the importance of the ability to track moving objects such as mates, predators, or prey. C1 [Kalinoski, Mieka; Hirons, Amy] Nova SE Univ, Oceanog Ctr, Dania, FL 33004 USA. [Horodysky, Andrij] Hampton Univ, Dept Marine & Environm Sci, Hampton, VA 23668 USA. [Brill, Richard] Northeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, James J Howard Marine Sci Lab, Highlands, NJ 07732 USA. [Brill, Richard] VIMS, Gloucester Point, VA 23062 USA. RP Brill, R (reprint author), VIMS, POB 1346, Gloucester Point, VA 23062 USA. EM rbrill@vims.edu FU South Florida Chapter of the Explorer's Club FX All animal capture, care, and experimental protocols complied with relevant laws of the United States and were approved by the Institutional Animal Care and Use Committees of the College of William and Mary, Nova Southeastern University, and the University of Massachusetts Dartmouth. The authors thank the staff at the Virginia Institute of Marine Science-Eastern Shore Laboratory for their continuing hospitality and help in acquiring sandbar sharks and smooth dogfish, D. Bernal (University of Massachusetts, Dartmouth) for making it possible to perform experiments on spiny dogfish, and L. Litherland for her support and discussions regarding experimental design, execution, and data analysis. M. Kalinoski's participation was funded in part by a scholarship from the South Florida Chapter of the Explorer's Club. This paper is contribution 3409 from the Virginia Institute of Marine Science, College of William & Mary. The opinions expressed herein are those of the authors and do not necessarily reflect the views of the U.S. Department of Commerce-National Oceanic and Atmospheric Administration (NOAA) or any of its subagencies. Mention of trade names, products, or commercial companies is for identification purposes only and likewise does not imply endorsement by NOAA or any of its subagencies. NR 116 TC 3 Z9 3 U1 4 U2 36 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-7594 EI 1432-1351 J9 J COMP PHYSIOL A JI J. Comp. Physiol. A -Neuroethol. Sens. Neural Behav. Physiol. PD DEC PY 2014 VL 200 IS 12 BP 997 EP 1013 DI 10.1007/s00359-014-0950-y PG 17 WC Behavioral Sciences; Neurosciences; Physiology; Zoology SC Behavioral Sciences; Neurosciences & Neurology; Physiology; Zoology GA AU0SF UT WOS:000345333900002 PM 25319537 ER PT J AU Georgiev, GT Butler, JJ Thome, KJ Ramos-Izquierdo, LA Ding, L Graziani, LJ Meadows, GA AF Georgiev, G. T. Butler, J. J. Thome, K. J. Ramos-Izquierdo, L. A. Ding, L. Graziani, L. J. Meadows, G. A. TI Initial studies of the directional reflectance changes in pressed and sintered PTFE diffusers following exposure to contamination and ionizing radiation SO METROLOGIA LA English DT Article DE BRDF; PTFE; diffuse reflectance; calibration; optical instruments; remote sensing ID ULTRAVIOLET AB Changes in the directional reflectance properties of pressed and sintered polytetrafluoroethylene (PTFE) diffusers induced by exposure to vacuum ultraviolet (VUV) irradiation before and after controlled contamination with Pennzane are presented in this paper. A set of 99% reflective, white, optical grade diffuse calibration standards were irradiated with a VUV source positioned at 60 degrees to the diffuser normal. The bidirectional reflectance distribution functions before and after contamination and VUV irradiation were measured and compared at a number of scatter geometries and wavelengths in the UV, VIS and IR spectral ranges. The 8 degrees directional hemispherical reflectance's were also measured and compared from 200 nm to 2500 nm. Our results indicate a measureable impact of VUV irradiation on pressed and sintered PTFE diffusers as manifested by a directional dependent change in their reflectance. Such an effect needs to be considered in the on-orbit deployment of PTFE diffusers. C1 [Georgiev, G. T.; Ding, L.] Sigma Space Corp, Lanham, MD 20706 USA. [Butler, J. J.; Thome, K. J.; Ramos-Izquierdo, L. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Graziani, L. J.; Meadows, G. A.] SGT, Greenbelt, MD 20770 USA. RP Georgiev, GT (reprint author), Sigma Space Corp, Lanham, MD 20706 USA. EM georgi.t.georgiev@nasa.gov RI Thome, Kurtis/D-7251-2012 NR 6 TC 2 Z9 2 U1 2 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0026-1394 EI 1681-7575 J9 METROLOGIA JI Metrologia PD DEC PY 2014 VL 51 IS 6 BP S319 EP S328 DI 10.1088/0026-1394/51/6/S319 PG 10 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA AU2DJ UT WOS:000345426000012 ER PT J AU Poston, DI McClure, PR Dixon, DD Gibson, MA Mason, LS AF Poston, David I. McClure, Patrick R. Dixon, David D. Gibson, Marc A. Mason, Lee S. TI EXPERIMENTAL DEMONSTRATION OF A HEAT PIPE-STIRLING ENGINE NUCLEAR REACTORLE SO NUCLEAR TECHNOLOGY LA English DT Article DE space nuclear power; heat pipe reactor; fission power system AB Los Alamos National Laboratory and Glenn Research Center with the help of National Security Technologies demonstrated the use of a nuclear fission system as a power source that transferred heat via a water-based heat pipe to a small Stirling engine-based power converter to produce electricity. This experimental setup demonstrated that a small reactor based on heat pipes and Stirling engines is possible and produces a system with well-characterized nuclear feedback between the reactor and the power conversion system. This paper describes the experimental setup, modeling of the system, and results that confirm the basic physics of the experiment. C1 [Poston, David I.; McClure, Patrick R.; Dixon, David D.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Gibson, Marc A.; Mason, Lee S.] Glenn Res Ctr, Natl Aeronaut & Space Adm, Cleveland, OH 44135 USA. RP Poston, DI (reprint author), Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87545 USA. EM poston@lanl.gov NR 11 TC 2 Z9 2 U1 0 U2 3 PU AMER NUCLEAR SOC PI LA GRANGE PK PA 555 N KENSINGTON AVE, LA GRANGE PK, IL 60526 USA SN 0029-5450 EI 1943-7471 J9 NUCL TECHNOL JI Nucl. Technol. PD DEC PY 2014 VL 188 IS 3 BP 229 EP 237 PG 9 WC Nuclear Science & Technology SC Nuclear Science & Technology GA AU3CC UT WOS:000345489400001 ER PT J AU Blaber, E Sato, K Almeida, EAC AF Blaber, Elizabeth Sato, Kevin Almeida, Eduardo A. C. TI Stem Cell Health and Tissue Regeneration in Microgravity SO STEM CELLS AND DEVELOPMENT LA English DT Article ID SKELETAL-MUSCLE ATROPHY; SPACE-FLIGHT; DURATION SPACEFLIGHT; GENE-EXPRESSION; BONE-RESORPTION; PHYSIOLOGY; ADAPTATIONS; METABOLISM; ACTIVATION; EXERCISE AB Exposure to microgravity causes significant mechanical unloading of mammalian tissues, resulting in rapid alterations of their physiology, which poses a significant risk for long-duration manned spaceflight. The immediate degenerative effects of spaceflight we understand best are those studied during short-term low-Earth-orbit experiments, and include rapid microgravity-adaptive bone and muscle loss, loss of cardiovascular capacity, defects in wound and bone fracture healing, and impaired immune function. Over the long-term, exposure to microgravity may cause severe deficits in mammalian stem cell-based tissue regenerative health, including, osteogenesis, hematopoiesis, and lymphopoeisis, as well as cause significant stem cell-based tissue degeneration in amphibian tail and lens regeneration. To address the needs for stem cell and other cell science research on the International Space Station (ISS), NASA has developed the new Bioculture System that will allow investigators to initiate and conduct on-orbit experiments that astronauts will be able to monitor and interact with during the course of cell cultures. This cell culture capability combined with advanced technologies for molecular biology and on-orbit measurement of gene expression (WetLab2) and other tools that are now coming online bring the ISS National Laboratory a step closer to becoming a fully functional space laboratory for advancing space biological sciences. C1 [Blaber, Elizabeth; Sato, Kevin; Almeida, Eduardo A. C.] NASA, Ames Res Ctr, Space Biosci Div, Moffett Field, CA 94035 USA. RP Almeida, EAC (reprint author), NASA, Ames Res Ctr, Space Biosci Div, Moffett Field, CA 94035 USA. EM e.almeida@nasa.gov FU NASA Space Biology Program; NASA Fundamental Space Biology Grants [NNH08ZTT003N, NNH07ZTT001N]; NASA Postdoctoral Program Fellowship FX This work was supported by the NASA Space Biology Program, NASA Fundamental Space Biology Grants NNH08ZTT003N and NNH07ZTT001N to E. Almeida, and NASA Postdoctoral Program Fellowship to E. Blaber. NR 49 TC 7 Z9 7 U1 6 U2 24 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1547-3287 EI 1557-8534 J9 STEM CELLS DEV JI Stem Cells Dev. PD DEC 1 PY 2014 VL 23 SU 1 BP 73 EP 78 DI 10.1089/scd.2014.0408 PG 6 WC Cell & Tissue Engineering; Hematology; Medicine, Research & Experimental; Transplantation SC Cell Biology; Hematology; Research & Experimental Medicine; Transplantation GA AU4FB UT WOS:000345564200019 PM 25457968 ER PT J AU Ashley, T Elmegreen, BG Johnson, M Nidever, DL Simpson, CE Pokhrel, NR AF Ashley, Trisha Elmegreen, Bruce G. Johnson, Megan Nidever, David L. Simpson, Caroline E. Pokhrel, Nau Raj TI THE HI CHRONICLES OF LITTLE THINGS BCDs II: THE ORIGIN OF IC 10's HI STRUCTURE SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: dwarf; galaxies: individual (IC 10); galaxies: star formation ID BLUE COMPACT DWARF; IRREGULAR GALAXY IC-10; STAR-FORMATION; NEARBY GALAXIES; LARGE-SAMPLE; GAS; COLD; ENVIRONMENT; STARBURSTS; KINEMATICS AB In this paper we analyze Very Large Array (VLA) telescope and Green Bank Telescope (GBT) atomic hydrogen (HI) data for the LITTLE THINGS (Local Irregulars That Trace Luminosity Extremes, The HI Nearby Galaxy Survey; https://science.nrao.edu/science/surveys/littlethings) blue compact dwarf galaxy IC 10. The VLA data allow us to study the detailed HI kinematics and morphology of IC 10 at high resolution while the GBT data allow us to search the surrounding area at high sensitivity for tenuous HI. IC 10's HI appears highly disturbed in both the VLA and GBT HI maps with a kinematically distinct northern HI extension, a kinematically distinct southern plume, and several spurs in the VLA data that do not follow the general kinematics of the main disk. We discuss three possible origins of its HI structure and kinematics in detail: a current interaction with a nearby companion, an advanced merger, and accretion of intergalactic medium. We find that IC 10 is most likely an advanced merger or a galaxy undergoing accretion. C1 [Ashley, Trisha; Simpson, Caroline E.; Pokhrel, Nau Raj] Florida Int Univ, Dept Phys, Miami, FL 33199 USA. [Elmegreen, Bruce G.] IBM Corp, TJ Watson Res Ctr, Yorktown Hts, NY 10598 USA. [Johnson, Megan] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Nidever, David L.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Ashley, T (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM trisha.l.ashley@nasa.gov; bge@us.ibm.com; megan.johnson@csiro.au; dnidever@umich.edu; simpsonc@fiu.edu; npokh001@fiu.edu OI Ashley, Trisha/0000-0002-6541-869X FU Florida International University; National Science Foundation [AST-0707563, AST-0707426, AST-0707468, AST 0707835]; University of Michigan FX We thank Se-Heon Oh for allowing us to use his mass estimate of IC 10. We also thank the anonymous referee for helpful comments that improved the presentation of this paper. Trisha Ashley was supported in part by the Dissertation Year Fellowship at Florida International University. This project was funded in part by the National Science Foundation under grant numbers AST-0707563, AST-0707426, AST-0707468, and AST 0707835 to Deidre A. Hunter, Bruce G. Elmegreen, Caroline E. Simpson, and Lisa M. Young. David Nidever was supported by a Dean B. McLaughlin fellowship at the University of Michigan. 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 (NASA). The National Radio Astronomy Observatory is operated by Associated Universities, Inc., under cooperative agreement with the National Science Foundation. NR 51 TC 8 Z9 8 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2014 VL 148 IS 6 AR 130 DI 10.1088/0004-6256/148/6/130 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9BP UT WOS:000345223200027 ER PT J AU Bally, J Ginsburg, A Probst, R Reipurth, B Shirley, YL Stringfellow, GS AF Bally, John Ginsburg, Adam Probst, Ron Reipurth, Bo Shirley, Yancy L. Stringfellow, Guy S. TI OUTFLOWS, DUSTY CORES, AND A BURST OF STAR FORMATION IN THE NORTH AMERICA AND PELICAN NEBULAE SO ASTRONOMICAL JOURNAL LA English DT Article DE Herbig-Haro objects; ISM: individual objects (NGC 7000, IC 5070, LDN 935); ISM: jets and outflows; stars: formation ID FU ORIONIS CANDIDATE; DARK CLOUD; MASSIVE PROTOSTARS; DRIVEN TURBULENCE; CONTINUUM SOURCES; MOLECULAR CLOUDS; MULTIPLE SYSTEMS; BOLOCAM; EMISSION; CATALOG AB We present observations of near-infrared 2.12 mu m molecular hydrogen outflows emerging from 1.1 mm dust continuum clumps in the North America and Pelican Nebula (NAP) complex selected from the Bolocam Galactic Plane Survey (BGPS). Hundreds of individual shocks powered by over 50 outflows from young stars are identified, indicating that the dusty molecular clumps surrounding the NGC 7000/IC 5070/W80 HII region are among the most active sites of ongoing star formation in the solar vicinity. A spectacular X-shaped outflow, MHO 3400, emerges from a young star system embedded in a dense clump more than a parsec from the ionization front associated with the Pelican Nebula (IC 5070). Suspected to be a binary, the source drives a pair of outflows with orientations differing by 80 degrees. Each flow exhibits S-shaped symmetry and multiple shocks indicating a pulsed and precessing jet. The "Gulf of Mexico," located south of the North America Nebula (NGC 7000), contains a dense cluster of molecular hydrogen objects (MHOs), Herbig-Haro (HH) objects, and over 300 young stellar objects (YSOs), indicating a recent burst of star formation. The largest outflow detected thus far in the North America and Pelican Nebula complex, the 1.6 parsec long MHO 3417 flow, emerges from a 500 M-circle dot BGPS clump and may be powered by a forming massive star. Several prominent outflows such as MHO 3427 appear to be powered by highly embedded YSOs only visible lambda > 70 mu m. An "activity index" formed by dividing the number of shocks by the mass of the cloud containing their source stars is used to estimate the relative evolutionary states of Bolocam clumps. Outflows can be used as indicators of the evolutionary state of clumps detected in millimeter and submillimeter dust continuum surveys. C1 [Bally, John] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Ginsburg, Adam] European So Observ, D-85748 Garching, Germany. [Probst, Ron] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Reipurth, Bo] Univ Hawaii Manoa, Inst Astron, Hilo, HI 96720 USA. [Reipurth, Bo] Univ Hawaii Manoa, NASA, Astrobiol Inst, Hilo, HI 96720 USA. [Shirley, Yancy L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Stringfellow, Guy S.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. RP Bally, J (reprint author), Univ Colorado, Dept Astrophys & Planetary Sci, UCB 389, Boulder, CO 80309 USA. EM John.Bally@colorado.edu; aginsburg@eso.org; probst@noao.edu; reipurth@ifa.hawaii.edu; yshirley@as.arizona.edu; Guy.Stringfellow@colorado.edu OI Ginsburg, Adam/0000-0001-6431-9633 FU NSF [AST 0708403, AST 1009847]; National Aeronautics and Space Administration [NNA09DA77A]; NASA; National Science Foundation FX This research was supported by NSF grant Nos. AST 0708403 (The Bolocam Millimeter Wavelength Survey of the Northern Galactic Plane) and AST 1009847 (Formation of Galactic massive Stars and Star Clusters). B. R. acknowledges support by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement No. NNA09DA77A issued through the Office of Space Science. G. S. S. is supported through grants received from NASA. This project made use of ds9 (http://hea-www.harvard.edu/RD/ds9/site/Home.html). This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. Observations reported here were obtained at the Kitt Peak National Observatory, which is operated by the National Optical Astronomy Observatories and AURA, Inc. with support from the National Science Foundation. We thank an anonymous referee for a very thorough reading of the manuscript and useful suggestions that improved the paper and figures. NR 46 TC 3 Z9 3 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2014 VL 148 IS 6 AR 120 DI 10.1088/0004-6256/148/6/120 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9BP UT WOS:000345223200017 ER PT J AU Benedict, GF Tanner, AM Cargile, PA Ciardi, DR AF Benedict, G. Fritz Tanner, Angelle M. Cargile, Phillip A. Ciardi, David R. TI A TECHNIQUE TO DERIVE IMPROVED PROPER MOTIONS FOR KEPLER OBJECTS OF INTEREST SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; planetary systems; proper motions; stars: distances ID HUBBLE-SPACE-TELESCOPE; CANDIDATE EXOPLANET COMPANION; PRECISION RADIAL-VELOCITIES; GUIDANCE SENSOR 3; SKY SURVEY 2MASS; INTERFEROMETRIC ASTROMETRY; PLANET SYSTEMS; PARALLAXES; SELECTION; CATALOG AB We outline an approach yielding proper motions with higher precision than exists in present catalogs for a sample of stars in the Kepler field. To increase proper-motion precision, we combine first-moment centroids of Kepler pixel data from a single season with existing catalog positions and proper motions. We use this astrometry to produce improved reduced-proper-motion diagrams, analogous to a Hertzsprung-Russell (H-R) diagram, for stars identified as Kepler objects of interest. The more precise the relative proper motions, the better the discrimination between stellar luminosity classes. Using UCAC4 and PPMXL epoch 2000 positions (and proper motions from those catalogs as quasi-Bayesian priors), astrometry for a single test Channel (21) and Season (0) spanning 2 yr yields proper motions with an average per-coordinate proper-motion error of 1.0 mas yr(-1), which is over a factor of three better than existing catalogs. We apply a mapping between a reduced-proper-motion diagram and an H-R diagram, both constructed using Hubble Space Telescope parallaxes and proper motions, to estimate Kepler object of interest K-band absolute magnitudes. The techniques discussed apply to any future small-field astrometry as well as to the rest of the Kepler field. C1 [Benedict, G. Fritz] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Tanner, Angelle M.] Mississippi State Univ, Dept Phys & Astron, Starkville, MS 39762 USA. [Cargile, Phillip A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Cargile, Phillip A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. RP Benedict, GF (reprint author), Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. EM fritz@astro.as.utexas.edu OI Ciardi, David/0000-0002-5741-3047 FU NASA Science Mission directorate; NASA contract [NAS5-26555]; NASA Office of Space Science [NNX13AC07G]; NASA [NNX13AC22G, NNX12AF76G]; NSF Astronomy and Astrophysics grant [AST-1109612]; NASA; NSF; National Aeronautics and Space Administration under the Exoplanet Exploration Program; W. M. Keck Foundation FX This paper includes data collected by the Kepler mission. Funding for Kepler is provided by the NASA Science Mission directorate. All of the Kepler data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute (STScI). 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 NNX13AC07G and by other grants and contracts. Direct support for this work was provided to G. F. B. by NASA through grant NNX13AC22G. Direct support for this work was provided to A. M. T. by NASA through grant NNX12AF76G. P. A. C. acknowledges NSF Astronomy and Astrophysics grant AST-1109612. 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 NASA and the NSF. This research has made use of the SIMBAD and Vizier databases and Aladin, operated at CDS, Strasbourg, France; the NASA/IPAC Extra-galactic Database (NED) which is operated by JPL, California Institute of Technology, under contract with the NASA; and NASA's Astrophysics Data System Abstract Service. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. G. F. B. thanks Bill Jefferys, Tom Harrison, and Barbara McArthur who, over many years, contributed to the techniques reported in this paper. G. F. B. and A. M. T. thank Dave Monet for several stimulating discussions that should have warned us off from this project, but did not. G. F. B. thanks Debra Winegarten for her able assistance, allowing progress on this project. We thank an anonymous referee for a thorough, careful, and useful review which materially improved the final paper. NR 49 TC 4 Z9 4 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2014 VL 148 IS 6 AR 108 DI 10.1088/0004-6256/148/6/108 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9BP UT WOS:000345223200005 ER PT J AU Gunther, HM Cody, AM Covey, KR Hillenbrand, LA Plavchan, P Poppenhaeger, K Rebull, LM Stauffer, JR Wolk, SJ Allen, L Bayo, A Gutermuth, RA Hora, JL Meng, HYA Morales-Calderon, M Parks, JR Song, I AF Guenther, H. M. Cody, A. M. Covey, K. R. Hillenbrand, L. A. Plavchan, P. Poppenhaeger, K. Rebull, L. M. Stauffer, J. R. Wolk, S. J. Allen, L. Bayo, A. Gutermuth, R. A. Hora, J. L. Meng, H. Y. A. Morales-Calderon, M. Parks, J. R. Song, Inseok TI YSOVAR: MID-INFRARED VARIABILITY IN THE STAR-FORMING REGION LYNDS 1688 SO ASTRONOMICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars: formation; stars: pre-main sequence; stars: protostars; stars: variables: T Tauri, Herbig Ae/Be ID T-TAURI-STARS; YOUNG STELLAR OBJECTS; MAIN-SEQUENCE STARS; RHO-OPHIUCHI CLOUD; INFRARED PHOTOMETRIC VARIABILITY; SPITZER-SPACE-TELESCOPE; INITIAL MASS FUNCTION; ORION NEBULA CLUSTER; BROWN DWARF DISKS; X-RAY AB The emission from young stellar objects (YSOs) in the mid-infrared (mid-IR) is dominated by the inner rim of their circumstellar disks. We present IR data from the Young Stellar Object VARiability (YSOVAR) survey of similar to 800 objects in the direction of the Lynds 1688 (L1688) star-forming region over four visibility windows spanning 1.6 yr using the Spitzer Space Telescope in its warm mission phase. Among all light curves, 57 sources are cluster members identified based on their spectral energy distribution and X-ray emission. Almost all cluster members show significant variability. The amplitude of the variability is larger in more embedded YSOs. Ten out of 57 cluster members have periodic variations in the light curves with periods typically between three and seven days, but even for those sources, significant variability in addition to the periodic signal can be seen. No period is stable over 1.6 yr. Nonperiodic light curves often still show a preferred timescale of variability that is longer for more embedded sources. About half of all sources exhibit redder colors in a fainter state. This is compatible with time-variable absorption toward the YSO. The other half becomes bluer when fainter. These colors can only be explained with significant changes in the structure of the inner disk. No relation between mid-IR variability and stellar effective temperature or X-ray spectrum is found. C1 [Guenther, H. M.; Poppenhaeger, K.; Wolk, S. J.; Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cody, A. M.; Rebull, L. M.; Stauffer, J. R.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Covey, K. R.] Lowell Observ, Flagstaff, AZ 86001 USA. [Hillenbrand, L. A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Plavchan, P.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Allen, L.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Bayo, A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Bayo, A.] Univ Valparaiso, Fac Ciencias, Dept Fis & Astron, Valparaiso, Chile. [Gutermuth, R. A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Meng, H. Y. A.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Meng, H. Y. A.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Morales-Calderon, M.] INTA CSIC, Ctr Astrobiol, E-28691 Villanueva De La Canada, Spain. [Parks, J. R.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Song, Inseok] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. RP Gunther, HM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hguenther@cfa.harvard.edu RI Morales-Calderon, Maria/C-8384-2017; OI Morales-Calderon, Maria/0000-0001-9526-9499; Poppenhaeger, Katja/0000-0003-1231-2194; Gunther, Hans Moritz/0000-0003-4243-2840; Rebull, Luisa/0000-0001-6381-515X; Covey, Kevin/0000-0001-6914-7797; Meng, Huan/0000-0003-0006-7937 FU NASA; National Aeronautics and Space Administration; National Science Foundation; Spitzer [1490851]; IPAC Visiting Graduate Fellowship program at Caltech/IPAC; JPL Research and Technology Development and Exoplanet Exploration programs; NASA ADAP [NNX11AD14G, NNX13AF08G]; Caltech/JPL awards [1373081, 1424329, 1440160]; Spitzer Space Telescope observing programs; NASA [NAS8-03060] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This research made use of Astropy, a community-developed core Python package for astronomy (The Astropy Collaboration et al. 2013). This research has made use of the SIMBAD database and the VizieR catalogue access tool (Ochsenbein et al. 2000), both operated at CDS, Strasbourg, France, and 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. H. M. G. acknowledges Spitzer grant 1490851. H.Y.A.M. and P. P. acknowledge support by the IPAC Visiting Graduate Fellowship program at Caltech/IPAC. P. P. also acknowledges the JPL Research and Technology Development and Exoplanet Exploration programs. R. A. G. gratefully acknowledges funding support from NASA ADAP grants NNX11AD14G and NNX13AF08G and Caltech/JPL awards 1373081, 1424329, and 1440160 in support of Spitzer Space Telescope observing programs. S.J.W. was supported by NASA contract NAS8-03060. NR 109 TC 15 Z9 15 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2014 VL 148 IS 6 AR 122 DI 10.1088/0004-6256/148/6/122 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9BP UT WOS:000345223200019 ER PT J AU Sagiv, I Gal-Yam, A Ofek, EO Waxman, E Aharonson, O Kulkarni, SR Nakar, E Maoz, D Trakhtenbrot, B Gottesman, O Phinney, ES Topaz, J Beichman, C Murthy, J Worden, SP AF Sagiv, I. Gal-Yam, A. Ofek, E. O. Waxman, E. Aharonson, O. Kulkarni, S. R. Nakar, E. Maoz, D. Trakhtenbrot, B. Gottesman, O. Phinney, E. S. Topaz, J. Beichman, C. Murthy, J. Worden, S. P. TI SCIENCE WITH A WIDE-FIELD UV TRANSIENT EXPLORER (vol 147, pg 79, 2014) SO ASTRONOMICAL JOURNAL LA English DT Correction C1 [Sagiv, I.; Gal-Yam, A.; Ofek, E. O.; Waxman, E.; Trakhtenbrot, B.; Gottesman, O.; Topaz, J.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Aharonson, O.] Weizmann Inst Sci, Helen Kimmel Ctr Planetary Sci, IL-76100 Rehovot, Israel. [Kulkarni, S. R.; Phinney, E. S.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Nakar, E.; Maoz, D.] Tel Aviv Univ, Sch Phys & Astron, IL-93387 Tel Aviv, Israel. [Beichman, C.] CALTECH, Div Geophys & Planetary Sci, Pasadena, CA 91105 USA. [Murthy, J.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Worden, S. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Sagiv, I (reprint author), Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. NR 1 TC 0 Z9 0 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2014 VL 148 IS 6 AR 138 DI 10.1088/0004-6256/148/6/138 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9BP UT WOS:000345223200034 ER PT J AU Seale, JP Meixner, M Sewilo, M Babler, B Engelbracht, CW Gordon, K Hony, S Misselt, K Montiel, E Okumura, K Panuzzo, P Roman-Duval, J Sauvage, M Boyer, ML Chen, CHR Indebetouw, R Matsuura, M Oliveira, JM Srinivasan, S van Loon, JT Whitney, B Woods, PM AF Seale, Jonathan P. Meixner, Margaret Sewilo, Marta Babler, Brian Engelbracht, Charles W. Gordon, Karl Hony, Sacha Misselt, Karl Montiel, Edward Okumura, Koryo Panuzzo, Pasquale Roman-Duval, Julia Sauvage, Marc Boyer, Martha L. Chen, C. -H. Rosie Indebetouw, Remy Matsuura, Mikako Oliveira, Joana M. Srinivasan, Sundar van Loon, Jacco Th. Whitney, Barbara Woods, Paul M. TI HERschel KEY PROGRAM HERITAGE: A FAR-INFRARED SOURCE CATALOG FOR THE MAGELLANIC CLOUDS SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; galaxies: dwarf; infrared: stars; Magellanic Clouds; stars: formation; stars: pre-main sequence ID YOUNG STELLAR OBJECTS; ACTIVE GALACTIC NUCLEI; GALAXY EVOLUTION SAGE; STAR-FORMATION; SPITZER SURVEY; EVOLVED STARS; AGB-STARS; INTERSTELLAR-MEDIUM; PHYSICAL CONDITIONS; INITIAL HIGHLIGHTS AB Observations from the HERschel Inventory of the Agents of Galaxy Evolution (HERITAGE) have been used to identify dusty populations of sources in the Large and Small Magellanic Clouds (LMC and SMC). We conducted the study using the HERITAGE catalogs of point sources available from the Herschel Science Center from both the Photodetector Array Camera and Spectrometer (PACS; 100 and 160 mu m) and Spectral and Photometric Imaging Receiver (SPIRE; 250, 350, and 500 mu m) cameras. These catalogs are matched to each other to create a Herschel band-merged catalog and then further matched to archival Spitzer IRAC and MIPS catalogs from the Spitzer Surveying the Agents of Galaxy Evolution (SAGE) and SAGE-SMC surveys to create single mid- to far-infrared (far-IR) point source catalogs that span the wavelength range from 3.6 to 500 mu m. There are 35,322 unique sources in the LMC and 7503 in the SMC. To be bright in the FIR, a source must be very dusty, and so the sources in the HERITAGE catalogs represent the dustiest populations of sources. The brightest HERITAGE sources are dominated by young stellar objects (YSOs), and the dimmest by background galaxies. We identify the sources most likely to be background galaxies by first considering their morphology (distant galaxies are point-like at the resolution of Herschel) and then comparing the flux distribution to that of the Herschel Astrophysical Terahertz Large Area Survey (ATLAS) survey of galaxies. We find a total of 9745 background galaxy candidates in the LMC HERITAGE images and 5111 in the SMC images, in agreement with the number predicted by extrapolating from the ATLAS flux distribution. The majority of the Magellanic Cloud-residing sources are either very young, embedded forming stars or dusty clumps of the interstellar medium. Using the presence of 24 mu m emission as a tracer of star formation, we identify 3518 YSO candidates in the LMC and 663 in the SMC. There are far fewer far-IR bright YSOs in the SMC than the LMC due to both the SMC's smaller size and its lower dust content. The YSO candidate lists may be contaminated at low flux levels by background galaxies, and so we differentiate between sources with a high ("probable") and moderate ("possible") likelihood of being a YSO. There are 2493/425 probable YSO candidates in the LMC/SMC. Approximately 73% of the Herschel YSO candidates are newly identified in the LMC, and 35% in the SMC. We further identify a small population of dusty objects in the late stages of stellar evolution including extreme and post-asymptotic giant branch, planetary nebulae, and supernova remnants. These populations are identified by matching the HERITAGE catalogs to lists of previously identified objects in the literature. Approximately half of the LMC sources and one quarter of the SMC sources are too faint to obtain accurate ample FIR photometry and are unclassified. C1 [Seale, Jonathan P.; Meixner, Margaret; Sewilo, Marta] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Seale, Jonathan P.; Meixner, Margaret; Gordon, Karl; Roman-Duval, Julia] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Babler, Brian; Whitney, Barbara] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Engelbracht, Charles W.; Misselt, Karl; Montiel, Edward] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Engelbracht, Charles W.] Raytheon Co, Tucson, AZ 85756 USA. [Hony, Sacha; Okumura, Koryo; Panuzzo, Pasquale; Sauvage, Marc] CEA, Lab AIM, Irfu SAp, F-91191 Gif Sur Yvette, France. [Panuzzo, Pasquale] CNRS, Observ Paris, Lab GEPI, F-92195 Meudon, France. [Montiel, Edward] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Boyer, Martha L.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Chen, C. -H. Rosie] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Indebetouw, Remy] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Indebetouw, Remy] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Matsuura, Mikako] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Oliveira, Joana M.; van Loon, Jacco Th.] Keele Univ, Lennard Jones Labs, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. [Srinivasan, Sundar] UPMC CNRS UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Srinivasan, Sundar] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Woods, Paul M.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. RP Seale, JP (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 366 Bloomberg Ctr,3400 N Charles St, Baltimore, MD 21218 USA. RI Woods, Paul/E-6926-2011 OI Woods, Paul/0000-0003-4340-3590 FU NASA Herschel Science Center, JPL contracts [1381522, 1381650, 1350371]; European Space Agency (ESA); PACS team; Herschel Science Center; NASA Herschel Science Center; PACS instrument control center; NASA ADAP award [NNX11AG50G]; SPIRE team; SPIRE instrument control center FX The authors thank the anonymous referee for comments that improved the quality of the paper. This work makes use of data collected by the Herschel Space Observatory. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. HIPE is a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS, and SPIRE consortia. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. We acknowledge financial support from the NASA Herschel Science Center, JPL contracts #1381522, #1381650, #1350371. We thank the contributions and support from the European Space Agency (ESA), the PACS and SPIRE teams, the Herschel Science Center (esp. L. Conversi), and the NASA Herschel Science Center (esp. A. Barbar and R. Paladini) and the PACS and SPIRE instrument control centers (esp. George Bendo), without which none of this work would be possible. M. Sewilo acknowledges financial support from the NASA ADAP award NNX11AG50G. NR 85 TC 11 Z9 11 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2014 VL 148 IS 6 AR 124 DI 10.1088/0004-6256/148/6/124 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9BP UT WOS:000345223200021 ER PT J AU Aartsen, MG Ackermann, M Adams, J Aguilar, JA Ahlers, M Ahrens, M Altmann, D Anderson, T Arguelles, C Arlen, TC Auffenberg, J Bai, X Barwick, SW Baum, V Beatty, JJ Tjus, JB Becker, KH BenZvi, S Berghaus, P Berley, D Bernardini, E Bernhard, A Besson, DZ Binder, G Bindig, D Bissok, M Blaufuss, E Blumenthal, J Boersma, DJ Bohm, C Bos, F Bose, D Boser, S Botner, O Brayeur, L Bretz, HP Brown, AM Casey, J Casier, M Cheung, E Chirkin, D Christov, A Christy, B Clark, K Classen, L Clevermann, F Coenders, S Cowen, DF Silva, AHC Danninger, M Daughhetee, J Davis, JC Day, M de Andre, JPAM De Clercq, C De Ridder, S Desiati, P de Vries, KD de With, M DeYoung, T Diaz-Velez, JC Dunkman, M Eagan, R Eberhardt, B Eichmann, B Eisch, J Euler, S Evenson, PA Fadiran, O Fazely, AR Fedynitch, A Feintzeig, J Felde, J Feusels, T Filimonov, K Finley, C Fischer-Wasels, T Flis, S Franckowiak, A Frantzen, K Fuchs, T Gaisser, TK Gallagher, J Gerhardt, L Gier, D Gladstone, L Glusenkamp, T Goldschmidt, A Golup, G Gonzalez, JG Goodman, JA Gora, D Grandmont, DT Grant, D Gretskov, P Groh, JC Gross, A Ha, C Haack, C Ismail, AH Hallen, P Hallgren, A Halzen, F Hanson, K Hebecker, D Heereman, D Heinen, D Helbing, K Hellauer, R Hellwig, D Hickford, S Hill, GC Hoffman, KD Hoffmann, R Homeier, A Hoshina, K Huang, F Huelsnitz, W Hulth, PO Hultqvist, K Hussain, S Ishihara, A Jacobi, E Jacobsen, J Jagielski, K Japaridze, GS Jero, K Jlelati, O Jurkovic, M Kaminsky, B Kappes, A Karg, T Karle, A Kauer, M Kelley, JL Kheirandish, A Kiryluk, J Klas, J Klein, SR Kohne, JH Kohnen, G Kolanoski, H Koob, A Kopke, L Kopper, C Kopper, S Koskinen, DJ Kowalski, M Kriesten, A Krings, K Kroll, G Kroll, M Kunnen, J Kurahashi, N Kuwabara, T Labare, M Larsen, DT Larson, MJ Lesiak-Bzdak, M Leuermann, M Leute, J Lunemann, J Macias, O Madsen, J Maggi, G Maruyama, R Mase, K Matis, HS Maunu, R McNally, F Meagher, K Medici, M Meli, A Meures, T Miarecki, S Middell, E Middlemas, E Milke, N Miller, J Mohrmann, L Montaruli, T Morse, R Nahnhauer, R Naumann, U Niederhausen, H Nowicki, SC Nygren, DR Obertacke, A Odrowski, S Olivas, A Omairat, A O'Murchadha, A Palczewski, T Paul, L Penek, O Pepper, JA Heros, CPD Pfendner, C Pieloth, D Pinat, E Posselt, J Price, PB Przybylski, GT Putz, J Quinnan, M Radel, L Rameez, M Rawlins, K Redl, P Rees, I Reimann, R Resconi, E Rhode, W Richman, M Riedel, B Robertson, S Rodrigues, JP Rongen, M Rott, C Ruhe, T Ruzybayev, B Ryckbosch, D Saba, SM Sander, HG Sandroos, J Santander, M Sarkar, S Schatto, K Scheriau, F Schmidt, T Schmitz, M Schoenen, S Schoneberg, S Schonwald, A Schukraft, A Schulte, L Schulz, O Seckel, D Sestayo, Y Seunarine, S Shanidze, R Sheremata, C Smith, MWE Soldin, D Spiczak, GM Spiering, C Stamatikos, M Stanev, T Stanisha, NA Stasik, A Stezelberger, T Stokstad, RG Stossl, A Strahler, EA Strom, R Strotjohann, NL Sullivan, GW Taavola, H Taboada, I Tamburro, A Tepe, A Ter-Antonyan, S Terliuk, A Tesic, G Tilav, S Toale, PA Tobin, MN Tosi, D Tselengidou, M Unger, E Usner, M Vallecorsa, S van Eijndhoven, N Vandenbroucke, J van Santen, J Vehring, M Voge, M Vraeghe, M Walck, C Wallraff, M Weaver, C Wellons, M Wendt, C Westerhoff, S Whelan, BJ Whitehorn, N Wichary, C Wiebe, K Wiebusch, CH Williams, DR Wissing, H Wolf, M Wood, TR Woschnagg, K Xu, DL Xu, XW Yanez, JP Yodh, G Yoshida, S Zarzhitsky, P Ziemann, J Zierke, S Zoll, M AF Aartsen, M. G. Ackermann, M. Adams, J. Aguilar, J. A. Ahlers, M. Ahrens, M. Altmann, D. Anderson, T. Arguelles, C. Arlen, T. C. Auffenberg, J. Bai, X. Barwick, S. W. Baum, V. Beatty, J. J. Tjus, J. Becker Becker, K. -H. BenZvi, S. Berghaus, P. Berley, D. Bernardini, E. Bernhard, A. Besson, D. Z. Binder, G. Bindig, D. Bissok, M. Blaufuss, E. Blumenthal, J. Boersma, D. J. Bohm, C. Bos, F. Bose, D. Boeser, S. Botner, O. Brayeur, L. Bretz, H. -P. Brown, A. M. Casey, J. Casier, M. Cheung, E. Chirkin, D. Christov, A. Christy, B. Clark, K. Classen, L. Clevermann, F. Coenders, S. Cowen, D. F. Silva, A. H. Cruz Danninger, M. Daughhetee, J. Davis, J. C. Day, M. de Andre, J. P. A. M. De Clercq, C. De Ridder, S. Desiati, P. de Vries, K. D. de With, M. DeYoung, T. Diaz-Velez, J. C. Dunkman, M. Eagan, R. Eberhardt, B. Eichmann, B. Eisch, J. Euler, S. Evenson, P. A. Fadiran, O. Fazely, A. R. Fedynitch, A. Feintzeig, J. Felde, J. Feusels, T. Filimonov, K. Finley, C. Fischer-Wasels, T. Flis, S. Franckowiak, A. Frantzen, K. Fuchs, T. Gaisser, T. K. Gallagher, J. Gerhardt, L. Gier, D. Gladstone, L. Gluesenkamp, T. Goldschmidt, A. Golup, G. Gonzalez, J. G. Goodman, J. A. Gora, D. Grandmont, D. T. Grant, D. Gretskov, P. Groh, J. C. Gross, A. Ha, C. Haack, C. Ismail, A. Haj Hallen, P. Hallgren, A. Halzen, F. Hanson, K. Hebecker, D. Heereman, D. Heinen, D. Helbing, K. Hellauer, R. Hellwig, D. Hickford, S. Hill, G. C. Hoffman, K. D. Hoffmann, R. Homeier, A. Hoshina, K. Huang, F. Huelsnitz, W. Hulth, P. O. Hultqvist, K. Hussain, S. Ishihara, A. Jacobi, E. Jacobsen, J. Jagielski, K. Japaridze, G. S. Jero, K. Jlelati, O. Jurkovic, M. Kaminsky, B. Kappes, A. Karg, T. Karle, A. Kauer, M. Kelley, J. L. Kheirandish, A. Kiryluk, J. Klaes, J. Klein, S. R. Koehne, J. -H. Kohnen, G. Kolanoski, H. Koob, A. Koepke, L. Kopper, C. Kopper, S. Koskinen, D. J. Kowalski, M. Kriesten, A. Krings, K. Kroll, G. Kroll, M. Kunnen, J. Kurahashi, N. Kuwabara, T. Labare, M. Larsen, D. T. Larson, M. J. Lesiak-Bzdak, M. Leuermann, M. Leute, J. Luenemann, J. Macias, O. Madsen, J. Maggi, G. Maruyama, R. Mase, K. Matis, H. S. Maunu, R. McNally, F. Meagher, K. Medici, M. Meli, A. Meures, T. Miarecki, S. Middell, E. Middlemas, E. Milke, N. Miller, J. Mohrmann, L. Montaruli, T. Morse, R. Nahnhauer, R. Naumann, U. Niederhausen, H. Nowicki, S. C. Nygren, D. R. Obertacke, A. Odrowski, S. Olivas, A. Omairat, A. O'Murchadha, A. Palczewski, T. Paul, L. Penek, O. Pepper, J. A. Heros, C. Perez De Los Pfendner, C. Pieloth, D. Pinat, E. Posselt, J. Price, P. B. Przybylski, G. T. Puetz, J. Quinnan, M. Raedel, L. Rameez, M. Rawlins, K. Redl, P. Rees, I. Reimann, R. Resconi, E. Rhode, W. Richman, M. Riedel, B. Robertson, S. Rodrigues, J. P. Rongen, M. Rott, C. Ruhe, T. Ruzybayev, B. Ryckbosch, D. Saba, S. M. Sander, H. -G. Sandroos, J. Santander, M. Sarkar, S. Schatto, K. Scheriau, F. Schmidt, T. Schmitz, M. Schoenen, S. Schoeneberg, S. Schoenwald, A. Schukraft, A. Schulte, L. Schulz, O. Seckel, D. Sestayo, Y. Seunarine, S. Shanidze, R. Sheremata, C. Smith, M. W. E. Soldin, D. Spiczak, G. M. Spiering, C. Stamatikos, M. Stanev, T. Stanisha, N. A. Stasik, A. Stezelberger, T. Stokstad, R. G. Stoessl, A. Strahler, E. A. Strom, R. Strotjohann, N. L. Sullivan, G. W. Taavola, H. Taboada, I. Tamburro, A. Tepe, A. Ter-Antonyan, S. Terliuk, A. Tesic, G. Tilav, S. Toale, P. A. Tobin, M. N. Tosi, D. Tselengidou, M. Unger, E. Usner, M. Vallecorsa, S. van Eijndhoven, N. Vandenbroucke, J. van Santen, J. Vehring, M. Voge, M. Vraeghe, M. Walck, C. Wallraff, M. Weaver, Ch. Wellons, M. Wendt, C. Westerhoff, S. Whelan, B. J. Whitehorn, N. Wichary, C. Wiebe, K. Wiebusch, C. H. Williams, D. R. Wissing, H. Wolf, M. Wood, T. R. Woschnagg, K. Xu, D. L. Xu, X. W. Yanez, J. P. Yodh, G. Yoshida, S. Zarzhitsky, P. Ziemann, J. Zierke, S. Zoll, M. CA IceCube Collaboration TI SEARCHES FOR EXTENDED AND POINT-LIKE NEUTRINO SOURCES WITH FOUR YEARS OF ICECUBE DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE astroparticle physics; galaxies: active; galaxies: clusters: general; galaxies: starburst; ISM: supernova remnants; neutrinos ID HIGH-ENERGY NEUTRINOS; ACTIVE GALACTIC NUCLEI; GAMMA-RAY EMISSION; SUPERNOVA-REMNANTS; PARTICLE-ACCELERATION; COSMIC-RAYS; FERMI LAT; TELESCOPE; ASTRONOMY; MILAGRO AB We present results on searches for point-like sources of neutrinos using four years of IceCube data, including the first year of data from the completed 86 string detector. The total livetime of the combined data set is 1373 days. For an E-2 spectrum, the observed 90% C. L. flux upper limits are similar to 10(-12) TeV-1 cm(-2) s(-1) for energies between 1 TeV and 1 PeV in the northern sky and similar to 10(-11) TeV-1 cm(-2) s(-1) for energies between 100 TeV and 100 PeV in the southern sky. This represents a 40% improvement compared to previous publications, resulting from both the additional year of data and the introduction of improved reconstructions. In addition, we present the first results from an all-sky search for extended sources of neutrinos. We update the results of searches for neutrino emission from stacked catalogs of sources and test five new catalogs; two of Galactic supernova remnants and three of active galactic nuclei. In all cases, the data are compatible with the background-only hypothesis, and upper limits on the flux of muon neutrinos are reported for the sources considered. C1 [Aartsen, M. G.; Hill, G. C.; Robertson, S.; Whelan, B. J.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. [Ackermann, M.; Berghaus, P.; Bernardini, E.; Bretz, H. -P.; Silva, A. H. Cruz; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Kaminsky, B.; Karg, T.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Schoenwald, A.; Shanidze, R.; Spiering, C.; Stoessl, A.; Terliuk, A.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany. [Adams, J.; Hickford, S.; Macias, O.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [Aguilar, J. A.; Christov, A.; Montaruli, T.; Rameez, M.; Vallecorsa, S.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland. [Ahlers, M.; Arguelles, C.; BenZvi, S.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; Kopper, C.; Kurahashi, N.; Larsen, D. T.; Maruyama, R.; McNally, F.; Middlemas, E.; Morse, R.; Rees, I.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Tobin, M. 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R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Grandmont, D. T.; Grant, D.; Nowicki, S. C.; Odrowski, S.; Sheremata, C.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Hanson, K.; Heereman, D.; Meures, T.; O'Murchadha, A.; Pinat, E.] Univ Libre Bruxelles, Fac Sci, B-1050 Brussels, Belgium. [Hoshina, K.] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, Tokyo 1130032, Japan. [Ishihara, A.; Mase, K.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan. [Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA. [Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Kohnen, G.] Univ Mons, B-7000 Mons, Belgium. [Koskinen, D. J.; Larson, M. J.; Medici, M.; Sandroos, J.; Sarkar, S.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Madsen, J.; Seunarine, S.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA. [Palczewski, T.; Pepper, J. A.; Toale, P. A.; Williams, D. R.; Xu, D. L.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. [Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA. [Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England. [Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Aartsen, MG (reprint author), Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. RI Koskinen, David/G-3236-2014; Auffenberg, Jan/D-3954-2014; Maruyama, Reina/A-1064-2013; Aguilar Sanchez, Juan Antonio/H-4467-2015; Tjus, Julia/G-8145-2012; Sarkar, Subir/G-5978-2011; Beatty, James/D-9310-2011; Wiebusch, Christopher/G-6490-2012; Taavola, Henric/B-4497-2011; OI Schukraft, Anne/0000-0002-9112-5479; Larsen, Dag Toppe/0000-0002-9898-2174; Koskinen, David/0000-0002-0514-5917; Auffenberg, Jan/0000-0002-1185-9094; Maruyama, Reina/0000-0003-2794-512X; Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952; Wiebusch, Christopher/0000-0002-6418-3008; Rott, Carsten/0000-0002-6958-6033; Ter-Antonyan, Samvel/0000-0002-5788-1369; Groh, John/0000-0001-9880-3634; Taavola, Henric/0000-0002-2604-2810; Perez de los Heros, Carlos/0000-0002-2084-5866; Strotjohann, Nora Linn/0000-0002-4667-6730; Arguelles Delgado, Carlos/0000-0003-4186-4182 FU U. S. National Science Foundation-Office of Polar Programs; U. S. National Science Foundation-Physics Division; University of Wisconsin Alumni Research Foundation; Grid Laboratory of Wisconsin (GLOW); University of Wisconsin-Madison; Open Science Grid (OSG); U.S. Department of Energy; National Energy Research Scientific Computing Center; Louisiana Optical Network Initiative (LONI); Natural Sciences and Engineering Research Council of Canada; West-Grid and Compute/Calcul Canada; Swedish Research Council; Swedish Polar Research Secretariat; Swedish National Infrastructure for Computing (SNIC); Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Helmholtz Alliance for Astroparticle Physics (HAP); Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO Odysseus programme; Flanders Institute to encourage scientific and technological research in industry (IWT); Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF); Danish National Research Foundation, Denmark (DNRF) FX We acknowledge the support from the following agencies: U. S. National Science Foundation-Office of Polar Programs, U.S. National Science Foundation-Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; Natural Sciences and Engineering Research Council of Canada, West-Grid and Compute/Calcul Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF); Danish National Research Foundation, Denmark (DNRF). NR 70 TC 49 Z9 50 U1 1 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 DEC 1 PY 2014 VL 796 IS 2 AR 109 DI 10.1088/0004-637X/796/2/109 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT4AI UT WOS:000344878900038 ER PT J AU Abeysekara, AU Alfaro, R Alvarez, C Alvarez, JD Arceo, R Arteaga-Velazquez, JC Solares, HAA Barber, AS Baughman, BM Bautista-Elivar, N Belmont, E BenZvi, SY Berley, D Rosales, MB Braun, J Caballero-Mora, KS Carraminana, A Castillo, M Cotti, U Cotzomi, J De La Fuente, E De Leon, C DeYoung, T Hernandez, RD Diaz-Velez, JC Dingus, BL DuVernois, MA Ellsworth, RW Fiorino, DW Fraija, N Galindo, A Garfias, F Gonzalez, MM Goodman, JA Gussert, M Hampel-Arias, Z Harding, JP Huntemeyer, P Hui, CM Imran, A Iriarte, A Karn, P Kieda, D Kunde, GJ Lara, A Lauer, RJ Lee, WH Lennarz, D Vargas, HL Linnemann, JT Longo, M Luna-Garcia, R Malone, K Marinelli, A Marinelli, SS Martinez, H Martinez, O Martinez-Castro, J Matthews, JAJ McEnery, J Torres, EM Miranda-Romagnoli, P Moreno, E Mostafa, M Nellen, L Newbold, M Noriega-Papaqui, R Oceguera-Becerra, T Patricelli, B Pelayo, R Perez-Perez, EG Pretz, J Riviere, C Rosa-Gonzalez, D Ruiz-Velasco, E Ryan, J Salazar, H Greus, FS Sandoval, A Schneider, M Sinnis, G Smith, AJ Woodle, KS Springer, RW Taboada, I Toale, PA Tollefson, K Torres, I Ukwatta, TN Villasenor, L Weisgarber, T Westerhoff, S Wisher, IG Wood, J Yodh, GB Younk, PW Zaborov, D Zepeda, A Zhou, H AF Abeysekara, A. U. Alfaro, R. Alvarez, C. Alvarez, J. D. Arceo, R. Arteaga-Velazquez, J. C. Solares, H. A. Ayala Barber, A. S. Baughman, B. M. Bautista-Elivar, N. Belmont, E. BenZvi, S. Y. Berley, D. Bonilla Rosales, M. Braun, J. Caballero-Mora, K. S. Carraminana, A. Castillo, M. Cotti, U. Cotzomi, J. De La Fuente, E. De Leon, C. DeYoung, T. Diaz Hernandez, R. Diaz-Velez, J. C. Dingus, B. L. DuVernois, M. A. Ellsworth, R. W. Fiorino, D. W. Fraija, N. Galindo, A. Garfias, F. Gonzalez, M. M. Goodman, J. A. Gussert, M. Hampel-Arias, Z. Harding, J. P. Huentemeyer, P. Hui, C. M. Imran, A. Iriarte, A. Karn, P. Kieda, D. Kunde, G. J. Lara, A. Lauer, R. J. Lee, W. H. Lennarz, D. Leon Vargas, H. Linnemann, J. T. Longo, M. Luna-Garcia, R. Malone, K. Marinelli, A. Marinelli, S. S. Martinez, H. Martinez, O. Martinez-Castro, J. Matthews, J. A. J. McEnery, J. Mendoza Torres, E. Miranda-Romagnoli, P. Moreno, E. Mostafa, M. Nellen, L. Newbold, M. Noriega-Papaqui, R. Oceguera-Becerra, T. Patricelli, B. Pelayo, R. Perez-Perez, E. G. Pretz, J. Riviere, C. Rosa-Gonzalez, D. Ruiz-Velasco, E. Ryan, J. Salazar, H. Greus, F. Salesa Sandoval, A. Schneider, M. Sinnis, G. Smith, A. J. Woodle, K. Sparks Springer, R. W. Taboada, I. Toale, P. A. Tollefson, K. Torres, I. Ukwatta, T. N. Villasenor, L. Weisgarber, T. Westerhoff, S. Wisher, I. G. Wood, J. Yodh, G. B. Younk, P. W. Zaborov, D. Zepeda, A. Zhou, H. CA HAWC Collaboration TI OBSERVATION OF SMALL-SCALE ANISOTROPY IN THE ARRIVAL DIRECTION DISTRIBUTION OF TeV COSMIC RAYS WITH HAWC SO ASTROPHYSICAL JOURNAL LA English DT Article DE astroparticle physics; cosmic rays ID AIR-SHOWER ARRAY; POWER SPECTRA; GAMMA-RAYS; ICECUBE; MILAGRO AB The High-Altitude Water Cherenkov ( HAWC) Observatory is sensitive to gamma rays and charged cosmic rays at TeV energies. The detector is still under construction, but data acquisition with the partially deployed detector started in 2013. An analysis of the cosmic- ray arrival direction distribution based on 4.9 x 10(10) events recorded between 2013 June and 2014 February shows anisotropy at the 10(-4) level on angular scales of about 10 degrees.. The HAWC cosmic- ray sky map exhibits three regions of significantly enhanced cosmic- ray flux; two of these regions were first reported by the Milagro experiment. A third region coincides with an excess recently reported by the ARGO-YBJ experiment. An angular power spectrum analysis of the sky shows that all terms up to l = 15 contribute significantly to the excesses. C1 [Abeysekara, A. U.; DeYoung, T.; Linnemann, J. T.; Marinelli, S. S.; Tollefson, K.; Ukwatta, T. N.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Abeysekara, A. U.; Barber, A. S.; Kieda, D.; Newbold, M.; Springer, R. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT USA. [Alfaro, R.; Belmont, E.; Leon Vargas, H.; Marinelli, A.; Oceguera-Becerra, T.; Ruiz-Velasco, E.; Sandoval, A.] Univ Nacl Autonoma Mexico, Inst Fis, Mexico City 01000, DF, Mexico. [Alvarez, C.; Arceo, R.] Univ Autonoma Chiapas, CEFyMAP, Tuxtla Gutierrez, Chiapas, Mexico. [Alvarez, J. D.; Arteaga-Velazquez, J. C.; Cotti, U.; De Leon, C.; Villasenor, L.] Univ Michoacana, Morelia, Michoacan, Mexico. [Solares, H. A. Ayala; Huentemeyer, P.; Hui, C. M.; Zhou, H.] Michigan Technol Univ, Dept Phys, Houghton, MI 49931 USA. [Baughman, B. M.; Berley, D.; Braun, J.; Ellsworth, R. W.; Goodman, J. A.; Riviere, C.; Smith, A. J.; Wood, J.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Bautista-Elivar, N.; Perez-Perez, E. G.] Univ Politecn Pachuca, Pachuca, Hidalgo, Mexico. [BenZvi, S. Y.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [BenZvi, S. Y.; Braun, J.; Diaz-Velez, J. C.; DuVernois, M. A.; Fiorino, D. W.; Hampel-Arias, Z.; Imran, A.; Karn, P.; Weisgarber, T.; Westerhoff, S.; Wisher, I. G.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI USA. [BenZvi, S. Y.; Diaz-Velez, J. C.; DuVernois, M. A.; Fiorino, D. W.; Hampel-Arias, Z.; Imran, A.; Karn, P.; Weisgarber, T.; Westerhoff, S.; Wisher, I. G.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Bonilla Rosales, M.; Carraminana, A.; Diaz Hernandez, R.; Galindo, A.; Mendoza Torres, E.; Rosa-Gonzalez, D.; Torres, I.] Inst Nacl Astrofis Opt & Electr, Puebla, Mexico. [Caballero-Mora, K. S.; Martinez, H.; Zepeda, A.] Inst Politecn Nacl, Ctr Invest & Estudios Avanzados, Mexico City, DF, Mexico. [Castillo, M.; Cotzomi, J.; Martinez, O.; Moreno, E.; Salazar, H.] Benemerita Univ Autonoma Puebla, Fac Ciencias Fis, Puebla 72570, Mexico. [De La Fuente, E.; Oceguera-Becerra, T.] Univ Guadalajara, IAM Dept Fis, Guadalajara, Jalisco, Mexico. [De La Fuente, E.; Oceguera-Becerra, T.] Univ Guadalajara, Dept Elect CUCEI, IT Phd CUCEA, Phys Mat Phd CUVALLES, Guadalajara, Jalisco, Mexico. [Dingus, B. L.; Harding, J. P.; Imran, A.; Kunde, G. J.; Sinnis, G.; Ukwatta, T. N.; Younk, P. W.] Los Alamos Natl Lab, Div Phys, Los Alamos, NM 87545 USA. [Ellsworth, R. W.] George Mason Univ, Sch Phys Astron & Computat Sci, Fairfax, VA 22030 USA. [Fraija, N.; Garfias, F.; Gonzalez, M. M.; Iriarte, A.; Lee, W. H.; Patricelli, B.; Riviere, C.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Gussert, M.; Longo, M.] Colorado State Univ, Dept Phys, Ft Collins, CO 80523 USA. [Karn, P.; Yodh, G. B.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA USA. [Lara, A.] Univ Nacl Autonoma Mexico, Inst Geofis, Mexico City 04510, DF, Mexico. [Lauer, R. J.; Matthews, J. A. J.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Lennarz, D.; Taboada, I.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Lennarz, D.; Taboada, I.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Luna-Garcia, R.; Martinez-Castro, J.; Pelayo, R.] Inst Politecn Nacl, Ctr Invest Computac, Mexico City, DF, Mexico. [Malone, K.; Mostafa, M.; Pretz, J.; Greus, F. Salesa; Woodle, K. Sparks; Zaborov, D.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [McEnery, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Miranda-Romagnoli, P.; Noriega-Papaqui, R.] Univ Autonoma Estado Hidalgo, Pachuca, Hidalgo, Mexico. [Nellen, L.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. [Pelayo, R.] Inst Politecn Nacl, Unidad Profes Interdisciplinaria Ingn & Tecnol Av, Mexico City, DF, Mexico. [Ryan, J.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Schneider, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Toale, P. A.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. RP Abeysekara, AU (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. EM dan.fiorino@wipac.wisc.edu OI Lara, Alejandro/0000-0001-6336-5291 FU US National Science Foundation (NSF); US Department of Energy Office of High- Energy Physics; Laboratory Directed Research and Development (LDRD) program of Los Alamos National Laboratory; Consejo Nacional de Ciencia y Tecnologia (CONACyT), Mexico [55155, 105666, 122331, 132197]; Red de Fisica de Altas Energias, Mexico, DGAPAUNAM [IG100414- 3, IN108713, IN121309, IN115409, IN113612]; VIEP-BUAP [161-EXC-2011]; University of Wisconsin Alumni Research Foundation; Institute of Geophysics, Planetary Physics, and Signatures at Los Alamos National Laboratory; Luc Binette Foundation UNAM FX We gratefully acknowledge Scott DeLay for his dedicated efforts in the construction and maintenance of the HAWC experiment. This work has been supported by the US National Science Foundation (NSF), the US Department of Energy Office of High- Energy Physics, the Laboratory Directed Research and Development (LDRD) program of Los Alamos National Laboratory, Consejo Nacional de Ciencia y Tecnologia (CONACyT), Mexico (grants 55155, 105666, 122331, and 132197), Red de Fisica de Altas Energias, Mexico, DGAPAUNAM (grants IG100414- 3, IN108713, and IN121309, IN115409, IN113612), VIEP-BUAP (grant 161-EXC-2011), the University of Wisconsin Alumni Research Foundation, the Institute of Geophysics, Planetary Physics, and Signatures at Los Alamos National Laboratory, and the Luc Binette Foundation UNAM Postdoctoral Fellowship program. NR 34 TC 19 Z9 19 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2014 VL 796 IS 2 AR 108 DI 10.1088/0004-637X/796/2/108 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT4AI UT WOS:000344878900037 ER PT J AU Fornasini, FM Tomsick, JA Bodaghee, A Krivonos, RA An, HJ Rahoui, F Gotthelf, EV Bauer, FE Stern, D AF Fornasini, Francesca M. Tomsick, John A. Bodaghee, Arash Krivonos, Roman A. An, Hongjun Rahoui, Farid Gotthelf, Eric V. Bauer, Franz E. Stern, Daniel TI THE NORMA ARM REGION CHANDRA SURVEY CATALOG: X-RAY POPULATIONS IN THE SPIRAL ARMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; catalogs; Galaxy: disk; novae, cataclysmic variables; X-rays: binaries; X-rays: stars ID XMM-NEWTON OBSERVATIONS; GALACTIC PLANE SURVEY; 5 INTEGRAL SOURCES; MILKY-WAY; POINT SOURCES; CATACLYSMIC VARIABLES; INFRARED IDENTIFICATION; LUMINOSITY FUNCTION; SUPERNOVA REMNANT; CONFIDENCE-LIMITS AB We present a catalog of 1415 X-ray sources identified in the Norma Arm Region Chandra Survey (NARCS), which covers a 2 degrees x 0 degrees.8 region in the direction of the Norma spiral arm to a depth of approximate to 20 ks. Of these sources, 1130 are point-like sources detected with >= 3 sigma confidence in at least one of three energy bands (0.5-10, 0.5-2, and 2-10 keV), five have extended emission, and the remainder are detected at low significance. Since most sources have too few counts to permit individual classification, they are divided into five spectral groups defined by their quantile properties. We analyze stacked spectra of X-ray sources within each group, in conjunction with their fluxes, variability, and infrared counterparts, to identify the dominant populations in our survey. We find that similar to 50% of our sources are foreground sources located within 1-2 kpc, which is consistent with expectations from previous surveys. Approximately 20% of sources are likely located in the proximity of the Scutum-Crux and near Norma arm, while 30% are more distant, in the proximity of the far Norma arm or beyond. We argue that a mixture of magnetic and nonmagnetic cataclysmic variables dominates the Scutum-Crux and near Norma arms, while intermediate polars and high-mass stars (isolated or in binaries) dominate the far Norma arm. We also present the cumulative number count distribution for sources in our survey that are detected in the hard energy band. A population of very hard sources in the vicinity of the far Norma arm and active galactic nuclei dominate the hard X-ray emission down to f(X) approximate to 10(-14) erg cm(-2) s(-1), but the distribution curve flattens at fainter fluxes. We find good agreement between the observed distribution and predictions based on other surveys. C1 [Fornasini, Francesca M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Fornasini, Francesca M.; Tomsick, John A.; Bodaghee, Arash; Krivonos, Roman A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Bodaghee, Arash] Georgia Coll & State Univ, Milledgeville, GA 31061 USA. [Krivonos, Roman A.] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. [An, Hongjun] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Rahoui, Farid] European So Observ, D-85748 Garching, Germany. [Rahoui, Farid] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Gotthelf, Eric V.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Bauer, Franz E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, Franz E.] Millennium Inst Astrophys, Santiago, Chile. [Bauer, Franz E.] Space Sci Inst, Boulder, CO 80301 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Fornasini, FM (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM f.fornasini@berkeley.edu FU NASA [G01-12068A, NAS8-03060]; National Science Foundation Graduate Research Fellowship; Berkeley Fellowship; Basal-CATA [PFB-06/2007]; CONICYT-Chile FONDECYT [1141218]; "EMBIGGEN" Anillo [ACT1101]; "Millennium Institute of Astrophysics (MAS)" of Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo [IC120009] FX We thank the referee and the editor for their suggestions, which helped us improve the scientific quality of these results. We thank G.K. Keating and C. Heiles for helpful discussions about various components of the statistical analysis carried out for this work. We are also grateful to B. Lehmer for clarifications regarding the maximum likelihood number-flux computation, to J. Hong for providing his quantile analysis tools, and to L. Blitz and M. Ajello for valuable conversations. The scientific results reported in this article are based on observations made by the Chandra X-Ray Observatory. Our analysis of IR counterparts was based on data products from observations made with ESO Telescopes at the La Silla or Paranal Observatories under ESO programme ID 179.B-2002. This research has made use of software provided by the Chandra X-Ray Center (CXC) in the application packages CIAO and Sherpa. This work was supported in part by NASA through Chandra Award Number G01-12068A issued by the Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. In addition, FMF received support from the National Science Foundation Graduate Research Fellowship and the Berkeley Fellowship. F.E.B. acknowledges support from Basal-CATA PFB-06/2007, CONICYT-Chile FONDECYT 1141218 and "EMBIGGEN" Anillo ACT1101, and Project IC120009 "Millennium Institute of Astrophysics (MAS)" of Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo. NR 81 TC 3 Z9 3 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2014 VL 796 IS 2 AR 105 DI 10.1088/0004-637X/796/2/105 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT4AI UT WOS:000344878900034 ER PT J AU Fortenberry, RC Huang, XC Crawford, TD Lee, TJ AF Fortenberry, Ryan C. Huang, Xinchuan Crawford, T. Daniel Lee, Timothy J. TI QUANTUM CHEMICAL ROVIBRATIONAL DATA FOR THE INTERSTELLAR DETECTION OF c-C3H- SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; circumstellar matter; ISM: lines and bands; ISM: molecules; molecular data; radio lines: ISM ID QUARTIC FORCE-FIELDS; AB-INITIO MO; VIBRATIONAL FREQUENCIES; SPECTROSCOPIC CONSTANTS; ASTRONOMICAL IDENTIFICATION; ELECTRON-AFFINITIES; LINEAR C3H3+; BASIS-SETS; CYCLOPROPENYLIDENE; ISOTOPOLOGUES AB The anion chemistry of the interstellar medium ( ISM) has almost exclusively been limited to linear hydrocarbons and cyanocarbons. Of the hydrocarbons, only the even n CnH- chains have been detected in the ISM, and lines hypothesized to originate with b-C3H- have been conclusively linked to the corresponding cation, as originally claimed. However, no reason has yet been provided as to why other anions cannot form, and the cyclic form of C3H- is actually the lowest-energy isomer on the anion's potential energy surface. As such, this work provides the necessary rovibrational reference data for the potential detection of this anion in the ISM or related laboratory experiments. Improvements over previously calculated rovibrational spectroscopic constants are contained herein along with graphical depictions of the pure rotational spectra at 100 K, 40 K, 20 K, and 2.7 K. C1 [Fortenberry, Ryan C.] Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA. [Fortenberry, Ryan C.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA. [Crawford, T. Daniel] Dept Chem, Virginia Tech, Blacksburg, VA 24061 USA. RP Fortenberry, RC (reprint author), Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA. EM rfortenberry@georgiasouthern.edu; Timothy.J.Lee@nasa.gov RI Lee, Timothy/K-2838-2012; HUANG, XINCHUAN/A-3266-2013; Crawford, Thomas/A-9271-2017 OI Crawford, Thomas/0000-0002-7961-7016 FU Georgia Southern University; Oak Ridge Associated Universities through the NASA Postdoctoral Program; NASA's Laboratory Astrophysics "Carbon in the Galaxy" Consortium grant [NNH10ZDA001N]; U.S. National Science Foundation (NSF) award [NSF-1058420]; NSF Multi-User Chemistry Research Instrumentation and Facility (CRIF:MU) award [CHE-0741927]; NASA [12-APRA12-0107] FX R.C.F. received support from Georgia Southern University for startup funds and from Oak Ridge Associated Universities through the NASA Postdoctoral Program during the lifetime of this project. NASA's Laboratory Astrophysics "Carbon in the Galaxy" Consortium grant (NNH10ZDA001N) is gratefully acknowledged. The U.S. National Science Foundation (NSF) award NSF-1058420 has supported T.D.C. NSF Multi-User Chemistry Research Instrumentation and Facility (CRIF:MU) award CHE-0741927 provided the computational hardware. Additionally, R.C.F., X.H., and T.J.L. acknowledge support from the NASA 12-APRA12-0107 grant. The authors also thank Dr. David W.Schwenke of the NASA Ames Research Center for teaching us new things about Feshbach resonances and related phenomena. NR 59 TC 7 Z9 7 U1 2 U2 19 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2014 VL 796 IS 2 AR 139 DI 10.1088/0004-637X/796/2/139 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT4AI UT WOS:000344878900068 ER PT J AU Homan, DC Kadler, M Kellermann, KI Kovalev, YY Lister, ML Ros, E Savolainen, T Zensus, A AF Homan, D. C. Kadler, M. Kellermann, K. I. Kovalev, Y. Y. Lister, M. L. Ros, E. Savolainen, T. Zensus, A. TI MOJAVE: MONITORING OF JETS IN ACTIVE GALACTIC NUCLEI WITH VLBA EXPERIMENTS. VII. BLAZAR JET ACCELERATION (vol 706, pg 1253, 2009) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Homan, D. C.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Kadler, M.] Univ Erlangen Nurnberg, Dr Remeis Sternwarte Bamberg, D-96049 Bamberg, Germany. [Kadler, M.] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany. [Kadler, M.] NASA, CRESST, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kadler, M.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Kellermann, K. I.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Kovalev, Y. Y.; Ros, E.; Savolainen, T.; Zensus, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Kovalev, Y. Y.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Lister, M. L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Ros, E.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain. RP Homan, DC (reprint author), Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. EM homand@denison.edu; matthias.kadler@sternwarte.uni-erlangen.de; kkellerm@nrao.edu; yyk@asc.rssi.ru; mlister@purdue.edu; Eduardo.Ros@uv.es; tsavolainen@mpifr-bonn.mpg.de; zensus@mpifr-bonn.mpg.de RI Kovalev, Yuri/J-5671-2013 OI Kovalev, Yuri/0000-0001-9303-3263 NR 2 TC 0 Z9 0 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2014 VL 796 IS 2 AR 147 DI 10.1088/0004-637X/796/2/147 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT4AI UT WOS:000344878900076 ER PT J AU Kirk, MS Balasubramaniam, KS Jackiewicz, J McAteer, RTJ AF Kirk, Michael S. Balasubramaniam, K. S. Jackiewicz, Jason McAteer, R. T. James TI QUALITIES OF SEQUENTIAL CHROMOSPHERIC BRIGHTENINGS OBSERVED IN H alpha AND UV IMAGES SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: chromosphere; Sun: coronal mass ejections (CMEs); Sun: flares ID SOLAR-FLARES; ENERGY-RELEASE; EVAPORATION AB Chromospheric flare ribbons observed in H alpha appear well-organized when first examined: ribbons impulsively brighten, morphologically evolve, and exponentially decay back to pre-flare levels. Upon closer inspection of the H alpha flares, there is often a significant number of compact areas brightening in concert with the flare eruption but are spatially separated from the evolving flare ribbon. One class of these brightenings is known as sequential chromospheric brightenings (SCBs). SCBs are often observed in the immediate vicinity of erupting flares and are associated with coronal mass ejections. In the past decade there have been several previous investigations of SCBs. These studies have exclusively relied upon H alpha images to discover and analyze these ephemeral brightenings. This work employs the automated detection algorithm of Kirk et al. to extract the physical qualities of SCBs in observations of ground-based H alpha images and complementary Atmospheric Imaging Assembly images in He II, C IV, and 1700 angstrom. The metadata produced in this tracking process are then culled using complementary Doppler velocities to isolate three distinguishable types of SCBs. From a statistical analysis, we find that the SCBs at the chromospheric H alpha layer appear earlier and last longer than their corresponding signatures measured in AIA. From this multi-layer analysis, we infer that SCBs are spatially constrained to the mid-chromosphere. We also derive an energy budget to explain SCBs which have a postulated energy of not more than 0.01% of the total flare energy. C1 [Kirk, Michael S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kirk, Michael S.; Balasubramaniam, K. S.; Jackiewicz, Jason; McAteer, R. T. James] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Balasubramaniam, K. S.] Air Force Res Lab, Space Vehicles Directorate, Kirtland AFB, NM 87114 USA. RP Kirk, MS (reprint author), NASA, Goddard Space Flight Ctr, Code 670, Greenbelt, MD 20771 USA. EM michael.s.kirk@nasa.gov FU NASA FX The authors acknowledge: (1) USAF/AFRL Space Scholar Program, (2) NSO/AURA for the use of their sunspot, NM facilities, (3) AFRL/RVBXS, and (4) NMSU. This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 24 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2014 VL 796 IS 2 AR 78 DI 10.1088/0004-637X/796/2/78 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT4AI UT WOS:000344878900007 ER PT J AU Nowak, M Flagey, N Noriega-Crespo, A Billot, N Carey, SJ Paladini, R Van Dyk, SD AF Nowak, M. Flagey, N. Noriega-Crespo, A. Billot, N. Carey, S. J. Paladini, R. Van Dyk, S. D. TI SPITZER/INFRARED SPECTROGRAPH INVESTIGATION OF MIPSGAL 24 mu m COMPACT BUBBLES: LOW-RESOLUTION OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; planetary nebulae: general; stars: emission-line, Be; stars: variables: S Doradus; stars: Wolf-Rayet ID WOLF-RAYET STARS; LUMINOUS BLUE VARIABLES; SPITZER-SPACE-TELESCOPE; LARGE-MAGELLANIC-CLOUD; INNER GALACTIC PLANE; SUPERNOVA REMNANT; INFRARED SURVEY; VIITH CATALOG; MASSIVE STARS; NEBULA AB We present Spitzer/InfraRed Spectrograph (IRS) low-resolution observations of 11 compact circumstellar bubbles from the MIPSGAL 24 mu m Galactic plane survey. We find that this set of MIPSGAL bubbles (MBs) is divided into two categories and that this distinction correlates with the morphologies of the MBs in the mid-infrared (IR). The four MBs with central sources in the mid-IR exhibit dust-rich, low-excitation spectra, and their 24 mu m emission is accounted for by the dust continuum. The seven MBs without central sources in the mid-IR have spectra dominated by high-excitation gas lines (e.g., [O IV] 26.0 mu m, [Ne v] 14.3 and 24.3 mu m, and [Ne III] 15.5 mu m), and the [O IV] line accounts for 50% to almost 100% of the 24 mu m emission in five of them. In the dust-poor MBs, the [Ne v] and [Ne III] line ratios correspond to high-excitation conditions. Based on comparisons with published IRS spectra, we suggest that the dust-poor MBs are highly excited planetary nebulae (PNs) with peculiar white dwarfs (e. g., Wolf-Rayet [WR] and novae) at their centers. The central stars of the four dust-rich MBs are all massive star candidates. Dust temperatures range from 40 to 100 K in the outer shells. We constrain the extinction along the lines of sight from the IRS spectra. We then derive distance, dust masses, and dust production rate estimates for these objects. These estimates are all consistent with the nature of the central stars. We summarize the identifications of MBs made to date and discuss the correlation between their mid-IR morphologies and natures. Candidate Be/B[e]/luminous blue variable and WR stars are mainly "rings" with mid-IR central sources, whereas PNs are mostly "disks" without mid-IR central sources. Therefore we expect that most of the 300 remaining unidentified MBs will be classified as PNs. C1 [Nowak, M.] Ecole Normale Super, Dept Phys, F-94235 Cachan, France. [Nowak, M.; Noriega-Crespo, A.; Carey, S. J.; Van Dyk, S. D.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Flagey, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Flagey, N.] Inst Astron, Hilo, HI 96720 USA. [Noriega-Crespo, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Billot, N.] Inst Radio Astron Millimetr, E-18012 Granada, Spain. [Paladini, R.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. RP Nowak, M (reprint author), Ecole Normale Super, Dept Phys, 61 Ave President Wilson, F-94235 Cachan, France. EM mathias.nowak@ens-cachan.fr FU NASA; NASA through an award issued by JPL/Caltech FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 52 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2014 VL 796 IS 2 AR 116 DI 10.1088/0004-637X/796/2/116 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT4AI UT WOS:000344878900045 ER PT J AU Wright, MCH Hull, CLH Pillai, T Zhao, JH Sandell, G AF Wright, M. C. H. Hull, Charles L. H. Pillai, Thushara Zhao, Jun-Hui Sandell, Goeran TI NGC 7538 IRS. 1. INTERACTION OF A POLARIZED DUST SPIRAL AND A MOLECULAR OUTFLOW SO ASTROPHYSICAL JOURNAL LA English DT Article DE H II regions; ISM: jets and outflows; ISM: kinematics and dynamics; ISM: magnetic fields; ISM: molecules; stars: formation ID PROTOSTELLAR CORES; CIRCUMSTELLAR DISK; METHANOL MASERS; NGC-7538 IRS-1; HII-REGIONS; STAR; RESOLUTION; PROTOSTARS; ACCRETION; VELOCITY AB We present dust polarization and CO molecular line images of NGC 7538 IRS 1. We combined data from the Submillimeter Array, the Combined Array for Research in Millimeter-wave Astronomy, and the James Clerk Maxwell Telescope to make images with similar to 2 ''.5 resolution at 230 and 345 GHz. The images show a remarkable spiral pattern in both the dust polarization and molecular outflow. These data dramatically illustrate the interplay between a high infall rate onto IRS 1 and a powerful outflow disrupting the dense, clumpy medium surrounding the star. The images of the dust polarization and the CO outflow presented here provide observational evidence for the exchange of energy and angular momentum between the infall and the outflow. The spiral dust pattern, which rotates through over 180 degrees from IRS 1, may be a clumpy filament wound up by conservation of angular momentum in the infalling material. The redshifted CO emission ridge traces the dust spiral closely through the MM dust cores, several of which may contain protostars. We propose that the CO maps the boundary layer where the outflow is ablating gas from the dense gas in the spiral. C1 [Wright, M. C. H.; Hull, Charles L. H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Pillai, Thushara] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Zhao, Jun-Hui] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sandell, Goeran] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. RP Wright, MCH (reprint author), Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. EM jzhao@cfa.harvard.edu FU NSF Graduate Fellowship; Ford Foundation Dissertation Fellowship; states of California Gordon and Betty Moore Foundation; states of California Kenneth T. and Eileen L. Norris Foundation; states of California Associates of the California Institute of Technology; states of California National Science Foundation; states of Illinois Gordon and Betty Moore Foundation; states of Illinois Kenneth T. and Eileen L. Norris Foundation; states of Illinois Associates of the California Institute of Technology; states of Illinois National Science Foundation; states of Maryland Gordon and Betty Moore Foundation; states of Maryland Kenneth T. and Eileen L. Norris Foundation; states of Maryland Associates of the California Institute of Technology; states of Maryland National Science Foundation; National Science Foundation; CARMA partner universities FX C.L.H.H. acknowledges support from an NSF Graduate Fellowship and from a Ford Foundation Dissertation Fellowship. Support for CARMA construction was derived from the states of California, Illinois, and Maryland, the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the Associates of the California Institute of Technology, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. The James Clerk Maxwell Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the National Research Council of Canada, and (until 2013 March 31) the Netherlands Organisation for Scientific Research. We thank the anonymous referee for a careful reading and some good questions and suggestions which have improved this paper. NR 31 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 DEC 1 PY 2014 VL 796 IS 2 AR 112 DI 10.1088/0004-637X/796/2/112 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT4AI UT WOS:000344878900041 ER PT J AU Zanardo, G Staveley-Smith, L Indebetouw, R Chevalier, RA Matsuura, M Gaensler, BM Barlow, MJ Fransson, C Manchester, RN Baes, M Kamenetzky, JR Lakicevic, M Lundqvist, P Marcaide, JM Marti-Vidal, I Meixner, M Ng, CY Park, S Sonneborn, G Spyromilio, J van Loon, JT AF Zanardo, Giovanna Staveley-Smith, Lister Indebetouw, Remy Chevalier, Roger A. Matsuura, Mikako Gaensler, Bryan M. Barlow, Michael J. Fransson, Claes Manchester, Richard N. Baes, Maarten Kamenetzky, Julia R. Lakicevic, Masa Lundqvist, Peter Marcaide, Jon M. Marti-Vidal, Ivan Meixner, Margaret Ng, C. -Y. Park, Sangwook Sonneborn, George Spyromilio, Jason van Loon, Jacco Th. TI SPECTRAL AND MORPHOLOGICAL ANALYSIS OF THE REMNANT OF SUPERNOVA 1987A WITH ALMA AND ATCA SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: supernova remnants; radiation mechanisms: non-thermal; radiation mechanisms: thermal; radio continuum: general; stars: neutron; supernovae: individual (SN 1987A) ID GALACTIC RADIO EMISSION; SN 1987A; MAGNETIC-FIELD; PARTICLE-ACCELERATION; NEUTRINO BURST; RAY-EMISSION; LIGHT-CURVE; EVOLUTION; PULSAR; SN-1987A AB We present a comprehensive spectral and morphological analysis of the remnant of supernova (SN) 1987A with the Australia Telescope Compact Array (ATCA) and the Atacama Large Millimeter/submillimeter Array (ALMA). The non-thermal and thermal components of the radio emission are investigated in images from 94 to 672 GHz (lambda 3.2 mm to 450 mu m), with the assistance of a high-resolution 44 GHz synchrotron template from the ATCA, and a dust template from ALMA observations at 672 GHz. An analysis of the emission distribution over the equatorial ring in images from 44 to 345 GHz highlights a gradual decrease of the east-to-west asymmetry ratio with frequency. We attribute this to the shorter synchrotron lifetime at high frequencies. Across the transition from radio to far infrared, both the synchrotron/dust-subtracted images and the spectral energy distribution (SED) suggest additional emission beside the main synchrotron component (S-nu proportional to nu(-0.73)) and the thermal component originating from dust grains at T similar to 22 K. This excess could be due to free-free flux or emission from grains of colder dust. However, a second flat-spectrum synchrotron component appears to better fit the SED, implying that the emission could be attributed to a pulsar wind nebula (PWN). The residual emission is mainly localized west of the SN site, as the spectral analysis yields -0.4 less than or similar to alpha less than or similar to -0.1 across the western regions, with alpha similar to 0 around the central region. If there is a PWN in the remnant interior, these data suggest that the pulsar may be offset westward from the SN position. C1 [Zanardo, Giovanna; Staveley-Smith, Lister] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia. [Indebetouw, Remy; Chevalier, Roger A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Indebetouw, Remy] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Matsuura, Mikako; Barlow, Michael J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Gaensler, Bryan M.] Univ Sydney, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Fransson, Claes; Lundqvist, Peter] Stockholm Univ, Oskar Klein Ctr, Dept Astron, SE-10691 Stockholm, Sweden. [Manchester, Richard N.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Baes, Maarten] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium. [Kamenetzky, Julia R.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Lakicevic, Masa; van Loon, Jacco Th.] Keele Univ, Lennard Jones Labs, Inst Environm Phys Sci & Appl Math, Keele ST5 5BG, Staffs, England. [Marcaide, Jon M.] Univ Valencia, Dept Astron, E-46100 Burjassot, Spain. [Marcaide, Jon M.] Donostia Int Phys Ctr, E-20018 Donostia San Sebastian, Spain. [Marti-Vidal, Ivan] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden. [Meixner, Margaret] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Meixner, Margaret] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Ng, C. -Y.] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Park, Sangwook] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA. [Sonneborn, George] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Spyromilio, Jason] European So Observ, D-85748 Garching, Germany. RP Zanardo, G (reprint author), Univ Western Australia, Int Ctr Radio Astron Res, M468, Crawley, WA 6009, Australia. EM giovanna.zanardo@gmail.com RI Ng, Chi Yung/A-7639-2013; Barlow, Michael/A-5638-2009; DONOSTIA INTERNATIONAL PHYSICS CTR., DIPC/C-3171-2014; Marti-Vidal, Ivan/A-8799-2017; Staveley-Smith, Lister/A-1683-2011; OI Ng, Chi Yung/0000-0002-5847-2612; Barlow, Michael/0000-0002-3875-1171; Marti-Vidal, Ivan/0000-0003-3708-9611; Staveley-Smith, Lister/0000-0002-8057-0294; Gaensler, Bryan/0000-0002-3382-9558 FU Commonwealth of Australia; CAASTRO [CE110001020]; NASA [NNX12AF90G]; ESO/Keele University studentship FX We thank Philipp Podsiadlowski and Bruno Leibundgut for useful discussions; Richard McCray, Craig Wheeler, and Eli Dwek for feedback on the drafts. We thank Robert Kirshner and Peter Challis for providing the IIST images. Figures 9 and 10 utilize the cube helix color scheme introduced by Green (2011). This paper makes use of the following ALMA data: ADS/JAO.ALMA #2011.0.00273.S (PI: Indebetouw). ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The Australia Telescope Compact Array is part of the Australia Telescope, which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. L.S.S. and B.M.G. acknowledge the support of CAASTRO, through project number CE110001020. R.A.C. acknowledges the support of NASA grant NNX12AF90G. M.L. acknowledges an ESO/Keele University studentship. NR 93 TC 14 Z9 14 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2014 VL 796 IS 2 AR 82 DI 10.1088/0004-637X/796/2/82 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT4AI UT WOS:000344878900011 ER PT J AU Zhao, M O'Rourke, JG Wright, JT Knutson, HA Burrows, A Fortney, J Ngo, H Fulton, BJ Baranec, C Riddle, R Law, NM Muirhead, PS Hinkley, S Showman, AP Curtis, J Burruss, R AF Zhao, Ming O'Rourke, Joseph G. Wright, Jason T. Knutson, Heather A. Burrows, Adam Fortney, Johnathan Ngo, Henry Fulton, Benjamin J. Baranec, Christoph Riddle, Reed Law, Nicholas M. Muirhead, Philip S. Hinkley, Sasha Showman, Adam P. Curtis, Jason Burruss, Rick TI CHARACTERIZATION OF THE ATMOSPHERE OF THE HOT JUPITER HAT-P-32Ab AND THE M-DWARF COMPANION HAT-P-32B SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; infrared: planetary systems; planetary systems; stars: individual (HAT-P-32A, HAT-P-32B); techniques: high angular resolution; techniques: photometric ID INFRARED THERMAL EMISSION; SYSTEMATIC RETRIEVAL ANALYSIS; EXTRASOLAR GIANT PLANETS; GROUND-BASED DETECTIONS; LASER ADAPTIVE OPTICS; SECONDARY ECLIPSE; LIGHT CURVES; TRANSMISSION SPECTRUM; RECIPROCITY FAILURE; TRANSITING PLANETS AB We report secondary eclipse photometry of the hot Jupiter HAT-P-32Ab, taken with Hale/Wide-field Infra-Red Camera (WIRC) in H and K-S bands and with Spitzer/IRAC at 3.6 and 4.5 mu m. We carried out adaptive optics imaging of the planet host star HAT-P-32A and its companion HAT-P-32B in the near-IR and the visible. We clearly resolve the two stars from each other and find a separation of 2 ''.923 +/- 0 ''.004 and a position angle 110 degrees.64 +/- 0 degrees.12. We measure the flux ratios of the binary in g'r'i'z' and H and KS bands, and determine T-eff = 3565 +/- 82 K for the companion star, corresponding to an M1.5 dwarf. We use PHOENIX stellar atmosphere models to correct the dilution of the secondary eclipse depths of the hot Jupiter due to the presence of the M1.5 companion. We also improve the secondary eclipse photometry by accounting for the non-classical, flux-dependent nonlinearity of the WIRC IR detector in the H band. We measure planet-to-star flux ratios of 0.090% +/- 0.033%, 0.178% +/- 0.057%, 0.364% +/- 0.016%, and 0.438% +/- 0.020% in the H, K-S, 3.6 and 4.5 mu m bands, respectively. We compare these with planetary atmospheric models, and find they prefer an atmosphere with a temperature inversion and inefficient heat redistribution. However, we also find that the data are equally well described by a blackbody model for the planet with T-p = 2042 +/- 50 K. Finally, we measure a secondary eclipse timing offset of 0.3 +/- 1.3 minutes from the predicted mid-eclipse time, which constrains e = 0.0072(-0.0064)(+0.0700) when combined with radial velocity data and is more consistent with a circular orbit. C1 [Zhao, Ming; Wright, Jason T.; Curtis, Jason] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Zhao, Ming; Wright, Jason T.; Curtis, Jason] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [O'Rourke, Joseph G.; Knutson, Heather A.; Ngo, Henry] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Fortney, Johnathan] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Fulton, Benjamin J.; Baranec, Christoph] Univ Hawaii Manoa, Inst Astron, Hilo, HI 96720 USA. [Riddle, Reed; Hinkley, Sasha] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Law, Nicholas M.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. [Muirhead, Philip S.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Showman, Adam P.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Burruss, Rick] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Zhao, M (reprint author), Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. EM mingzhao@psu.edu RI Muirhead, Philip/H-2273-2014; OI Muirhead, Philip/0000-0002-0638-8822; O'Rourke, Joseph/0000-0002-1180-996X; Wright, Jason/0000-0001-6160-5888; Ngo, Henry/0000-0001-5172-4859 FU NASA Origins of Solar Systems [NNX14AD22G]; Center for Exoplanets and Habitable Worlds at the Pennsylvania State University; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium; National Science Foundation's Graduate Research Fellowship Program; Natural Science and Engineering Research Council of Canada; NASA HST [HST-GO-12181.04-A, HST-GO-12314.03-A, HST-GO-12473.06-A, HST-GO-12550.02]; JPL/Spitzer Agreements [1417122, 1348668, 1371432, 1377197, 1439064]; NASA Sagan Fellowship at California Institute of Technology; Alfred P. Sloan Foundation; California Institute of Technology; Inter-University Centre for Astronomy and Astrophysics; National Science Foundation [AST-0906060, AST-0960343, AST-1207891]; Mt. Cuba Astronomical Foundation; W.M. Keck Foundation FX We thank the anonymous referee for valuable comments for the paper. We thank the Palomar staff for their help with the observations. M.Z. is supported by funding from NASA Origins of Solar Systems grant NNX14AD22G and the Center for Exoplanets and Habitable Worlds at the Pennsylvania State University. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium.; J.G.O. receives support from the National Science Foundation's Graduate Research Fellowship Program. H.N. acknowledges funding support from the Natural Science and Engineering Research Council of Canada. A. B. acknowledges support in part under NASA HST grants HST-GO-12181.04-A, HST-GO-12314.03-A, HST-GO-12473.06-A, and HST-GO-12550.02, and JPL/Spitzer Agreements 1417122, 1348668, 1371432, 1377197, and 1439064. S.H. acknowledges support from the NASA Sagan Fellowship at California Institute of Technology. C.B. acknowledges support from the Alfred P. Sloan Foundation.; The Robo-AO system is supported by collaborating partner institutions, the California Institute of Technology and the Inter-University Centre for Astronomy and Astrophysics, by the National Science Foundation under grant Nos. AST-0906060, AST-0960343, and AST-1207891, by a grant from the Mt. Cuba Astronomical Foundation and by a gift from Samuel Oschin.; Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. NR 73 TC 9 Z9 9 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2014 VL 796 IS 2 AR 115 DI 10.1088/0004-637X/796/2/115 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT4AI UT WOS:000344878900044 ER PT J AU Dauphas, N Chen, JH Zhang, JJ Papanastassiou, DA Davis, AM Travaglio, C AF Dauphas, Nicolas Chen, James H. Zhang, Junjun Papanastassiou, Dimitri A. Davis, Andrew M. Travaglio, Claudia TI Calcium-48 isotopic anomalies in bulk chondrites and achondrites: Evidence for a uniform isotopic reservoir in the inner protoplanetary disk SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE calcium-48; isotopes; anomalies; meteorites; bulk chondrites; nucleosynthesis; accretion ID MURCHISON CARBONACEOUS CHONDRITE; FORMING GIANT IMPACT; EARLY SOLAR-SYSTEM; OXYGEN-ISOTOPE; REFRACTORY INCLUSIONS; CHEMICAL-COMPOSITION; PROTOSOLAR NEBULA; ALLENDE METEORITE; MURRAY HIBONITES; EARTH AB Thermal ionization mass spectrometry (TIMS) was used to measure the calcium isotopic compositions of carbonaceous, ordinary, enstatite chondrites as well as eucrites and aubrites. We find that after correction for mass-fractionation by internal normalization to a fixed Ca-42/Ca-44 ratio, the Ca-43/Ca-44 and Ca-46/Ca-44 ratios are indistinguishable from terrestrial ratios. In contrast, the Ca-49/Ca-44 ratios show significant departure from the terrestrial composition (from -2 epsilon in eucrites to +4 epsilon in CO and CV chondrites). Isotopic anomalies in epsilon Ca-48 correlate with epsilon Ti-50: epsilon Ca-48 = (1.09 +/- 0.11) x epsilon Ti-50 + (0.03 +/- 0.14). Further work is needed to identify the carrier phase of Ca-48-Ti-50 anomalies but we suggest that it could be perovskite and that the stellar site where these anomalies were created was also responsible for the nucleosynthesis of the bulk of the solar system inventory of these nuclides. The Earth has identical Ca-48 isotopic composition to enstatite chondrites (EH and EL) and aubrites. This adds to a long list of elements that display nucleosynthetic anomalies at a bulk planetary scale but show identical or very similar isotopic compositions between enstatite chondrites, aubrites, and Earth. This suggests that the inner protoplanetary disk was characterized by a uniform isotopic composition (IDUR for Inner Disk Uniform Reservoir), sampled by enstatite chondrites and aubrites, from which the Earth drew most of its constituents. The terrestrial isotopic composition for O-17, (48) ca, Ti-50, Ni-62 and Mo-92 is well reproduced by a mixture of 91% enstatite, 7% ordinary, and 2% carbonaceous chondrites. The Earth was not simply made of enstatite chondrites but it formed from the same original material that was later modified by nebular and disk processes. The Moon-forming impactor probably came from the same region as the other embryos that made the Earth, explaining the strong isotopic similarity between lunar and terrestrial rocks. (C) 2014 Elsevier B.V. All rights reserved. C1 [Dauphas, Nicolas; Zhang, Junjun; Davis, Andrew M.] Univ Chicago, Dept Geophys Sci, Origins Lab, Chicago, IL 60637 USA. [Dauphas, Nicolas; Zhang, Junjun; Davis, Andrew M.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Chen, James H.; Papanastassiou, Dimitri A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, Junjun] Hong Kong Polytech Univ, Dept Civil & Environm Engn, Kowloon, Hong Kong, Peoples R China. [Papanastassiou, Dimitri A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Travaglio, Claudia] INAF Astrophys Observ Turin, I-10015 Pino Torinese, Italy. RP Dauphas, N (reprint author), Univ Chicago, Dept Geophys Sci, Origins Lab, 5734 South Ellis Ave, Chicago, IL 60637 USA. EM dauphas@uchicago.edu FU NASA Cosmochemistry [NNX12AH6OG, NNX09AG39G, 811073.02.02.04.69]; NSF [EAR1144429] FX This paper benefited from discussions with H.-W. Chen, C. Burkhardt, H. Kobayashi, A. Morbidelli, L. Grossman, and H. O'Neill. Justin Simon, two anonymous reviewers, and editor Tim Elliott provided comments that helped improve the manuscript. This work was supported by grants from the NASA Cosmochemistry (NNX12AH6OG to ND; NNX09AG39G to AMD; 811073.02.02.04.69 to JHC) and NSF (EAR1144429 to ND) programs. The samples were generously provided by the Field Museum, United States National Museum, and Museum National d'Histoire Naturelle. NR 99 TC 26 Z9 27 U1 8 U2 36 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD DEC 1 PY 2014 VL 407 BP 96 EP 108 DI 10.1016/j.eps1.2014.09.015 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AT8JH UT WOS:000345179300009 ER PT J AU Casner, SM Geven, RW Recker, MP Schooler, JW AF Casner, Stephen M. Geven, Richard W. Recker, Matthias P. Schooler, Jonathan W. TI The Retention of Manual Flying Skills in the Automated Cockpit SO HUMAN FACTORS LA English DT Article DE manual flying skills; atrophy; retention; procedural; mind wandering ID PILOTS AB Objective: The aim of this study was to understand how the prolonged use of cockpit automation is affecting pilots' manual flying skills. Background: There is an ongoing concern about a potential deterioration of manual flying skills among pilots who assume a supervisory role while cockpit automation systems carry out tasks that were once performed by human pilots. Method: We asked 16 airline pilots to fly routine and nonroutine flight scenarios in a Boeing 747-400 simulator while we systematically varied the level of automation that they used, graded their performance, and probed them about what they were thinking about as they flew. Results: We found pilots' instrument scanning and manual control skills to be mostly intact, even when pilots reported that they were infrequently practiced. However, when pilots were asked to manually perform the cognitive tasks needed for manual flight (e.g., tracking the aircraft's position without the use of a map display, deciding which navigational steps come next, recognizing instrument system failures), we observed more frequent and significant problems. Furthermore, performance on these cognitive tasks was associated with measures of how often pilots engaged in task-unrelated thought when cockpit automation was used. Conclusion: We found that while pilots' instrument scanning and aircraft control skills are reasonably well retained when automation is used, the retention of cognitive skills needed for manual flying may depend on the degree to which pilots remain actively engaged in supervising the automation. C1 [Casner, Stephen M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Geven, Richard W.; Recker, Matthias P.] San Jose State Univ, Res Fdn, Moffett Field, CA USA. [Schooler, Jonathan W.] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA. RP Casner, SM (reprint author), NASA, Ames Res Ctr, Mail Stop 262-4, Moffett Field, CA 94035 USA. EM stephen.casner@nasa.gov NR 11 TC 8 Z9 8 U1 1 U2 12 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 0018-7208 EI 1547-8181 J9 HUM FACTORS JI Hum. Factors PD DEC PY 2014 VL 56 IS 8 BP 1506 EP 1516 DI 10.1177/0018720814535628 PG 11 WC Behavioral Sciences; Engineering, Industrial; Ergonomics; Psychology, Applied; Psychology SC Behavioral Sciences; Engineering; Psychology GA AT9FC UT WOS:000345232300012 PM 25509828 ER PT J AU Nicholson, DE Padula, SA Noebe, RD Benafan, O Vaidyanathan, R AF Nicholson, D. E. Padula, S. A., II Noebe, R. D. Benafan, O. Vaidyanathan, R. TI Thermomechanical behavior of NiTiPdPt high temperature shape memory alloy springs SO SMART MATERIALS AND STRUCTURES LA English DT Article DE shape memory; thermomechanical behavior; springs ID HELICAL SPRINGS; DEFORMATION; ACTUATORS; TRANSFORMATION; STABILITY; EVOLUTION; DESIGN; STRAIN AB Transformation strains in high temperature shape memory alloys (HTSMAs) are generally smaller than for conventional NiTi alloys and can be purposefully limited in cases where stability and repeatability at elevated temperatures are desired. Yet such alloys can still be used in actuator applications that require large strokes when used in the form of springs. Thus there is a need to understand the thermomechanical behavior of shape memory alloy spring actuators, particularly those consisting of alternative alloys. In this work, a modular test setup was assembled with the objective of acquiring stroke, stress, temperature, and moment data in real time during joule heating and forced convective cooling of Ni19.5Ti50.5Pd25Pt5 HTSMA springs. The spring actuators were subjected to both monotonic axial loading and thermomechanical cycling. The role of rotational constraints (i.e., by restricting rotation or allowing for free rotation at the ends of the springs) on stroke performance was also assessed. Finally, recognizing that evolution in the material microstructure can result in changes in HTSMA spring geometry, the effect of material microstructural evolution on spring performance was examined. This was done by taking into consideration the changes in geometry that occurred during thermomechanical cycling. This work thus provides insight into designing with HTSMA springs and predicting their thermomechanical performance. C1 [Nicholson, D. E.; Vaidyanathan, R.] Univ Cent Florida, Adv Mat Proc & Anal Ctr, Orlando, FL 32816 USA. [Padula, S. A., II; Noebe, R. D.; Benafan, O.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Nicholson, DE (reprint author), Univ Cent Florida, Adv Mat Proc & Anal Ctr, 4000 Cent Florida Blvd, Orlando, FL 32816 USA. EM raj@ucf.edu FU NASA FAP Supersonics Project [NNX08AB51A]; Subsonic Fixed Wing Project [NNX11AI57A]; Aeronautical Sciences Project; Florida Center for Advanced Aero-Propulsion (FCAAP) FX Useful discussions with Dr Aaron Stebner (Colorado School of Mines) on the testing set up are gratefully acknowledged. The authors would also like to acknowledge Dr Jian Liu and Albert Mak of Dr Chenyging Xu's group at the University of Central Florida for contributions in developing the DAQ system. Financial support for this work came from the NASA FAP Supersonics Project (NNX08AB51A), Subsonic Fixed Wing Project (NNX11AI57A), and most recently the Aeronautical Sciences Project and the Florida Center for Advanced Aero-Propulsion (FCAAP). NR 32 TC 3 Z9 3 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0964-1726 EI 1361-665X J9 SMART MATER STRUCT JI Smart Mater. Struct. PD DEC PY 2014 VL 23 IS 12 AR 125009 DI 10.1088/0964-1726/23/12/125009 PG 13 WC Instruments & Instrumentation; Materials Science, Multidisciplinary SC Instruments & Instrumentation; Materials Science GA AT9WU UT WOS:000345275400010 ER PT J AU Hurwitz, MM Calvo, N Garfinkel, CI Butler, AH Ineson, S Cagnazzo, C Manzini, E Pena-Ortiz, C AF Hurwitz, Margaret M. Calvo, Natalia Garfinkel, Chaim I. Butler, Amy H. Ineson, Sarah Cagnazzo, Chiara Manzini, Elisa Pena-Ortiz, Cristina TI Extra-tropical atmospheric response to ENSO in the CMIP5 models SO CLIMATE DYNAMICS LA English DT Article DE ENSO; Stratosphere; Teleconnections; CMIP5 ID POOL EL-NINO; TELECONNECTIONS; STRATOSPHERE; TEMPERATURES; VARIABILITY; EVENTS; WINTER AB The seasonal mean extra-tropical atmospheric response to El Nino/ Southern Oscillation (ENSO) is assessed in the historical and pre-industrial control CMIP5 simulations. This analysis considers two types of El Nino events, characterized by positive sea surface temperature (SST) anomalies in either the central equatorial Pacific (CP) or eastern equatorial Pacific (EP), as well as EP and CP La Nina events, characterized by negative SST anomalies in the same two regions. Seasonal mean geopotential height anomalies in key regions typify the magnitude and structure of the disruption of the Walker circulation cell in the tropical Pacific, upper tropospheric ENSO teleconnections and the polar stratospheric response. In the CMIP5 ensembles, the magnitude of the Walker cell disruption is correlated with the strength of the mid-latitude responses in the upper troposphere i.e., the North Pacific and South Pacific lows strengthen during El Nino events. The simulated responses to El Nino and La Nina have opposite sign. The seasonal mean extra-tropical, upper tropospheric responses to EP and CP events are indistinguishable. The ENSO responses in the MERRA reanalysis lie within the model scatter of the historical simulations. Similar responses are simulated in the pre-industrial and historical CMIP5 simulations. Overall, there is a weak correlation between the strength of the tropical response to ENSO and the strength of the polar stratospheric response. ENSO-related polar stratospheric variability is best simulated in the "high-top'' subset of models with a well-resolved stratosphere. C1 [Hurwitz, Margaret M.] Morgan State Univ, Goddard Earth Sci Technol & Res GESTAR, Baltimore, MD 21239 USA. [Hurwitz, Margaret M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Calvo, Natalia] Univ Complutense Madrid, Madrid, Spain. [Garfinkel, Chaim I.] Hebrew Univ Jerusalem, Jerusalem, Israel. [Butler, Amy H.] NOAA, CIRES, Earth Sci Res Lab, Boulder, CO USA. [Ineson, Sarah] Hadley Ctr, Met Off, Exeter, Devon, England. [Cagnazzo, Chiara] Consiglio Nazl Ric ISAC CNR, Ist Fis Atmosfera Clima, Rome, Italy. [Manzini, Elisa] Max Planck Inst Meteorol, D-20146 Hamburg, Germany. [Pena-Ortiz, Cristina] Univ Pablo Olavide, Seville, Spain. RP Hurwitz, MM (reprint author), NASA, Goddard Space Flight Ctr, Code 614, Greenbelt, MD 20771 USA. EM margaret.m.hurwitz@nasa.gov RI Butler, Amy/K-6190-2012; Cagnazzo, Chiara/C-7194-2015; garfinkel, chaim/H-6215-2012; Manager, CSD Publications/B-2789-2015; OI Butler, Amy/0000-0002-3632-0925; garfinkel, chaim/0000-0001-7258-666X; CALVO FERNANDEZ, NATALIA/0000-0001-6213-1864 FU NASA; DECC/Defra Met Office Hadley Centre [GA01101] FX Margaret M. Hurwitz thanks the NASA Atmospheric Composition, Modeling and Analysis Program (ACMAP) and Modeling, Analysis and Prediction (MAP) program for funding, and the World Climate Research Programme (WCRP) and Stratospheric Processes and their Role in Climate (SPARC) DynVar for travel support. Sarah Ineson was supported by the Joint DECC/Defra Met Office Hadley Centre Climate Programme (GA01101). The authors thank two anonymous reviewers for their helpful feedback. NR 34 TC 6 Z9 6 U1 3 U2 33 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 EI 1432-0894 J9 CLIM DYNAM JI Clim. Dyn. PD DEC PY 2014 VL 43 IS 12 BP 3367 EP 3376 DI 10.1007/s00382-014-2110-z PG 10 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AT3UX UT WOS:000344861900010 ER PT J AU Lin, NH Sayer, AM Wang, SH Loftus, AM Hsiao, TC Sheu, GR Hsu, NC Tsay, SC Chantara, S AF Lin, Neng-Huei Sayer, Andrew M. Wang, Sheng-Hsiang Loftus, Adrian M. Hsiao, Ta-Chih Sheu, Guey-Rong Hsu, N. Christina Tsay, Si-Chee Chantara, Somporn TI Interactions between biomass-burning aerosols and clouds over Southeast Asia: Current status, challenges, and perspectives SO ENVIRONMENTAL POLLUTION LA English DT Article DE Biomass-burning aerosol; Aerosol-cloud interaction; 7-SEAS; Remote sensing; Aerosol chemistry; Southeast Asia ID MARINE BOUNDARY-LAYER; BULK MICROPHYSICS PARAMETERIZATION; LARGE-EDDY SIMULATION; EAST CHINA SEA; OPTICAL DEPTH; STRATOCUMULUS CLOUDS; EFFECTIVE RADIUS; SATELLITE DATA; 7-SEAS/DONGSHA EXPERIMENT; TROPOSPHERIC AEROSOLS AB The interactions between aerosols, clouds, and precipitation remain among the largest sources of uncertainty in the Earth's energy budget. Biomass-burning aerosols are a key feature of the global aerosol system, with significant annually-repeating fires in several parts of the world, including Southeast Asia (SEA). SEA in particular provides a "natural laboratory" for these studies, as smoke travels from source regions downwind in which it is coupled to persistent stratocumulus decks. However, SEA has been under-exploited for these studies. This review summarizes previous related field campaigns in SEA, with a focus on the ongoing Seven South East Asian Studies (7-SEAS) and results from the most recent BASELInE deployment. Progress from remote sensing and modeling studies, along with the challenges faced for these studies, are also discussed. We suggest that improvements to our knowledge of these aerosol/cloud effects require the synergistic use of field measurements with remote sensing and modeling tools. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Lin, Neng-Huei; Wang, Sheng-Hsiang; Sheu, Guey-Rong] Natl Cent Univ, Dept Atmospher Sci, Chungli 32054, Taiwan. [Lin, Neng-Huei; Chantara, Somporn] Chiang Mai Univ, Fac Sci, Chem Dept & Environm Sci Program, Chiang Mai 50200, Thailand. [Sayer, Andrew M.; Loftus, Adrian M.; Hsu, N. Christina; Tsay, Si-Chee] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sayer, Andrew M.] Univ Space Res Assoc, Columbia, MD USA. [Loftus, Adrian M.] Oak Ridge Associated Univ, Oak Ridge, TN USA. [Hsiao, Ta-Chih] Natl Cent Univ, Grad Inst Environm Engn, Chungli 32054, Taiwan. RP Lin, NH (reprint author), Natl Cent Univ, Dept Atmospher Sci, Chungli 32054, Taiwan. EM nhlin@cc.ncu.edu.tw RI Sayer, Andrew/H-2314-2012; Wang, Sheng-Hsiang/F-4532-2010 OI Sayer, Andrew/0000-0001-9149-1789; Wang, Sheng-Hsiang/0000-0001-9675-3135 FU Taiwan Environmental Protection Administration [EPA-99-FA11-03-A097, EPA-102-U1L1-02-101]; National Science Council of Taiwan [101-2119-M-008-012] FX The authors thank the continuous support by the Taiwan Environmental Protection Administration under contracts No. EPA-99-FA11-03-A097, EPA-102-U1L1-02-101, and the National Science Council of Taiwan under grant No. 101-2119-M-008-012 for the field operation of 2013 BASELInE. We also thank the Deployments of SMARTLabs and AERONET/MPLNET in Southeast Asia, as part of NASA Radiation Sciences Program managed by Dr. Hal B. Maring. The authors also gratefully acknowledge the team efforts led by Serm Janjai (Silpakorn University, Thailand), Somporn Chantara (Chiang Mai University, Thailand) and Anh X. Nguyen (Institute of Geophysics at Vietnam Academy of Science and Technology, Vietnam) in supporting 7-SEAS/BASELInE over northern Southeast Asia. National Central University, National Museum of Marine Biology and Aquarium, Middle of Central Regional Hydro-Meteorological Observatory, National Hydro-Meteorological Service of Vietnam, and Doi Ang Khang Meteorological Station, facilitated site operations at Lulin, Hengchun, Son La/Yen Bai, and Doi Ang Khang, respectively. Thanks are also given to all assistants and graduate students involving in the site operation, data analysis and technical support for making 2013 BASELInE campaign successful. NR 176 TC 16 Z9 16 U1 5 U2 54 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0269-7491 EI 1873-6424 J9 ENVIRON POLLUT JI Environ. Pollut. PD DEC PY 2014 VL 195 BP 292 EP 307 DI 10.1016/j.envpol.2014.06.036 PG 16 WC Environmental Sciences SC Environmental Sciences & Ecology GA AS7LM UT WOS:000344437600037 PM 25085565 ER PT J AU Hecht, BC Valle, ME Thrower, FP Nichols, KM AF Hecht, Benjamin C. Valle, Madeline E. Thrower, Frank P. Nichols, Krista M. TI Divergence in Expression of Candidate Genes for the Smoltification Process Between Juvenile Resident Rainbow and Anadromous Steelhead Trout SO MARINE BIOTECHNOLOGY LA English DT Article DE Gene expression; Maturation; Migration; Smoltification; Trout ID SALMON SALMO-SALAR; PARR-SMOLT TRANSFORMATION; GROWTH-FACTOR-I; ZEBRAFISH DANIO-RERIO; TIME RT-PCR; ONCORHYNCHUS-MYKISS; ATLANTIC SALMON; SEAWATER ADAPTATION; CHINOOK SALMON; PACIFIC SALMON AB Rainbow and steelhead trout (Oncorhynchus mykiss), among other salmonid fishes, exhibit tremendous life history diversity, foremost of which is variation in migratory propensity. While some individuals possess the ability to undertake an anadromous marine migration, others remain resident in freshwater throughout their life cycle. Those that will migrate undergo tremendous physiological, morphological, and behavioral transformations in a process called smoltification which transitions freshwater-adapted parr to marine-adapted smolts. While the behavior, ecology, and physiology of smoltification are well described, our understanding of the proximate genetic mechanisms that trigger the process are not well known. Quantitative genetic analyses have identified several genomic regions associated with smoltification and migration-related traits within this species. Here we investigate the divergence in gene expression of 18 functional and positional candidate genes for the smoltification process in the brain, gill, and liver tissues of migratory smolts, resident parr, and precocious mature male trout at the developmental stage of out-migration. Our analysis reveals several genes differentially expressed between life history classes and validates the candidate nature of several genes in the parr-smolt transformation including Clock1 alpha, FSH beta, GR, GH2, GHR1, GHR2, NDK7, p53, SC6a7, Taldo1, THR alpha, THR beta, and Vdac2. C1 [Hecht, Benjamin C.; Valle, Madeline E.; Nichols, Krista M.] Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA. [Nichols, Krista M.] Purdue Univ, Dept Forestry & Nat Resources, W Lafayette, IN 47907 USA. [Hecht, Benjamin C.] Univ Idaho, Inst Aquaculture Res, Hagerman Fish Culture Expt Stn, Moscow, ID 83844 USA. [Hecht, Benjamin C.] Fishery Sci Dept, Columbia River Intertribal Fish Commiss, Hagerman, ID 83332 USA. [Thrower, Frank P.] NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK 99801 USA. [Nichols, Krista M.] NOAA, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Seattle, WA 98112 USA. RP Nichols, KM (reprint author), NOAA, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2725 Montlake Blvd East, Seattle, WA 98112 USA. EM krista.nichols@noaa.gov FU Ecological Genetics Area of Excellence in the Department of Forestry and Natural Resources, Purdue University; [NSF-DEB-0845265] FX The authors would like to thank the research and support staff at the Little Port Walter Marine Research Station, National Oceanic and Atmospheric Administration, Baranof Island, AK, particularly Pat Malecha, Dan Koenig, Don Cummins, and Charlie Waters for the rearing and husbandry of the juvenile rainbow and steelhead trout used in this experiment. We thank and acknowledge Katlin Walls, Julie Scardina, Matt Hale, Ashley Chin-Baarstad, Roxanne Croxall, and Shannon Torstrom for their tremendous and invaluable assistance in the lab both in design and execution of qPCR experiments and the selection of candidate genes. We thank Andreas Brezas and Barrie Robison for valuable insight on qPCR analysis. We additionally thank Shawn Narum, Ken Overturf, and Ron Hardy for support and use of lab equipment, and anonymous reviewers for suggestions that improved this manuscript. This work was partially funded by a NSF-DEB-0845265 Career Award to KMN and by funding through the Ecological Genetics Area of Excellence in the Department of Forestry and Natural Resources, Purdue University. NR 94 TC 3 Z9 3 U1 10 U2 53 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1436-2228 EI 1436-2236 J9 MAR BIOTECHNOL JI Mar. Biotechnol. PD DEC PY 2014 VL 16 IS 6 BP 638 EP 656 DI 10.1007/s10126-014-9579-7 PG 19 WC Biotechnology & Applied Microbiology; Marine & Freshwater Biology SC Biotechnology & Applied Microbiology; Marine & Freshwater Biology GA AS9DQ UT WOS:000344543800003 PM 24952010 ER PT J AU Nitta, NV Liu, W Gopalswamy, N Yashiro, S AF Nitta, Nariaki V. Liu, Wei Gopalswamy, Nat Yashiro, Seiji TI The Relation Between Large-Scale Coronal Propagating Fronts and Type II Radio Bursts SO SOLAR PHYSICS LA English DT Article DE Shock waves; Coronal mass ejections; Solar Dynamics Observatory; Extreme Ultraviolet emission; Radio emission ID EXTREME-ULTRAVIOLET WAVE; EIT WAVES; MASS EJECTION; SOHO/EIT OBSERVATIONS; SOLAR ERUPTIONS; MORETON WAVES; FLARE WAVES; EUV IMAGES; SDO/AIA; SHOCK AB Large-scale, wave-like disturbances in extreme-ultraviolet (EUV) and type II radio bursts are often associated with coronal mass ejections (CMEs). Both phenomena may signify shock waves driven by CMEs. Taking EUV full-disk images at an unprecedented cadence, the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory has observed the so-called EIT waves or large-scale coronal propagating fronts (LCPFs) from their early evolution, which coincides with the period when most metric type II bursts occur. This article discusses the relation of LCPFs as captured by AIA with metric type II bursts. We show examples of type II bursts without a clear LCPF and fast LCPFs without a type II burst. Part of the disconnect between the two phenomena may be due to the difficulty in identifying them objectively. Furthermore, it is possible that the individual LCPFs and type II bursts may reflect different physical processes and external factors. In particular, the type II bursts that start at low frequencies and high altitudes tend to accompany an extended arc-shaped feature, which probably represents the 3D structure of the CME and the shock wave around it, and not just its near-surface track, which has usually been identified with EIT waves. This feature expands and propagates toward and beyond the limb. These events may be characterized by stretching of field lines in the radial direction and may be distinct from other LCPFs, which may be explained in terms of sudden lateral expansion of the coronal volume. Neither LCPFs nor type II bursts by themselves serve as necessary conditions for coronal shock waves, but these phenomena may provide useful information on the early evolution of the shock waves in 3D when both are clearly identified in eruptive events. C1 [Nitta, Nariaki V.; Liu, Wei] Lockheed Martin Solar & Astrophys Lab, Dept A021S, Palo Alto, CA 94304 USA. [Liu, Wei] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Gopalswamy, Nat; Yashiro, Seiji] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Yashiro, Seiji] Catholic Univ Amer, Washington, DC 20064 USA. RP Nitta, NV (reprint author), Lockheed Martin Solar & Astrophys Lab, Dept A021S, Bldg 252,3251 Hanover St, Palo Alto, CA 94304 USA. EM nitta@lmsal.com; weiliu@lmsal.com; Nat.Gopalswamy@nasa.gov; Seiji.Yashiro@nasa.gov FU NSF [AGS-1259549]; NASA AIA [NNG04EA00C]; NASA STEREO mission under NRL [N00173-02-C-2035]; NASA [NNX11AO68G]; NASA LWS TRT program FX This work has been supported by the NSF grant AGS-1259549, NASA AIA contract NNG04EA00C and the NASA STEREO mission under NRL Contract No. N00173-02-C-2035. NASA grant NNX11AO68G supported the work of WL. The work of NG and SY was supported by the NASA LWS TR&T program. NR 58 TC 4 Z9 4 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD DEC PY 2014 VL 289 IS 12 BP 4589 EP 4606 DI 10.1007/s11207-014-0602-y PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT0FI UT WOS:000344612200010 ER PT J AU Kovaltsov, GA Usoskin, IG Cliver, EW Dietrich, WF Tylka, AJ AF Kovaltsov, G. A. Usoskin, I. G. Cliver, E. W. Dietrich, W. F. Tylka, A. J. TI Fluence Ordering of Solar Energetic Proton Events Using Cosmogenic Radionuclide Data SO SOLAR PHYSICS LA English DT Article DE Solar energetic particles; Cosmogenic radioisotopes ID TREE-RINGS; SPACE WEATHER; C-14 CONTENT; COSMIC-RAYS; AD 774-775; ATMOSPHERE; INCREASE; MODEL; SUN AB While data on the cosmogenic isotopes C-14 and Be-10 made it possible to evaluate extreme solar proton events (SPEs) in the past, their relation to standard parameters quantifying the SPE strengths, viz. the integrated fluence of protons with energy above 30 MeV, F (30), is ambiguous and strongly depends on the assumed shape of the energy spectrum. Here we propose a new index, the integral fluence of an SPE above 200 MeV, F (200), which is related to the production of the cosmogenic isotopes C-14 and Be-10 in the Earth atmosphere, independently of the assumptions on the energy spectrum of the event. The F (200) fluence is reconstructed from past cosmogenic isotope data, which provides an assessment of the occurrence probability density function for extreme SPEs. In particular, we evaluate that extreme SPEs with F (200)> 10(10) cm(-2) occur no more frequently than once per 10 -aEuro parts per thousand 15 kyr. C1 [Kovaltsov, G. A.] AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia. [Usoskin, I. G.] Univ Oulu, Oulu Unit, Sodankyla Geophys Observ, Oulu, Finland. [Usoskin, I. G.] Univ Oulu, Dept Phys, FIN-90570 Oulu, Finland. [Cliver, E. W.] Air Force Res Lab, Space Vehicles Directorate, Albuquerque, NM 87117 USA. [Cliver, E. W.] Natl Solar Observ, Sunspot, NM 88349 USA. [Dietrich, W. F.] Praxis Inc, Alexandria, VA 22303 USA. [Tylka, A. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Usoskin, IG (reprint author), Univ Oulu, Oulu Unit, Sodankyla Geophys Observ, Oulu, Finland. EM ilya.usoskin@oulu.fi FU Academy of Finland; ReSoLVE Centre of Excellence (Academy of Finland) [272157]; Air Force Office of Scientific Research; NASA Solar & Heliophysics SRT [NNH12AT09I] FX G.A. Kovaltsov is grateful to the Academy of Finland for partial support. I. G. Usoskin's contribution was made in the framework of the ReSoLVE Centre of Excellence (Academy of Finland, project no. 272157). E. W. Cliver acknowledges support from the Air Force Office of Scientific Research. A.J. Tylka and W.F. Dietrich are supported by NASA Solar & Heliophysics SR&T under NNH12AT09I. NR 36 TC 10 Z9 10 U1 0 U2 8 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD DEC PY 2014 VL 289 IS 12 BP 4691 EP 4700 DI 10.1007/s11207-014-0606-7 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT0FI UT WOS:000344612200016 ER PT J AU Reynolds, RL Goldstein, HL Moskowitz, BM Bryant, AC Skiles, SM Kokaly, RF Flagg, CB Yauk, K Berquo, T Breit, G Ketterer, M Fernandez, D Miller, ME Painter, TH AF Reynolds, Richard L. Goldstein, Harland L. Moskowitz, Bruce M. Bryant, Ann C. Skiles, S. McKenzie Kokaly, Raymond F. Flagg, Cody B. Yauk, Kimberly Berquo, Thelma Breit, George Ketterer, Michael Fernandez, Daniel Miller, Mark E. Painter, Thomas H. TI Composition of dust deposited to snow cover in the Wasatch Range (Utah, USA): Controls on radiative properties of snow cover and comparison to some dust-source sediments SO AEOLIAN RESEARCH LA English DT Article DE Atmospheric dust; Magnetic properties; Goethite; Hematite; Black carbon; Metals ID M-RS/M-S; ROCKY-MOUNTAINS; MINERAL DUST; DESERT DUST; ENVIRONMENTAL MAGNETISM; MOSSBAUER-SPECTROSCOPY; PARTICULATE MATTER; HYPERFINE FIELD; AIR-POLLUTION; PARTICLE-SIZE AB Dust layers deposited to snow cover of the Wasatch Range (northern Utah) in 2009 and 2010 provide rare samples to determine the relations between their compositions and radiative properties. These studies are required to comprehend and model how such dust-on-snow (DOS) layers affect rates of snow melt through changes in the albedo of snow surfaces. We evaluated several constituents as potential contributors to the absorption of solar radiation indicated by values of absolute reflectance determined from biconical reflectance spectroscopy. Ferric oxide minerals and carbonaceous matter appear to be the primary influences on lowering snow-cover albedo. Techniques of reflectance and Mossbauer spectroscopy as well as rock magnetism provide information about the types, amounts, and grain sizes of ferric oxide minerals. Relatively high amounts of ferric oxide, indicated by hard isothermal remanent magnetization (HIRM), are associated with relatively low average reflectance (<0.25) across the visible wavelengths of the electromagnetic spectrum. Mossbauer spectroscopy indicates roughly equal amounts of hematite and goethite, representing about 35% of the total Fe-bearing phases. Nevertheless, goethite (alpha-FeOOH) is the dominant ferric oxide found by reflectance spectroscopy and thus appears to be the main iron oxide control on absorption of solar radiation. At least some goethite occurs as nano-phase grain coatings less than about 50 nm thick. Relatively high amounts of organic carbon, indicating as much as about 10% organic matter, are also associated with lower reflectance values. The organic matter, although not fully characterized by type, correlates strongly with metals (e.g., Cu, Pb, As, Cd, Mo, Zn) derived from distal urban and industrial settings, probably including mining and smelting sites. This relation suggests anthropogenic sources for at least some of the carbonaceous matter, such as emissions from transportation and industrial activities. The composition of the DOS samples can be compared with sediments in a likely dust-source setting at the Milford Flat Fire (MFF) area about 225 km southwest of Salt Lake City. The MFF area represents geologically and physiographically similar and widespread dust sources west-southwest of the Wasatch Range and heavily populated Wasatch Front. The DOS layers and MFF sediments are similar in some textural, chemical, and magnetic properties, as well as in the common presence of goethite, hematite, magnetite-bearing basalt fragments, quartz, plagioclase, illite, and kaolinite. Textural and some chemical differences among these deposits can be explained by atmospheric sorting as well as by inputs from other settings, such as salt-crusted playas and contaminant sources. Published by Elsevier B.V. C1 [Reynolds, Richard L.; Goldstein, Harland L.; Kokaly, Raymond F.; Breit, George] US Geol Survey, Denver, CO 80225 USA. [Moskowitz, Bruce M.; Yauk, Kimberly] Univ Minnesota, Dept Earth Sci, Inst Rock Magnetism, Minneapolis, MN USA. [Bryant, Ann C.] Univ Utah, Dept Geog, Salt Lake City, UT USA. [Skiles, S. McKenzie] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90024 USA. [Kokaly, Raymond F.] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA. [Flagg, Cody B.] US Geol Survey, Moab, UT USA. [Berquo, Thelma] Concordia Coll, Dept Phys, Moorhead, MN USA. [Ketterer, Michael] No Arizona Univ, Dept Chem, Flagstaff, AZ 86011 USA. [Fernandez, Daniel] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. [Miller, Mark E.] Natl Pk Serv, Moab, UT USA. [Painter, Thomas H.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Reynolds, RL (reprint author), US Geol Survey, Bldg 53,Entrance 5-1,Box 25046,MS 980, Denver, CO 80225 USA. EM rreynolds@usgs.gov RI Painter, Thomas/B-7806-2016; Kokaly, Raymond/A-6817-2017 OI Kokaly, Raymond/0000-0003-0276-7101 FU U.S. Geological Survey's Climate and Land Use Change Program; NSF [CHE-0118604]; Arizona Technology Research and Innovation Fund; Instruments and Facilities Program of the National Science Foundation Division of Earth Science FX We are grateful to Jeff Deems and two anonymous reviewers for improving this manuscript. For motivating discussions and assistance in the field, we thank Marith Reheis and Jim Yount, and for laboratory analyses, we thank Jiang Xiao, Gary Skipp, and Eric Fisher. We are also grateful to Roger Clark and Todd Hoeffen for use of the USGS Spectroscopy Laboratory, Denver, and to Subir Banerjee for critical discussion of the magnetic and Mossbauer results. Collection of the dust-on-snow samples was part of a joint University of Utah-U.S. Forest Service project. Support was provided by U.S. Geological Survey's Climate and Land Use Change Program and (for MEK) by NSF CHE-0118604 and the Arizona Technology Research and Innovation Fund for the ICPMS lab facilities. Part of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. The Institute for Rock Magnetism is supported by grants from the Instruments and Facilities Program of the National Science Foundation Division of Earth Science. This is IRM Contribution 1302. NR 103 TC 11 Z9 11 U1 5 U2 39 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1875-9637 EI 2212-1684 J9 AEOLIAN RES JI Aeolian Res. PD DEC PY 2014 VL 15 BP 73 EP 90 DI 10.1016/j.aeolia.2013.08.001 PG 18 WC Geography, Physical SC Physical Geography GA AS7FT UT WOS:000344423300006 ER PT J AU Kelley, CA Nicholson, BE Beaudoin, CS Detweiler, AM Bebout, BM AF Kelley, Cheryl A. Nicholson, Brooke E. Beaudoin, Claire S. Detweiler, Angela M. Bebout, Brad M. TI Trimethylamine and Organic Matter Additions Reverse Substrate Limitation Effects on the delta C-13 Values of Methane Produced in Hypersaline Microbial Mats SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID CARBON-ISOTOPE FRACTIONATION; METHANOSARCINA-BARKERI; BAJA-CALIFORNIA; GLYCINE BETAINE; GUERRERO NEGRO; METHANOGENESIS; ENVIRONMENTS; DIVERSITY; SEDIMENTS; HYDROGEN AB Methane production has been observed in a number of hypersaline environments, and it is generally thought that this methane is produced through the use of noncompetitive substrates, such as the methylamines, dimethylsulfide and methanol. Stable isotope measurements of the produced methane have also suggested that the methanogens are operating under conditions of substrate limitation. Here, substrate limitation in gypsum-hosted endoevaporite and soft-mat hypersaline environments was investigated by the addition of trimethylamine, a noncompetitive substrate for methanogenesis, and dried microbial mat, a source of natural organic matter. The delta C-13 values of the methane produced after amendments were compared to those in unamended control vials. At all hypersaline sites investigated, the delta C-13 values of the methane produced in the amended vials were statistically lower (by 10 to 71%) than the unamended controls, supporting the hypothesis of substrate limitation at these sites. When substrates were added to the incubation vials, the methanogens within the vials fractionated carbon isotopes to a greater degree, resulting in the production of more C-13-depleted methane. Trimethylamine-amended samples produced lower methane delta C-13 values than the mat-amended samples. This difference in the delta C-13 values between the two types of amendments could be due to differences in isotope fractionation associated with the dominant methane production pathway (or substrate used) within the vials, with trimethylamine being the main substrate used in the trimethylamine-amended vials. It is hypothesized that increased natural organic matter in the mat-amended vials would increase fermentation rates, leading to higher H-2 concentrations and increased CO2/H-2 methanogenesis. C1 [Kelley, Cheryl A.; Nicholson, Brooke E.; Beaudoin, Claire S.] Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. [Detweiler, Angela M.; Bebout, Brad M.] NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA USA. RP Kelley, CA (reprint author), Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. EM kelleyc@missouri.edu RI Kelley, Cheryl/K-9392-2015 FU NASA exobiology grants FX This study was supported by NASA exobiology grants to C.A.K. and B.M.B. NR 40 TC 5 Z9 5 U1 1 U2 13 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 EI 1098-5336 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD DEC PY 2014 VL 80 IS 23 BP 7316 EP 7323 DI 10.1128/AEM.02641-14 PG 8 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA AS3FW UT WOS:000344163700022 PM 25239903 ER PT J AU Zhang, YG Guanter, L Berry, JA Joiner, J van der Tol, C Huete, A Gitelson, A Voigt, M Kohler, P AF Zhang, Yongguang Guanter, Luis Berry, Joseph A. Joiner, Joanna van der Tol, Christiaan Huete, Alfredo Gitelson, Anatoly Voigt, Maximilian Koehler, Philipp TI Estimation of vegetation photosynthetic capacity from space-based measurements of chlorophyll fluorescence for terrestrial biosphere models SO GLOBAL CHANGE BIOLOGY LA English DT Article DE Farquhar model Cropland; GPP; photosynthesis; SCOPE; Solar-induced fluorescence; V-cmax ID GROSS PRIMARY PRODUCTION; LEAF OPTICAL-PROPERTIES; NET ECOSYSTEM EXCHANGE; LIGHT USE EFFICIENCY; STOMATAL CONDUCTANCE; CO2 ASSIMILATION; DECIDUOUS FOREST; BIOCHEMICAL-MODEL; SEASONAL PATTERN; ENERGY-BALANCE AB Photosynthesis simulations by terrestrial biosphere models are usually based on the Farquhar's model, in which the maximum rate of carboxylation (V-cmax) is a key control parameter of photosynthetic capacity. Even though V-cmax is known to vary substantially in space and time in response to environmental controls, it is typically parameterized in models with tabulated values associated to plant functional types. Remote sensing can be used to produce a spatially continuous and temporally resolved view on photosynthetic efficiency, but traditional vegetation observations based on spectral reflectance lack a direct link to plant photochemical processes. Alternatively, recent space-borne measurements of sun-induced chlorophyll fluorescence (SIF) can offer an observational constraint on photosynthesis simulations. Here, we show that top-of-canopy SIF measurements from space are sensitive to V-cmax at the ecosystem level, and present an approach to invert V-cmax from SIF data. We use the Soil-Canopy Observation of Photosynthesis and Energy (SCOPE) balance model to derive empirical relationships between seasonal V-cmax and SIF which are used to solve the inverse problem. We evaluate our V-cmax estimation method at six agricultural flux tower sites in the midwestern US using spaced-based SIF retrievals. Our V-cmax estimates agree well with literature values for corn and soybean plants (average values of 37 and 101molm(-2)s(-1), respectively) and show plausible seasonal patterns. The effect of the updated seasonally varying V-cmax parameterization on simulated gross primary productivity (GPP) is tested by comparing to simulations with fixed V-cmax values. Validation against flux tower observations demonstrate that simulations of GPP and light use efficiency improve significantly when our time-resolved V-cmax estimates from SIF are used, with R-2 for GPP comparisons increasing from 0.85 to 0.93, and for light use efficiency from 0.44 to 0.83. Our results support the use of space-based SIF data as a proxy for photosynthetic capacity and suggest the potential for global, time-resolved estimates of V-cmax. C1 [Zhang, Yongguang; Guanter, Luis; Voigt, Maximilian; Koehler, Philipp] Free Univ Berlin, Inst Space Sci, D-12165 Berlin, Germany. [Berry, Joseph A.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. [Joiner, Joanna] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [van der Tol, Christiaan] Int Inst Geoinformat Sci & Earth Observat, NL-7500 AA Enschede, Netherlands. [Huete, Alfredo] Univ Technol Sydney, Plant Funct Biol & Climate Change Cluster, Sydney, NSW 2007, Australia. [Gitelson, Anatoly] Univ Nebraska, Sch Nat Resources, Lincoln, NE 68583 USA. RP Zhang, YG (reprint author), Free Univ Berlin, Inst Space Sci, D-12165 Berlin, Germany. EM yongguang.zhang@wew.fu-berlin.de RI Guanter, Luis/I-1588-2015; Huete, Alfredo/C-1294-2008; van der Tol, Christiaan/A-2403-2010; OI Guanter, Luis/0000-0002-8389-5764; Huete, Alfredo/0000-0003-2809-2376; van der Tol, Christiaan/0000-0002-2484-8191; Zhang, Yongguang/0000-0001-8286-300X FU Emmy Noether Programme (GlobFluo project) of the German Research Foundation - NASA Carbon Cycle Science program [NNH10DA001N] FX We would like to thank the two reviewers for their valuable comments and suggestions. The work by YZ and LG has been funded by the Emmy Noether Programme (GlobFluo project) of the German Research Foundation. JJ was supported by the NASA Carbon Cycle Science program (NNH10DA001N). We acknowledge Eumetsat for the GOME-2 data. MODIS MOD13 EVI/NDVI data were obtained from the MODIS LP DAAC archive and MERIS-MTCI from the Infoterra Ltd server. This work used eddy covariance data acquired by AmeriFlux. We further thank PIs of the flux tower sites: T. Meyers (NOAA/ARL), D. Cook and R. Matamala (Argonne National Laboratory), and A. Suyker (Univ. Nebraska). NR 78 TC 48 Z9 50 U1 17 U2 127 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1354-1013 EI 1365-2486 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD DEC PY 2014 VL 20 IS 12 BP 3727 EP 3742 DI 10.1111/gcb.12664 PG 16 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AS6LS UT WOS:000344375700015 PM 24953485 ER PT J AU Fu, YSH Piao, SL Zhao, HF Jeong, SJ Wang, XH Vitasse, Y Ciais, P Janssens, IA AF Fu, Yongshuo H. Piao, Shilong Zhao, Hongfang Jeong, Su-Jong Wang, Xuhui Vitasse, Yann Ciais, Philippe Janssens, Ivan A. TI Unexpected role of winter precipitation in determining heat requirement for spring vegetation green-up at northern middle and high latitudes SO GLOBAL CHANGE BIOLOGY LA English DT Article DE green-up onset; growing degree days; phenology; precipitation; spatial pattern; winter chilling ID TERRESTRIAL BIOSPHERE MODEL; NDVI TIME-SERIES; CLIMATE VARIABILITY; SPECIES-RICHNESS; SATELLITE DATA; THERMAL TIME; MODIS DATA; BUD BURST; PHENOLOGY; TREES AB Heat requirement, expressed in growing degree days (GDD), is a widely used method to assess and predict the effect of temperature on plant development. Until recently, the analysis of spatial patterns of GDD requirement for spring vegetation green-up onset was limited to local and regional scales, mainly because of the sparse and aggregated spatial availability of ground phenology data. Taking advantage of the large temporal and spatial scales of remote sensing-based green-up onset data, we studied the spatial patterns of GDD requirement for vegetation green-up at northern middle and high latitudes. We further explored the correlations between GDD requirement for vegetation green-up and previous winter season chilling temperatures and precipitation, using spatial partial correlations. We showed that GDD requirement for vegetation green-up onset declines towards the north at a mean rate of 18.8 degrees C-days per degree latitude between 35 degrees N and 70 degrees N, and vary significantly among different vegetation types. Our results confirmed that the GDD requirement for vegetation green-up is negatively correlated with previous winter chilling, which was defined as the number of chilling days from the day when the land surface froze in the previous autumn to the day of green-up onset. This negative correlation is a well-known phenomenon from local studies. Interestingly, irrespective of the vegetation type, we also found a positive correlation between the GDD requirement and previous winter season precipitation, which was defined as the sum of the precipitation of the month when green-up onset occur and the precipitation that occurred during the previous 2months. Our study suggests that GDD requirement, chilling and precipitation may have complex interactions in their effects on spring vegetation green-up phenology. These findings have important implications for improving phenology models and could therefore advance our understanding of the interplay between spring phenology and carbon fluxes. C1 [Fu, Yongshuo H.; Piao, Shilong; Zhao, Hongfang; Wang, Xuhui] Peking Univ, Coll Urban & Environm Sci, Beijing 100871, Peoples R China. [Fu, Yongshuo H.; Janssens, Ivan A.] Univ Antwerp, Dept Biol, Res Grp Plant & Vegetat Ecol PLECO, B-2610 Antwerp, Belgium. [Piao, Shilong] Chinese Acad Sci, Inst Tibetan Plateau Res, Beijing 100085, Peoples R China. [Jeong, Su-Jong] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Vitasse, Yann] Univ Basel, Inst Bot, CH-4056 Basel, Switzerland. [Ciais, Philippe] CEA CNRS UVSQ, Lab Sci Climat & Environm, Gif Sur Yvette, France. RP Piao, SL (reprint author), Peking Univ, Coll Urban & Environm Sci, Yiheyuan Rd 5, Beijing 100871, Peoples R China. EM slpiao@pku.edu.cn RI Janssens, Ivan/P-1331-2014; Jeong, Su-Jong/J-4110-2014; OI Janssens, Ivan/0000-0002-5705-1787; Vitasse, Yann/0000-0002-7454-505X FU National Natural Science Foundation of China [41125004]; National Basic Research Program of China [2013CB956303]; 111 Project [B14001]; National Youth Top-notch Talent Support Program in China FX We thank Prof. Hanninen Heikki, Dr. Peng Shushi and two anonymous reviewers for constructive comments on a previous version, and we also thank Emmerich Barbara for polishing the English. This study was supported by the National Natural Science Foundation of China (41125004), National Basic Research Program of China (2013CB956303), the 111 Project (B14001) and National Youth Top-notch Talent Support Program in China. NR 76 TC 23 Z9 25 U1 8 U2 98 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1354-1013 EI 1365-2486 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD DEC PY 2014 VL 20 IS 12 BP 3743 EP 3755 DI 10.1111/gcb.12610 PG 13 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AS6LS UT WOS:000344375700016 PM 24753114 ER PT J AU Cheng, B Price, S Lydon, J Cooper, K Chou, K AF Cheng, Bo Price, Steven Lydon, James Cooper, Kenneth Chou, Kevin TI On Process Temperature in Powder-Bed Electron Beam Additive Manufacturing: Model Development and Validation SO JOURNAL OF MANUFACTURING SCIENCE AND ENGINEERING-TRANSACTIONS OF THE ASME LA English DT Article ID THERMAL-CONDUCTIVITY; NUMERICAL-SIMULATION; HEAT-TRANSFER; FLUID-FLOW; LASER; TITANIUM; OPTIMIZATION; EMISSIVITY; PREDICTION; COMPONENTS AB Powder-bed beam-based metal additive manufacturing (AM) such as electron beam additive manufacturing (EBAM) has a potential to offer innovative solutions to many challenges and difficulties faced in the manufacturing industry. However, the complex process physics of EBAM has not been fully understood, nor has process metrology such as temperatures been thoroughly studied, hindering part quality consistency, efficient process development and process optimizations, etc., for effective EBAM usage. In this study, numerical and experimental approaches were combined to research the process temperatures and other thermal characteristics in EBAM using Ti-6Al-4V powder. The objective of this study was to develop a comprehensive thermal model, using a finite element (FE) method, to predict temperature distributions and history in the EBAM process. On the other hand, a near infrared (NIR) thermal imager, with a spectral range of 0.78 mu m-1.08 mu m, was employed to acquire build surface temperatures in EBAM, with subsequent data processing for temperature profile and melt pool size analysis. The major results are summarized as follows. The thermal conductivity of Ti-6Al-4V powder is porosity dependent and is one of critical factors for temperature predictions. The measured thermal conductivity of preheated powder (of 50% porosity) is 2.44 W/mK versus 10.17 W/mK for solid Ti-6Al-4V at 750 degrees C. For temperature measurements in EBAM by NIR thermography, a method was developed to compensate temperature profiles due to transmission loss and unknown emissivity of liquid Ti-6Al-4V. At a beam speed of about 680 mm/s, a beam current of about 7.0mA and a diameter of 0.55 mm, the peak process temperature is on the order around 2700 degrees C, and the melt pools have dimensions of about 2.94 mm, 1.09 mm, and 0.12 mm, in length, width, and depth, respectively. In general, the simulations are in reasonable agreement with the experimental results with an average error of 32% for the melt pool sizes. From the simulations, the powder porosity is found critical to the thermal characteristics in EBAM. Increasing the powder porosity will elevate the peak process temperature and increase the melt pool size. C1 [Cheng, Bo; Price, Steven; Chou, Kevin] Univ Alabama, Dept Mech Engn, Tuscaloosa, AL 35487 USA. [Lydon, James; Cooper, Kenneth] NASA, George C Marshall Space Flight Ctr, Addit Mfg Lab, Huntsville, AL 35812 USA. RP Chou, K (reprint author), Univ Alabama, Dept Mech Engn, Tuscaloosa, AL 35487 USA. EM kchou@eng.ua.edu FU NASA [NNX11AM11A]; Marshall Space Flight Center (Huntsville, AL), Advanced Manufacturing Team in Nonmetallic Branch FX This research was supported by NASA, No. NNX11AM11A, and is in collaboration with Marshall Space Flight Center (Huntsville, AL), Advanced Manufacturing Team in Nonmetallic Branch. NR 48 TC 2 Z9 2 U1 7 U2 64 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 1087-1357 EI 1528-8935 J9 J MANUF SCI E-T ASME JI J. Manuf. Sci. Eng.-Trans. ASME PD DEC PY 2014 VL 136 IS 6 SI SI AR 061018 DI 10.1115/1.4028484 PG 12 WC Engineering, Manufacturing; Engineering, Mechanical SC Engineering GA AS6SQ UT WOS:000344393000020 ER PT J AU Price, S Cheng, B Lydon, J Cooper, K Chou, K AF Price, Steven Cheng, Bo Lydon, James Cooper, Kenneth Chou, Kevin TI On Process Temperature in Powder-Bed Electron Beam Additive Manufacturing: Process Parameter Effects SO JOURNAL OF MANUFACTURING SCIENCE AND ENGINEERING-TRANSACTIONS OF THE ASME LA English DT Article ID FINITE-ELEMENT-ANALYSIS; LASER; MICROSTRUCTURE; DEPOSITION; STEEL; SIZE AB Build part certification has been one of the primary roadblocks for effective usage and broader applications of metal additive manufacturing (AM) technologies including powder-bed electron beam additive manufacturing (EBAM). Process sensitivity to operating parameters, among others such as powder stock variations, is one major source of property scattering in EBAM parts. Thus, it is important to establish quantitative relations between the process parameters and process thermal characteristics that are closely correlated with the AM part properties. In this study, the experimental techniques, fabrications, and temperature measurements, developed in recent work (Cheng et al., 2014, "On Process Temperature in Powder-Bed Electron Beam Additive Manufacturing: Model Development and Experimental Validation," ASME J. Manuf. Sci. Eng., (in press)) were applied to investigate the process parameter effects on the thermal characteristics in EBAM with Ti-6Al-4 V powder, using the system-specific setting called " speed function (SF)" index that controls the beam speed and the beam current during a build. EBAM parts were fabricated using different levels of SF index (20-65) and examined in the part surface morphology and microstructures. In addition, process temperatures were measured by near infrared (NIR) thermography with further analysis of the temperature profiles and the melt pool size. The thermal model, also developed in recent work, was further employed for EBAM temperature predictions, and then compared with the experimental results. The major results are summarized as follows. SF index noticeably affects the thermal characteristics in EBAM, e. g., a melt pool length of 1.72mm and 1.26mm for SF20 and SF65, respectively, at 24.43 mm build height. SF setting also strongly affects the EBAM part quality including the surface morphology, surface roughness and part microstructures. In general, a higher SF index tends to produce parts of rougher surfaces with more pore features and large beta grain columnar widths. Increasing the beam speed will reduce the peak temperatures, also reduce the melt pool sizes. Simulations conducted to evaluate the beam speed effects are in reasonable agreement compared to the experimental measurements in temperatures and melt pools sizes. However, the results of a lower SF case, SF20, show larger differences between the simulations and the experiments, about 58% for the melt pool size. Moreover, the higher the beam current, the higher the peak process temperatures, also the larger the melt pool. On the other hand, increasing the beam diameter monotonically decreases the peak temperature and the melt pool length. C1 [Price, Steven; Cheng, Bo; Chou, Kevin] Univ Alabama, Dept Mech Engn, Tuscaloosa, AL 35487 USA. [Lydon, James; Cooper, Kenneth] NASA, George C Marshall Space Flight Ctr, Addit Mfg Lab, Huntsville, AL 35812 USA. RP Chou, K (reprint author), Univ Alabama, Dept Mech Engn, Tuscaloosa, AL 35487 USA. EM kchou@eng.ua.edu FU NSF [1335481]; NASA [NNX11AM11A]; Marshall Space Flight Center (Huntsville, AL), Advanced Manufacturing Team in Nonmetallic Branch FX This research was supported by NSF (No. 1335481) and NASA, (No. NNX11AM11A), and is in collaboration with Marshall Space Flight Center (Huntsville, AL), Advanced Manufacturing Team in Nonmetallic Branch. X. Gong conducted metallographic analysis of the samples and provided microstructural images. NR 27 TC 1 Z9 1 U1 3 U2 47 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 1087-1357 EI 1528-8935 J9 J MANUF SCI E-T ASME JI J. Manuf. Sci. Eng.-Trans. ASME PD DEC PY 2014 VL 136 IS 6 SI SI AR 061019 DI 10.1115/1.4028485 PG 10 WC Engineering, Manufacturing; Engineering, Mechanical SC Engineering GA AS6SQ UT WOS:000344393000021 ER PT J AU Tayon, WA Shenoy, RN Redding, MR Bird, RK Hafley, RA AF Tayon, Wesley A. Shenoy, Ravi N. Redding, MacKenzie R. Bird, R. Keith Hafley, Robert A. TI Correlation Between Microstructure and Mechanical Properties in an Inconel 718 Deposit Produced Via Electron Beam Freeform Fabrication SO JOURNAL OF MANUFACTURING SCIENCE AND ENGINEERING-TRANSACTIONS OF THE ASME LA English DT Article ID TEXTURE AB Electron beam freeform fabrication (EBF3), a metallic layer-additive manufacturing process, uses a high-power electron beam in conjunction with a metal feed wire to create a molten pool on a substrate, which on solidification produces a component of the desired configuration made of sequentially deposited layers. During the build-up of each solidified layer, the substrate is translated with respect to the electron beam and the feed wire. EBF3 products are similar to conventional cast products with regard to the as-deposited (AD) microstructure and typical mechanical properties. Inconel 718 (IN 718), a high-temperature superalloy with attractive mechanical and oxidation properties well suited for aerospace applications, is typically used in the wrought form. The present study examines the evolution of microstructure, crystallographic texture, and mechanical properties of a block of IN 718 fabricated via the EBF3 process. Specimens extracted out of this block, both in the AD and in a subsequently heat treated (HT) condition, were subjected to (1) microstructural characterization using scanning electron microscopy (SEM); (2) in-plane elastic modulus, tensile strength, and microhardness evaluations; and (3) crystallographic texture characterization using electron backscatter diffraction (EBSD). Salient conclusions stemming from this study are: (1) mechanical properties of the EBF3-processed IN 718 block are strongly affected by texture as evidenced by their dependence on orientation relative to the EBF3 fabrication direction, with the AD EBF3 properties generally being significantly reduced compared to wrought IN 718; (2) significant improvement in both strength and modulus of the EBF3 product to levels nearly equal to those for wrought IN 718 may be achieved through heat treatment. C1 [Tayon, Wesley A.; Bird, R. Keith; Hafley, Robert A.] NASA Langley Res Ctr, Hampton, VA 23681 USA. [Shenoy, Ravi N.] Northrop Grumman, Tech Serv, Hampton, VA 23681 USA. [Redding, MacKenzie R.] Univ Virginia, Dept Engn Phys, Charlottesville, VA 22904 USA. RP Tayon, WA (reprint author), NASA Langley Res Ctr, Hampton, VA 23681 USA. EM wesley.a.tayon@nasa.gov NR 21 TC 3 Z9 3 U1 4 U2 49 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 1087-1357 EI 1528-8935 J9 J MANUF SCI E-T ASME JI J. Manuf. Sci. Eng.-Trans. ASME PD DEC PY 2014 VL 136 IS 6 SI SI AR 061005 DI 10.1115/1.4028509 PG 7 WC Engineering, Manufacturing; Engineering, Mechanical SC Engineering GA AS6SQ UT WOS:000344393000007 ER PT J AU Johnston, CO Brandis, AM AF Johnston, C. O. Brandis, A. M. TI Modeling of nonequilibrium CO Fourth-Positive and CN Violet emission in CO2-N-2 gases SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE CO 4th Positive; Nonequilibrium; Chemical kinetics; Shock tube ID CHEMICAL-KINETIC PROBLEMS; LUNAR-RETURN CONDITIONS; SHOCK-LAYER RADIATION; FUTURE NASA MISSIONS; RATE CONSTANTS; DISSOCIATION KINETICS; CO-N-2 MIXTURE; TUBE; ABSORPTION; ENTRIES AB This work develops a chemical kinetic rate model for simulating nonequilibrium radiation from CO2-N-2 gases, representative of Mars or Venus entry shock layers. Using recent EAST shock tube measurements of nonequilibrium CO 4th Positive and CN Violet emission at pressures and velocities ranging from 0.10 to 1.0 Tort and 6 to 8 km/s, the rate model is developed through an optimization procedure that minimizes the disagreement between the measured and simulated nonequilibrium radiance profiles. Only the dissociation rates of CO2, CO, and NO, along with the CN + O and CO + N rates were treated as unknown in this optimization procedure, as the nonequilibrium radiance was found to be most sensitive to them. The other rates were set to recent values from the literature. Increases in over a factor of 5 in the CO dissociation rate relative to the previous widely used value were found to provide the best agreement with measurements, while the CO2 rate was not changed. The developed model is found to capture the measured nonequilibrium radiance of CO 4th Positive and CN Violet within error bars of +/- 30%. Published by Elsevier Ltd. C1 [Johnston, C. O.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Brandis, A. M.] NASA Ames, ERC Corp, Moffett Field, CA 94035 USA. RP Johnston, CO (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM Christopher.O.Johnston@nasa.gov; Aaron.M.Brandis@nasa.gov FU NASA Space Technology Mission Directorate Entry Systems and Modeling (ESM) project FX The authors would like to thank Brett Cruden for providing the EAST measurements. The present work was funded by the NASA Space Technology Mission Directorate Entry Systems and Modeling (ESM) project, with tasks leads Michael Wright and Michael Barnhardt. NR 47 TC 2 Z9 2 U1 0 U2 6 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 DEC PY 2014 VL 149 BP 303 EP 317 DI 10.1016/j.jqsrt.2014.08.025 PG 15 WC Optics; Spectroscopy SC Optics; Spectroscopy GA AS7FJ UT WOS:000344422300029 ER PT J AU Bontempi, PS AF Bontempi, Paula S. TI Paula S. Bontempi SO OCEANOGRAPHY LA English DT Biographical-Item C1 [Bontempi, Paula S.] NASA, Ocean Biol & Biogeochem Program, Washington, DC 20546 USA. RP Bontempi, PS (reprint author), NASA, Ocean Biol & Biogeochem Program, Washington, DC 20546 USA. EM paula.bontempi@nasa.gov NR 1 TC 0 Z9 0 U1 0 U2 0 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD DEC PY 2014 VL 27 IS 4 SU S BP 68 EP 68 PG 1 WC Oceanography SC Oceanography GA V44BO UT WOS:000209724700029 ER PT J AU Romanou, A AF Romanou, Anastasia TI Anastasia Romanou SO OCEANOGRAPHY LA English DT Biographical-Item C1 [Romanou, Anastasia] Columbia Univ, Appl Phys & Appl Math, New York, NY USA. [Romanou, Anastasia] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Romanou, A (reprint author), Columbia Univ, Appl Phys & Appl Math, New York, NY USA. EM ar2235@columbia.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD DEC PY 2014 VL 27 IS 4 SU S BP 209 EP 209 PG 1 WC Oceanography SC Oceanography GA V44BO UT WOS:000209724700170 ER PT J AU Hertz, P AF Hertz, Paul TI The Present and Future of Space Science at NASA SO PROCEEDINGS OF THE AMERICAN PHILOSOPHICAL SOCIETY LA English DT Article C1 NASA, Sci Mission Directorate, New York, NY 10025 USA. RP Hertz, P (reprint author), NASA, Sci Mission Directorate, New York, NY 10025 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER PHILOSOPHICAL SOC PI PHILADELPHIA PA 104 SOUTH FIFTH ST, PHILADELPHIA, PA 19106-3387 USA SN 0003-049X EI 2326-9243 J9 P AM PHILOS SOC JI Proc. Amer. Philos. Soc. PD DEC PY 2014 VL 158 IS 4 BP 329 EP 353 PG 25 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA CV4SW UT WOS:000364257800001 ER PT J AU Stanford, BK Jutte, CV Wu, KC AF Stanford, Bret K. Jutte, Christine V. Wu, K. Chauncey TI Aeroelastic benefits of tow steering for composite plates SO COMPOSITE STRUCTURES LA English DT Article DE Aeroelasticity; Tow-steering; Certifiable composites ID DESIGN AB The use of tow steered composites, where fibers follow prescribed curvilinear paths within a laminate, can improve upon existing capabilities related to aeroelastic tailoring of wing structures, though this tailoring method has received relatively little attention in the literature. This paper demonstrates the technique for a cantilevered flat plate in low-speed flow. A genetic algorithm is used to locate the Pareto front between static aeroelastic stresses and dynamic flutter boundaries. The impact of various tailoring choices upon the aeroelastic performance is quantified: curvilinear fiber steering versus straight fiber steering and certifiable versus non-certifiable stacking sequences. Published by Elsevier Ltd. C1 [Stanford, Bret K.; Wu, K. Chauncey] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Jutte, Christine V.] Craig Technol Inc, Cape Canaveral, FL 32920 USA. RP Stanford, BK (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM bret.k.stanford@nasa.gov; christine.vjutte@nasa.gov; k.c.wu@nasa.gov FU Fixed Wing project under NASA's Fundamental Aeronautics Program FX This work is funded by the Fixed Wing project under NASA's Fundamental Aeronautics Program. NR 11 TC 5 Z9 5 U1 1 U2 6 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0263-8223 EI 1879-1085 J9 COMPOS STRUCT JI Compos. Struct. PD DEC PY 2014 VL 118 BP 416 EP 422 DI 10.1016/j.compstruct.2014.08.007 PG 7 WC Materials Science, Composites SC Materials Science GA AR8QE UT WOS:000343838900042 ER PT J AU Yamakov, V Park, C Kang, JH Wise, KE Fay, C AF Yamakov, Vesselin Park, Cheol Kang, Jin Ho Wise, Kristopher E. Fay, Catharine TI Piezoelectric molecular dynamics model for boron nitride nanotubes SO COMPUTATIONAL MATERIALS SCIENCE LA English DT Article DE H-BN; BNNT; Piezoelectricity; Molecular dynamics ID MONTE-CARLO CALCULATIONS; BINARY-LIQUID MIXTURES; CARBON NANOTUBES; SIMULATION; ENSEMBLE; DEFORMATION AB A classical molecular dynamics model with an incorporated strain-dependent dipole potential energy term is introduced to represent the piezoelectric properties of boron nitride nanotubes (BNNTs). The model allows for an analytical expression of the piezoelectric tensor of hexagonal BN monolayers in terms of the properties of the interatomic potential and two fitting parameters. The deformation-induced polarization predicted by this model is verified against the results of previously published electronic structure (ab-initio and tight-binding) calculations. The model works well for BNNTs over the full range of chiral angles from phi = 0 degrees (zig-zag tubes) to phi = 30 degrees (armchair tubes) and under loading in both tensile and twist modes. The presented model can be a foundation for atomic-level modeling of the electroactive properties of large systems of BNNTs and BNNT composites, as well as a base for analytical studies. (C) 2014 Elsevier B.V. All rights reserved. C1 [Yamakov, Vesselin; Kang, Jin Ho] Natl Inst Aerosp, Hampton, VA 23666 USA. [Park, Cheol; Wise, Kristopher E.; Fay, Catharine] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Park, Cheol] Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22904 USA. RP Yamakov, V (reprint author), Natl Inst Aerosp, Hampton, VA 23666 USA. EM yamakov@nianet.org FU National Institute of Aerospace [NNL09AA00A]; US Air Force Office of Scientific Research - Low Density Materials program [FA9550-11-1-0042]; NASA Langley Research Center IRAD program FX V. Yamakov is sponsored through cooperative agreement NNL09AA00A with the National Institute of Aerospace. C. Park acknowledges that his work was funded in part by the US Air Force Office of Scientific Research - Low Density Materials program under Grant No. FA9550-11-1-0042. We appreciate the support of the NASA Langley Research Center IRAD program. NR 26 TC 5 Z9 5 U1 5 U2 47 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-0256 EI 1879-0801 J9 COMP MATER SCI JI Comput. Mater. Sci. PD DEC PY 2014 VL 95 BP 362 EP 370 DI 10.1016/j.commatsci.2014.07.047 PG 9 WC Materials Science, Multidisciplinary SC Materials Science GA AR7TC UT WOS:000343781700047 ER PT J AU Mackey, J Sehirlioglu, A Dynys, F AF Mackey, J. Sehirlioglu, A. Dynys, F. TI Analytic thermoelectric couple optimization introducing Device Design Factor and Fin Factor SO APPLIED ENERGY LA English DT Article DE Thermoelectric modeling; Seebeck coefficient; Peltier effect ID IRREVERSIBLE-PROCESSES; RECIPROCAL RELATIONS; GENERATOR AB An analytic solution of a thermocouple has been developed in order to gain a deeper understanding of the physics of a real device. The model is established for both rectangular and cylindrical couples and is made to account for thermal resistance of the hot and cold shoes and lateral heat transfer. A set of dimensionless parameters have been developed to determine couple behavior and serve as simplifying justifications. New dimensionless parameters, Device Design Factor and Fin Factor, are introduced to account for the thermal resistance and lateral heat transfer, respectively. Design guidelines on couple length and cross-sectional area have been established to account for conditions encountered by a realistic couple. As a result of thermal resistances a lower limit on the length of the couple can be established. In the case of a lateral heat transfer couple the efficiency is found to depend upon cross-sectional area of the leg in such a fashion as to suggest the need to design large area couples. The classic thermoelectric solution neglects the effect of thermal resistance and lateral heat transfer, leading to an over estimated conversion efficiency. The work presented provides a path to incorporate these neglected factors and offers a simplified estimation for couple performance based on analytic solutions of governing equations. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Mackey, J.] Univ Akron, Dept Mech Engn, Akron, OH 44325 USA. [Sehirlioglu, A.] Case Western Reserve Univ, Dept Mat Sci & Engn, Cleveland, OH 44106 USA. [Dynys, F.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Mackey, J (reprint author), Univ Akron, Dept Mech Engn, Akron, OH 44325 USA. EM jam151@zips.uakron.edu OI Mackey, Jonathan/0000-0003-1053-7007 FU National Aeronautics and Space Administration (NASA/USRA) [04555-004] FX The authors gratefully acknowledge the National Aeronautics and Space Administration for their financial support a this work (NASA/USRA contract 04555-004). The authors would also like to thank Benjamin Kowalski for helpful discussion. NR 23 TC 3 Z9 3 U1 2 U2 21 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0306-2619 EI 1872-9118 J9 APPL ENERG JI Appl. Energy PD DEC 1 PY 2014 VL 134 BP 374 EP 381 DI 10.1016/j.apenergy.2014.08.034 PG 8 WC Energy & Fuels; Engineering, Chemical SC Energy & Fuels; Engineering GA AR1HP UT WOS:000343336600036 ER PT J AU Ruzmaikin, A Guillaume, A AF Ruzmaikin, Alexander Guillaume, Alexandre TI Clustering of atmospheric data by the deterministic annealing SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Satellite data; Clustering; Temperature; Water vapor; Deep convective clouds ID VECTOR QUANTIZATION; ARCTIC OSCILLATION; AIRS/AMSU/HSB; CLIMATOLOGY; REGIMES; CLOUDS AB The Deterministic Annealing (DA) clustering method, which determines the cluster centers, their sizes, and probability with which data are associated with each cluster, is tested using artificial data and applied to atmospheric satellite data. It is also shown how the method can be advantageously used to characterize data outliers. The method is based on the optimization of a cost function that depends both on the averaged distance of data points to cluster centers and the Shannon entropy of the data. The cost function uses two independent parameters in a close analog to the Gibbs' thermodynamics (with the averaged distance similar to the internal energy) allowing a sufficient control of the formation of new clusters as "phase transitions" by changing the clustering parameter similar to the thermodynamical temperature. The satellite data used are a temperature-water vapor data set and the positions of deep convective clouds obtained from the measurements of the Atmospheric InfraRed Sounder (AIRS) on the Aqua satellite. The clustering of these data is demonstrated for the 2D case (at fixed pressure level) and for the 3D case at multiple pressure levels indicating potential applications to investigation of distributions of atmospheric profiles. Published by Elsevier Ltd. C1 [Ruzmaikin, Alexander; Guillaume, Alexandre] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ruzmaikin, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Alexander.Ruzmaikin@jpl.nasa.gov; Alexandre.Guillaume@jpl.nasa.gov FU NASA Earth System Data Records Uncertainty Analysis program [A32]; National Aeronautics and Space Administration FX We thank two reviewers for useful, critical suggestions that led to improvement of the presentation. The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. It is supported by the NASA Earth System Data Records Uncertainty Analysis program A32. NR 29 TC 0 Z9 0 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD DEC PY 2014 VL 120 BP 121 EP 131 DI 10.1016/j.jastp.2014.09.009 PG 11 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AR5JZ UT WOS:000343622400015 ER PT J AU Chang, CW Maduraiveeran, G Xu, JC Hunter, GW Dutta, PK AF Chang, C. W. Maduraiveeran, G. Xu, J. C. Hunter, G. W. Dutta, P. K. TI Design, fabrication, and testing of MEMS-based miniaturized potentiometric nitric oxide sensors SO SENSORS AND ACTUATORS B-CHEMICAL LA English DT Article DE MEMS; NOx sensor; Microfabrication; Potentiometric; Harsh environment sensor ID NOX-GAS SENSORS; ELECTRODE; SENSITIVITY; FILTER; YSZ AB We report on the development of miniaturized potentiometric nitric oxide (NO) sensors. This work covers the design, fabrication and testing of these NO sensors. In particular, microelectromechanical systems (MEMS) fabrication techniques were utilized to miniaturize the size of the sensors. Sensors were fabricated using both shadow mask and photoresist mask fabrication methods. Arrays of up to 15 sensors were electrically connected in series during the fabrication process to improve the signal of the overall device for a given NO concentration. Testing on these sensor arrays toward NO was carried out at 550 degrees C to compare the performance of the various designs of the sensor. Sensitivity below the ppm level was demonstrated with the photoresist-masked 15-sensor array. Long-term stability of the miniaturized sensor array when operating at high temperatures needs to be improved before practical applications of this MEMS sensor technology can be realized. (C) 2014 Elsevier B.V. All rights reserved. C1 [Chang, C. W.] Vantage Partners LLC, Cleveland, OH 44135 USA. [Maduraiveeran, G.; Dutta, P. K.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Xu, J. C.; Hunter, G. W.] NASA, Glenn Res Ctr, Cleveland, OH USA. RP Chang, CW (reprint author), Vantage Partners LLC, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA. EM carl.w.chang@nasa.gov FU Third Frontier of the state of Ohio; Cleveland Clinic Foundation; NASA Glenn Research Center; Respiratory Institute & Department of Pathobiology at the Cleveland Clinic Foundation FX The work was completed under a grant from the Third Frontier of the state of Ohio. The authors thank the Cleveland Clinic Foundation for their support of this work. We thank J. Gonzalez of Gilcrest; M. Artale, P. Lampard, M. Mrdenovich, and B. Osborn of Sierra Lobo, Inc.; D. Lukco of Vantage Partners; and E. Mcquaid and L. Evans ofNASA Glenn Research Center for their technical assistance. The authors thank L. Matus and M. Zeller of NASA Glenn Research Center for their support. The authors thank G. Beheim for reviewing this paper. We also thank R. Dweik M.D. and D. Laskowski of the Respiratory Institute & Department of Pathobiology at the Cleveland Clinic Foundation for their support and work. Fabrication of the sensorsin this work was carried out at the NASA Glenn Research Center, and testing of the sensors in this work was carried out at the Ohio State University. NR 27 TC 5 Z9 5 U1 1 U2 30 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0925-4005 J9 SENSOR ACTUAT B-CHEM JI Sens. Actuator B-Chem. PD DEC 1 PY 2014 VL 204 BP 183 EP 189 DI 10.1016/j.snb.2014.06.108 PG 7 WC Chemistry, Analytical; Electrochemistry; Instruments & Instrumentation SC Chemistry; Electrochemistry; Instruments & Instrumentation GA AQ8VX UT WOS:000343116400022 ER PT J AU Burleigh, S Cerf, VG Crowcroft, J Tsaoussidis, V AF Burleigh, Scott Cerf, Vinton G. Crowcroft, Jon Tsaoussidis, Vassilis TI Space for Internet and Internet for space SO AD HOC NETWORKS LA English DT Article DE Space; Internet; DTN AB Space flight and Internet service are technologies that are currently complementary but seem to be on the verge of integration into a new "space internetworking" discipline. The authors believe a comprehensive realization of space internetworking technology could dramatically enhance space exploration, augment terrestrial industry and commerce, benefit the economically disadvantaged, and nurture human and civil rights. (C) 2014 Elsevier B.V. All rights reserved. C1 [Burleigh, Scott] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Cerf, Vinton G.] Google, Mountain View, CA USA. [Crowcroft, Jon] Univ Cambridge, Comp Lab, Cambridge CB2 1TN, England. [Tsaoussidis, Vassilis] Democritus Univ Thrace, Space Internetworking Ctr, Komotini, Greece. RP Burleigh, S (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Scott.C.Burleigh@jpl.nasa.gov OI Crowcroft, Jon/0000-0002-7013-0121 FU National Aeronautics and Space Administration FX This research was performed in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 12 TC 5 Z9 7 U1 0 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1570-8705 EI 1570-8713 J9 AD HOC NETW JI Ad Hoc Netw. PD DEC PY 2014 VL 23 BP 80 EP 86 DI 10.1016/j.adhoc.2014.06.005 PG 7 WC Computer Science, Information Systems; Telecommunications SC Computer Science; Telecommunications GA AP7IS UT WOS:000342251600006 ER PT J AU Loftus, AM Cotton, WR AF Loftus, A. M. Cotton, W. R. TI A triple-moment hail bulk microphysics scheme. Part II: Verification and comparison with two-moment bulk microphysics SO ATMOSPHERIC RESEARCH LA English DT Article DE Hail; Microphysics; Supercell convection; Cloud-resolving model ID NORTHEASTERN COLORADO CUMULUS; SIMULATED CONVECTIVE STORMS; CLOUD MICROPHYSICS; SUPERCELL STORMS; AIR-FLOW; SENSITIVITY EXPERIMENTS; PRECIPITATION FORMATION; NUMERICAL SIMULATIONS; GRAVITY CURRENTS; ICE PARTICLES AB Microphysical parameterizations in numerical cloud models continue to grow in complexity as our capability to represent microphysical processes increases owing to greater knowledge of these processes as well as advances in computing power. In Part I of this study, a new triple-moment bulk hail microphysics scheme (3MHAIL) that predicts the spectral shape parameter of the hail size distribution was presented and evaluated against lower order-moment schemes. In this paper, the 3MHAIL scheme is verified in simulations of a well-observed supercell storm that occurred over northwest Kansas on 29 June 2000 during the Severe Thunderstorm and Electrification and Precipitation Study (STEPS). Comparisons of the simulation results with the observations for this case, as well as with results of simulations using two different two-moment (2M) configurations of the RAMS microphysics schemes, suggest a significant improvement of the simulated storm structure and evolution is achieved with the 3MHAIL scheme. The generation of large hail and subsequent fallout in the simulation using 3MHA1L microphysics show particularly good agreement with surface hail reports for this storm as well as with previous studies of hail-producing supercell storms. On the other hand, the simulation with 2M microphysics produces only small hail aloft and virtually no hail at the surface, whereas a 2M version of the 3MHAIL scheme (with a fixed spectral shape parameter) produces unrealistically high amounts of large hail at low levels as a result of artificial shifts in the hail size spectra towards larger diameter hail during the melting process. (C) 2014 Elsevier B.V. All rights reserved. C1 [Loftus, A. M.; Cotton, W. R.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. RP Loftus, AM (reprint author), NASA, Goddard Space Flight Ctr, Climate & Radiat & Lab, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM adrian.m.loftus@nasa.gov FU NSF [ATM-0324324, ATM-0638910, AGS-1005041] FX The authors wish to thank Louie Grasso and Sue van den Heever for their insightful discussions on microphysical processes in deep convection, as well as Patrick Kennedy and Brenda Dolan for their assistance with the T-matrix and Mueller matrix codes. Thanks also to Jason Milbrandt and one other anonymous reviewer for their helpful suggestions on improving the paper. This research was supported by NSF grants ATM-0324324, ATM-0638910, and AGS-1005041. NR 97 TC 5 Z9 5 U1 1 U2 18 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0169-8095 EI 1873-2895 J9 ATMOS RES JI Atmos. Res. PD DEC PY 2014 VL 150 BP 97 EP 128 DI 10.1016/j.atmosres.2014.07.016 PG 32 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AP7OL UT WOS:000342266500009 ER PT J AU Singels, A Jones, M Marin, F Ruane, A Thorburn, P AF Singels, Abraham Jones, Matthew Marin, Fabio Ruane, Alexander Thorburn, Peter TI Predicting Climate Change Impacts on Sugarcane Production at Sites in Australia, Brazil and South Africa Using the Canegro Model SO SUGAR TECH LA English DT Article DE Climate change; Crop model; Cane yield; Canopy cover; Global climate model ID BIOMASS AB Reliable predictions of sugarcane response to climate change are necessary to plan adaptation strategies. The objective of this study was to assess the use of global climate models (GCMs) and a crop simulation model for predicting climate change impacts on sugarcane production. The Canegro model was used to simulate growth and development of sugarcane crops under typical management conditions at three sites (irrigated crops at Ayr, Australia; rainfed crops at Piracicaba, Brazil and La Mercy, South Africa) for current and three future climate scenarios. The baseline scenario consisted of a 30-year time series of historical weather records and atmospheric CO2 concentration ([CO2]) set at 360 ppm. Future climate scenarios were derived from three GCMs and [CO2] set at 734 ppm. Future cane yields are expected to increase at all three sites, ranging from +4 % for Ayr, to +9 and +20 % for Piracicaba and La Mercy. Canopy development was accelerated at all three sites by increased temperature, which led to increased interception of radiation, increased transpiration, and slight increases in drought stress at rainfed sites. For the high potential sites (Ayr and Piracicaba), yield increases were limited by large increases in maintenance respiration which consumed most of the daily assimilate when high biomass was achieved. A weakness of the climate data used was the assumption of no change in rainfall distribution, solar radiation and relative humidity. Crop model aspects that need refinement include improved simulation of (1) elevated [CO2] effects on crop photosynthesis and transpiration, and (2) high temperature effects on crop development, photosynthesis and respiration. C1 [Singels, Abraham; Jones, Matthew] South African Sugarcane Res Inst, Mt Edgecombe, South Africa. [Marin, Fabio] Embrapa Agr Informat, Campinas, SP, Brazil. [Ruane, Alexander] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Thorburn, Peter] CSIRO Ecosyst Sci, Brisbane, Qld, Australia. RP Singels, A (reprint author), South African Sugarcane Res Inst, Mt Edgecombe, South Africa. EM abraham.singels@sugar.org.za RI Thorburn, Peter/A-6884-2011; OI Singels, Abraham/0000-0003-4558-3003 FU AgMIP; SASRI; CSIRO; Embrapa FX This work was conducted under the auspices of AgMIP, with support from SASRI, CSIRO and Embrapa. The authors thank Jody Biggs of CSIRO for assistance in preparing data for Ayr. We acknowledge the global climate modelling groups, the Program for Climate Model Diagnosis and Intercomparison (PCMDI) and the WCRP's Working Group on Coupled Modelling (WGCM), for their roles in making available the WCRP CMIP3 multi-model dataset. Support of this dataset is provided by the Office of Science, U.S. Department of Energy. NR 23 TC 6 Z9 7 U1 2 U2 86 PU SPRINGER INDIA PI NEW DELHI PA 7TH FLOOR, VIJAYA BUILDING, 17, BARAKHAMBA ROAD, NEW DELHI, 110 001, INDIA SN 0972-1525 J9 SUGAR TECH JI Sugar Tech. PD DEC PY 2014 VL 16 IS 4 BP 347 EP 355 DI 10.1007/s12355-013-0274-1 PG 9 WC Agronomy SC Agriculture GA AP6EL UT WOS:000342170300003 ER PT J AU Liang, L Schwartz, MD Wang, ZS Gao, F Schaaf, CB Tan, B Morisette, JT Zhang, XY AF Liang, Liang Schwartz, Mark D. Wang, Zhuosen Gao, Feng Schaaf, Crystal B. Tan, Bin Morisette, Jeffrey T. Zhang, Xiaoyang TI A Cross Comparison of Spatiotemporally Enhanced Springtime Phenological Measurements From Satellites and Ground in a Northern U.S. Mixed Forest SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Daily Moderate Resolution Imaging Spectroradiometer (MODIS); Earth Observing System (EOS) land validation core sites; landscape phenology (LP); land surface phenology (LSP); phenology; Spatial and Temporal Adaptive Reflectance Fusion Model (STARFM) ID DECIDUOUS BROADLEAF FOREST; LAND-SURFACE PHENOLOGY; IMAGING SPECTRORADIOMETER MODIS; REFLECTANCE FUSION MODEL; LEAF-AREA INDEX; VEGETATION PHENOLOGY; CANOPY PHENOLOGY; TEMPORAL RESOLUTION; NEAR-SURFACE; DYNAMICS AB Cross comparison of satellite-derived land surface phenology (LSP) and ground measurements is useful to ensure the relevance of detected seasonal vegetation change to the underlying biophysical processes. While standard 16-day and 250-m Moderate Resolution Imaging Spectroradiometer (MODIS) vegetation index (VI)-based springtime LSP has been evaluated in previous studies, it remains unclear whether LSP with enhanced temporal and spatial resolutions can capture additional details of ground phenology. In this paper, we compared LSP derived from 500-m daily MODIS and 30-m MODIS-Landsat fused VI data with landscape phenology (LP) in a northern U. S. mixed forest. LP was previously developed from intensively observed deciduous and coniferous tree phenology using an upscaling approach. Results showed that daily MODIS-based LSP consistently estimated greenup onset dates at the study area (625 m x 625 m) level with 4.48 days of mean absolute error (MAE), slightly better than that of using 16-day standard VI (4.63 days MAE). For the observed study areas, the time series with increased number of observations confirmed that post-bud burst deciduous tree phenology contributes the most to vegetation reflectance change. Moreover, fused VI time series demonstrated closer correspondences with LP at the community level (0.1-20 ha) than using MODIS alone at the study area level (390 ha). The fused LSP captured greenup onset dates for respective forest communities of varied sizes and compositions with four days of the overall MAE. This study supports further use of spatiotemporally enhanced LSP for more precise phenological monitoring. C1 [Liang, Liang] Univ Kentucky, Dept Geog, Lexington, KY 40506 USA. [Schwartz, Mark D.] Univ Wisconsin, Dept Geog, Milwaukee, WI 53201 USA. [Wang, Zhuosen; Schaaf, Crystal B.] Univ Massachusetts, Sch Environm, Boston, MA 02125 USA. [Wang, Zhuosen] NASA, Terr Informat Syst Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wang, Zhuosen] Oak Ridge Associated Univ, NASA, Postdoctoral Program, Oak Ridge, TN 37831 USA. [Gao, Feng] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA. [Tan, Bin] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA. [Morisette, Jeffrey T.] Colorado State Univ, North Cent Climate Sci Ctr, US Geol Survey, Ft Collins, CO 80525 USA. [Zhang, Xiaoyang] S Dakota State Univ, Geospatial Sci Ctr Excellence, Brookings, SD 57007 USA. RP Liang, L (reprint author), Univ Kentucky, Dept Geog, Lexington, KY 40506 USA. EM liang.liang@uky.edu FU National Science Foundation [BCS-0649380, BCS-0703360]; National Aeronautics and Space Administration [NNX12AL38G] FX This work was supported in part by the National Science Foundation under Grant BCS-0649380 and Grant BCS-0703360 and in part by the National Aeronautics and Space Administration under Grant NNX12AL38G. NR 70 TC 8 Z9 8 U1 8 U2 58 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 DEC PY 2014 VL 52 IS 12 BP 7513 EP 7526 DI 10.1109/TGRS.2014.2313558 PG 14 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA AO7KM UT WOS:000341532100004 ER PT J AU Franch, B Vermote, EF Sobrino, JA Julien, Y AF Franch, Belen Vermote, Eric F. Sobrino, Jose A. Julien, Yves TI Retrieval of Surface Albedo on a Daily Basis: Application to MODIS Data SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Albedo; bidirectional reflectance distribution function (BRDF) inversion; MODerate Resolution Imaging Spectroradiometer (MODIS); VJB method ID REFLECTANCE DISTRIBUTION FUNCTION; BIDIRECTIONAL REFLECTANCE; PRODUCTS; VARIABILITY AB In this paper, we will evaluate the Vermote et al. method, hereafter referred to as VJB, in comparison to the MCD43 MODerate Resolution Imaging Spectroradiometer (MODIS) product, focusing on the white sky albedo parameter. We also present and study three different methods based on the VJB assumption, the 4param, 5param Rsqr, and 5param Vsqr. We use daily MODIS Climate Modeling Grid data both from Terra and Aqua platforms from 2002 to 2011 for all the pixels over Europe. We obtain an overall root-mean-square error of 5% when using the VJB method and 6.1%, 5.1%, and 5.3% for the 4param, 5param Rsqr, and 5param Vsqr methods, respectively. The main differences between the methods are located in areas where only few cloud-free snow-free samples were available that correspond mainly to mountainous areas during the winter. We finally conclude that the VJB method has an equivalent performance in deriving the white sky albedo results to the MODIS product with the advantage of daily temporal resolution. Additionally, we propose the 5param Rsqr method as an alternative to the VJB method due to its decreased data processing time. C1 [Franch, Belen] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Vermote, Eric F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sobrino, Jose A.; Julien, Yves] Univ Valencia, Global Change Unit, Image Proc Lab UCG IPL, E-46100 Valencia, Spain. RP Franch, B (reprint author), Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. RI Julien, Yves/M-5224-2014 OI Julien, Yves/0000-0001-5334-7137 FU Spanish Ministerio de Economia y Competitividad (EODIX) [AYA2008-0595-C04-01]; Spanish Ministerio de Economia y Competitividad (CEOS-SPAIN) [AYA2011-29334-C02-01]; European Union (CEOP-AEGIS) [212921, 036946] FX This work was supported in part by the Spanish Ministerio de Economia y Competitividad (EODIX, project AYA2008-0595-C04-01; CEOS-SPAIN, project AYA2011-29334-C02-01) and in part by the European Union (CEOP-AEGIS, project FP7-ENV-2007-1 proposal No. 212921; WATCH, project 036946). NR 20 TC 6 Z9 6 U1 0 U2 21 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 DEC PY 2014 VL 52 IS 12 BP 7549 EP 7558 DI 10.1109/TGRS.2014.2313842 PG 10 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA AO7KM UT WOS:000341532100007 ER PT J AU Turk, FJ Li, L Haddad, ZS AF Turk, Francis Joseph Li, Li Haddad, Ziad S. TI A Physically Based Soil Moisture and Microwave Emissivity Data Set for Global Precipitation Measurement (GPM) Applications SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Emissivity; Global Precipitation Measurement (GPM); land; microwave; precipitation; radiometer; satellite; Tropical Rainfall Measuring Mission (TRMM); vegetation ID LAND-SURFACE EMISSIVITIES; PRINCIPAL COMPONENTS; UNITED-STATES; SMAP MISSION; B-FACTOR; AMSR-E; RETRIEVAL; VEGETATION; MODEL; SYSTEM AB The joint National Aeronautics and Space Administration and Japanese Aerospace Exploration Agency (JAXA) Global Precipitation Measurement (GPM) mission will provide considerably more observations over complex and dynamically changing land backgrounds. A physically based precipitation retrieval using GPM's satellite constellation of passive microwave (PMW) observations has to accommodate the spatially and temporally varying radiometric signature of the land surface to constrain the set of candidate rainfall solutions. The challenge for retrieval algorithms is to identify and isolate precipitation profiles whose simulated observations agree with the satellite observations and are also representative of the surface conditions. Microwave emissivity modeling results are presented from a physically based land algorithm that retrieves soil moisture, vegetation water content, and surface temperature, along with the emissivity using polarized 10, 18, and 37 GHz channel measurements from the WindSat sensor onboard the Coriolis satellite, and results from the Tropical Rainfall Measuring Mission (TRMM) Microwave Imager (TMI). The emissivity mean, coefficient of variation, covariance, and correlation slope are examined for the range of clear-scene surface properties observed by WindSat and TRMM between 2003-2012 and 2002-2011, respectively, under a range of seasons, time of day, rain events, etc. These joint data provide a means to examine the extent to which the surface geophysical properties control the microwave land surface emissivity covariability, to better utilize these lower frequency observations in overland PMW-based precipitation retrievals. C1 [Turk, Francis Joseph; Haddad, Ziad S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Li, Li] Naval Res Lab, Washington, DC 20375 USA. RP Turk, FJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM jturk@jpl.nasa.gov; li.li@nrl.navy.mil RI Measurement, Global/C-4698-2015 FU National Aeronautics and Space Administration (NASA) Precipitation Measurement Missions (PMM); NASA FX The authors acknowledge the support from the National Aeronautics and Space Administration (NASA) Precipitation Measurement Missions (PMM) through Dr. R. Kakar. TRMM data are provided courtesy of the Precipitation Processing System at the Goddard Space Flight Center. The authors would like to thank Dr. P. Kirstetter and Dr. J. Zhang from the University of Oklahoma and the National Severe Storms Laboratory for their assistance with the National Mosaic and Multi-Sensor QPE radar processing. The authors would also like to thank Dr. Y. Tian and others from the PMM Land Surface Working Group for the valuable comments. The work by F. J. Turk and Z. S. Haddad was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 49 TC 7 Z9 7 U1 1 U2 53 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 DEC PY 2014 VL 52 IS 12 BP 7637 EP 7650 DI 10.1109/TGRS.2014.2315809 PG 14 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA AO7KM UT WOS:000341532100014 ER PT J AU Tadic, JM Loewenstein, M Frankenberg, C Butz, A Roby, M Iraci, LT Yates, EL Gore, W Kuze, A AF Tadic, Jovan M. Loewenstein, Max Frankenberg, Christian Butz, Andre Roby, Matthew Iraci, Laura T. Yates, Emma L. Gore, Warren Kuze, Akihiko TI A Comparison of In Situ Aircraft Measurements of Carbon Dioxide and Methane to GOSAT Data Measured Over Railroad Valley Playa, Nevada, USA SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Air pollution; atmosphere; atmospheric measurements; calibration; Earth observing system; measurement techniques; remote sensing ID GASES OBSERVING SATELLITE; RING-DOWN SPECTROSCOPY; FOURIER-TRANSFORM SPECTROMETER; CO2 RETRIEVAL ALGORITHM; CALIBRATION AB In this paper, we report the vertical profiles of CO2 and CH4 measured with a cavity ring-down spectrometer (CRDS) on a research aircraft from near-ground level to 8 km above mean sea level. The airborne platform employed in this paper is an Alpha Jet aircraft operated from NASA's Ames Research Center. Flights were undertaken to Railroad Valley, NV, USA, to coincide with overpasses of the Greenhouse Gases Observing Satellite (GOSAT). Ground-based CO2 and CH4 were simultaneously measured using CRDS, at the time and location of the airborne and satellite measurements. Results of three GOSAT coordinated aircraft profiles and ground-based measurements in June 2011 are presented and discussed in this paper. The accuracy of the CO2 and CH4 measurements has been determined based upon laboratory calibrations (World Meteorological Organisation traceable standard) and pressure/temperature flight simulations in a test chamber. The overall uncertainty for the airborne measurements ranged from 0.31 to 0.39 ppm for CO2 and from 3.5 to 5.6 ppb for CH4. Our column-averaged CO2 and CH4 measurements, which include about 61% of the total atmospheric mass, are extrapolated, using different techniques, to include the remainder of the tropospheric and stratospheric CO2 and CH4. The CO2 data are then analyzed using the Atmospheric CO2 Observations from Space 2.9 and 3.3 algorithms. For methane data, the RemoTeC v2.1 algorithm was used in its full physics setup. Column-averaged CO2 and XCO2, measured by GOSAT and analyzed from our data, ranged from 388.1 to 396.4 ppm, andXCH(4) ranged from 1.743 to 1.822 ppm. The agreement of the satellite and aircraft CO2 mixing ratios, as well as ground measurements, falls within the uncertainties of the methods employed to acquire these numbers. C1 [Tadic, Jovan M.; Loewenstein, Max; Roby, Matthew; Iraci, Laura T.; Yates, Emma L.; Gore, Warren] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. [Frankenberg, Christian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Butz, Andre] Karlsruhe Inst Technol, Inst Meteorol & Climate Res Atmospher Trace Gases, D-76344 Eggenstein Leopoldshafen, Germany. [Yates, Emma L.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Kuze, Akihiko] Japan Aerosp Explorat Agcy, Tsukuba, Ibaraki 3058505, Japan. RP Tadic, JM (reprint author), NASA, Ames Res Ctr, Mountain View, CA 94035 USA. EM max.loewenstein@nasa.gov; Laura.T.Iraci@nasa.gov RI Butz, Andre/A-7024-2013; KUZE, AKIHIKO/J-2074-2016; Tadic, Jovan/P-3677-2016; Frankenberg, Christian/A-2944-2013 OI Butz, Andre/0000-0003-0593-1608; KUZE, AKIHIKO/0000-0001-5415-3377; Frankenberg, Christian/0000-0002-0546-5857 FU NASA's Earth Science Division; Oak Ridge Associated Universities through NASA Postdoctoral Program FX This work was supported by the NASA's Earth Science Division and Oak Ridge Associated Universities through the NASA Postdoctoral Program (E.L.Y., J.M.T) NR 31 TC 8 Z9 9 U1 1 U2 67 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 DEC PY 2014 VL 52 IS 12 BP 7764 EP 7774 DI 10.1109/TGRS.2014.2318201 PG 11 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA AO7KM UT WOS:000341532100025 ER PT J AU Ritt, PJ Williams, PA Splinter, SC Perepezko, JH AF Ritt, P. J. Williams, P. A. Splinter, S. C. Perepezko, J. H. TI Arc jet testing and evaluation of Mo-Si-B coated Mo and SiC-ZrB2 ceramics SO JOURNAL OF THE EUROPEAN CERAMIC SOCIETY LA English DT Article DE Arc jet testing; Coatings; Oxidation protection; Ceramics; Refractory metals ID ATMOSPHERIC REENTRY CONDITIONS; DOPED MOLYBDENUM SILICIDES; HIGH TEMPERATURE CERAMICS; CARBON-CARBON COMPOSITES; OXIDATION BEHAVIOR; CARBON/CARBON COMPOSITES; ABLATION BEHAVIOR; OXYGEN DIFFUSION; MATRIX COMPOSITES; ALLOYS AB The transition from blunt leading edges to sharp leading edges on re-entry aircrafts is necessary to increase both maneuverability and safety. However, the oxidation resistance of current materials is inadequate for the extreme conditions experienced by sharp leading edge re-entry vehicles. The Mo-Si-B alloy system has been utilized to design a multilayer coating that has the ability to protect from 800 to 1700 degrees C. Substrates of Mo and ZrB2-50 vol% SiC with a flat profile were coated with the MO-Si-B based coating and evaluated using arc jet testing performed at NASA Langley Research Center. Heat fluxes of 2.5 to nearly 3.5 MW/m(2) and surface temperatures of 1500-1650 degrees C were achieved during the 20-min tests. The samples presented in this study showed <3% mass loss and retention of sample shape and integrity, demonstrating the robust environmental protection under a simulated hypersonic environment offered by the Mo-Si-B based coating on refractory metals and ceramics. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Ritt, P. J.; Williams, P. A.; Perepezko, J. H.] Univ Wisconsin, Dept Mat Sci & Engn, Madison, WI 53706 USA. [Splinter, S. C.] NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA. RP Ritt, PJ (reprint author), 1213 Engn Res Bldg,1500 Engn Dr, Madison, WI 53706 USA. EM pritt@wisc.edu; peter.a.williams@intel.com FU National Aeronautics and Space Administration [NNX08AB35A]; Air Force Office of Scientific Research [FA9550-11-1-0201] FX The support from the National Aeronautics and Space Administration (Cooperative Agreement: NNX08AB35A) for the initial stage of research, and the continuing support of the Air Force Office of Scientific Research (Grant. number: FA9550-11-1-0201) is gratefully acknowledged. The technical assistance of J. G. Gragg during testing at the HyMETS facility is appreciated. NR 59 TC 2 Z9 2 U1 6 U2 59 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0955-2219 EI 1873-619X J9 J EUR CERAM SOC JI J. Eur. Ceram. Soc. PD DEC PY 2014 VL 34 IS 15 BP 3521 EP 3533 DI 10.1016/j.jeurceramsoc.2014.06.011 PG 13 WC Materials Science, Ceramics SC Materials Science GA AO0CH UT WOS:000340976200008 ER PT J AU Wang, L Habibi, MH Eldridge, JI Guo, SM AF Wang, Li Habibi, M. H. Eldridge, Jeffrey I. Guo, S. M. TI Infrared radiative properties of plasma-sprayed BaZrO3 coatings SO JOURNAL OF THE EUROPEAN CERAMIC SOCIETY LA English DT Article DE BaZrO3; TBCs; Thermal radiation; Plasma spray; Scattering ID THERMAL BARRIER COATINGS; BARIUM ZIRCONATE; ABSORPTION-COEFFICIENTS; POLYCRYSTALLINE BAZRO3; OPTICAL-PROPERTIES; MATRIX COMPOSITES; POWDERS; PHOTOLUMINESCENCE; SCATTERING; TEMPERATURE AB The room temperature directional-hemispherical reflectance and transmittance spectra of free-standing atmospheric plasma-sprayed BaZrO3 coatings with different thicknesses were measured in the wavelength range of 0.8-15.0 mu m, and the absorption coefficient and scattering coefficient as a function of wavelength were extracted using the modified four-flux model. Results showed that BaZrO3 is a high scattering, low absorption material at the wavelength <6 mu m, where turbine engine thermal radiation is most concentrated. The absorption coefficient of BaZrO3 starts to increase rapidly at wavelength of 6 mu m, indicating that BaZrO3 is high absorbing and opaque in the long wavelength range. A pronounced absorption peak occurs at a wavelength of 7 mu m, and is associated with a BaCO3 coating impurity. The scattering coefficient of BaZrO3 decreases with the increase of wavelength in the whole measured wavelength range, caused by the decrease of the relative size of the scattering center compared with the wavelength. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Wang, Li; Habibi, M. H.; Guo, S. M.] Louisiana State Univ, Turbine Innovat & Res Ctr TIER, Dept Mech & Ind Engn, Baton Rouge, LA 70803 USA. [Eldridge, Jeffrey I.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Guo, SM (reprint author), Louisiana State Univ, Turbine Innovat & Res Ctr TIER, Dept Mech & Ind Engn, Baton Rouge, LA 70803 USA. EM sguo2@lsu.edu FU NASA [NNX09AP72A] FX This research is sponsored by NASA under Cooperative Agreement Number NNX09AP72A. NR 59 TC 10 Z9 10 U1 0 U2 50 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0955-2219 EI 1873-619X J9 J EUR CERAM SOC JI J. Eur. Ceram. Soc. PD DEC PY 2014 VL 34 IS 15 BP 3941 EP 3949 DI 10.1016/j.jeurceramsoc.2014.05.015 PG 9 WC Materials Science, Ceramics SC Materials Science GA AO0CH UT WOS:000340976200055 ER PT J AU Schumann, GJP Vernieuwe, H De Baets, B Verhoest, NEC AF Schumann, G. J. -P. Vernieuwe, H. De Baets, B. Verhoest, N. E. C. TI ROC-based calibration of flood inundation models SO HYDROLOGICAL PROCESSES LA English DT Article DE spatial patterns of inundation; SAR image; flood inundation model; calibration; ROC ID REMOTE-SENSING OBSERVATIONS; SYNTHETIC-APERTURE RADAR; AMAZON FLOODPLAIN; IMAGERY; AREA; UNCERTAINTIES; DELINEATION; INTEGRATION; MANAGEMENT; VEGETATION AB The use of spatial patterns of flood inundation (often obtained from remotely sensed imagery) to calibrate flood inundation models has been widespread over the last 15 years. Model calibration is most often achieved by employing one or even several performance measures derived from the well-known confusion matrix based on a binary classification of flooding. However, relatively early on, it has been recognized that the use of commonly reported performance measures for calibrating flood inundation models (such as the F measure) is hampered because the calibration procedure commonly utilizes only one possible solution of a wet/dry classification of a remote sensing image [most often acquired by a synthetic aperture radar (SAR)] to calibrate or validate models and are biased towards either over-prediction or under-prediction of flooding. Despite the call in several studies for an alternative statistic, to this date, very few, if any, unbiased performance measure based on the confusion matrix has been proposed for flood model calibration/validation studies. In this paper, we employ a robust statistical measure that operates in the receiver operating characteristics (ROC) space and allows automated model calibration with high identifiability of the best model parameter set but without the need of a classification of the SAR image. The ROC-based method for flood model calibration is demonstrated using two different flood event test cases with floodmodels of varying degree of complexity and boundary conditions with varying degree of accuracy. Verification of the calibration results and optional SAR classification is successfully performed with independent observations of the events. We believe that this proposed alternative approach to flood model calibration using spatial patterns of flood inundation should be employed instead of performance measures commonly used in conjunction with a binary flood map. (C) 2013 California Institute of Technology. Hydrological Processes (C) 2013 John Wiley & Sons, Ltd. C1 [Schumann, G. J. -P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Vernieuwe, H.; De Baets, B.] Univ Ghent, Dept Math Modelling Stat & Bioinformat, B-9000 Ghent, Belgium. [Verhoest, N. E. C.] Univ Ghent, Lab Hydrol & Water Management, B-9000 Ghent, Belgium. RP Schumann, GJP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Guy.J.Schumann@jpl.nasa.gov RI Verhoest, Niko/C-9726-2010; Schumann, Guy/F-9760-2011; OI Verhoest, Niko/0000-0003-4116-8881; De Baets, Bernard/0000-0002-3876-620X FU Research Foundation Flanders (FWO) [G.0837.10]; STEREO by Belgian Science Policy Office (BELSPO) [SR/02/152]; National Aeronautics and Space Administration FX This research was performed in the framework of project G.0837.10 granted by the Research Foundation Flanders (FWO) and the STEREO project (SR/02/152) financed by the Belgian Science Policy Office (BELSPO). Part of this research was also carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 46 TC 3 Z9 3 U1 2 U2 26 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0885-6087 EI 1099-1085 J9 HYDROL PROCESS JI Hydrol. Process. PD NOV 30 PY 2014 VL 28 IS 22 BP 5495 EP 5502 DI 10.1002/hyp.10019 PG 8 WC Water Resources SC Water Resources GA AR9AH UT WOS:000343862400003 ER PT J AU Ridley, DA Solomon, S Barnes, JE Burlakov, VD Deshler, T Dolgii, SI Herber, AB Nagai, T Neely, RR Nevzorov, AV Ritter, C Sakai, T Santer, BD Sato, M Schmidt, A Uchino, O Vernier, JP AF Ridley, D. A. Solomon, S. Barnes, J. E. Burlakov, V. D. Deshler, T. Dolgii, S. I. Herber, A. B. Nagai, T. Neely, R. R., III Nevzorov, A. V. Ritter, C. Sakai, T. Santer, B. D. Sato, M. Schmidt, A. Uchino, O. Vernier, J. P. TI Total volcanic stratospheric aerosol optical depths and implications for global climate change SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE volcanic aerosol; forcing uncertainty; warming hiatus; AERONET retrieval; lower stratospheric AOD; stratospheric aerosol ID SIZE DISTRIBUTION MEASUREMENTS AB Understanding the cooling effect of recent volcanoes is of particular interest in the context of the post-2000 slowing of the rate of global warming. Satellite observations of aerosol optical depth above 15km have demonstrated that small-magnitude volcanic eruptions substantially perturb incoming solar radiation. Here we use lidar, Aerosol Robotic Network, and balloon-borne observations to provide evidence that currently available satellite databases neglect substantial amounts of volcanic aerosol between the tropopause and 15km at middle to high latitudes and therefore underestimate total radiative forcing resulting from the recent eruptions. Incorporating these estimates into a simple climate model, we determine the global volcanic aerosol forcing since 2000 to be -0.190.09Wm(-2). This translates into an estimated global cooling of 0.05 to 0.12 degrees C. We conclude that recent volcanic events are responsible for more post-2000 cooling than is implied by satellite databases that neglect volcanic aerosol effects below 15km. C1 [Ridley, D. A.] MIT, Dept Civil & Environm Engn, Cambridge, MA 02139 USA. [Solomon, S.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. [Barnes, J. E.] NOAA, Mauna Loa Observ, Hilo, HI USA. [Burlakov, V. D.; Dolgii, S. I.; Nevzorov, A. V.] Russian Acad Sci, Siberian Branch, VE Zuev Inst Atmospher Opt, Tomsk, Russia. [Deshler, T.] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA. [Herber, A. B.] Helmholtz Ctr Polar & Marine Res, Alfred Wegener Inst, Bremerhaven, Germany. [Nagai, T.; Sakai, T.; Uchino, O.] Meteorol Res Inst, Tsukuba, Ibaraki 305, Japan. [Neely, R. R., III] Natl Ctr Atmospher Res, Adv Study Program, Boulder, CO 80307 USA. [Ritter, C.] Helmholtz Ctr Polar & Marine Res, Alfred Wegener Inst, Potsdam, Germany. [Santer, B. D.] Lawrence Livermore Natl Lab, Program Climate Model Diag & Intercomparison, Livermore, CA USA. [Sato, M.] Columbia Univ, Earth Inst, New York, NY USA. [Schmidt, A.] Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England. [Vernier, J. P.] Sci Syst & Applicat Inc, Hampton, VA USA. [Vernier, J. P.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Ridley, DA (reprint author), MIT, Dept Civil & Environm Engn, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM daridley@mit.edu RI Santer, Benjamin/F-9781-2011; Schmidt, Anja/C-9617-2012; Neely, Ryan/F-8702-2010; OI Neely, Ryan/0000-0003-4560-4812; Nevzorov, Aleksey/0000-0002-5493-8657; Schmidt, Anja/0000-0001-8759-2843 FU National Science Foundation [1011827]; Ministry of Science and Education of the Russian Federation [14.604.21.0046, 14.604.21.0100]; Russian Science Foundation [14-27-00022] FX The Laramie in situ aerosol measurements have been supported primarily by the National Science Foundation, with the current measurements funded under grant 1011827. Measurements at Tomsk were supported in part by the Ministry of Science and Education of the Russian Federation (agreements 14.604.21.0046 and 14.604.21.0100) and the Russian Science Foundation (agreement 14-27-00022). The authors would like to thank the PIs of AERONET stations used in this study, the data from which can be obtained at http://aeronet.gsfc.nasa.gov/. NR 21 TC 41 Z9 44 U1 8 U2 79 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 NOV 28 PY 2014 VL 41 IS 22 BP 7763 EP 7769 DI 10.1002/2014GL061541 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AX0LT UT WOS:000346644600001 ER PT J AU Pan, LL Homeyer, CR Honomichl, S Ridley, BA Weisman, M Barth, MC Hair, JW Fenn, MA Butler, C Diskin, GS Crawford, JH Ryerson, TB Pollack, I Peischl, J Huntrieser, H AF Pan, Laura L. Homeyer, Cameron R. Honomichl, Shawn Ridley, Brian A. Weisman, Morris Barth, Mary C. Hair, Johnathan W. Fenn, Marta A. Butler, Carolyn Diskin, Glenn S. Crawford, James H. Ryerson, Thomas B. Pollack, Ilana Peischl, Jeff Huntrieser, Heidi TI Thunderstorms enhance tropospheric ozone by wrapping and shedding stratospheric air SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE tropospheric ozone; convective transport; stratosphere-troposphere exchange ID MESOSCALE CONVECTIVE COMPLEX; EXCHANGE; TROPOPAUSE; TRANSPORT; MECHANISM AB A significant source of ozone in the troposphere is transport from the stratosphere. The stratospheric contribution has been estimated mainly using global models that attribute the transport process largely to the global-scale Brewer-Dobson circulation and synoptic-scale dynamics associated with upper tropospheric jet streams. We report observations from research aircraft that reveal additional transport of ozone-rich stratospheric air downward into the upper troposphere by a leading-line-trailing-stratiform mesoscale convective system with convection overshooting the tropopause altitude. The fine-scale transport demonstrated by these observations poses a significant challenge to global models that currently do not resolve storm-scale dynamics. Thus, the upper tropospheric ozone budget simulated by global chemistry-climate models where large-scale dynamics and photochemical production from lightning-produced NO are the controlling factors may require modification. C1 [Pan, Laura L.; Homeyer, Cameron R.; Honomichl, Shawn; Ridley, Brian A.; Weisman, Morris; Barth, Mary C.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Hair, Johnathan W.; Fenn, Marta A.; Butler, Carolyn; Diskin, Glenn S.; Crawford, James H.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Ryerson, Thomas B.; Pollack, Ilana; Peischl, Jeff] NOAA, Chem Sci Div, Earth Syst Res Lab, Boulder, CO USA. [Pollack, Ilana; Peischl, Jeff] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Huntrieser, Heidi] German Aerosp Ctr, Inst Atmospher Phys, Oberpfaffenhofen, Germany. RP Pan, LL (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. EM liwen@ucar.edu RI Pan, Laura/A-9296-2008; Peischl, Jeff/E-7454-2010; Homeyer, Cameron/D-5034-2013; Ryerson, Tom/C-9611-2009; Pollack, Ilana/F-9875-2012; Manager, CSD Publications/B-2789-2015 OI Pan, Laura/0000-0001-7377-2114; Peischl, Jeff/0000-0002-9320-7101; Homeyer, Cameron/0000-0002-4883-6670; FU National Science Foundation (NSF) via National Center for Atmospheric Research; NSF; National Aeronautics and Space Administration (NASA); Deutsches Zentrum fur Luft- und Raumfahrt (DLR) FX Funding for this work was provided by the National Science Foundation (NSF) via its sponsorship of the National Center for Atmospheric Research. The DC3 experiment was funded by NSF and the National Aeronautics and Space Administration (NASA). The Falcon aircraft participation was funded by Deutsches Zentrum fur Luft- und Raumfahrt (DLR). The DC3 data are available to the public and can be accessed at http://data.eol.ucar.edu/master_list/?project=DC3. NR 28 TC 16 Z9 17 U1 2 U2 22 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD NOV 28 PY 2014 VL 41 IS 22 BP 7785 EP 7790 DI 10.1002/2014GL061921 PG 6 WC Geosciences, Multidisciplinary SC Geology GA AX0LT UT WOS:000346644600004 ER PT J AU Huang, XL Chen, XH Soden, BJ Liu, X AF Huang, Xianglei Chen, Xiuhong Soden, Brian J. Liu, Xu TI The spectral dimension of longwave feedback in the CMIP3 and CMIP5 experiments SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE radiative feedback; spectral feedback; lapse rate feedback; water vapor feedback ID GENERAL-CIRCULATION MODELS; RADIATIVE KERNEL TECHNIQUE; CLIMATE FEEDBACKS; CLOUD FEEDBACK AB Radiative feedback is normally discussed in terms of the change of broadband flux. Yet it has an intrinsic dimension of spectrum. A set of longwave (LW) spectral radiative kernels (SRKs) is constructed and validated in a similar way as the broadband radiative kernel. The LW broadband feedback derived using this SRK are consistent with those from the broadband radiative kernels. As an application, the SRK is applied to 12 general circulation models (GCMs) from the Coupled Model Intercomparison Project Phase 3 and 12 GCMs from the Coupled Model Intercomparison Project Phase 5 simulations to derive the spectrally resolved Planck, lapse rate, and LW water vapor feedback. The spectral details of the Planck feedback from different GCMs are essentially the same, but the lapse rate and LW water vapor feedback do reveal spectrally dependent difference among GCMs. Spatial distributions of the feedback at different spectral regions are also discussed. The spectral feedback analysis provides us another dimension to understand and evaluate the modeled radiative feedback. C1 [Huang, Xianglei; Chen, Xiuhong] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Soden, Brian J.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. [Liu, Xu] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Huang, XL (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. EM xianglei@umich.edu RI Chen, Xiuhong/P-4030-2014; Huang, Xianglei/G-6127-2011; Richards, Amber/K-8203-2015 OI Huang, Xianglei/0000-0002-7129-614X; FU NASA [NNX11AE68G, NNX14AF18G] FX We wish to thank K. Shell for the thorough and insightful comments, which greatly improved the quality and presentation of our manuscript. We thank the GFDL modeling team for carrying out the Cess +/- 2 K SST simulations. We acknowledge the modeling groups, the Program for Climate Model Diagnosis and Intercomparison and the WCRP's Working Group on Coupled Modeling, for their roles in making available the WCRP CMIP3 and CMIP5 multimodel data sets. We are thankful to K. Shell for making her radiative kernels freely available at http://people.oregonstate.edu/similar to shellk/kernel.html. This research is supported by NASA under grants NNX11AE68G and NNX14AF18G awarded to the University of Michigan. NR 21 TC 3 Z9 3 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD NOV 28 PY 2014 VL 41 IS 22 BP 7830 EP 7837 DI 10.1002/2014GL061938 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AX0LT UT WOS:000346644600010 ER PT J AU Zhang, DX McPhaden, MJ Lee, T AF Zhang, Dongxiao McPhaden, Michael J. Lee, Tong TI Observed interannual variability of zonal currents in the equatorial Indian Ocean thermocline and their relation to Indian Ocean Dipole SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE tropical Indian Ocean; climate variability; ocean circulation; Indian Ocean Dipole; thermocline currents ID MERIDIONAL OVERTURNING CIRCULATION; SEA-SURFACE TEMPERATURE; DECADAL VARIABILITY; PACIFIC-OCEAN; DYNAMICS; EVENTS; LEVEL; CLIMATE; IMPACT; MODEL AB Interannual variability of zonal currents in the eastern equatorial Indian Ocean thermocline is significantly correlated with sea surface temperature (SST) in the eastern pole of the Indian Ocean Dipole (IOD). This relationship is more significant than for zonal currents and the Dipole Mode Index, the latter of which measures zonal SST anomaly gradient. The variability of zonal currents in the thermocline is consistent with the variations of eastward pressure gradient force in the thermocline and the equatorward geostrophic thermocline flows associated with the shallow meridional overturning circulations in the eastern tropical Indian Ocean. Our analysis suggests a positive feedback between zonal currents in the thermocline and SST in the eastern pole of IOD. The combination of equatorial wind and off-equatorial wind stress curls associated with SST anomalies in the eastern pole of the IOD drives interannual variability in equatorial zonal thermocline flows and its covariability with the shallow meridional overturning cells. C1 [Zhang, Dongxiao] Univ Washington, JISAO, Seattle, WA 98195 USA. [McPhaden, Michael J.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. [Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Zhang, DX (reprint author), Univ Washington, JISAO, Seattle, WA 98195 USA. EM dzhang@uw.edu RI McPhaden, Michael/D-9799-2016 FU NASA/Physical Oceanography program; NOAA's Climate Program Office; National Aeronautics and Space Administration; Joint Institute for the Study of the Atmosphere and Ocean under NOAA Cooperative Agreement [NA10OAR4320148] FX Gridded temperature and salinity product are kindly provided by Coriolis data center. Satellite winds and ECCO2 data assimilation are obtained from http://podaac.jpl.nasa.gov. Current measurements are available at www.pmel.noaa.gov/tao. The study is supported by the NASA/Physical Oceanography program. M.J.M. acknowledges support from NOAA's Climate Program Office. This research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This publication is partially funded by the Joint Institute for the Study of the Atmosphere and Ocean under NOAA Cooperative Agreement NA10OAR4320148, contribution 2307; PMEL contribution number 4212. NR 46 TC 5 Z9 5 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD NOV 28 PY 2014 VL 41 IS 22 BP 7933 EP 7941 DI 10.1002/2014GL061449 PG 9 WC Geosciences, Multidisciplinary SC Geology GA AX0LT UT WOS:000346644600023 ER PT J AU Kuang, W Jiang, W Roberts, J Frey, HV AF Kuang, W. Jiang, W. Roberts, J. Frey, H. V. TI Could giant basin-forming impacts have killed Martian dynamo? SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Martian dynamo; giant impacts; thermal heterogeneity; numerical simulation ID MARS AB The observed strong remanent crustal magnetization at the surface of Mars suggests an active dynamo in the past and ceased to exist around early to middle Noachian era, estimated by examining remagnetization strengths in extant and buried impact basins. We investigate whether the Martian dynamo could have been killed by these large basin-forming impacts, via numerical simulation of subcritical dynamos with impact-induced thermal heterogeneity across the core-mantle boundary. We find that subcritical dynamos are prone to the impacts centered on locations within 30 degrees of the equator but can easily survive those at higher latitudes. Our results further suggest that magnetic timing places a strong constraint on postimpact polar reorientation, e.g., a minimum 16 degrees polar reorientation is needed if Utopia is the dynamo killer. C1 [Kuang, W.; Frey, H. V.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Jiang, W.] Sci Syst & Applicat Inc, Lanham, MD USA. [Roberts, J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Kuang, W (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. EM Weijia.Kuang-1@nasa.gov RI Roberts, James/I-9030-2012; Kuang, Weijia/K-5141-2012 OI Kuang, Weijia/0000-0001-7786-6425 FU NASA Mars Fundamental Research Program; NASA Mars Data Analysis Program FX This research is supported by NASA Mars Fundamental Research Program and by NASA Mars Data Analysis Program. We also thank NASA NAS on high-end scientific computation support. The data (dynamo simulation results) used for this paper are available upon request (weijia.kuang-1@nasa.gov). NR 24 TC 1 Z9 1 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD NOV 28 PY 2014 VL 41 IS 22 BP 8006 EP 8012 DI 10.1002/2014GL061818 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AX0LT UT WOS:000346644600032 ER PT J AU Velicogna, I Sutterley, TC van den Broeke, MR AF Velicogna, I. Sutterley, T. C. van den Broeke, M. R. TI Regional acceleration in ice mass loss from Greenland and Antarctica using GRACE time-variable gravity data SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE mass balance; time-variable gravity; Greenland; sea level; Antarctica; remote sensing ID SEA-LEVEL; RECONCILED ESTIMATE; SHEET; VARIABILITY; GLACIERS; BALANCE; DISCHARGE; FIELD AB We use Gravity Recovery and Climate Experiment (GRACE) monthly gravity fields to determine the regional acceleration in ice mass loss in Greenland and Antarctica for 2003-2013. We find that the total mass loss is controlled by only a few regions. In Greenland, the southeast and northwest generate 70% of the loss (28058 Gt/yr) mostly from ice dynamics, the southwest accounts for 54% of the total acceleration in loss (25.41.2 Gt/yr(2)) from a decrease in surface mass balance (SMB), followed by the northwest (34%), and we find no significant acceleration in the northeast. In Antarctica, the Amundsen Sea (AS) sector and the Antarctic Peninsula account for 64% and 17%, respectively, of the total loss (18010 Gt/yr) mainly from ice dynamics. The AS sector contributes most of the acceleration in loss (114 Gt/yr(2)), and Queen Maud Land, East Antarctica, is the only sector with a significant mass gain due to a local increase in SMB (63 +/- 5 Gt/yr). C1 [Velicogna, I.; Sutterley, T. C.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Velicogna, I.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [van den Broeke, M. R.] Univ Utrecht, Inst Marine & Atmospher Res, Utrecht, Netherlands. RP Velicogna, I (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. EM isabella@uci.edu RI Van den Broeke, Michiel/F-7867-2011; Sutterley, Tyler/Q-8325-2016 OI Van den Broeke, Michiel/0000-0003-4662-7565; Sutterley, Tyler/0000-0002-6964-1194 FU NASA [JPL-1390432, UTA12-000609, UTA13-000917] FX This work was performed at the UCI and JPL-Caltech; it was supported by the NASA's Cryosphere, Terrestrial Hydrology and IDS Programs, JPL-1390432, UTA12-000609, and UTA13-000917 contracts. Data used in this paper are available upon request to the authors. NR 36 TC 43 Z9 46 U1 7 U2 64 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 NOV 28 PY 2014 VL 41 IS 22 BP 8130 EP 8137 DI 10.1002/2014GL061052 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AX0LT UT WOS:000346644600048 ER PT J AU Seo, DJ Liu, YQ Moradkhani, H Weerts, A AF Seo, Dong-Jun Liu, Yuqiong Moradkhani, Hamid Weerts, Albrecht TI Ensemble prediction and data assimilation for operational hydrology SO JOURNAL OF HYDROLOGY LA English DT Editorial Material ID UNCERTAINTY C1 [Seo, Dong-Jun] Univ Texas Arlington, Dept Civil Engn, Arlington, TX 76019 USA. [Liu, Yuqiong] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Moradkhani, Hamid] Portland State Univ, Dept Civil Engn, Portland, OR 97201 USA. [Weerts, Albrecht] Deltares, NL-2600 MH Delft, Netherlands. [Weerts, Albrecht] Wageningen Univ, Hydrol & Quantitat Water Management Grp, Dept Environm Sci, NL-6700 AP Wageningen, Netherlands. RP Seo, DJ (reprint author), Univ Texas Arlington, Dept Civil Engn, Box 19308,Rm 248E Nedderman Hall,416 Yates St, Arlington, TX 76019 USA. EM djseo@uta.edu; yuqiong.liu@nasa.gov; hamidm@pdx.edu; albrecht.weerts@deltares.nl RI Moradkhani, Hamid/B-1571-2012 NR 15 TC 6 Z9 6 U1 0 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-1694 EI 1879-2707 J9 J HYDROL JI J. Hydrol. PD NOV 27 PY 2014 VL 519 BP 2661 EP 2662 DI 10.1016/j.jhydro1.2014.11.035 PN D PG 2 WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA AY5BZ UT WOS:000347589600001 ER PT J AU Pavelsky, TM Durand, MT Andreadis, KM Beighley, RE Paiva, RCD Allen, GH Miller, ZF AF Pavelsky, Tamlin M. Durand, Michael T. Andreadis, Konstantinos M. Beighley, R. Edward Paiva, Rodrigo C. D. Allen, George H. Miller, Zachary F. TI Assessing the potential global extent of SWOT river discharge observations SO JOURNAL OF HYDROLOGY LA English DT Article DE Remote sensing; River discharge; Global hydrology; Downstream hydraulic geometry; SWOT ID FRESH-WATER DISCHARGE; LAND-COVER DATABASE; INUNDATION; ELEVATION; RUNOFF; SLOPE; OCEAN; BASIN; WIDTH; GIS AB Despite its importance as a major element of the global hydrologic cycle, runoff remains poorly constrained except at the largest spatial scales due to limitations of the global stream gauge network and inadequate data sharing. Efforts using remote sensing to infer runoff from discharge estimates are limited by characteristics of present-day sensors. The proposed Surface Water and Ocean Topography (SWOT) mission, a joint project between the United States and France, aims to substantially improve space-based estimates of river discharge. However, the extent of rivers observable by SWOT, likely limited to those wider than 50-100 m, remains unknown. Here, we estimate the extent of SWOT river observability globally using a downstream hydraulic geometry (DHG) approach combining basin areas from the Hydrol k and Hydrosheds elevation products, discharge from the Global Runoff Data Centre (GRDC), and width estimates from a global width-discharge relationship. We do not explicitly consider SWOT-specific errors associated with layover and other phenomena in this analysis, although they have been considered in formulation of the 50-100 m width thresholds. We compare the extent of SWOT-observable rivers with GRDC and USGS gauge datasets, the most complete datasets freely available to the global scientific community. In the continental US, SWOT would match USGS river basin coverage only at large scales (>25,000 km(2)). Globally, SWOT would substantially improve on GRDC observation extent: SWOT observation of 100 m (50 m) rivers will allow discharge estimation in >60% of 50,000 km(2) (10,000 km(2)) river basins. In contrast, the GRDC observes fewer than 30% (15%) of these basins. SWOT could improve characterization of global runoff processes, especially with a 50 m observability threshold, but in situ gauge data remains essential and must be shared more freely with the international scientific community. (C) 2014 Elsevier B.V. All rights reserved. C1 [Pavelsky, Tamlin M.; Allen, George H.; Miller, Zachary F.] Univ N Carolina, Dept Geol Sci, Chapel Hill, NC 27515 USA. [Durand, Michael T.] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA. [Andreadis, Konstantinos M.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA. [Beighley, R. Edward] Northeastern Univ, Dept Civil & Environm Engn, Boston, MA USA. [Paiva, Rodrigo C. D.] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA. RP Pavelsky, TM (reprint author), Univ N Carolina, Dept Geol Sci, Chapel Hill, NC 27515 USA. OI Paiva, Rodrigo/0000-0003-2918-6681 FU NASA Terrestrial Hydrology [NNX13ADO5G, NNX12AQ36G]; NASA SWOT Science Definition Team [NNX13AD96G]; NASA Terrestrial Hydrology Grant [NNX12AQ36G, NNX13AD05G]; NASA SWOT Science Definition Team Grant [NNX13AD96G] FX This work was funded by NASA Terrestrial Hydrology Grant # NNX13AD05G (PI: T. Pavelsky) and # NNX12AQ36G (PI: E. Beighley) and NASA SWOT Science Definition Team Grant # NNX13AD96G (PI: M. Durand). Thanks to Ms. Rui Wei for help working with the GIS datasets. We also thank two anonymous reviewers for their useful comments. NR 49 TC 24 Z9 24 U1 4 U2 28 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-1694 EI 1879-2707 J9 J HYDROL JI J. Hydrol. PD NOV 27 PY 2014 VL 519 BP 1516 EP 1525 DI 10.1016/j.jhydrol.2014.08.044 PN B PG 10 WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA AX6FH UT WOS:000347018100021 ER PT J AU Brown, ME Racoviteanu, AE Tarboton, DG Sen Gupta, A Nigro, J Policelli, F Habib, S Tokay, M Shrestha, MS Bajracharya, S Hummel, P Gray, M Duda, P Zaitchik, B Mahat, V Artan, G Tokar, S AF Brown, M. E. Racoviteanu, A. E. Tarboton, D. G. Sen Gupta, A. Nigro, J. Policelli, F. Habib, S. Tokay, M. Shrestha, M. S. Bajracharya, S. Hummel, P. Gray, M. Duda, P. Zaitchik, B. Mahat, V. Artan, G. Tokar, S. TI An integrated modeling system for estimating glacier and snow melt driven streamflow from remote sensing and earth system data products in the Himalayas SO JOURNAL OF HYDROLOGY LA English DT Article DE Himalayas; Glacier melt; Energy balance; Stream flow ID BAND ALBEDO CONVERSION; CLIMATE-CHANGE; SPATIAL-DISTRIBUTION; WATER AVAILABILITY; DEBRIS THICKNESS; MASS-BALANCE; ICE; BASIN; RIVER; TEMPERATURE AB Quantification of the contribution of the hydrologic components (snow, ice and rain) to river discharge in the Hindu Kush Himalayan (HKH) region is important for decision-making in water sensitive sectors, and for water resources management and flood risk reduction. In this area, access to and monitoring of the glaciers and their melt outflow is challenging due to difficult access, thus modeling based on remote sensing offers the potential for providing information to improve water resources management and decision making. This paper describes an integrated modeling system developed using downscaled NASA satellite based and earth system data products coupled with in-situ hydrologic data to assess the contribution of snow and glaciers to the flows of the rivers in the HKH region. Snow and glacier melt was estimated using the Utah Energy Balance (UEB) model, further enhanced to accommodate glacier ice melt over clean and debris-covered tongues, then meltwater was input into the USGS Geospatial Stream Flow Model (GeoSFM). The two model components were integrated into Better Assessment Science Integrating point and Nonpoint Sources modeling framework (BASINS) as a user-friendly open source system and was made available to countries in high Asia. Here we present a case study from the Langtang Khola watershed in the monsoon-influenced Nepal Himalaya, used to validate our energy balance approach and to test the applicability of our modeling system. The snow and glacier melt model predicts that for the eight years used for model evaluation (October 2003-September 2010), the total surface water input over the basin was 9.43 m, originating as 62% from glacier melt, 30% from snowmelt and 8% from rainfall. Measured streamflow for those years were 5.02 m, reflecting a runoff coefficient of 0.53. GeoSFM simulated streamflow was 5.31 m indicating reasonable correspondence between measured and model confirming the capability of the integrated system to provide a quantification of water availability. Published by Elsevier B.V. C1 [Brown, M. E.; Nigro, J.; Policelli, F.; Habib, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Racoviteanu, A. E.] Lab Glaciol & Geophys Environm, Paris, France. [Tarboton, D. G.; Sen Gupta, A.] Utah State Univ, Logan, UT 84322 USA. [Nigro, J.; Tokay, M.] Sci Syst & Applicat Inc, Lanham, MD USA. [Shrestha, M. S.; Bajracharya, S.] Int Ctr Integrated Mt Dev ICIMOD, Kathmandu, Nepal. [Hummel, P.; Gray, M.; Duda, P.] AquaTerra Consultants, Decatur, GA USA. [Zaitchik, B.] Johns Hopkins Univ, Baltimore, MD USA. [Mahat, V.] Colorado State Univ, Ft Collins, CO 80523 USA. [Artan, G.] US Geol Survey, Sioux Falls, SD USA. [Tokar, S.] US Agcy Int Dev, Off Foreign Disaster Assistance, Washington, DC 20523 USA. RP Brown, ME (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM molly.brown@nasa.gov RI Sen Gupta, Avirup/L-8938-2014; Brown, Molly/E-2724-2010; OI Sen Gupta, Avirup/0000-0001-5972-5186; Brown, Molly/0000-0001-7384-3314; Tarboton, David/0000-0002-1998-3479; Racoviteanu, Adina/0000-0003-4954-1871 FU National Aeronautics and Space Administration [NNH08ZDA001N-DECISIONS]; Centre National d'Etudes Spatiales (CNES), France; Office of U.S. Foreign Disaster Assistance; Bureau for Democracy; Conflict and Humanitarian Assistance; U.S. Agency for International Development [AID-OFDA-T-11-00002] FX This work was supported by a grant from the National Aeronautics and Space Administration's Applied Sciences Program through its 2008 Decision Support through Earth Science Research Results Grant Number NNH08ZDA001N-DECISIONS. A. Racoviteanu's post-doctoral studies were supported by the Centre National d'Etudes Spatiales (CNES), France. This publication was made possible through partial support provided by the Office of U.S. Foreign Disaster Assistance, Bureau for Democracy, Conflict and Humanitarian Assistance, U.S. Agency for International Development, under the terms Award No. AID-OFDA-T-11-00002. The opinions expressed in this publication are those of the authors and do not necessarily reflect views of the U.S. Agency for International Development. NR 65 TC 5 Z9 6 U1 3 U2 34 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-1694 EI 1879-2707 J9 J HYDROL JI J. Hydrol. PD NOV 27 PY 2014 VL 519 BP 1859 EP 1869 DI 10.1016/j.jhydrol.2014.09.050 PN B PG 11 WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA AX6FH UT WOS:000347018100051 ER PT J AU Dessler, AE Schoeberl, MR Wang, T Davis, SM Rosenlof, KH Vernier, JP AF Dessler, A. E. Schoeberl, M. R. Wang, T. Davis, S. M. Rosenlof, K. H. Vernier, J. -P. TI Variations of stratospheric water vapor over the past three decades SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TROPICAL TROPOPAUSE; VOLCANIC-ERUPTIONS; INTERANNUAL VARIABILITY; TROPOSPHERE EXCHANGE; GENERAL-CIRCULATION; DEUTERATED WATER; RADIOSONDE DATA; TRENDS; CLIMATE; REANALYSES AB We examine variations in water vapor in air entering the stratosphere through the tropical tropopause layer (TTL) over the past three decades in satellite data and in a trajectory model. Most of the variance can be explained by three processes that affect the TTL: the quasi-biennial oscillation, the strength of the Brewer-Dobson circulation, and the temperature of the tropical troposphere. When these factors act in phase, significant variations in water entering the stratosphere are possible. We also find that volcanic eruptions, which inject aerosol into the TTL, affect the amount of water entering the stratosphere. While there is clear decadal variability in the data and models, we find little evidence for a long-term trend in water entering the stratosphere through the TTL over the past 3 decades. C1 [Dessler, A. E.; Wang, T.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. [Schoeberl, M. R.] Sci & Technol Corp, Columbia, MD USA. [Wang, T.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Davis, S. M.; Rosenlof, K. H.] NOAA, Earth Syst Res Lab, Boulder, CO USA. [Davis, S. M.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Vernier, J. -P.] Sci Syst & Applicat Inc, Hampton, VA USA. [Vernier, J. -P.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Dessler, AE (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA. EM adessler@tamu.edu RI Davis, Sean/C-9570-2011; Rosenlof, Karen/B-5652-2008; Wang, Tao/C-2381-2011; Dessler, Andrew/G-8852-2012; Manager, CSD Publications/B-2789-2015 OI Davis, Sean/0000-0001-9276-6158; Rosenlof, Karen/0000-0002-0903-8270; Wang, Tao/0000-0003-3430-8508; Dessler, Andrew/0000-0003-3939-4820; FU NSF [AGS-1261948]; NASA [NNX13AK25G] FX This work was supported by NSF grant AGS-1261948 and NASA grant NNX13AK25G, both to Texas A&M University. We thank Bernard Legras for help with the ERAi model runs. The quality-controlled satellite data, compiled in the SWOOSH data set, can be found at http://www.esrl.noaa.gov/csd/groups/csd8/swoosh/. The met fields used in the trajectory calculation can be found at http://data-portal.ecmwf.int/data/d/interim_daily/ and http://disc.sci.gsfc.nasa.gov/. NR 57 TC 23 Z9 23 U1 3 U2 34 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 NOV 27 PY 2014 VL 119 IS 22 BP 12588 EP 12598 DI 10.1002/2014JD021712 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AW5YA UT WOS:000346345600011 ER PT J AU Liu, CX Tian, BJ Li, KF Manney, GL Livesey, NJ Yung, YL Waliser, DE AF Liu, Chuanxi Tian, Baijun Li, King-Fai Manney, Gloria L. Livesey, Nathaniel J. Yung, Yuk L. Waliser, Duane E. TI Northern Hemisphere mid-winter vortex-displacement and vortex-split stratospheric sudden warmings: Influence of the Madden-Julian Oscillation and Quasi-Biennial Oscillation SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MULTIVARIATE MJO INDEX; POLAR VORTEX; SOUTHERN OSCILLATION; SOLAR-CYCLE; ARCTIC OSCILLATION; WAVE-PROPAGATION; WINTER; QBO; TROPOSPHERE; CIRCULATION AB We investigate the connection between the equatorial Madden-Julian Oscillation (MJO) and different types of the Northern Hemisphere mid-winter major stratospheric sudden warmings (SSWs), i.e., vortex-displacement and vortex-split SSWs. The MJO-SSW relationship for vortex-split SSWs is stronger than that for vortex-displacement SSWs, as a result of the stronger and more coherent eastward propagating MJOs before vortex-split SSWs than those before vortex-displacement SSWs. Composite analysis indicates that both the intensity and propagation features of MJO may influence the MJO-related circulation pattern at high latitudes and the type of SSWs. A pronounced Quasi-Biennial Oscillation (QBO) dependence is found for vortex-displacement and vortex-split SSWs, with vortex-displacement (-split) SSWs occurring preferentially in easterly (westerly) QBO phases. The lagged composites suggest that the MJO-related anomalies in the Arctic are very likely initiated when the MJO-related convection is active over the equatorial Indian Ocean (around the MJO phase 3). Further analysis suggests that the QBO may modulate the MJO-related wave disturbances via its influence on the upper tropospheric subtropical jet. As a result, the MJO-related circulation pattern in the Arctic tends to be wave number-one/wave number-two similar to 25-30 days following phase 3 (i.e., approximately phases 7-8, when the MJO-related convection is active over the western Pacific) during easterly/westerly QBO phases, which resembles the circulation pattern associated with vortex-displacement/vortex-split SSWs. C1 [Liu, Chuanxi; Tian, Baijun; Livesey, Nathaniel J.; Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Liu, Chuanxi] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. [Li, King-Fai] Univ Corp Atmospher Res, Boulder, CO USA. [Li, King-Fai] Univ Washington, Dept Appl Math, Seattle, WA 98195 USA. [Manney, Gloria L.] NorthWest Res Associates, Socorro, NM USA. [Manney, Gloria L.] New Mexico Inst Min & Technol, Socorro, NM 87801 USA. [Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Liu, CX (reprint author), Chinese Acad Sci, Inst Atmospher Phys, Key Lab Middle Atmosphere & Global Environm Obser, Beijing, Peoples R China. EM tenkeiliu@gmail.com RI Tian, Baijun/A-1141-2007; OI Tian, Baijun/0000-0001-9369-2373; Li, King-Fai/0000-0003-0150-2910 FU National Science Foundation [ATM-0840755]; Jack Eddy Fellowship FX This research was supported by the National Science Foundation award ATM-0840755 to University of California, Los Angeles. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. KFL was supported by the Jack Eddy Fellowship, managed by the University Corporation for Atmospheric research. We thank George Kiladis and two anonymous reviewers for their helpful comments. We thank Guang J. Zhang for helpful discussions. The NCEP-NCAR reanalysis data were kindly provided by the NOAA/OAR/ESRL-PSD, Boulder, Colorado, from their website (http://www.esrl.noaa.gov/psd/). NR 75 TC 6 Z9 7 U1 0 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD NOV 27 PY 2014 VL 119 IS 22 BP 12599 EP 12620 DI 10.1002/2014JD021876 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AW5YA UT WOS:000346345600012 ER PT J AU Huang, M Bowman, KW Carmichael, GR Chai, TF Pierce, RB Worden, JR Luo, M Pollack, IB Ryerson, TB Nowak, JB Neuman, JA Roberts, JM Atlas, EL Blake, DR AF Huang, Min Bowman, Kevin W. Carmichael, Gregory R. Chai, Tianfeng Pierce, R. Bradley Worden, John R. Luo, Ming Pollack, Ilana B. Ryerson, Thomas B. Nowak, John B. Neuman, J. Andrew Roberts, James M. Atlas, Elliot L. Blake, Donald R. TI Changes in nitrogen oxides emissions in California during 2005-2010 indicated from top-down and bottom-up emission estimates SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ADJOINT SENSITIVITY-ANALYSIS; OZONE MONITORING INSTRUMENT; CONTINENTAL UNITED-STATES; TROPOSPHERIC NO2 COLUMNS; ARCTAS-CARB PERIOD; AIR-QUALITY; SURFACE OZONE; IN-SITU; SATELLITE RETRIEVALS; ERROR ANALYSIS AB In California, emission control strategies have been implemented to reduce air pollutants. Here we estimate the changes in nitrogen oxides (NOx = NO+ NO2) emissions in 2005-2010 using a state-of-the-art four-dimensional variational approach. We separately and jointly assimilate surface NO2 concentrations and tropospheric NO2 columns observed by Ozone Monitoring Instrument (OMI) into the regional-scale Sulfur Transport and dEposition Model (STEM) chemical transport model on a 12 x 12 km(2) horizontal resolution grid in May 2010. The assimilation generates grid-scale top-down emission estimates, and the updated chemistry fields are evaluated with independent aircraft measurements during the NOAA California Nexus (CalNex) field experiment. The emission estimates constrained only by NO2 columns, only by surface NO2, and by both indicate statewide reductions of 26%, 29%, and 30% from similar to 0.3 Tg N/yr in the base year of 2005, respectively. The spatial distributions of the emission changes differ in these cases, which can be attributed to many factors including the differences in the observation sampling strategies and their uncertainties, as well as those in the sensitivities of column and surface NO2 with respect to NOx emissions. The updates in California's NOx emissions reduced the mean error in modeled surface ozone in the Western U.S., even though the uncertainties in some urban areas increased due to their NOx-saturated chemical regime. The statewide reductions in NOx emissions indicated from our observationally constrained emission estimates are also reflected in several independently developed inventories: similar to 30% in the California Air Resources Board bottom-up inventory, similar to 4% in the 2008 National Emission Inventory, and similar to 20% in the annual mean top-down estimates by Lamsal et al. using the global Goddard Earth Observing System (GEOS)-Chem model and OMI NO2 columns. Despite the grid-scale differences among all top-down and bottom-up inventories, they all indicate stronger emission reductions in the urban regions. This study shows the potential of using space-/ground-based monitoring data and advanced data assimilation approach to timely and independently update NOx emission estimates on a monthly scale and at a fine grid resolution. The well-evaluated results here suggest that these approaches can be applied more broadly. C1 [Huang, Min; Bowman, Kevin W.; Worden, John R.; Luo, Ming] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Carmichael, Gregory R.] Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA USA. [Chai, Tianfeng] NOAA Air Resources Lab, College Pk, MD USA. [Pierce, R. Bradley] NOAA Natl Environm Satellite Data & Informat Serv, Madison, WI USA. [Pollack, Ilana B.; Nowak, John B.; Neuman, J. Andrew] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Pollack, Ilana B.; Ryerson, Thomas B.; Nowak, John B.; Neuman, J. Andrew; Roberts, James M.] NOAA Earth Syst Res Lab, Boulder, CO USA. [Atlas, Elliot L.] Univ Miami, Dept Atmospher Sci, Miami, FL USA. [Blake, Donald R.] Univ Calif Irvine, Dept Chem, Irvine, CA 92717 USA. RP Huang, M (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM min.huang@jpl.nasa.gov RI Neuman, Andy/A-1393-2009; Chai, Tianfeng/E-5577-2010; Roberts, James/A-1082-2009; Pierce, Robert Bradley/F-5609-2010; Nowak, John/B-1085-2008; Ryerson, Tom/C-9611-2009; Atlas, Elliot/J-8171-2015; Pollack, Ilana/F-9875-2012; Manager, CSD Publications/B-2789-2015 OI Neuman, Andy/0000-0002-3986-1727; Chai, Tianfeng/0000-0003-3520-2641; Roberts, James/0000-0002-8485-8172; Pierce, Robert Bradley/0000-0002-2767-1643; Nowak, John/0000-0002-5697-9807; FU NASA [NNX11AI52G]; NASA Aura project FX This work was initiated at the University of Iowa and supported by a NASA award NNX11AI52G. It was continued at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA, supported by the NASA Aura project. We thank the CalNex and Aura science teams, and the open access to the used observation data and the NOx emission scaling factors created by Lamsal et al. The sources of data are cited in text and Table 1. We also acknowledge the computational resources at the University of Iowa and at NASA Ames Research Center. The views, opinions, and findings contained in this paper are those of the authors and should not be construed as an official NOAA or U.S. Government position, policy, or decision. NR 107 TC 4 Z9 4 U1 2 U2 44 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 NOV 27 PY 2014 VL 119 IS 22 BP 12928 EP 12952 DI 10.1002/2014JD022268 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AW5YA UT WOS:000346345600029 ER PT J AU Baker, DN Jaynes, AN Hoxie, VC Thorne, RM Foster, JC Li, X Fennell, JF Wygant, JR Kanekal, SG Erickson, PJ Kurth, W Li, W Ma, Q Schiller, Q Blum, L Malaspina, DM Gerrard, A Lanzerotti, LJ AF Baker, D. N. Jaynes, A. N. Hoxie, V. C. Thorne, R. M. Foster, J. C. Li, X. Fennell, J. F. Wygant, J. R. Kanekal, S. G. Erickson, P. J. Kurth, W. Li, W. Ma, Q. Schiller, Q. Blum, L. Malaspina, D. M. Gerrard, A. Lanzerotti, L. J. TI An impenetrable barrier to ultrarelativistic electrons in the Van Allen radiation belts SO NATURE LA English DT Article ID INNER ZONE ELECTRONS; RELATIVISTIC ELECTRONS; MAGNETIC STORM; SOLAR-WIND; PRECIPITATION; EVOLUTION; DIFFUSION; MISSION; EARTH; RING AB Early observations(1,2) indicated that the Earth's Van Allen radiation belts could be separated into an inner zone dominated by high-energy protons and an outer zone dominated by high-energy electrons. Subsequent studies(3,4) showed that electrons of moderate energy (less than about one megaelectronvolt) often populate both zones, with a deep 'slot' region largely devoid of particles between them. There is a region of dense cold plasma around the Earth known as the plasmasphere, the outer boundary of which is called the plasmapause. The two-belt radiation structure was explained as arising from strong electron interactions with plasmaspheric hiss just inside the plasmapause boundary(5), with the inner edge of the outer radiation zone corresponding to the minimum plasmapause location(6). Recent observations have revealed unexpected radiation belt morphology(7,8), especially at ultrarelativistic kinetic energies(9,10) (more than five megaelectronvolts). Here we analyse an extended data set that reveals an exceedingly sharp inner boundary for the ultrarelativistic electrons. Additional, concurrently measured data(11) reveal that this barrier to inward electron radial transport does not arise because of a physical boundary within the Earth's intrinsic magnetic field, and that inward radial diffusion is unlikely to be inhibited by scattering by electromagnetic transmitter wave fields. Rather, we suggest that exceptionally slow natural inward radial diffusion combined with weak, but persistent, wave-particle pitch angle scattering deep inside the Earth's plasmasphere can combine to create an almost impenetrable barrier through which the most energetic Van Allen belt electrons cannot migrate. C1 [Baker, D. N.; Jaynes, A. N.; Hoxie, V. C.; Li, X.; Schiller, Q.; Blum, L.; Malaspina, D. M.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. [Thorne, R. M.; Li, W.; Ma, Q.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA. [Foster, J. C.; Erickson, P. J.] MIT, Haystack Observ, Westford, MA 01886 USA. [Fennell, J. F.] Aerosp Corp, Space Sci Lab, Los Angeles, CA 90009 USA. [Wygant, J. R.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Kanekal, S. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kurth, W.] Univ Iowa, Dept Phys, Iowa City, IA 52242 USA. [Gerrard, A.; Lanzerotti, L. J.] New Jersey Inst Technol, Ctr Solar Terr Res, Newark, NJ 07102 USA. RP Baker, DN (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA. EM daniel.baker@lasp.colorado.edu FU JHU/APL [967399]; JHU/APL under NASA [NAS5-01072] FX We thank the entire Van Allen Probes mission team for suggestions about this work. Data access was provided through the Johns Hopkins University/Applied Physics Lab Mission Operations Center and the Los Alamos National Laboratory Science Operations Center. This work was supported by JHU/APL contract 967399 under NASA's prime contract NAS5-01072. All Van Allen Probes data used are publicly available at http://www.rbsp-ect.lanl.gov. NR 29 TC 36 Z9 36 U1 3 U2 23 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD NOV 27 PY 2014 VL 515 IS 7528 BP 531 EP + DI 10.1038/nature13956 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AW4JP UT WOS:000346247600048 PM 25428500 ER PT J AU Vu, TH Gloesener, E Choukroun, M Ibourichene, A Hodyss, R AF Tuan Hoang Vu Gloesener, Elodie Choukroun, Mathieu Ibourichene, Anais Hodyss, Robert TI Experimental Study on the Effect of Ammonia on the Phase Behavior of Tetrahydrofuran Clathrates SO JOURNAL OF PHYSICAL CHEMISTRY B LA English DT Article ID RAMAN-SPECTROSCOPY; NEUTRON-DIFFRACTION; TITANS ATMOSPHERE; HYDRATE FORMATION; GAS; METHANE; ETHANE; CONSTITUENTS; KINETICS; SPECTRA AB Clathrate hydrates, ice-like crystalline compounds in which small guest molecules are enclosed inside cages formed by tetrahedrally hydrogen-bonded water molecules, are naturally abundant on Earth and are generally expected to exist on icy celestial bodies. A prototypical example is Saturns moon Titan, where dissociation of methane clathrates, a major crustal component, could contribute significantly to the replenishment of atmospheric methane. Ammonia is an important clathrate inhibiting agent that may be present (potentially at high concentrations) in Titans interior. In this study, low-temperature Raman experiments are conducted to examine the dissociation point of tetrahydrofuran clathrates, an ambient-pressure analogue of methane clathrates, over a wide range of ammonia concentrations from 0 to 25 wt %. A phase diagram for the H2O-THF-NH-3 system is generated, showing two main results: (i) ammonia lowers the dissociation point of clathrate hydrates to a similar extent compared to the melting of water ice and (ii) THF clathrate exhibits a liquidus-like behavior in the presence of ammonia, with a eutectic temperature of about 203.6 K. As temperatures higher than this estimated eutectic are anticipated within Titans icy crust, these results imply that partial dissociation of clathrates can occur readily and may contribute to outgassing from the interior. C1 [Tuan Hoang Vu; Choukroun, Mathieu; Hodyss, Robert] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA. [Gloesener, Elodie] Observ Royal Belgique, B-1180 Uccle, Belgium. [Ibourichene, Anais] Ecole Normale Super, F-75005 Paris, France. RP Choukroun, M (reprint author), CALTECH, NASA Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mathieu.choukroun@jpl.nasa.gov RI Choukroun, Mathieu/F-3146-2017; Vu, Tuan/F-5223-2017 OI Choukroun, Mathieu/0000-0001-7447-9139; Vu, Tuan/0000-0001-6839-9765 FU NASA; FRIA Ph.D. grant (Fonds pour la formation a la Recherche dans l'Industrie et dans l'Agriculture) FX This work was conducted at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. E.G. was funded through the FRIA Ph.D. grant (Fonds pour la formation a la Recherche dans l'Industrie et dans l'Agriculture). Financial support from the NASA Outer Planets Research Program and government sponsorship are gratefully acknowledged. NR 35 TC 2 Z9 2 U1 8 U2 33 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1520-6106 J9 J PHYS CHEM B JI J. Phys. Chem. B PD NOV 27 PY 2014 VL 118 IS 47 SI SI BP 13371 EP 13377 DI 10.1021/jp5042487 PG 7 WC Chemistry, Physical SC Chemistry GA AU6OU UT WOS:000345722900008 PM 24940841 ER PT J AU Betancourt-Martinez, GL Beiersdorfer, P Brown, GV Kelley, RL Kilbourne, CA Koutroumpa, D Leutenegger, MA Porter, FS AF Betancourt-Martinez, Gabriele L. Beiersdorfer, Peter Brown, Gregory V. Kelley, Richard L. Kilbourne, Caroline A. Koutroumpa, Dimitra Leutenegger, Maurice A. Porter, F. Scott TI Observation of highly disparate K-shell x-ray spectra produced by charge exchange with bare mid-Z ions SO PHYSICAL REVIEW A LA English DT Article ID MULTIPLE-ELECTRON CAPTURE; CROSS-SECTIONS; SOLAR-SYSTEM; HYDROGEN-ATOMS; EXCITED-STATES; BEAM INJECTION; CYGNUS LOOP; PDX TOKAMAK; HEAVY-IONS; COLLISIONS AB We performed charge-exchange experiments with the electron-beam ion trap and an x-ray calorimeter spectrometer at the Lawrence Livermore National Laboratory. We compare the relative strength of the high-n Lyman series emission for different combinations of ions and neutral gases. Theoretical predictions show good agreement with experimental data on the relative capture cross section as a function of principal quantum number n; however, the few published predictions of the distribution of captures as a function of orbital angular momentum l do not agree with experiments. Our experimental results show that the relative strength of high-n Lyman series emission varies more widely than previous experiments have found and models predict. We find that hardness ratios from charge exchange with helium and molecular hydrogen are more disparate than charge exchange with many-electron neutral species, which is likely due to differences in the relative importance of multielectron capture. We also find that there is no clear scaling of the hardness ratio with the ionization potential of the neutral species, the number of valence electrons in the neutral species, or the atomic number of the ion. C1 [Betancourt-Martinez, Gabriele L.] CRESST, College Pk, MD 20742 USA. [Betancourt-Martinez, Gabriele L.] Univ Maryland, College Pk, MD 20742 USA. [Betancourt-Martinez, Gabriele L.; Kelley, Richard L.; Kilbourne, Caroline A.; Leutenegger, Maurice A.; Porter, F. Scott] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Beiersdorfer, Peter; Brown, Gregory V.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Koutroumpa, Dimitra] CNRS, LATMOS IPSL, Guyancourt, France. [Leutenegger, Maurice A.] CRESST, Baltimore, MD 21250 USA. [Leutenegger, Maurice A.] Univ Maryland, Baltimore, MD 21250 USA. RP Betancourt-Martinez, GL (reprint author), CRESST, College Pk, MD 20742 USA. RI Porter, Frederick/D-3501-2012 OI Porter, Frederick/0000-0002-6374-1119 FU U.S. Department of Energy [DE-AC52-07NA27344]; NASA APRA FX The authors would like to thank E. Magee and D. Layne at LLNL for their technical support. We also thank the anonymous referees for their helpful comments. Work at the Lawrence Livermore National Laboratory was performed under the auspices of the U.S. Department of Energy under Contract No. DE-AC52-07NA27344 and was supported by NASA APRA grants to LLNL and NASA-GSFC. NR 62 TC 2 Z9 2 U1 0 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD NOV 26 PY 2014 VL 90 IS 5 AR 052723 DI 10.1103/PhysRevA.90.052723 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AY5KN UT WOS:000347611100004 ER PT J AU Barton, HA Giarrizzo, JG Suarez, P Robertson, CE Broering, MJ Banks, ED Vaishampayan, PA Venkateswaran, K AF Barton, Hazel A. Giarrizzo, Juan G. Suarez, Paula Robertson, Charles E. Broering, Mark J. Banks, Eric D. Vaishampayan, Parag A. Venkateswaran, Kasthisuri TI Microbial diversity in a Venezuelan orthoquartzite cave is dominated by the Chloroflexi (Class Ktedonobacterales) and Thaumarchaeota Group I.1c SO FRONTIERS IN MICROBIOLOGY LA English DT Article DE orthoquartzite; cave; Ktedonobacterales; Thaumarchaeota; geomicrobiology ID MOLECULAR PHYLOGENETIC ANALYSIS; ARCHAEAL AMMONIA OXIDIZERS; BACTERIAL COMMUNITY; MOUNT EREBUS; ACID SOILS; SP NOV.; CRENARCHAEOTA; ENVIRONMENTS; ANTARCTICA; OXIDATION AB The majority of caves are formed within limestone rock and hence our understanding of cave microbiology comes from carbonate-buffered systems. In this paper, we describe the microbial diversity of Roraima Sur Cave (RSC), an orthoquartzite (SiO4) cave within Roraima Tepui, Venezuela. The cave contains a high level of microbial activity when compared with other cave systems, as determined by an ATP-based luminescence assay and cell counting. Molecular phylogenetic analysis of microbial diversity within the cave demonstrates the dominance of Actinomycetales and Alphaproteobacteria in endolithic bacterial communities close to the entrance, while communities from deeper in the cave are dominated (82-84%) by a unique clade of Ktedonobacterales within the Chloroflexi. While members of this phylum are commonly found in caves, this is the first identification of members of the Class Ktedonobacterales. An assessment of archaeal species demonstrates the dominance of phylotypes from the Thaumarchaeota Group I.1c (100%), which have previously been associated with acidic environments. While the Thaumarchaeota have been seen in numerous cave systems, the dominance of Group I.1c in RSC is unique and a departure from the traditional archaeal community structure. Geochemical analysis of the cave environment suggests that water entering the cave, rather than the nutrient-limited orthoquartzite rock, provides the carbon and energy necessary for microbial community growth and subsistence, while the poor buffering capacity of quartzite or the low pH of the environment may be selecting for this unusual community structure. Together these data suggest that pH, imparted by the geochemistry of the host rock, can play as important a role in niche-differentiation in caves as in other environmental systems. C1 [Barton, Hazel A.] Univ Akron, Dept Biol, Akron, OH 44325 USA. [Barton, Hazel A.] Univ Akron, Dept Geosci, Akron, OH 44325 USA. [Giarrizzo, Juan G.; Broering, Mark J.; Banks, Eric D.] No Kentucky Univ, Dept Biol Sci, Highland Hts, KY 41076 USA. [Suarez, Paula] Univ Simon Bolivar, Dept Biol Organismos, Caracas, Venezuela. [Robertson, Charles E.] Univ Colorado, Dept Mol Cellular & Dev Biol, Boulder, CO 80309 USA. [Vaishampayan, Parag A.; Venkateswaran, Kasthisuri] CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91125 USA. RP Barton, HA (reprint author), Univ Akron, Dept Biol, 185 East Mill St, Akron, OH 44325 USA. EM bartonh@uakron.edu OI ROBERTSON, CHARLES/0000-0002-4136-4121 FU NSF CAREER award [0643462]; Explorer's Club Grant; Northern Kentucky University; Venezuelan Environmental Ministry at the Vice Ministry of Environmental Management and Administration, Caracas, Venezuela FX The presented research was supported in part by the NSF CAREER award (NSF# 0643462) to Hazel A. Barton, along with an Explorer's Club Grant to Eric D. Banks, and Northern Kentucky University support to both Eric D. Banks and Mark J. Broering, The authors declare no other conflicts of interest. The authors would like to thank Henry Francis for carrying out the elemental analysis and XRD, and Frank Huggins for carrying out the Mossbauer spectroscopy. We would also like to than Akanan Travel and Tours for logistical support within the field and cavers from the Oxford University Caving Club for their useful discussions. This research was supported by sampling permits #I-111 and #3953 provided by The Venezuelan Environmental Ministry at the Vice Ministry of Environmental Management and Administration, Caracas, Venezuela. NR 95 TC 5 Z9 5 U1 6 U2 34 PU FRONTIERS RESEARCH FOUNDATION PI LAUSANNE PA PO BOX 110, LAUSANNE, 1015, SWITZERLAND SN 1664-302X J9 FRONT MICROBIOL JI Front. Microbiol. PD NOV 26 PY 2014 VL 5 AR 615 DI 10.3389/fmicb.2014.00615 PG 14 WC Microbiology SC Microbiology GA AW0OD UT WOS:000345991200001 PM 25505450 ER PT J AU Wiesner, VL Bansal, NP AF Wiesner, Valerie L. Bansal, Narottam P. TI Crystallization kinetics of calcium-magnesium aluminosilicate (CMAS) glass SO SURFACE & COATINGS TECHNOLOGY LA English DT Article DE CMAS; Glass; CMAS-coating interactions; Differential thermal analysis; X-ray diffraction; Activation energy ID THERMAL-BARRIER COATINGS; HIGH-TEMPERATURE ATTACK; STEEL FLY-ASH; CRYSTAL-GROWTH; PHASE-CHANGE; DEGRADATION; DEPOSITS; DELAMINATION; CERAMICS; MICROSTRUCTURE AB The crystallization kinetics of a calcium-magnesium aluminosilicate (CMAS) glass with composition relevant for aerospace applications, like air-breathing engines, were evaluated using differential thermal analysis (DTA) in powder and bulk forms. Activation energy and frequency factor values for crystallization of the glass were evaluated. X-ray diffraction (XRD) was used to investigate the onset of crystallization and the phases that developed after heat treating bulk glass at temperatures ranging from 690 degrees C to 960 degrees C for various times. Samples annealed at temperatures below 900 degrees C remained amorphous, while specimens heat treated at and above 900 degrees C exhibited crystallinity originating at the surface. The crystalline phases were identified as wollastonite (CaSiO3) and aluminum diopside (Ca(Mg,Al)(Si,Al)(2)O-6). Scanning electron microscopy (SEM) and energy dispersive spectroscopy (EDS) were employed to examine the microstructure and chemical compositions of crystalline phases formed after heat treatment Published by Elsevier B.V. C1 [Wiesner, Valerie L.; Bansal, Narottam P.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA. RP Wiesner, VL (reprint author), NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA. EM valerie.l.wiesner@nasa.gov FU Pathways Program at NASA Glenn Research Center FX The authors thank Dr. Bryan Harder and Dr. Dongming Zhu for helpful discussions, Dr. Richard Rogers for XRD assistance, Mr. Dereck Johnson for DTA, Dr. Paul Angel for melting the synthetic sand into glass, Mr. Ray Babuder for assistance with grinding of the bulk glass and Ms. Joy Buehler for glass specimen preparation. A portion of this work was supported by the Pathways Program at NASA Glenn Research Center. NR 32 TC 4 Z9 6 U1 6 U2 26 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0257-8972 J9 SURF COAT TECH JI Surf. Coat. Technol. PD NOV 25 PY 2014 VL 259 BP 608 EP 615 DI 10.1016/j.surfcoat.2014.10.023 PN C PG 8 WC Materials Science, Coatings & Films; Physics, Applied SC Materials Science; Physics GA AY5IF UT WOS:000347605200030 ER PT J AU Chang, RYW Miller, CE Dinardo, SJ Karion, A Sweeney, C Daube, BC Henderson, JM Mountain, ME Eluszkiewicz, J Miller, JB Bruhwiler, LMP Wofsy, SC AF Chang, Rachel Y. -W. Miller, Charles E. Dinardo, Steven J. Karion, Anna Sweeney, Colm Daube, Bruce C. Henderson, John M. Mountain, Marikate E. Eluszkiewicz, Janusz Miller, John B. Bruhwiler, Lori M. P. Wofsy, Steven C. TI Methane emissions from Alaska in 2012 from CARVE airborne observations SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE methane; Alaska; tundra; Arctic; boreal ID PERMAFROST THAW; CARBON BALANCE; CLIMATE-CHANGE; MODEL; TUNDRA; OZONE; FLUXES; VULNERABILITY; TROPOSPHERE; DEPOSITION AB We determined methane (CH4) emissions from Alaska using airborne measurements from the Carbon Arctic Reservoirs Vulnerability Experiment (CARVE). Atmospheric sampling was conducted between May and September 2012 and analyzed using a customized version of the polar weather research and forecast model linked to a Lagrangian particle dispersion model (stochastic time-inverted Lagrangian transport model). We estimated growing season CH4 fluxes of 8 +/- 2 mg CH4.m(-2).d(-1) averaged over all of Alaska, corresponding to fluxes from wetlands of 56(-13)(+22) mg CH4.m(-2).d(-1) if we assumed that wetlands are the only source from the land surface (all uncertainties are 95% confidence intervals from a bootstrapping analysis). Fluxes roughly doubled from May to July, then decreased gradually in August and September. Integrated emissions totaled 2.1 +/- 0.5 Tg CH4 for Alaska from May to September 2012, close to the average (2.3; a range of 0.7 to 6 Tg CH4) predicted by various land surface models and inversion analyses for the growing season. Methane emissions from boreal Alaska were larger than from the North Slope; the monthly regional flux estimates showed no evidence of enhanced emissions during early spring or late fall, although these bursts may be more localized in time and space than can be detected by our analysis. These results provide an important baseline to which future studies can be compared. C1 [Chang, Rachel Y. -W.; Daube, Bruce C.; Wofsy, Steven C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Miller, Charles E.; Dinardo, Steven J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Karion, Anna; Sweeney, Colm; Miller, John B.; Bruhwiler, Lori M. P.] NOAA, Global Monitoring Div, Earth Syst Res Lab, Boulder, CO 80305 USA. [Karion, Anna; Sweeney, Colm; Miller, John B.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Henderson, John M.; Mountain, Marikate E.; Eluszkiewicz, Janusz] Atmospher & Environm Res Inc, Lexington, MA 02421 USA. RP Chang, RYW (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. EM rachel.chang@dal.ca FU National Oceanic and Atmospheric Administration; Natural Sciences and Engineering Research Council of Canada FX We thank the CARVE Science team for helpful discussions; and P. Bergamaschi, X. Zhu, Q. Zhuang, C. Koven, and J. Melton and the Wetland and Wetland CH4 Intercomparison of Models Project team for sharing their model output. We also thank the pilots, flight crews, and NASA Airborne Science staff from the Wallops Flight Facility for enabling the CARVE Science flights. We acknowledge funding from the National Oceanic and Atmospheric Administration and Natural Sciences and Engineering Research Council of Canada (postdoctoral fellowship to R.Y.-W.C.). Computing resources for this work were provided by the NASA High-End Computing Program through the NASA Advanced Supercomputing Division at the Ames Research Center. The research described in this paper was performed as part of CARVE, an Earth Ventures investigation, under contract with NASA. NR 52 TC 11 Z9 12 U1 2 U2 42 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 NOV 25 PY 2014 VL 111 IS 47 BP 16694 EP 16699 DI 10.1073/pnas.1412953111 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AU5QX UT WOS:000345662700026 PM 25385648 ER PT J AU Tassis, K Willacy, K Yorke, HW Turner, NJ AF Tassis, K. Willacy, K. Yorke, Harold W. Turner, Neal J. TI Effect of OH depletion on measurements of the mass-to-flux ratio in molecular cloud cores SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE MHD; ISM: abundances; ISM: clouds; ISM: magnetic fields; ISM: molecules ID STAR-FORMATION; AMBIPOLAR-DIFFUSION; NONEQUILIBRIUM CHEMISTRY; MAGNETIC-FIELD; IONIZATION; CO AB The ratio of mass and magnetic flux determines the relative importance of magnetic and gravitational forces in the evolution of molecular clouds and their cores. Its measurement is thus central in discriminating between different theories of core formation and evolution. Here, we discuss the effect of chemical depletion on measurements of the mass-to-flux ratio using the same molecule (OH) both for Zeeman measurements of the magnetic field and the determination of the mass of the region. The uncertainties entering through the OH abundance in determining separately the magnetic field and the mass of a region have been recognized in the literature. It has been proposed however that, when comparing two regions of the same cloud, the abundance will in both cases be the same. We show that this assumption is invalid. We demonstrate that when comparing regions with different densities, the effect of OH depletion, in measuring changes of the mass-to-flux ratio between different parts of the same cloud can even reverse the direction of the underlying trends (for example, the mass-to-flux ratio may appear to decrease as we move to higher density regions). The systematic errors enter primarily through the inadequate estimation of the mass of the region. C1 [Tassis, K.] Univ Crete, Dept Phys, Iraklion 71003, Greece. [Tassis, K.] Univ Crete, ITCP, Iraklion 71003, Greece. [Tassis, K.] IESL, Fdn Res & Technol Hellas, Iraklion 7110, Greece. [Willacy, K.; Yorke, Harold W.; Turner, Neal J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Tassis, K (reprint author), Univ Crete, Dept Phys, Iraklion 71003, Greece. EM tassis@physics.uoc.gr RI Tassis, Konstantinos/C-3155-2011 FU FP7 through Marie Curie Career Integration Grant [PCIG-GA-2011-293531]; EU [PIRSES-GA-2012-31578]; 'RoboPol' project; European Social Fund (ESF); Greek National Resources; National Aeronautics and Space Administration (NASA) Origins of Solar Systems programme; NASA FX We thank Telemachos Mouschovias and Vasiliki Pavlidou for helpful discussions. KT is acknowledging support by FP7 through Marie Curie Career Integration Grant PCIG-GA-2011-293531 'SFOnset' and the EU FP7 Grant PIRSES-GA-2012-31578 'EuroCal'. This work was partially supported by the 'RoboPol' project, which is implemented under the 'ARISTEIA' Action of the 'OPERATIONAL PROGRAMME EDUCATION AND LIFELONG LEARNING' and is co-funded by the European Social Fund (ESF) and Greek National Resources. The project was supported in part by the National Aeronautics and Space Administration (NASA) Origins of Solar Systems programme. Portions of this research were conducted at the Jet Propulsion Laboratory, California Institute of Technology, which is supported by the NASA. (c) 2014. All rights reserved. NR 17 TC 2 Z9 2 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 21 PY 2014 VL 445 IS 1 BP L56 EP L59 DI 10.1093/mnrasl/slu130 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AS4GH UT WOS:000344231000012 ER PT J AU Hatch, NA Wylezalek, D Kurk, JD Stern, D De Breuck, C Jarvis, MJ Galametz, A Gonzalez, AH Hartley, WG Mortlock, A Seymour, N Stevens, JA AF Hatch, N. A. Wylezalek, D. Kurk, J. D. Stern, D. De Breuck, C. Jarvis, M. J. Galametz, A. Gonzalez, A. H. Hartley, W. G. Mortlock, A. Seymour, N. Stevens, J. A. TI Why z > 1 radio-loud galaxies are commonly located in protoclusters SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: high-redshift ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; INITIAL MASS FUNCTION; LESS-THAN 3.2; SIMILAR-TO 2; CLUSTER ENVIRONMENTS; LUMINOSITY FUNCTION; SKY SURVEY; DEEP SURVEY; QUIESCENT GALAXIES AB Distant powerful radio-loud active galactic nuclei (RLAGN) tend to reside in dense environments and are commonly found in protoclusters at z > 1.3. We examine whether this occurs because RLAGN are hosted by massive galaxies, which preferentially reside in rich environments. We compare the environments of powerful RLAGN at 1.3 < z < 3.2 from the Clusters Around Radio-Loud AGN survey to a sample of radio-quiet galaxies matched in mass and redshift. We find that the environments of RLAGN are significantly denser than those of radio-quiet galaxies, implying that not more than 50 per cent of massive galaxies in this epoch can host powerful radio-loud jets. This is not an observational selection effect as we find no evidence to suggest that it is easier to observe the radio emission when the galaxy resides in a dense environment. We therefore suggest that the dense Mpc-scale environment fosters the formation of a radio jet from an AGN. We show that the number density of potential RLAGN host galaxies is consistent with every >10(14) M-circle dot cluster having experienced powerful radio-loud feedback of duration similar to 60 Myr during 1.3 < z < 3.2. This feedback could heat the intracluster medium to the extent of 0.5-1 keV per gas particle, which could limit the amount of gas available for further star formation in the protocluster galaxies. C1 [Hatch, N. A.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Wylezalek, D.; De Breuck, C.] European So Observ, D-85748 Garching, Germany. [Kurk, J. D.; Galametz, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Jarvis, M. J.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Jarvis, M. J.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. [Galametz, A.] INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Hartley, W. G.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Mortlock, A.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Seymour, N.] CASS, Epping, NSW 1710, Australia. [Seymour, N.] Curtin Univ, Curtin Inst Radio Astron, Perth, WA 6845, Australia. [Stevens, J. A.] Univ Hertfordshire, STRI, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. RP Hatch, NA (reprint author), Univ Nottingham, Sch Phys & Astron, Univ Pk, Nottingham NG7 2RD, England. EM nina.hatch@nottingham.ac.uk OI Hatch, Nina/0000-0001-5600-0534; Seymour, Nicholas/0000-0003-3506-5536; De Breuck, Carlos/0000-0002-6637-3315 FU STFC through an Ernest Rutherford Fellowship; ARC Future Fellowship; South African SKA FX We sincerely thank the referee for providing useful and constructive comments which improved this paper. NAH acknowledges support from STFC through an Ernest Rutherford Fellowship. NS is the recipient of an ARC Future Fellowship. MJJ thanks the South African SKA for support. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology. NR 78 TC 23 Z9 24 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 21 PY 2014 VL 445 IS 1 BP 280 EP 289 DI 10.1093/mnras/stu1725 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR8LX UT WOS:000343827700021 ER PT J AU Gralla, MB Crichton, D Marriage, TA Mo, WL Aguirre, P Addison, GE Asboth, V Battaglia, N Bock, J Bond, JR Devlin, MJ Dunner, R Hajian, A Halpern, M Hilton, M Hincks, AD Hlozek, RA Huffenberger, KM Hughes, JP Ivison, RJ Kosowsky, A Lin, YT Marsden, D Menanteau, F Moodley, K Morales, G Niemack, MD Oliver, S Page, LA Partridge, B Reese, ED Rojas, F Sehgal, N Sievers, J Sifon, C Spergel, DN Staggs, ST Switzer, ER Viero, MP Wollack, EJ Zemcov, MB AF Gralla, Megan B. Crichton, Devin Marriage, Tobias A. Mo, Wenli Aguirre, Paula Addison, Graeme E. Asboth, V. Battaglia, Nick Bock, James Bond, J. Richard Devlin, Mark J. Duenner, Rolando Hajian, Amir Halpern, Mark Hilton, Matt Hincks, Adam D. Hlozek, Renee A. Huffenberger, Kevin M. Hughes, John P. Ivison, R. J. Kosowsky, Arthur Lin, Yen-Ting Marsden, Danica Menanteau, Felipe Moodley, Kavilan Morales, Gustavo Niemack, Michael D. Oliver, Seb Page, Lyman A. Partridge, Bruce Reese, Erik D. Rojas, Felipe Sehgal, Neelima Sievers, Jon Sifon, Cristobal Spergel, David N. Staggs, Suzanne T. Switzer, Eric R. Viero, Marco P. Wollack, Edward J. Zemcov, Michael B. TI A measurement of the millimetre emission and the Sunyaev-Zel'dovich effect associated with low-frequency radio sources SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: haloes; galaxies: statistics; radio continuum: galaxies ID ACTIVE GALACTIC NUCLEI; GALAXY REDSHIFT SURVEY; STAR-FORMING GALAXIES; STELLAR MASS FUNCTIONS; ANISOTROPY-PROBE DATA; LUMINOSITY FUNCTION; SOURCE CATALOG; NUMBER COUNTS; 1ST SURVEY; 1.4 GHZ AB We present a statistical analysis of the millimetre-wavelength properties of 1.4 GHz-selected sources and a detection of the Sunyaev-Zel'dovich (SZ) effect associated with the haloes that host them. We stack data at 148, 218 and 277 GHz from the Atacama Cosmology Telescope at the positions of a large sample of radio AGN selected at 1.4 GHz. The thermal SZ effect associated with the haloes that host the AGN is detected at the 5 sigma level through its spectral signature, representing a statistical detection of the SZ effect in some of the lowest mass haloes (average M-200 approximate to 10(13) M-circle dot h(70)(-1)) studied to date. The relation between the SZ effect and mass (based on weak lensing measurements of radio galaxies) is consistent with that measured by Planck for local bright galaxies. In the context of galaxy evolution models, this study confirms that galaxies with radio AGN also typically support hot gaseous haloes. Adding Herschel observations allows us to show that the SZ signal is not significantly contaminated by dust emission. Finally, we analyse the contribution of radio sources to the angular power spectrum of the cosmic microwave background. C1 [Gralla, Megan B.; Crichton, Devin; Marriage, Tobias A.; Mo, Wenli] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Mo, Wenli] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Aguirre, Paula; Duenner, Rolando; Morales, Gustavo; Rojas, Felipe] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Addison, Graeme E.; Asboth, V.; Halpern, Mark; Hincks, Adam D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Battaglia, Nick] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Bock, James; Viero, Marco P.; Zemcov, Michael B.] CALTECH, Pasadena, CA 91125 USA. [Bock, James; Zemcov, Michael B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bond, J. Richard; Hajian, Amir; Switzer, Eric R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Devlin, Mark J.; Reese, Erik D.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Hilton, Matt; Moodley, Kavilan; Sievers, Jon] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Hilton, Matt] Univ Nottingham, Sch Phys & Astron, Ctr Astron & Particle Theory, Nottingham NG7 2RD, England. [Hlozek, Renee A.; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Huffenberger, Kevin M.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Ivison, R. J.] Univ Edinburgh, Sci & Technol Facil Council, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Lin, Yen-Ting] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Marsden, Danica] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Menanteau, Felipe] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA. [Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Oliver, Seb] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Page, Lyman A.; Sievers, Jon; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. [Reese, Erik D.] Moorpark Coll, Dept Phys Astron & Engn, Moorpark, CA 93021 USA. [Sehgal, Neelima] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Sifon, Cristobal] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Switzer, Eric R.; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gralla, MB (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. EM mgralla@pha.jhu.edu RI Wollack, Edward/D-4467-2012; Ivison, R./G-4450-2011; OI Wollack, Edward/0000-0002-7567-4451; Ivison, R./0000-0001-5118-1313; Sievers, Jonathan/0000-0001-6903-5074; Huffenberger, Kevin/0000-0001-7109-0099; Menanteau, Felipe/0000-0002-1372-2534; Sifon, Cristobal/0000-0002-8149-1352 FU US National Science Foundation [AST-0408698, AST-0965625, PHY-0855887, PHY-1214379]; Princeton University; University of Pennsylvania; Canada Foundation for Innovation (CFI) award; Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT); CFI under Compute Canada; Government of Ontario; Ontario Research Fund - Research Excellence; University of Toronto; Johns Hopkins University; CATA [FONDECYT 11100147, BASAL] FX This work was supported by the US National Science Foundation through awards AST-0408698 and AST-0965625 for the ACT project, as well as awards PHY-0855887 and PHY-1214379. Funding was also provided by Princeton University, the University of Pennsylvania, and a Canada Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque Astronomic Atacama in northern Chile under the auspices of the Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT). Computations were performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by the CFI under the auspices of Compute Canada, the Government of Ontario, the Ontario Research Fund - Research Excellence; and the University of Toronto. MBG and TAM acknowledge support from Johns Hopkins University. RD, PA, FR and GM received funding from the Chilean grants FONDECYT 11100147 and BASAL (CATA). This research made use of ASTROPY, a community-developed core PYTHON package for Astronomy (Astropy Collaboration 2013). NR 134 TC 15 Z9 15 U1 0 U2 8 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 21 PY 2014 VL 445 IS 1 BP 460 EP 478 DI 10.1093/mnras/stu1592 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR8LX UT WOS:000343827700036 ER PT J AU Koss, M Blecha, L Mushotzky, R Hung, CL Veilleux, S Trakhtenbrot, B Schawinski, K Stern, D Smith, N Li, YX Man, A Filippenko, AV Mauerhan, JC Stanek, K Sanders, D AF Koss, Michael Blecha, Laura Mushotzky, Richard Hung, Chao Ling Veilleux, Sylvain Trakhtenbrot, Benny Schawinski, Kevin Stern, Daniel Smith, Nathan Li, Yanxia Man, Allison Filippenko, Alexei V. Mauerhan, Jon C. Stanek, Kris Sanders, David TI SDSS1133: an unusually persistent transient in a nearby dwarf galaxy SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general; galaxies: active; galaxies: dwarf ID SUPERMASSIVE BLACK-HOLE; GRAVITATIONAL-WAVE RECOIL; DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEUS; STAR-FORMING GALAXIES; X-RAY SOURCE; TIDAL DISRUPTION; DUST FORMATION; IIN SUPERNOVA; CIRCUMSTELLAR INTERACTION AB While performing a survey to detect recoiling supermassive black holes, we have identified an unusual source having a projected offset of 800 pc from a nearby dwarf galaxy. The object, SDSS J113323.97+550415.8, exhibits broad emission lines and strong variability. While originally classified as a supernova (SN) because of its non-detection in 2005, we detect it in recent and past observations over 63 yr and find over a magnitude of rebrightening in the last 2 yr. Using high-resolution adaptive optics observations, we constrain the source emission region to be less than or similar to 12 pc and find a disturbed host-galaxy morphology indicative of recent merger activity. Observations taken over more than a decade show narrow [O III] lines, constant ultraviolet emission, broad Balmer lines, a constant putative black hole mass over a decade of observations despite changes in the continuum, and optical emission-line diagnostics consistent with an active galactic nucleus (AGN). However, the optical spectra exhibit blueshifted absorption, and eventually narrow Fe II and [Ca II] emission, each of which is rarely found in AGN spectra. While this peculiar source displays many of the observational properties expected of a potential black hole recoil candidate, some of the properties could also be explained by a luminous blue variable star (LBV) erupting for decades since 1950, followed by a Type IIn SN in 2001. Interpreted as an LBV followed by an SN analogous to SN 2009ip, the multidecade LBV eruptions would be the longest ever observed, and the broad Ha emission would be the most luminous ever observed at late times (> 10 yr), larger than that of unusually luminous SNe such as SN 1988Z, suggesting one of the most extreme episodes of pre-SN mass-loss ever discovered. C1 [Koss, Michael; Trakhtenbrot, Benny; Schawinski, Kevin] Swiss Fed Inst Technol, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. [Koss, Michael; Hung, Chao Ling; Li, Yanxia; Sanders, David] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Blecha, Laura; Mushotzky, Richard; Veilleux, Sylvain] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Smith, Nathan; Mauerhan, Jon C.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Man, Allison] Univ Copenhagen, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Stanek, Kris] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. RP Koss, M (reprint author), Swiss Fed Inst Technol, Inst Astron, Dept Phys, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. EM mkoss@phys.ethz.ch RI Koss, Michael/B-1585-2015; OI Koss, Michael/0000-0002-7998-9581; Schawinski, Kevin/0000-0001-5464-0888 FU Swiss National Science Foundation (SNSF) [PP00P2 138979/1]; SNSF through the Ambizione fellowship; National Aeronautics and Space Administration (NASA) issued by the Chandra X-ray Observatory Center [AR3-14010X]; NASA [NAS8-03060, PF2-130093]; Gary and Cynthia Bengier; Christopher R. Redlich Fund; Richard and Rhoda Goldman Fund; TABASGO Foundation; NSF [AST-1211916, AST-1238877]; W. M. Keck Foundation; Alfred P. Sloan Foundation; NSF; U.S. Department of Energy; NASA; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; Max Planck Institute for Astronomy (Heidelberg); Max Planck Institute for Extraterrestrial Physics (Garching); Johns Hopkins University; Durham University; University of Edinburgh; Queen's University Belfast; Harvard-Smithsonian Center for Astrophysics; Las Cumbres Observatory Global Telescope Network Incorporated; National Central University of Taiwan; Space Telescope Science Institute; NASA issued through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; University of Maryland; Eotvos Lorand University (ELTE) FX We are grateful to Jessica Lu and Aaron Barth for useful discussion and suggestions. We thank Neil Gehrels and the Swift team for approving and executing a ToO observation. MK and KS acknowledge support from Swiss National Science Foundation (SNSF) grant PP00P2 138979/1. MK acknowledges support from the SNSF through the Ambizione fellowship. MK also acknowledges support for this work provided by the National Aeronautics and Space Administration (NASA) through Chandra Award Number AR3-14010X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. Support for LB was provided by NASA through the Einstein Fellowship Program, grant PF2-130093. AVF received generous financial assistance from Gary and Cynthia Bengier, the Christopher R. Redlich Fund, the Richard and Rhoda Goldman Fund, the TABASGO Foundation, and NSF grant AST-1211916. The work of DS was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA.; Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Data reported here were obtained in part at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the NSF, the U.S. Department of Energy, NASA, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS website is http://www.sdss.orgt. The PS1 data have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS1 Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy (Heidelberg) and the Max Planck Institute for Extraterrestrial Physics (Garching), The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, NASA under grant NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the NSF under grant AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE). NR 86 TC 9 Z9 9 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 21 PY 2014 VL 445 IS 1 BP 515 EP 527 DI 10.1093/mnras/stu1673 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR8LX UT WOS:000343827700039 ER PT J AU Zemko, P Orio, M Mukai, K Shugarov, S AF Zemko, P. Orio, M. Mukai, K. Shugarov, S. TI X-ray observations of VY Scl-type nova-like binaries in the high and low state SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; novae, cataclysmic variables; X-rays: binaries ID VARIABLE MV-LYRAE; OPTICAL LOW-STATE; CATACLYSMIC VARIABLES; TT-ARIETIS; DWARF NOVA; BZ-CAMELOPARDALIS; SCULPTORIS STARS; WHITE-DWARFS; FAR-ULTRAVIOLET; BOUNDARY-LAYER AB Four VY Scl-type nova-like systems were observed in X-rays during both the low-and the high-optical states. We examined Chandra, ROSAT, Swift and Suzaku archival observations of BZ Cam, MV Lyr, TT Ari and V794 Aql. The X-ray flux of BZ Cam is higher during the low state, but there is no supersoft X-ray source (SSS) as hypothesized in previous articles. No SSS was detected in the low state of the any of the other systems, with the X-ray flux decreasing by a factor between 2 and 50. The best fit to the Swift X-ray spectra is obtained with a multicomponent model of plasma in collisional ionization equilibrium. The high-state high-resolution spectra of TT Ari taken with Chandra Advanced CCD Imaging Spectrometer (ACIS-S) and the Chandra High Energy Transmission Grating (HETG) shows a rich emission line spectrum, with prominent lines of Mg, Si, Ne and S. The complexity of this spectrum seems to have origin in more than one region, or more than one single physical mechanism. While several emission lines are consistent with a cooling flow in an accretion stream, there is at least an additional component. We discuss the origin of this component, which is probably arising in a wind from the system. We also examine the possibility that the VY Scl systems may be intermediate polars, and that while the boundary layer of the accretion disc emits only in the extreme ultraviolet, part of the X-ray flux may be due to magnetically driven accretion. C1 [Zemko, P.] Univ Padua, Dept Phys & Astron, I-35122 Padua, Italy. [Orio, M.] Osservatorio Padova, INAF, I-35122 Padua, Italy. [Orio, M.] Univ Wisconsin, Dept Astron, Madison, WI 53704 USA. [Mukai, K.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Mukai, K.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Mukai, K.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Shugarov, S.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. [Shugarov, S.] Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960, Slovakia. RP Zemko, P (reprint author), Univ Padua, Dept Phys & Astron, Vicolo Osservatorio 3, I-35122 Padua, Italy. EM polina.zemko@studenti.unipd.it RI XRAY, SUZAKU/A-1808-2009 FU National Scholarship Programme SAIA; CARIPARO foundation at the University of Padova; VEGA [2/0002/13] FX Polina Zemko acknowledges the grant of the National Scholarship Programme SAIA and a pre-doctoral grant of the CARIPARO foundation at the University of Padova. Dr Shugarov acknowledges the VEGA grant no. 2/0002/13. We acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this research. NR 73 TC 1 Z9 1 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 21 PY 2014 VL 445 IS 1 BP 869 EP 880 DI 10.1093/mnras/stu1783 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR8LX UT WOS:000343827700064 ER PT J AU Xiong, XX Angal, A Sun, JQ Choi, TY Johnson, E AF Xiong, Xiaoxiong Angal, Amit Sun, Junqiang Choi, Taeyoung Johnson, Eric TI On-orbit performance of MODIS solar diffuser stability monitor SO JOURNAL OF APPLIED REMOTE SENSING LA English DT Article DE optics MODIS; Visible Infrared Imaging Radiometer Suite; radiometer; calibration; solar diffuser; solar diffuser stability monitor; solar diffuser degradation ID TERRA MODIS; BANDS; CALIBRATION AB Moderate Resolution Imaging Spectroradiometer (MODIS) is currently operated on both the Terra and Aqua spacecraft. It collects data in 20 reflective solar bands (RSB) and 16 thermal emissive bands. MODIS RSB calibration is reflectance based via an on-board solar diffuser (SD). On-orbit changes in the SD bidirectional reflectance factor are tracked by an on-board solar diffuser stability monitor (SDSM). The SDSM functions as an independent ratioing radiometer with nine filtered detectors, covering wavelengths in the visible (VIS) and near-infrared (NIR) spectral regions. A brief overview of SDSM design functions, on-orbit operations, and performance for both Terra and Aqua MODIS is provided. In addition to the SD on-orbit degradation at different wavelengths, the changes in SDSM detector responses and their potential impact on tracking SD on-orbit degradation are examined. After more than 12 years of on-orbit operation, Aqua MODIS SD has shown degradation varying from 0.6% at 0.94 mu m to 19.0% at 0.41 mu m. Due to more frequent solar exposure and longer operation time, the Terra MODIS SD has experienced a much larger degradation, varying from 2.3% at 0.94 mu m to 48.0% at 0.41 mu m. For both Terra and Aqua MODIS, the SD has experienced more degradation at shorter wavelengths. Meanwhile, the SDSM detector responses have also experienced wavelength-dependent degradation. The largest change in the SDSM detector responses, however, occurred at longer NIR wavelengths. Since launch, the SDSM systems on both Terra and Aqua MODIS have continued their nominal operations, enabling critical parameters to be derived in support of the RSB on-orbit calibration. The calibration strategies developed for and lessons learned from MODIS SDSM operations, and a preliminary performance comparison with the S-NPP VIIRS SDSM are discussed. (C) 2014 Society of Photo-Optical Instrumentation Engineers (SPIE) C1 [Xiong, Xiaoxiong] NASA, GSFC, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. [Angal, Amit] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Sun, Junqiang; Choi, Taeyoung] Sigma Space Co, Lanham, MD 20706 USA. [Johnson, Eric] Raytheon Space & Airborne Syst, El Segundo, CA 90245 USA. RP Angal, A (reprint author), Sci Syst & Applicat Inc, 10210 Greenbelt Rd, Lanham, MD 20706 USA. EM amit.angal@ssaihq.com RI Choi, Taeyoung/E-4437-2016 OI Choi, Taeyoung/0000-0002-4596-989X NR 23 TC 5 Z9 8 U1 2 U2 9 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1931-3195 J9 J APPL REMOTE SENS JI J. Appl. Remote Sens. PD NOV 20 PY 2014 VL 8 AR 083514 DI 10.1117/1.JRS.8.083514 PG 14 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA CA1LQ UT WOS:000348674500001 ER PT J AU Zeng, N Zhao, F Collatz, GJ Kalnay, E Salawitch, RJ West, TO Guanter, L AF Zeng, Ning Zhao, Fang Collatz, George J. Kalnay, Eugenia Salawitch, Ross J. West, Tristram O. Guanter, Luis TI Agricultural Green Revolution as a driver of increasing atmospheric CO2 seasonal amplitude SO NATURE LA English DT Article ID NET PRIMARY PRODUCTION; CARBON-DIOXIDE; MAUNA-LOA; CHLOROPHYLL FLUORESCENCE; HUMAN APPROPRIATION; VEGETATION; BALANCE; MODELS; CYCLE; PHOTOSYNTHESIS AB The atmospheric carbon dioxide (CO2) record displays a prominent seasonal cycle that arises mainly from changes in vegetation growth and the corresponding CO2 uptake during the boreal spring and summer growing seasons and CO2 release during the autumn and winter seasons(1). The CO2 seasonal amplitude has increased over the past five decades, suggesting an increase in Northern Hemisphere biospheric activity(2,5,6). It has been proposed that vegetation growth may have been stimulated by higher concentrations of CO2 as well as by warming in recent decades, but such mechanisms have been unable to explain the full range and magnitude of the observed increase in CO2 seasonal amplitude(2,6-13). Here we suggest that the intensification of agriculture (the Green Revolution, in which much greater crop yield per unit area was achieved by hybridization, irrigation and fertilization) during the past five decades is a driver of changes in the seasonal characteristics of the global carbon cycle. Our analysis of CO2 data and atmospheric inversions shows a robust 15 per cent long-term increase in CO2 seasonal amplitude from 1961 to 2010, punctuated by large decadal and interannual variations. Using a terrestrial carbon cycle model that takes into account high-yield cultivars, fertilizer use and irrigation, we find that the long-term increase in CO2 seasonal amplitude arises from two major regions: the midlatitude cropland between 25 degrees N and 60 degrees N and the high-latitude natural vegetation between 50 degrees N and 70 degrees N. The long-term trend of seasonal amplitude increase is 0.311 +/- 0.027 per cent per year, of which sensitivity experiments attribute 45,29 and 26 per cent to land-use change, climate variability and change, and increased productivity due to CO2 fertilization, respectively. Vegetation growth was earlier by one to two weeks, as measured by the mid-point of vegetation carbon uptake, and took up 0.5 petagrams more carbon in July, the height of the growing season, during 2001-2010 than in 1961-1970, suggesting that human land use and management contribute to seasonal changes in the CO2 exchange between the biosphere and the atmosphere. C1 [Zeng, Ning; Zhao, Fang; Kalnay, Eugenia; Salawitch, Ross J.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Zeng, Ning; Zhao, Fang; Kalnay, Eugenia; Salawitch, Ross J.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Collatz, George J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [West, Tristram O.] Pacific NW Natl Lab, Joint Global Change Res Inst, College Pk, MD 20740 USA. [Guanter, Luis] Free Univ Berlin, Inst Space Sci, D-12165 Berlin, Germany. RP Zeng, N (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. EM zeng@atmos.umd.edu RI Salawitch, Ross/B-4605-2009; collatz, george/D-5381-2012; Zeng, Ning/A-3130-2008; Guanter, Luis/I-1588-2015; OI Salawitch, Ross/0000-0001-8597-5832; Zeng, Ning/0000-0002-7489-7629; Guanter, Luis/0000-0002-8389-5764; Kalnay, Eugenia/0000-0002-9984-9906 FU NOM [NA100AR4310248, NAO9NE54400006]; NSF [AGS-1129088]; NASA [NNH12AU351] FX We thank all data providers, especially the NOAA CO2 and Carbon Tracker team, and the Jena inversion team. M. Heimann suggested the flux data site comparison. This research was supported by NOM (NA100AR4310248 and NAO9NE54400006), the NSF (AGS-1129088), and NASA (NNH12AU351). NR 33 TC 29 Z9 30 U1 16 U2 109 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD NOV 20 PY 2014 VL 515 IS 7527 BP 394 EP + DI 10.1038/nature13893 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AU7HE UT WOS:000345770600041 PM 25409829 ER PT J AU Taylor, S Ellis, J Gair, J AF Taylor, Stephen Ellis, Justin Gair, Jonathan TI Accelerated Bayesian model-selection and parameter-estimation in continuous gravitational-wave searches with pulsar-timing arrays SO PHYSICAL REVIEW D LA English DT Article ID BLACK-HOLE BINARIES; COALESCENCE RATE; RADIATION; GALAXIES; SYSTEMS; LISA; BAND AB We describe several new techniques which accelerate Bayesian searches for continuous gravitational-wave emission from supermassive black-hole binaries using pulsar-timing arrays. These techniques mitigate the problematic increase of search dimensionality with the size of the pulsar array which arises from having to include an extra parameter per pulsar as the array is expanded. This extra parameter corresponds to searching over the phase of the gravitational wave as it propagates past each pulsar so that we can coherently include the pulsar term in our search strategies. Our techniques make the analysis tractable with powerful evidence-evaluation packages like MULTINEST. We find good agreement of our techniques with the parameter-estimation and Bayes factor evaluation performed with full signal templates and conclude that these techniques make excellent first-cut tools for detection and characterization of continuous gravitational-wave signals with pulsar-timing arrays. Crucially, at low to moderate signal-to-noise ratios the factor by which the analysis is sped up can be greater than or similar to 100, permitting rigorous programs of systematic injection and recovery of signals to establish robust detection criteria within a Bayesian formalism. C1 [Taylor, Stephen; Ellis, Justin] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Taylor, Stephen; Gair, Jonathan] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Ellis, Justin] Univ Wisconsin, Ctr Gravitat & Cosmol, Dept Phys, Milwaukee, WI 53201 USA. RP Taylor, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Stephen.R.Taylor@jpl.nasa.gov OI Taylor, Stephen/0000-0003-0264-1453 FU STFC; RAS; NASA; NASA through Einstein Fellowship [PF4-150120]; NSF CAREER Grant [0955929]; Wisconsin Space Grant Consortium; Royal Society; Higher Education Funding Council for England; NSF [0923409] FX S. T. acknowledges the support of the STFC and the RAS. This research was in part 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. J. E. is an Einstein fellow. J. E. acknowledges support by NASA through Einstein Fellowship Grant No. PF4-150120, and was partially funded through NSF CAREER Grant No. 0955929 and through the Wisconsin Space Grant Consortium. J. G. is supported by the Royal Society. 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 Higher Education Funding Council for England. Part of the computational work was performed on the Nemo cluster at UWM supported by NSF Grant No. 0923409. NR 59 TC 10 Z9 10 U1 2 U2 8 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD NOV 20 PY 2014 VL 90 IS 10 AR 104028 DI 10.1103/PhysRevD.90.104028 PG 16 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AU3SY UT WOS:000345535100001 ER PT J AU Lynch, HJ Schwaller, MR AF Lynch, Heather J. Schwaller, Mathew R. TI Mapping the Abundance and Distribution of Adelie Penguins Using Landsat-7: First Steps towards an Integrated Multi-Sensor Pipeline for Tracking Populations at the Continental Scale SO PLOS ONE LA English DT Article ID IMAGERY AB The last several years have seen an increased interest in the use of remote sensing to identify the location of penguin colonies in Antarctica, and the estimation of the abundance of breeding pairs contained therein. High-resolution (submeter) commercial satellite imagery (e.g., Worldview-1, Quickbird) is capable of colony detection and abundance estimation for both large and small colonies, and has already been used in a continental-scale survey of Adelie penguins. Medium-resolution Landsat imagery has been used successfully to detect the presence of breeding penguins, but has not been used previously for abundance estimation nor evaluated in terms of its minimum colony size detection threshold. We report on the first comprehensive analysis of the performance of these two methods for both detection and abundance estimation, identify the sensor-specific failure modes that can lead to both false positives and false negatives, and compare the abundance estimates of each method over multiple spatial scales. We find that errors of omission using Landsat imagery are low for colonies larger than similar to 10,000 breeding pairs. Both high-resolution and Landsat imagery can be used to obtain unbiased estimates of abundance, and while Landsat-derived abundance estimates have high variance for individual breeding colonies relative to estimates derived from high-resolution imagery, this difference declines as the spatial domain of interest is increased. At the continental scale, abundance estimates using the two methods are roughly equivalent. Our comparison of these two methods represents a bridge between the more developed high-resolution imagery, which can be expensive to obtain, and the medium-resolution Landsat-7 record, which is freely available; this comparison of methodologies represents an essential step towards integration of these disparate sources of data for regional assessments of Adelie population abundance and distribution. C1 [Lynch, Heather J.] SUNY Stony Brook, Dept Ecol & Evolut, Stony Brook, NY 11794 USA. [Schwaller, Mathew R.] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Lab, Greenbelt, MD 20771 USA. RP Lynch, HJ (reprint author), SUNY Stony Brook, Dept Ecol & Evolut, Stony Brook, NY 11794 USA. EM heather.lynch@stonybrook.edu FU National Science Foundation/Office of Polar Programs [1255058]; National Air and Space Administration [NNX14AC32G] FX HJL was supported by National Science Foundation/Office of Polar Programs - Award No. 1255058; http://www.nsf.gov. HJL and MRS were supported by the National Air and Space Administration - Award No. NNX14AC32G; http://www.nasa.gov. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 11 TC 3 Z9 3 U1 2 U2 18 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 NOV 20 PY 2014 VL 9 IS 11 AR e113301 DI 10.1371/journal.pone.0113301 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AT9ND UT WOS:000345253000036 PM 25412466 ER PT J AU Dudik, J Dzifcakova, E Cirtain, JW AF Dudik, Jaroslav Dzifcakova, Elena Cirtain, Jonathan W. TI ON THE AREA EXPANSION OF MAGNETIC FLUX TUBES IN SOLAR ACTIVE REGIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: magnetic fields; Sun: UV radiation; Sun: X-rays, gamma rays ID IMAGING SPECTROMETER OBSERVATIONS; STOKES PROFILE ANALYSIS; DYNAMICS-OBSERVATORY SDO; SOFT-X-RAY; CORONAL LOOPS; FORCE-FREE; TRANSITION-REGION; OPTICAL TELESCOPE; DOPPLER SHIFTS; TEMPERATURE STRUCTURE AB We calculated the three-dimensional (3D) distribution of the area expansion factors in a potential magnetic field, extrapolated from the high-resolution Hinode/SOT magnetogram of the quiescent active region NOAA 11482. Retaining only closed loops within the computational box, we show that the distribution of area expansion factors show significant structure. Loop-like structures characterized by locally lower values of the expansion factor are embedded in a smooth background. These loop-like flux tubes have squashed cross-sections and expand with height. The distribution of the expansion factors show an overall increase with height, allowing an active region core characterized by low values of the expansion factor to be distinguished. The area expansion factors obtained from extrapolation of the Solar Optical Telescope magnetogram are compared to those obtained from an approximation of the observed magnetogram by a series of 134 submerged charges. This approximation retains the general flux distribution in the observed magnetogram, but removes the small-scale structure in both the approximated magnetogram and the 3D distribution of the area expansion factors. We argue that the structuring of the expansion factor can be a significant ingredient in producing the observed structuring of the solar corona. However, due to the potential approximation used, these results may not be applicable to loops exhibiting twist or to active regions producing significant flares. C1 [Dudik, Jaroslav] Univ Cambridge, CMS, DAMTP, Cambridge CB3 0WA, England. [Dzifcakova, Elena] Acad Sci Czech Republic, Inst Astron, CS-25165 Ondrejov, Czech Republic. [Cirtain, Jonathan W.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Dudik, Jaroslav] Comenius Univ, Fac Math Phys & Comp Sci, DAPEM, Bratislava 84248, Slovakia. RP Dudik, J (reprint author), Univ Cambridge, CMS, DAMTP, Wilberforce Rd, Cambridge CB3 0WA, England. EM J.Dudik@damtp.cam.ac.uk; elena@asu.cas.cz RI Dudik, Jaroslav/D-5876-2013 FU Newton Fellowship Programme (Royal Society); Grant Agency of the Czech Republic [P209/12/1652]; LWS TRT Program of the Heliophysics Division of NASA's SMD; International Space Science Institute (ISSI) in Bern via its International Teams programme FX The authors thank G. Del Zanna and H. E. Mason for useful discussions. AIA and HMI data are courtesy of NASA/SDO and the respective science teams. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as a domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and NSC (Norway). The AIA and HMI data are courtesy of NASA/SDO and the AIA and HMI teams. J.D. acknowledges support from the Newton Fellowship Programme (Royal Society). E.D.Z. acknowledges the support by Grant Agency of the Czech Republic, grant no. P209/12/1652. J.W.C. is supported by funding from the LWS TRT Program of the Heliophysics Division of NASA's SMD. The authors acknowledge support from the International Space Science Institute (ISSI) in Bern via its International Teams programme. NR 122 TC 1 Z9 1 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2014 VL 796 IS 1 AR 20 DI 10.1088/0004-637X/796/1/20 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AS9GD UT WOS:000344550300020 ER PT J AU Fumagalli, M Labbe, I Patel, SG Franx, M van Dokkum, P Brammer, G da Cunha, E Schreiber, NMF Kriek, M Quadri, R Rix, HW Wake, D Whitaker, KE Lundgren, B Marchesini, D Maseda, M Momcheva, I Nelson, E Pacifici, C Skelton, RE AF Fumagalli, Mattia Labbe, Ivo Patel, Shannon G. Franx, Marijn van Dokkum, Pieter Brammer, Gabriel da Cunha, Elisabete Schreiber, Natascha M. Foerster Kriek, Mariska Quadri, Ryan Rix, Hans-Walter Wake, David Whitaker, Katherine E. Lundgren, Britt Marchesini, Danilo Maseda, Michael Momcheva, Ivelina Nelson, Erica Pacifici, Camilla Skelton, Rosalind E. TI HOW DEAD ARE DEAD GALAXIES? MID-INFRARED FLUXES OF QUIESCENT GALAXIES AT REDSHIFT 0.3 < z < 2.5: IMPLICATIONS FOR STAR FORMATION RATES AND DUST HEATING SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation ID SIMILAR-TO 2; DEEP-FIELD-SOUTH; SPECTRAL ENERGY-DISTRIBUTIONS; OLD STELLAR POPULATIONS; HUBBLE-SPACE-TELESCOPE; FORMING GALAXIES; MASSIVE GALAXIES; FORMATION HISTORIES; INFRARED PROPERTIES; INTERMEDIATE-AGE AB We investigate star formation rates (SFRs) of quiescent galaxies at high redshift (0.3 < z < 2.5) using 3D-HST WFC3 grism spectroscopy and Spitzer mid-infrared data. We select quiescent galaxies on the basis of the widely used UVJ color-color criteria. Spectral energy distribution (SED) fitting (rest-frame optical and near-IR) indicates very low SFRs for quiescent galaxies (sSFR similar to 10(-12) yr(-1)). However, SED fitting can miss star formation if it is hidden behind high dust obscuration and ionizing radiation is re-emitted in the mid-infrared. It is therefore fundamental to measure the dust-obscured SFRs with a mid-IR indicator. We stack the MIPS 24 mu m images of quiescent objects in five redshift bins centered on z = 0.5, 0.9, 1.2, 1.7, 2.2 and perform aperture photometry. Including direct 24 mu m detections, we find sSFR similar to 10(-11.9) x (1 + z)(4) yr(-1). These values are higher than those indicated by SED fitting, but at each redshift they are 20-40 times lower than those of typical star-forming galaxies. The true SFRs of quiescent galaxies might be even lower, as we show that the mid-IR fluxes can be due to processes unrelated to ongoing star formation, such as cirrus dust heated by old stellar populations and circumstellar dust. Our measurements show that star formation quenching is very efficient at every redshift. The measured SFR values are at z > 1.5 marginally consistent with the ones expected from gas recycling (assuming that mass loss from evolved stars refuels star formation) and well below that at lower redshifts. C1 [Fumagalli, Mattia; Labbe, Ivo; Patel, Shannon G.; Franx, Marijn] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dokkum, Pieter; Momcheva, Ivelina; Nelson, Erica] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Brammer, Gabriel] European So Observ, Santiago, Chile. [da Cunha, Elisabete; Rix, Hans-Walter; Maseda, Michael] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Schreiber, Natascha M. Foerster] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Kriek, Mariska] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Quadri, Ryan] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Wake, David; Lundgren, Britt] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Wake, David] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Whitaker, Katherine E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Marchesini, Danilo] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. [Pacifici, Camilla] Yonsei Univ, Yonsei Univ Observ, Seoul 120749, South Korea. [Skelton, Rosalind E.] S African Astron Observ, ZA-7935 Cape Town, South Africa. RP Fumagalli, M (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. RI Skelton, Rosalind/S-1845-2016; OI Skelton, Rosalind/0000-0001-7393-3336; Brammer, Gabriel/0000-0003-2680-005X FU ERC grant HIGHZ [227749]; NASA [NAS5-26555] FX We acknowledge funding from ERC grant HIGHZ No. 227749. This work is based on observations taken by the 3D-HST Treasury Program (GO 12177 and 12328) with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. NR 71 TC 22 Z9 22 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2014 VL 796 IS 1 AR UNSP 35 DI 10.1088/0004-637X/796/1/35 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AS9GD UT WOS:000344550300035 ER PT J AU Janches, D Plane, JMC Nesvorny, D Feng, W Vokrouhlicky, D Nicolls, MJ AF Janches, D. Plane, J. M. C. Nesvorny, D. Feng, W. Vokrouhlicky, D. Nicolls, M. J. TI RADAR DETECTABILITY STUDIES OF SLOW AND SMALL ZODIACAL DUST CLOUD PARTICLES. I. THE CASE OF ARECIBO 430 MHz METEOR HEAD ECHO OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE atmospheric effects; meteorites, meteors, meteoroids; methods: observational; zodiacal dust ID VELOCITY DISTRIBUTION; RADIANT DISTRIBUTION; SPORADIC METEORS; HIGH-RESOLUTION; COSMIC DUST; MU RADAR; MASS; MICROMETEORS; IONIZATION; MODEL AB Recent model development of the Zodiacal Dust Cloud (ZDC) argues that the incoming flux of meteoric material into the Earth's upper atmosphere is mostly undetected by radars because they cannot detect small extraterrestrial particles entering the atmosphere at low velocities due to the relatively small production of electrons. In this paper, we present a new methodology utilizing meteor head echo radar observations that aims to constrain the ZDC physical model by ground-based measurements. In particular, for this work, we focus on Arecibo 430 MHz observations since this is the most sensitive radar utilized for this type of observations to date. For this, we integrate and employ existing comprehensive models of meteoroid ablation, ionization, and radar detection to enable accurate interpretation of radar observations and show that reasonable agreement in the hourly rates is found between model predictions and Arecibo observations when (1) we invoke the lower limit of the model predicted flux (similar to 16 t d(-1)) and (2) we estimate the ionization probability of ablating metal atoms using laboratory measurements of the ionization cross sections of high-speed metal atom beams, resulting in values up to two orders of magnitude lower than the extensively utilized figure reported by Jones for low-speed meteors. However, even at this lower limit, the model overpredicts the slow portion of the Arecibo radial velocity distributions by a factor of three, suggesting that the model requires some revision. C1 [Janches, D.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. [Plane, J. M. C.; Feng, W.] Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England. [Nesvorny, D.] SouthWest Res Inst, Boulder, CO 80302 USA. [Vokrouhlicky, D.] Charles Univ Prague, Inst Astron, Prague, Czech Republic. [Nicolls, M. J.] SRI Int, Menlo Pk, CA 94025 USA. RP Janches, D (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Mail Code 674, Greenbelt, MD 20771 USA. EM diego.janches@nasa.gov; j.m.c.plane@leeds.ac.uk; davidn@boulder.swri.edu; w.feng@leeds.ac.uk; vokrouhl@cesnet.cz; Michael.Nicolls@sri.com RI Plane, John/C-7444-2015; FENG, WUHU/B-8327-2008; Janches, Diego/D-4674-2012 OI Plane, John/0000-0003-3648-6893; FENG, WUHU/0000-0002-9907-9120; Janches, Diego/0000-0001-8615-5166 FU NASA [12-PAST12-0007, 12-PATM12-0006]; NASA's Solar System Works; European Research Council [291332-CODITA]; Czech Grant Agency [P209-13-013085] FX D.J. is supported by NASA awards 12-PAST12-0007 and 12-PATM12-0006; D.N. has been supported through NASA's Solar System Works; J.M.C.P. and W.F. are supported by the European Research Council (project number 291332-CODITA) and the work of D.V. was partly supported by the Czech Grant Agency (grant P209-13-013085). The Arecibo Observatory is operated by SRI International under a cooperative agreement with the National Science Foundation. NR 65 TC 10 Z9 10 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2014 VL 796 IS 1 AR 41 DI 10.1088/0004-637X/796/1/41 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AS9GD UT WOS:000344550300041 ER PT J AU Magdis, GE Rigopoulou, D Hopwood, R Huang, JS Farrah, D Pearson, C Alonso-Herrero, A Bock, JJ Clements, D Cooray, A Griffin, MJ Oliver, S Fournon, IP Riechers, D Swinyard, BM Scott, D Thatte, N Valtchanov, I Vaccari, M AF Magdis, Georgios E. Rigopoulou, D. Hopwood, R. Huang, J. -S. Farrah, D. Pearson, C. Alonso-Herrero, Almudena Bock, J. J. Clements, D. Cooray, A. Griffin, M. J. Oliver, S. Perez Fournon, I. Riechers, D. Swinyard, B. M. Scott, D. Thatte, N. Valtchanov, I. Vaccari, M. TI A FAR-INFRARED SPECTROSCOPIC SURVEY OF INTERMEDIATE REDSHIFT (ULTRA) LUMINOUS INFRARED GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: star formation; gamma rays: ISM; infrared: galaxies; infrared: general ID STAR-FORMING GALAXIES; SIMILAR-TO 2; C-II LINE; SPECTRAL ENERGY-DISTRIBUTIONS; ACTIVE GALACTIC NUCLEI; SPACE-OBSERVATORY MEASUREMENTS; MOLECULAR INTERSTELLAR-MEDIUM; ULTRALUMINOUS IRAS GALAXIES; DEEP-FIELD-SOUTH; SUBMILLIMETER GALAXIES AB We present Herschel far-IR photometry and spectroscopy as well as ground-based CO observations of an intermediate redshift (0.21 <= z <= 0.88) sample of Herschel-selected (ultra)-luminous infrared galaxies (L-IR > 1011.5 L-circle dot). With these measurements, we trace the dust continuum, far-IR atomic line emission, in particular [C-II] 157.7 mu m, as well as the molecular gas of z similar to 0.3 luminous and ultraluminous infrared galaxies (LIRGs and ULIRGs) and perform a detailed investigation of the interstellar medium of the population. We find that the majority of Herschel-selected intermediate redshift (U) LIRGs have L-CII/L-FIR ratios that are a factor of about 10 higher than that of local ULIRGs and comparable to that of local normal and high-z star-forming galaxies. Using our sample to bridge local and high-z [C-II] observations, we find that the majority of galaxies at all redshifts and all luminosities follow an L-CII-L-FIR relation with a slope of unity, from which local ULIRGs and high-z active-galactic-nucleus-dominated sources are clear outliers. We also confirm that the strong anti-correlation between the L-CII/L-FIR ratio and the far-IR color L-60/L-100 observed in the local universe holds over a broad range of redshifts and luminosities, in the sense that warmer sources exhibit lower L-CII/L-FIR at any epoch. Intermediate redshift ULIRGs are also characterized by large molecular gas reservoirs and by lower star formation efficiencies compared to that of local ULIRGs. The high L-CII/L-FIR ratios, the moderate star formation efficiencies (L-IR/L-CO' or L-IR/M-H2), and the relatively low dust temperatures of our sample (which are also common characteristics of high-z star-forming galaxies with ULIRG-like luminosities) indicate that the evolution of the physical properties of (U) LIRGs between the present day and z > 1 is already significant by z similar to 0.3. C1 [Magdis, Georgios E.; Rigopoulou, D.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Magdis, Georgios E.; Swinyard, B. M.; Thatte, N.] Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote Sen, GR-15236 Athens, Greece. [Rigopoulou, D.; Pearson, C.] Rutherford Appleton Lab, RAL Space Sci & Technol Facil Council, Didcot OX11 0QX, Oxon, England. [Hopwood, R.; Clements, D.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England. [Huang, J. -S.] Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China. [Huang, J. -S.] Chinese Acad Sci, China Chile Joint Ctr Astron, Santiago, Chile. [Huang, J. -S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Pearson, C.] Open Univ, Milton Keynes MK7 6AA, Bucks, England. [Alonso-Herrero, Almudena] CSIC UC, Inst Fis Cantabria, E-39006 Santander, Spain. [Bock, J. J.] CALTECH, Pasadena, CA 91125 USA. [Bock, J. J.; Cooray, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Griffin, M. J.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Oliver, S.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Perez Fournon, I.] IAC, Tenerife 38200, Spain. [Perez Fournon, I.] Univ La Laguna, Dept Astrofs, E-38205 Tenerife, Spain. [Riechers, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Swinyard, B. M.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, E-28691 Madrid, Spain. [Vaccari, M.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Cape Town, South Africa. RP Magdis, GE (reprint author), Univ Oxford, Dept Phys, Keble Rd, Oxford OX1 3RH, England. EM ipf@iac.es RI Magdis, Georgios/C-7295-2014; Vaccari, Mattia/R-3431-2016; Alonso-Herrero, Almudena/H-1426-2015 OI Magdis, Georgios/0000-0002-4872-2294; Scott, Douglas/0000-0002-6878-9840; Vaccari, Mattia/0000-0002-6748-0577; Alonso-Herrero, Almudena/0000-0001-6794-2519 FU STFC [ST/K00106X/1]; John Fell Oxford University Press (OUP) Research Fund; University of Oxford; Universidad de Cantabria August G. Linares Programme; INSU/CNRS (France); MPG (Germany); IGN (Spain) FX We warmly thank the referee for constructive comments and suggestions. G.E.M. and D.R. acknowledge support from STFC through grant ST/K00106X/1. G.E.M. acknowledges support from the John Fell Oxford University Press (OUP) Research Fund and the University of Oxford. A.A.-H. acknowledges funding through the Universidad de Cantabria August G. Linares Programme. This work includes observations made with IRAM, which is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). Based on observations made with ESO Telescopes at the APEX Observatory under programme ID 090.B-0708A and 091.B-0312A. This paper uses data from Herschel's photometer SPIRE. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including: University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, University of Colorado (USA). NR 144 TC 14 Z9 14 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2014 VL 796 IS 1 AR 63 DI 10.1088/0004-637X/796/1/63 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AS9GD UT WOS:000344550300063 ER PT J AU Raja, KS Ramesh, R Hariharan, K Kathiravan, C Wang, TJ AF Raja, K. Sasikumar Ramesh, R. Hariharan, K. Kathiravan, C. Wang, T. J. TI AN ESTIMATE OF THE MAGNETIC FIELD STRENGTH ASSOCIATED WITH A SOLAR CORONAL MASS EJECTION FROM LOW FREQUENCY RADIO OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: magnetic fields; Sun: radio radiation ID SUN-EARTH CONNECTION; NOISE STORM; GAURIBIDANUR RADIOHELIOGRAPH; VLA OBSERVATIONS; WHITE-LIGHT; QUIET SUN; EMISSION; BURSTS; WAVELENGTHS; SPECTROGRAPH AB We report ground based, low frequency heliograph (80 MHz), spectral (85-35 MHz), and polarimeter (80 and 40 MHz) observations of drifting, non-thermal radio continuum associated with the "halo" coronal mass ejection that occurred in the solar atmosphere on 2013 March 15. The magnetic field strengths (B) near the radio source were estimated to be B approximate to 2.2 +/- 0.4 G at 80 MHz and B approximate to 1.4 +/- 0.2 G at 40 MHz. The corresponding radial distances (r) are r approximate to 1.9 R-circle dot (80 MHz) and r approximate to 2.2 R-circle dot (40 MHz). C1 [Raja, K. Sasikumar; Ramesh, R.; Hariharan, K.; Kathiravan, C.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Wang, T. J.] Catholic Univ Amer, Dept Phys, Greenbelt, MD 20771 USA. [Wang, T. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Raja, KS (reprint author), Indian Inst Astrophys, Bangalore 560034, Karnataka, India. EM sasikumar@iiap.res.in FU NASA Cooperative Agreement [NNG11PL10A]; NASA [NNX12AB34G] FX It is a pleasure to thank the staff of the Gauribidanur observatory for their help in observations, and maintenance of the antenna and receiver systems there. We also thank the referee for comments that helped bring out the results more clearly. The SOHO data are produced by a consortium of the Naval Research Laboratory (USA), Max-Planck-Institut fur Aeronomie (Germany), Laboratoire d'Astronomie (France), and the University of Birmingham (UK). SOHO is a project of international cooperation between ESA and NASA. The SOHO-LASCO CME catalog and STEREO movies are generated and maintained at the CDAW Data Center by NASA and the Catholic University of America in cooperation with the Naval Research Laboratory. The SDO/AIA data are courtesy of the NASA/SDO and the AIA science teams. The work of T.J.W. was supported by NASA Cooperative Agreement NNG11PL10A to CUA and NASA grant NNX12AB34G. NR 69 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2014 VL 796 IS 1 AR 56 DI 10.1088/0004-637X/796/1/56 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AS9GD UT WOS:000344550300056 ER PT J AU Ridgway, ST Matheson, T Mighell, KJ Olsen, KA Howell, SB AF Ridgway, Stephen T. Matheson, Thomas Mighell, Kenneth J. Olsen, Knut A. Howell, Steve B. TI THE VARIABLE SKY OF DEEP SYNOPTIC SURVEYS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; minor planets, asteroids: general; quasars: general; stars: general; surveys; techniques: miscellaneous ID CATACLYSMIC VARIABLES; LUMINOSITY FUNCTION; VARIABILITY SURVEY; FLARE RATE; STARS; NUMBER; CLASSIFICATION; MULTIPLICITY; TELESCOPE; EVOLUTION AB The discovery of variable and transient sources is an essential product of synoptic surveys. The alert stream will require filtering for personalized criteria-a process managed by a functionality commonly described as a Broker. In order to understand quantitatively the magnitude of the alert generation and Broker tasks, we have undertaken an analysis of the most numerous types of variable targets in the sky-Galactic stars, quasi-stellar objects (QSOs), active galactic nuclei (AGNs), and asteroids. It is found that the Large Synoptic Survey Telescope (LSST) will be capable of discovering similar to 10(5) high latitude (|b| > 20 degrees.) variable stars per night at the beginning of the survey. (The corresponding number for |b| < 20 degrees. is orders of magnitude larger, but subject to caveats concerning extinction and crowding.) However, the number of new discoveries may well drop below 100 per night within less than one year. The same analysis applied to GAIA clarifies the complementarity of the GAIA and LSST surveys. Discovery of AGNs and QSOs are each predicted to begin at similar to 3000 per night and decrease by 50 times over four years. Supernovae are expected at similar to 1100 per night, and after several survey years will dominate the new variable discovery rate. LSST asteroid discoveries will start at > 10(5) per night, and if orbital determination has a 50% success rate per epoch, they will drop below 1000 per night within two years. C1 [Ridgway, Stephen T.; Matheson, Thomas; Mighell, Kenneth J.; Olsen, Knut A.] Natl Opt Astron Observ, Tucson, AZ 85725 USA. [Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Ridgway, ST (reprint author), Natl Opt Astron Observ, Tucson, AZ 85725 USA. EM ridgway@noao.edu NR 50 TC 4 Z9 4 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2014 VL 796 IS 1 AR 53 DI 10.1088/0004-637X/796/1/53 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AS9GD UT WOS:000344550300053 ER PT J AU Zellem, RT Griffith, CA Deroo, P Swain, MR Waldmann, IP AF Zellem, Robert T. Griffith, Caitlin A. Deroo, Pieter Swain, Mark R. Waldmann, Ingo P. TI THE GROUND-BASED H-, K-, AND L-BAND ABSOLUTE EMISSION SPECTRA OF HD 209458b SO ASTROPHYSICAL JOURNAL LA English DT Article DE atmospheric effects; methods: numerical; planets and satellites: general; planets and satellites: individual (HD 209458b); techniques: spectroscopic ID MU-M; HEAT REDISTRIBUTION; BROWN DWARFS; HOT JUPITERS; 189733B; SPECTROSCOPY; EXTRACTION; PLANETS; SPECTROGRAPH; ATMOSPHERES AB Here we explore the capabilities of NASA's 3.0 m Infrared Telescope Facility (IRTF) and SpeX spectrometer and the 5.08 m Hale telescope with the TripleSpec spectrometer with near-infrared H-, K-, and L-band measurements of HD 209458b's secondary eclipse. Our IRTF/SpeX data are the first absolute L-band spectroscopic emission measurements of any exoplanet other than the hot Jupiter HD 189733b. Previous measurements of HD 189733b's L band indicate bright emission hypothesized to result from non-LTE CH4 nu(3) fluorescence. We do not detect a similar bright 3.3 mu m feature to similar to 3 sigma, suggesting that fluorescence does not need to be invoked to explain HD 209458b's L-band measurements. The validity of our observation and reduction techniques, which decrease the flux variance by up to 2.8 orders ofmagnitude, is reinforced by 1 sigma agreement with existent Hubble/NICMOS and Spitzer/IRAC1 observations that overlap the H, K, and L bands, suggesting that both IRTF/SpeX and Palomar/TripleSpec can measure an exoplanet's emission with high precision. C1 [Zellem, Robert T.; Griffith, Caitlin A.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Deroo, Pieter; Swain, Mark R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Waldmann, Ingo P.] UCL, Dept Phys & Astron, London WC1E 6BT, England. RP Zellem, RT (reprint author), Univ Arizona, Lunar & Planetary Lab, 1629 East Univ Blvd, Tucson, AZ 85721 USA. EM rzellem@lpl.arizona.edu OI Waldmann, Ingo/0000-0002-4205-5267; Zellem, Robert/0000-0001-7547-0398 FU NASA Planetary Atmospheres Program FX R.T.Z. and C.A.G. are supported by the NASA Planetary Atmospheres Program. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The authors thank Ming Zhao for observing HD 209458b with Palomar/TripleSpec. R.T.Z. thanks Ian J. M. Crossfield and Michael R. Line for their helpful discussions. We also thank the referee for helpful comments and suggestions. NR 37 TC 7 Z9 7 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2014 VL 796 IS 1 AR 48 DI 10.1088/0004-637X/796/1/48 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AS9GD UT WOS:000344550300048 ER PT J AU Bonev, BP DiSanti, MA Villanueva, GL Gibb, EL Paganini, L Mumma, MJ AF Bonev, Boncho P. DiSanti, Michal A. Villanueva, Geronimo L. Gibb, Erika L. Paganini, Lucas Mumma, Michael J. TI THE INNER COMA OF COMET C/2012 S1 (ISON) AT 0.53 AU AND 0.35 AU FROM THE SUN SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE comets: general; comets: individual (C/2012 S1 ISON); molecular processes ID ORTHO-PARA RATIO; 103P/HARTLEY 2; ROTATIONAL TEMPERATURES; WATER PRODUCTION; INFRARED WAVELENGTHS; P1 GARRADD; C/1996 B2; GAS COMA; RELEASE; ATMOSPHERES AB Using long-slit spectroscopy at the NASA Infrared Telescope Facility, we extracted H2O production rates and spatial profiles of gas rotational temperature and molecular column abundance in comet C/2012 S1 ISON, observed at heliocentric distances of 0.53 and 0.35 AU. These measurements uniquely probed the physical environment in the inner collisional coma of this comet during its first (and last) approach to the Sun since being emplaced in the Oort Cloud some 4.5 billion years ago. Our observations revealed a comet evolving on various timescales, both over hours and days. At 0.35 AU, ISON showed a considerable decrease in water production rate in less than 2 hr, likely declining from a major outburst. Our measured temperature spatial distributions reflect the competition between the processes that cause heating and cooling in the coma, and also provide insight about the prevalent mechanism(s) of releasing gas-phase H2O. The observed temperatures suggest that the comet was likely ejecting icy material continuously, which sublimated in the coma and heated the ambient gas, augmenting fast H-atoms produced by H2O photolysis. ISON adds to the very limited sample of comets for which spatial-spectral studies of water temperatures have been conducted. These studies are now feasible and can be extended to comets having a variety of gas production rates. Continued synergy of such observations with both space missions like Rosetta and with physical models is strongly encouraged in order to gain a deeper understanding of the processes in the inner collisional zone of the cometary coma. C1 [Bonev, Boncho P.; Villanueva, Geronimo L.; Paganini, Lucas] Catholic Univ Amer, Dept Phys, Washington, DC 20061 USA. [Bonev, Boncho P.; DiSanti, Michal A.; Villanueva, Geronimo L.; Gibb, Erika L.; Paganini, Lucas; Mumma, Michael J.] NASA GSFC, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [DiSanti, Michal A.; Mumma, Michael J.] NASA GSFC, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Gibb, Erika L.] Univ Missouri, Dept Phys & Astron, St Louis, MO 63121 USA. EM bonev@cua.edu OI Mumma, Michael/0000-0003-4627-750X FU National Science Foundation [AST-1211362] FX We are most fortunate to conduct observations from NASA IRTF and Maunakea, recognizing the very significant cultural role and reverence that the summit has always had within the indigenous Hawaiian community. We gratefully acknowledge NASA GSFC (Solar System Exploration Division) internal funding for comet ISON observing campaign, National Science Foundation Grant AST-1211362, and NASA's PATM, PAST, and Astrobiology programs for supporting various team members in this work. We are very grateful to NASA IRTF, Michael Combi, Nicolas Fougere, Neil Dello Russo, Adam McKay, Ron Vervack, and Jacqueline Keane for their exceptional support and fruitful discussions. NR 43 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 20 PY 2014 VL 796 IS 1 AR L6 DI 10.1088/2041-8205/796/1/L6 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT0TF UT WOS:000344647000006 ER PT J AU Cernicharo, J Teyssier, D Quintana-Lacaci, G Daniel, F Agundez, M Velilla-Prieto, L Decin, L Guelin, M Encrenaz, P Garcia-Lario, P de Beck, E Barlow, MJ Groenewegen, MAT Neufeld, D Pearson, J AF Cernicharo, J. Teyssier, D. Quintana-Lacaci, G. Daniel, F. Agundez, M. Velilla-Prieto, L. Decin, L. Guelin, M. Encrenaz, P. Garcia-Lario, P. de Beck, E. Barlow, M. J. Groenewegen, M. A. T. Neufeld, D. Pearson, J. TI DISCOVERY OF TIME VARIATION OF THE INTENSITY OF MOLECULAR LINES IN IRC+10216 IN THE SUBMILLIMETER AND FAR-INFRARED DOMAINS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; stars: AGB and post-AGB; stars: carbon; stars: individual (IRC, 10216) ID DUST FORMATION ZONE; THEORETICAL CALCULATION; CIRCUMSTELLAR ENVELOPE; STAR IRC+10216; CW LEONIS; C2H; IRC; SILICON; SIC2 AB We report on the discovery of strong intensity variations in the high rotational lines of abundant molecular species toward the archetypical circumstellar envelope of IRC+10216. The observations have been carried out with the Heterodyne Instrument for the Far-Infrared (HIFI) instrument on board Herschel and with the IRAM30 m telescope. They cover several observing periods spreading over three years. The line intensity variations for molecules produced in the external layers of the envelope most likely result from time variations in the infrared pumping rates. We analyze the main implications this discovery has on the interpretation of molecular line emission in the envelopes of Mira-type stars. Radiative transfer calculations must take into account both the time variability of infrared pumping and the possible variation of the dust and gas temperatures with stellar phase in order to reproduce the observation of molecular lines at different epochs. The effect of gas temperature variations with stellar phase could be particularly important for lines produced in the innermost regions of the envelope. Each layer of the circumstellar envelope sees the stellar light radiation with a different lag time (phase). Our results show that this effect must be included in the models. The submillimeter and far infrared lines of asymptotic giant branch stars can no longer be considered as safe intensity calibrators. C1 [Cernicharo, J.; Quintana-Lacaci, G.; Agundez, M.; Velilla-Prieto, L.] CSIC, ICMM, Grp Mol Astrophys, E-28049 Madrid, Spain. [Teyssier, D.; Garcia-Lario, P.] ESA, ESAC, E-28691 Madrid, Spain. [Daniel, F.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. [Daniel, F.] CNRS, IPAG, F-38000 Grenoble, France. [Decin, L.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3000 Louvain, Belgium. [Guelin, M.] Inst Radioastron Millimetr, F-38406 St Martin Dheres, France. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [de Beck, E.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden. [Barlow, M. J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Groenewegen, M. A. T.] Koninklijke Sterrenwacht Belgie, B-1180 Brussels, Belgium. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Pearson, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Cernicharo, J (reprint author), CSIC, ICMM, Grp Mol Astrophys, C Sor Juana Ines de La Cruz N3, E-28049 Madrid, Spain. RI Barlow, Michael/A-5638-2009; Agundez, Marcelino/I-5369-2012; OI Barlow, Michael/0000-0002-3875-1171; Agundez, Marcelino/0000-0003-3248-3564; De Beck, Elvire/0000-0002-7441-7189; Quintana-Lacaci, Guillermo/0000-0002-5417-1943 FU Spanish MICINN [AYA2009-07304, AYA2012-32032, CSD2009-00038]; ERC [ERC-2013-SyG, G.A. 610256 NANOCOSMOS]; Fund for Scientific Research-Flanders (FWO); INSU/CNRS (France); MPG (Germany); IGN (Spain) FX J.C., M.A., G.Q.L., and L.V.P. thank the Spanish MICINN for funding under grants AYA2009-07304, AYA2012-32032, CSD2009-00038, and ERC under ERC-2013-SyG, G.A. 610256 NANOCOSMOS. L.D. acknowledges financial support from the Fund for Scientific Research-Flanders (FWO). This work was based on observations carried out with the IRAM 30 m telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). NR 26 TC 8 Z9 8 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 20 PY 2014 VL 796 IS 1 AR L21 DI 10.1088/2041-8205/796/1/L21 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT0TF UT WOS:000344647000021 ER PT J AU Degenaar, N Miller, JM Harrison, FA Kennea, JA Kouveliotou, C Younes, G AF Degenaar, N. Miller, J. M. Harrison, F. A. Kennea, J. A. Kouveliotou, C. Younes, G. TI HIGH-RESOLUTION X-RAY SPECTROSCOPY OF THE BURSTING PULSAR GRO J1744-28 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; pulsars: individual (GRO J1744-28); stars: neutron; X-rays: binaries ID INNER ACCRETION DISKS; NEUTRON-STAR; SAX J1808.4-3658; EMISSION-LINE; JET FORMATION; CIRCINUS X-1; BLACK-HOLES; IRON LINE; CHANDRA; WIND AB The bursting pulsar GRO J1744-28 is a Galactic low-mass X-ray binary that distinguishes itself by displaying type-II X-ray bursts: brief, bright flashes of X-ray emission that likely arise from spasmodic accretion. Combined with its coherent 2.1 Hz X-ray pulsations and relatively high estimated magnetic field, it is a particularly interesting source to study the physics of accretion flows around neutron stars. Here we report on Chandra/High Energy Transmission Grating observations obtained near the peak of its bright 2014 accretion outburst. Spectral analysis suggests the presence of a broad iron emission line centered at E-1 similar or equal to 6.7 keV. Fits with a disk reflection model yield an inclination angle of i similar or equal to 52 degrees and an inner disk radius of R-in similar or equal to 85 GM/c(2), which is much further out than typically found for neutron star low-mass X-ray binaries. Assuming that the disk is truncated at the magnetospheric radius of the neutron star, we estimate a magnetic field strength of B similar or equal to (2-6) x 10(10) G. Furthermore, we identify an absorption feature near similar or equal to 6.85 keV that could correspond to blue-shifted Fe xxv and point to a fast disk wind with an outflow velocity of upsilon(out) similar or equal to (7.5-8.2) x 10(3) km s(-1) (similar or equal to 0.025c-0.027c). If the covering fraction and filling factor are large, this wind could be energetically important and perhaps account for the fact that the companion star lost significant mass while the magnetic field of the neutron star remained strong. C1 [Degenaar, N.; Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Harrison, F. A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Kouveliotou, C.] NASA, Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. [Younes, G.] Univ Space Res Assoc, Huntsville, AL 35806 USA. RP Degenaar, N (reprint author), Univ Michigan, Dept Astron, 1085 South Univ Ave, Ann Arbor, MI 48109 USA. EM degenaar@umich.edu FU NASA through Hubble Postdoctoral Fellowship grant from the Space Telescope Science Institute [HST-HF-51287.01-A]; NASA [NAS5-26555]; Chandra guest observer program FX N.D. is supported by NASA through Hubble Postdoctoral Fellowship grant No. HST-HF-51287.01-A from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. J.M. gratefully acknowledges support from the Chandra guest observer program. N.D. thanks Ed Cackett, Felix Furst and Rudy Wijnands for very helpful discussions. We extend our thanks to the anonymous referee. NR 50 TC 12 Z9 12 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 20 PY 2014 VL 796 IS 1 AR L9 DI 10.1088/2041-8205/796/1/L9 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT0TF UT WOS:000344647000009 ER PT J AU Roberge, A Welsh, BY Kamp, I Weinberger, AJ Grady, CA AF Roberge, Aki Welsh, Barry Y. Kamp, Inga Weinberger, Alycia J. Grady, Carol A. TI VOLATILE-RICH CIRCUMSTELLAR GAS IN THE UNUSUAL 49 CETI DEBRIS DISK SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; Kuiper belt: general; protoplanetary disks; stars: individual (49 Ceti) ID LOCAL INTERSTELLAR-MEDIUM; A-TYPE STARS; BETA-PICTORIS; MOLECULAR GAS; CO; BODIES AB We present Hubble Space Telescope Space Telescope Imaging Spectrograph far-UV spectra of the edge-on disk around 49 Ceti, one of the very few debris disks showing submillimeter CO emission. Many atomic absorption lines are present in the spectra, most of which arise from circumstellar gas lying along the line-of-sight to the central star. We determined the line-of-sight C I column density, estimated the total carbon column density, and set limits on the OI column density. Surprisingly, no line-of-sight CO absorption was seen. We discuss possible explanations for this non-detection, and present preliminary estimates of the carbon abundances in the line-of-sight gas. The C/Fe ratio is much greater than the solar value, suggesting that 49 Cet harbors a volatile-rich gas disk similar to that of beta Pictoris. C1 [Roberge, Aki; Grady, Carol A.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Welsh, Barry Y.; Grady, Carol A.] Eureka Sci, Oakland, CA 96002 USA. [Welsh, Barry Y.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Kamp, Inga] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Weinberger, Alycia J.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. RP Roberge, A (reprint author), NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA. EM Aki.Roberge@nasa.gov RI Roberge, Aki/D-2782-2012 OI Roberge, Aki/0000-0002-2989-3725 FU NASA through a grant from the Space Telescope Science Institute [GO-12901]; NASA [NAS5-26555]; Goddard Center for Astrobiology, NASA Astrobiology Institute FX Support for program number GO-12901 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. A. R. also acknowledges support by the Goddard Center for Astrobiology, part of the NASA Astrobiology Institute. NR 22 TC 9 Z9 9 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 20 PY 2014 VL 796 IS 1 AR L11 DI 10.1088/2041-8205/796/1/L11 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT0TF UT WOS:000344647000011 ER PT J AU Aartsen, MG Ackermann, M Adams, J Aguilar, JA Ahlers, M Ahrens, M Altmann, D Anderson, T Arguelles, C Arlen, TC Auffenberg, J Bai, X Barwick, SW Baum, V Beatty, JJ Tjus, JB Becker, KH BenZvi, S Berghaus, P Berley, D Bernardini, E Bernhard, A Besson, DZ Binder, G Bindig, D Bissok, M Blaufuss, E Blumenthal, J Boersma, DJ Bohm, C Bos, F Bose, D Boser, S Botner, O Brayeur, L Bretz, HP Brown, AM Casey, J Casier, M Chirkin, D Christov, A Christy, B Clark, K Classen, L Clevermann, F Coenders, S Cowen, DF Silva, AHC Danninger, M Daughhetee, J Davis, JC Day, M de Andre, JPAM De Clercq, C De Ridder, S Desiati, P de Vries, KD de With, M DeYoung, T Diaz-Velez, JC Dunkman, M Eagan, R Eberhardt, B Eichmann, B Eisch, J Euler, S Evenson, PA Fadiran, O Fazely, AR Fedynitch, A Feintzeig, J Felde, J Feusels, T Filimonov, K Finley, C Fischer-Wasels, T Flis, S Franckowiak, A Frantzen, K Fuchs, T Gaisser, TK Gallagher, J Gerhardt, L Gier, D Gladstone, L Glusenkamp, T Goldschmidt, A Golup, G Gonzalez, JG Goodman, JA Gora, D Grandmont, DT Grant, D Gretskov, P Groh, JC Gross, A Ha, C Haack, C Ismail, AH Hallen, P Hallgren, A Halzen, F Hanson, K Hebecker, D Heereman, D Heinen, D Helbing, K Hellauer, R Hellwig, D Hickford, S Hill, GC Hoffman, KD Hoffmann, R Homeier, A Hoshina, K Huang, F Huelsnitz, W Hulth, PO Hultqvist, K Hussain, S Ishihara, A Jacobi, E Jacobsen, J Jagielski, K Japaridze, GS Jero, K Jlelati, O Jurkovic, M Kaminsky, B Kappes, A Karg, T Karle, A Kauer, M Kelley, JL Kheirandish, A Kiryluk, J Klas, J Klein, SR Kohne, JH Kohnen, G Kolanoski, H Koob, A Kopke, L Kopper, C Kopper, S Koskinen, DJ Kowalski, M Kriesten, A Krings, K Kroll, G Kroll, M Kunnen, J Kurahashi, N Kuwabara, T Labare, M Larsen, DT Larson, MJ Lesiak-Bzdak, M Leuermann, M Leute, J Lunemann, J Macias, O Madsen, J Maggi, G Maruyama, R Mase, K Matis, HS McNally, F Meagher, K Medici, M Meli, A Meures, T Miarecki, S Middell, E Middlemas, E Milke, N Miller, J Mohrmann, L Montaruli, T Morse, R Nahnhauer, R Naumann, U Niederhausen, H Nowicki, SC Nygren, DR Obertacke, A Odrowski, S Olivas, A Omairat, A O'Murchadha, A Palczewski, T Paul, L Penek, O Pepper, JA de los Heros, CP Pfendner, C Pieloth, D Pinat, E Posselt, J Price, PB Przybylski, GT Putz, J Quinnan, M Radel, L Rameez, M Rawlins, K Redl, P Rees, I Reimann, R Resconi, E Rhode, W Richman, M Riedel, B Robertson, S Rodrigues, JP Rongen, M Rott, C Ruhe, T Ruzybayev, B Ryckbosch, D Saba, SM Sander, HG Sandroos, J Santander, M Sarkar, S Schatto, K Scheriau, F Schmidt, T Schmitz, M Schoenen, S Schoneberg, S Schonwald, A Schukraft, A Schulte, L Schulz, O Seckel, D Sestayo, Y Seunarine, S Shanidze, R Sheremata, C Smith, MWE Soldin, D Spiczak, GM Spiering, C Stamatikos, M Stanev, T Stanisha, NA Stasik, A Stezelberger, T Stokstad, RG Stossl, A Strahler, EA Strom, R Strotjohann, NL Sullivan, GW Taavola, H Taboada, I Tamburro, A Tepe, A Ter-Antonyan, S Terliuk, A Tesic, G Tilav, S Toale, PA Tobin, MN Tosi, D Tselengidou, M Unger, E Usner, M Vallecorsa, S van Eijndhoven, N Vandenbroucke, J van Santen, J Vehring, M Voge, M Vraeghe, M Walck, C Wallraff, M Weaver, C Wellons, M Wendt, C Westerhoff, S Whelan, BJ Whitehorn, N Wichary, C Wiebe, K Wiebusch, CH Williams, DR Wissing, H Wolf, M Wood, TR Woschnagg, K Xu, DL Xu, XW Yanez, JP Yodh, G Yoshida, S Zarzhitsky, P Ziemann, J Zierke, S Zoll, M Aasi, J Abbott, BP Abbott, R Abbott, T Abernathy, MR Acernese, F Ackley, K Adams, C Adams, T Addesso, P Adhikari, RX Affeldt, C Agathos, M Aggarwal, N Aguiar, OD Ajith, P Alemic, A Allen, B Allocca, A Amariutei, D Andersen, M Anderson, RA Anderson, SB Anderson, WG Arai, K Araya, MC Arceneaux, C Areeda, JS Ast, S Aston, SM Astone, P Aufmuth, P Augustus, H Aulbert, C Aylott, BE Babak, S Baker, PT Ballardin, G Ballmer, SW Barayoga, JC Barbet, M Barish, BC Barker, D Barone, F Barr, B Barsotti, L Barsuglia, M Barton, MA Bartos, I Bassiri, R Basti, A Batch, JC Bauchrowitz, J Bauer, TS Baune, C Bavigadda, V Behnke, B Bejger, M Beker, MG Belczynski, C Bell, AS Bell, C Bergmann, G Bersanetti, D Bertolini, A Betzwieser, J Bilenko, IA Billingsley, G Birch, J Biscans, S Bitossi, M Biwer, C Bizouard, MA Black, E Blackburn, JK Blackburn, L Blair, D Bloemen, S Bock, O Bodiya, TP Boer, M Bogaert, G Bogan, C Bojtos, P Bond, C Bondu, F Bonelli, L Bonnand, R Bork, R Born, M Boschi, V Bose, S Bosi, L Bradaschia, C Brady, PR Braginsky, VB Branchesi, M Brau, JE Briant, T Bridges, DO Brillet, A Brinkmann, M Brisson, V Brooks, AF Brown, DA Brown, DD Bruckner, F Buchman, S Buikema, A Bulik, T Bulten, HJ Buonanno, A Burman, R Buskulic, D Buy, C Cadonati, L Cagnoli, G Bustillo, JC Calloni, E Camp, JB Campsie, P Cannon, KC Canuel, B Cao, J Capano, CD Carbognani, F Carbone, L Caride, S Castaldi, G Caudill, S Cavaglia, M Cavalier, F Cavalieri, R Celerier, C Cella, G Cepeda, C Cesarini, E Chakraborty, R Chalermsongsak, T Chamberlin, SJ Chao, S Charlton, P Chassande-Mottin, E Chen, X Chen, Y Chincarini, A Chiummo, A Cho, HS Cho, M Chow, JH Christensen, N Chu, Q Chua, SSY Chung, S Ciani, G Clara, F Clark, DE Clark, JA Clayton, JH Cleva, F Coccia, E Cohadon, PF Colla, A Collette, C Colombini, M Cominsky, L Constancio, M Conte, A Cook, D Corbitt, TR Cornish, N Corsi, A Costa, CA Coughlin, MW Coulon, JP Countryman, S Couvares, P Coward, DM Cowart, MJ Coyne, DC Coyne, R Craig, K Creighton, JDE Croce, RP Crowder, SG Cumming, A Cunningham, L Cuoco, E Cutler, C Dahl, K Dal Canton, T Damjanic, M Danilishin, SL D'Antonio, S Danzmann, K Dattilo, V Daveloza, H Davier, M Davies, GS Daw, EJ Day, R Dayanga, T Debra, D Debreczeni, G Degallaix, J Deleglise, S Del Pozzo, W Del Pozzo, W Denker, T Dent, T Dereli, H Dergachev, V De Rosa, R DeRosa, RT DeSalvo, R Dhurandhar, S Diaz, M Dickson, J Di Fiore, L Di Lieto, A Di Palma, I Di Virgilio, A Dolique, V Dominguez, E Donovan, F Dooley, KL Doravari, S Douglas, R Downes, TP Drago, M Drever, RWP Driggers, JC Du, Z Ducrot, M Dwyer, S Eberle, T Edo, T Edwards, M Effler, A Eggenstein, HB Ehrens, P Eichholz, J Eikenberry, SS Endroczi, G Essick, R Etzel, T Evans, M Evans, T Factourovich, M Fafone, V Fairhurst, S Fan, X Fang, Q Farinon, S Farr, B Farr, WM Favata, M Fazi, D Fehrmann, H Fejer, MM Feldbaum, D Feroz, F Ferrante, I Ferreira, EC Ferrini, F Fidecaro, F Finn, LS Fiori, I Fisher, RP Flaminio, R Fournier, JD Franco, S Frasca, S Frasconi, F Frede, M Frei, Z Freise, A Frey, R Fricke, TT Fritschel, P Frolov, VV Fulda, P Fyffe, M Gair, JR Gammaitoni, L Gaonkar, S Garufi, F Gehrels, N Gemme, G Gendre, B Genin, E Gennai, A Ghosh, S Giaime, JA Giardina, KD Giazotto, A Gleason, J Goetz, E Goetz, R Gondan, L Gonzalez, G Gordon, N Gorodetsky, ML Gossan, S Gossler, S Gouaty, R Graf, C Graff, PB Granata, M Grant, A Gras, S Gray, C Greenhalgh, RJS Gretarsson, AM Groot, P Grote, H Grover, K Grunewald, S Guidi, GM Guido, CJ Gushwa, K Gustafson, EK Gustafson, R Ha, J Hall, ED Hamilton, W Hammer, D Hammond, G Hanke, M Hanks, J Hanna, C Hannam, MD Hanson, J Harms, J Harry, GM Harry, IW Harstad, ED Hart, M Hartman, MT Haster, CJ Haughian, K Heidmann, A Heintze, M Heitmann, H Hello, P Hemming, G Hendry, M Heng, IS Heptonstall, AW Heurs, M Hewitson, M Hild, S Hoak, D Hodge, KA Hofman, D Holt, K Hopkins, P Horrom, T Hoske, D Hosken, DJ Hough, J Howell, EJ Hu, Y Huerta, E Hughey, B Husa, S Huttner, SH Huynh, M Huynh-Dinh, T Idrisy, A Ingram, DR Inta, R Islas, G Isogai, T Ivanov, A Iyer, BR Izumi, K Jacobson, M Jang, H Jaranowski, P Ji, Y Jimenez-Forteza, F Johnson, WW Jones, DI Jones, R Jonker, RJG Ju, L Haris, K Kalmus, P Kalogera, V Kandhasamy, S Kang, G Kanner, JB Karlen, J Kasprzack, M Katsavounidis, E Katzman, W Kaufer, H Kaufer, S Kaur, T Kawabe, K Kawazoe, F Kefelian, F Keiser, GM Keitel, D Kelley, DB Kells, W Keppel, DG Khalaidovski, A Khalili, FY Khazanov, EA Kim, C Kim, K Kim, NG Kim, N Kim, S Kim, YM King, EJ King, PJ Kinzel, DL Kissel, JS Klimenko, S Kline, J Koehlenbeck, S Kokeyama, K Kondrashov, V Koranda, S Korth, WZ Kowalska, I Kozak, DB Kringel, V Krolak, A Kuehn, G Kumar, A Kumar, DN Kumar, P Kumar, R Kuo, L Kutynia, A Lam, PK Landry, M Lantz, B Larson, S Lasky, PD Lazzarini, A Lazzaro, C Leaci, P Leavey, S Lebigot, EO Lee, CH Lee, HK Lee, HM Lee, J Lee, PJ Leonardi, M Leong, JR Le Roux, A Leroy, N Letendre, N Levin, Y Levine, B Lewis, J Li, TGF Libbrecht, K Libson, A Lin, AC Littenberg, TB Lockerbie, NA Lockett, V Lodhia, D Loew, K Logue, J Lombardi, AL Lopez, E Lorenzini, M Loriette, V Lormand, M Losurdo, G Lough, J Lubinski, MJ Luck, H Lundgren, AP Ma, Y Macdonald, EP MacDonald, T Machenschalk, B MacInnis, M Macleod, DM Magana-Sandoval, F Magee, R Mageswaran, M Maglione, C Mailand, K Majorana, E Maksimovic, I Malvezzi, V Man, N Manca, GM Mandel, I Mandic, V Mangano, V Mangini, NM Mansell, G Mantovani, M Marchesoni, F Marion, F Marka, S Marka, Z Markosyan, A Maros, E Marque, J 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CA IceCube Collaboration LIGO Sci Collaboration Virgo Colla TI Multimessenger search for sources of gravitational waves and high-energy neutrinos: Initial results for LIGO-Virgo and IceCube SO PHYSICAL REVIEW D LA English DT Article ID GAMMA-RAY BURSTS; CORE-COLLAPSE SUPERNOVAE; MAGNETIZED NEUTRON-STARS; FOLLOW-UP OBSERVATIONS; ASTROPHYSICAL SOURCES; RELATIVISTIC STARS; MUON NEUTRINOS; GIANT FLARE; DETECTOR; ASTRONOMY AB We report the results of a multimessenger search for coincident signals from the LIGO and Virgo gravitational-wave observatories and the partially completed IceCube high-energy neutrino detector, including periods of joint operation between 2007-2010. These include parts of the 2005-2007 run and the 2009-2010 run for LIGO-Virgo, and IceCube's observation periods with 22, 59 and 79 strings. We find no significant coincident events, and use the search results to derive upper limits on the rate of joint sources for a range of source emission parameters. For the optimistic assumption of gravitational-wave emission energy of 10(-2) M(circle dot)c(2) at similar to 150 Hz with similar to 60 ms duration, and high-energy neutrino emission of 1051 erg comparable to the isotropic gamma-ray energy of gamma-ray bursts, we limit the source rate below 1.6 x 10(-2) Mpc(-3) yr(-1). We also examine how combining information from gravitational waves and neutrinos will aid discovery in the advanced gravitational-wave detector era. C1 [Auffenberg, J.; Bissok, M.; Blumenthal, J.; Gier, D.; Gretskov, P.; Haack, C.; Hallen, P.; Heinen, D.; Hellwig, D.; Jagielski, K.; Koob, A.; Kriesten, A.; Krings, K.; Leuermann, M.; Paul, L.; Penek, Oe.; Puetz, J.; Raedel, L.; Reimann, R.; Rongen, M.; Schoenen, S.; Schukraft, A.; Vehring, M.; Wallraff, M.; Wichary, C.; Wiebusch, C. H.; Zierke, S.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany. [Aartsen, M. G.; Hill, G. C.; Robertson, S.; Whelan, B. 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[Ballardin, G.; Bavigadda, V.; Canuel, B.; Carbognani, F.; Cavalieri, R.; Chiummo, A.; Cuoco, E.; Dattilo, V.; Day, R.; Ferrini, F.; Fiori, I.; Genin, E.; Hemming, G.; Kasprzack, M.; Marque, J.; Mohan, M.; Nocera, F.; Paoletti, F.; Pasqualetti, A.; Prijatelj, M.; Ruggi, P.; Sentenac, D.; Swinkels, B.] EGO, I-56021 Pisa, Italy. [Barker, D.; Barton, M. A.; Batch, J. C.; Clara, F.; Cook, D.; Dwyer, S.; Gray, C.; Hanks, J.; Ingram, D. R.; Izumi, K.; Kawabe, K.; Kissel, J. S.; Landry, M.; Levine, B.; Lubinski, M. J.; McCarthy, R.; Mendell, G.; Moraru, D.; Moreno, G.; Pele, A.; Raab, F. J.; Radkins, H.; Reed, C. M.; Ryan, K.; Sandberg, V.; Savage, R.; Sigg, D.; Thomas, P.; Vo, T.; Vorvick, C.; Weaver, B.; Wilkinson, C.; Worden, J.] LIGO Hanford Observ, Richland, WA 99352 USA. [Barr, B.; Bell, A. S.; Bell, C.; Campsie, P.; Craig, K.; Cumming, A.; Cunningham, L.; Davies, G. S.; Douglas, R.; Fan, X.; Gordon, N.; Graef, C.; Grant, A.; Hammond, G.; Hart, M.; Haughian, K.; Hendry, M.; Heng, I. 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RI Danilishin, Stefan/K-7262-2012; Khalili, Farit/D-8113-2012; Auffenberg, Jan/D-3954-2014; Gorodetsky, Michael/C-5938-2008; Gammaitoni, Luca/B-5375-2009; Koskinen, David/G-3236-2014; Prokhorov, Leonid/I-2953-2012; Gemme, Gianluca/C-7233-2008; Steinlechner, Sebastian/D-5781-2013; McClelland, David/E-6765-2010; Hild, Stefan/A-3864-2010; M, Manjunath/N-4000-2014; Maruyama, Reina/A-1064-2013; Vecchio, Alberto/F-8310-2015; Iyer, Bala R./E-2894-2012; Mow-Lowry, Conor/F-8843-2015; prodi, giovanni/B-4398-2010; Strigin, Sergey/I-8337-2012; Leonardi, Matteo/G-9694-2015; Aguilar Sanchez, Juan Antonio/H-4467-2015; Sigg, Daniel/I-4308-2015; Puppo, Paola/J-4250-2012; Tacca, Matteo/J-1599-2015; Graef, Christian/J-3167-2015; Bell, Angus/E-7312-2011; Ottaway, David/J-5908-2015; Garufi, Fabio/K-3263-2015; Deleglise, Samuel/B-1599-2015; Lam, Ping Koy/A-5276-2008; Neri, Igor/F-1482-2010; Aggarwal, Nancy/M-7203-2015; Shaddock, Daniel/A-7534-2011; Vicere, Andrea/J-1742-2012; Rocchi, Alessio/O-9499-2015; Martelli, Filippo/P-4041-2015; Branchesi, Marica/P-2296-2015; Gehring, Tobias/A-8596-2016; Tjus, Julia/G-8145-2012; Strain, Kenneth/D-5236-2011; Miao, Haixing/O-1300-2013; Heidmann, Antoine/G-4295-2016; Nelemans, Gijs/D-3177-2012; Sarkar, Subir/G-5978-2011; Marchesoni, Fabio/A-1920-2008; Zhu, Xingjiang/E-1501-2016; Frasconi, Franco/K-1068-2016; Groot, Paul/K-4391-2016; Lazzaro, Claudia/L-2986-2016; Pinto, Innocenzo/L-3520-2016; Ferrante, Isidoro/F-1017-2012; Beatty, James/D-9310-2011; Losurdo, Giovanni/K-1241-2014; Travasso, Flavio/J-9595-2016; Bartos, Imre/A-2592-2017; Punturo, Michele/I-3995-2012; Cella, Giancarlo/A-9946-2012; Wiebusch, Christopher/G-6490-2012; Cesarini, Elisabetta/C-4507-2017; Costa, Cesar/G-7588-2012; Chow, Jong/A-3183-2008; Frey, Raymond/E-2830-2016; Ciani, Giacomo/G-1036-2011; Di Virgilio, Angela Dora Vittoria/E-9078-2015; Sergeev, Alexander/F-3027-2017; Harms, Jan/J-4359-2012; Ward, Robert/I-8032-2014; Howell, Eric/H-5072-2014; Taavola, Henric/B-4497-2011; OI Danilishin, Stefan/0000-0001-7758-7493; Auffenberg, Jan/0000-0002-1185-9094; Gorodetsky, Michael/0000-0002-5159-2742; Gammaitoni, Luca/0000-0002-4972-7062; Koskinen, David/0000-0002-0514-5917; Gemme, Gianluca/0000-0002-1127-7406; Steinlechner, Sebastian/0000-0003-4710-8548; McClelland, David/0000-0001-6210-5842; M, Manjunath/0000-0001-8710-0730; Maruyama, Reina/0000-0003-2794-512X; Vecchio, Alberto/0000-0002-6254-1617; Iyer, Bala R./0000-0002-4141-5179; prodi, giovanni/0000-0001-5256-915X; Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Sigg, Daniel/0000-0003-4606-6526; Puppo, Paola/0000-0003-4677-5015; Tacca, Matteo/0000-0003-1353-0441; Graef, Christian/0000-0002-4535-2603; Bell, Angus/0000-0003-1523-0821; Garufi, Fabio/0000-0003-1391-6168; Deleglise, Samuel/0000-0002-8680-5170; Lam, Ping Koy/0000-0002-4421-601X; Neri, Igor/0000-0002-9047-9822; Shaddock, Daniel/0000-0002-6885-3494; Vicere, Andrea/0000-0003-0624-6231; Rocchi, Alessio/0000-0002-1382-9016; Martelli, Filippo/0000-0003-3761-8616; Gehring, Tobias/0000-0002-4311-2593; Strain, Kenneth/0000-0002-2066-5355; Miao, Haixing/0000-0003-4101-9958; Heidmann, Antoine/0000-0002-0784-5175; Nelemans, Gijs/0000-0002-0752-2974; Sarkar, Subir/0000-0002-3542-858X; Marchesoni, Fabio/0000-0001-9240-6793; Zhu, Xingjiang/0000-0001-7049-6468; Frasconi, Franco/0000-0003-4204-6587; Groot, Paul/0000-0002-4488-726X; Lazzaro, Claudia/0000-0001-5993-3372; Ferrante, Isidoro/0000-0002-0083-7228; Beatty, James/0000-0003-0481-4952; Losurdo, Giovanni/0000-0003-0452-746X; Travasso, Flavio/0000-0002-4653-6156; Punturo, Michele/0000-0001-8722-4485; Cella, Giancarlo/0000-0002-0752-0338; Wiebusch, Christopher/0000-0002-6418-3008; Cesarini, Elisabetta/0000-0001-9127-3167; Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Ciani, Giacomo/0000-0003-4258-9338; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Rott, Carsten/0000-0002-6958-6033; Aulbert, Carsten/0000-0002-1481-8319; Ter-Antonyan, Samvel/0000-0002-5788-1369; Schukraft, Anne/0000-0002-9112-5479; Groh, John/0000-0001-9880-3634; Larsen, Dag Toppe/0000-0002-9898-2174; Swinkels, Bas/0000-0002-3066-3601; Denker, Timo/0000-0003-1259-5315; Drago, Marco/0000-0002-3738-2431; Ward, Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447; Dolique, Vincent/0000-0001-5644-9905; Whelan, John/0000-0001-5710-6576; O'Shaughnessy, Richard/0000-0001-5832-8517; Vedovato, Gabriele/0000-0001-7226-1320; Howell, Eric/0000-0001-7891-2817; Boschi, Valerio/0000-0001-8665-2293; Matichard, Fabrice/0000-0001-8982-8418; Husa, Sascha/0000-0002-0445-1971; Papa, M.Alessandra/0000-0002-1007-5298; Vocca, Helios/0000-0002-1200-3917; Taavola, Henric/0000-0002-2604-2810; Pinto, Innocenzo M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200; Guidi, Gianluca/0000-0002-3061-9870; Collette, Christophe/0000-0002-4430-3703; Pierro, Vincenzo/0000-0002-6020-5521; Coccia, Eugenio/0000-0002-6669-5787; Vetrano, Flavio/0000-0002-7523-4296; Addesso, Paolo/0000-0003-0895-184X; Naticchioni, Luca/0000-0003-2918-0730; calloni, enrico/0000-0003-4819-3297; Scott, Jamie/0000-0001-6701-6515; Sorazu, Borja/0000-0002-6178-3198; Stuver, Amber/0000-0003-0324-5735; Bondu, Francois/0000-0001-6487-5197; Zweizig, John/0000-0002-1521-3397; Del Pozzo, Walter/0000-0003-3978-2030; Gendre, Bruce/0000-0002-9077-2025; Allen, Bruce/0000-0003-4285-6256; Granata, Massimo/0000-0003-3275-1186; Perez de los Heros, Carlos/0000-0002-2084-5866; Kanner, Jonah/0000-0001-8115-0577; Freise, Andreas/0000-0001-6586-9901; Strotjohann, Nora Linn/0000-0002-4667-6730; Mandel, Ilya/0000-0002-6134-8946; Whiting, Bernard F/0000-0002-8501-8669; Murphy, David/0000-0002-8538-815X; Pitkin, Matthew/0000-0003-4548-526X; Veitch, John/0000-0002-6508-0713; Davies, Gareth/0000-0002-4289-3439; Arguelles Delgado, Carlos/0000-0003-4186-4182 FU United States National Science Foundation; Science and Technology Facilities Council of the United Kingdom; Max-Planck-Society; State of Niedersachsen/Germany; Australian Research Council; International Science Linkages program of the Commonwealth of Australia; Council of Scientific and Industrial Research of India; Istituto Nazionale di Fisica Nucleare of Italy; Spanish Ministerio de Economia y Competitividad; Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears; Foundation for Fundamental Research on Matter - Netherlands Organisation for Scientific Research; Polish Ministry of Science and Higher Education; FOCUS Programme of Foundation for Polish Science; Royal Society; Scottish Funding Council; Scottish Universities Physics Alliance; National Aeronautics and Space Administration; Hungarian Scientific Research Fund; Lyon Institute of Origins (LIO); National Research Foundation of Korea, Industry Canada; Province of Ontario through the Ministry of Economic Development and Innovation; National Science and Engineering Research Council Canada; Carnegie Trust, the Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation; Alfred P. Sloan Foundation; U.S. National Science Foundation-Office of Polar Programs; U.S. National Science Foundation-Physics Division; University of Wisconsin Alumni Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin, Madison; Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy; National Energy Research Scientific Computing Center; Louisiana Optical Network Initiative (LONI) grid computing resources; Natural Sciences and Engineering Research Council of Canada; WestGrid and Compute/Calcul Canada; Swedish Research Council; Swedish Polar Research Secretariat; Swedish National Infrastructure for Computing (SNIC); Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF); Deutsche Forschungsgemeinschaft (DFG); Helmholtz Alliance for Astroparticle Physics (HAP); Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO Odysseus programme; Flanders Institute to encourage scientific and technological research in industry (IWT); Belgian Federal Science Policy Office (Belspo); University of Oxford, U.K.; Marsden Fund, New Zealand; Japan Society for Promotion of Science (JSPS); Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF); Danish National Research Foundation, Denmark (DNRF) FX The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector, and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Economia y Competitividad, the Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, Hungarian Scientific Research Fund, 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 National Science and Engineering Research Council Canada, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation. This article has LIGO document number LIGO-P1400046. We acknowledge the support from the following agencies: U.S. National Science Foundation-Office of Polar Programs, U.S. National Science Foundation-Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin, Madison; the Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; Natural Sciences and Engineering Research Council of Canada, WestGrid and Compute/Calcul Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); University of Oxford, U.K.; Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF); Danish National Research Foundation, Denmark (DNRF). NR 138 TC 8 Z9 8 U1 4 U2 63 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD NOV 17 PY 2014 VL 90 IS 10 AR UNSP 102002 DI 10.1103/PhysRevD.90.102002 PG 22 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AU6CY UT WOS:000345691400001 ER PT J AU Hagos, S Feng, Z Burleyson, CD Lim, KSS Long, CN Wu, D Thompson, G AF Hagos, Samson Feng, Zhe Burleyson, Casey D. Lim, Kyo-Sun Sunny Long, Charles N. Wu, Di Thompson, Greg TI Evaluation of convection-permitting model simulations of cloud populations associated with the Madden-Julian Oscillation using data collected during the AMIE/DYNAMO field campaign SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE dynamo; cold pools; s-pol radar; cloud permitting; tropical convection; Madden-Julian oscillation ID MICROPHYSICS PARAMETERIZATION; PART I; RESOLVING MODEL; CLIMATE MODELS; RADAR; PRECIPITATION; ORGANIZATION; EXPLICIT; SCHEME; SNOW AB Regional convection-permitting model simulations of cloud populations observed during the 2011 Atmospheric Radiation Measurement (ARM) Madden-Julian Oscillation Investigation Experiment/Dynamics of the Madden-Julian Oscillation Experiment (AMIE/DYNAMO) field campaign are evaluated against ground-based radar and ship-based observations. Sensitivity of model simulated reflectivity, surface rain rate, and cold pool statistics to variations of raindrop breakup/self-collection parameters in four state-of-the-art two-moment bulk microphysics schemes in the Weather Research and Forecasting (WRF) model is examined. The model simulations generally overestimate reflectivity from large and deep convective cells, and underestimate stratiform rain and the frequency of cold pools. In the sensitivity experiments, introduction of more aggressive raindrop breakup or decreasing the self-collection efficiency increases the cold pool occurrence frequency in all of the simulations, and slightly reduces the reflectivity and precipitation statistics bias in some schemes but has little effect on the overall mean surface precipitation. Both the radar observations and model simulations of cloud populations show an approximate power law relationship between convective echo-top height and equivalent convective cell radius. C1 [Hagos, Samson; Feng, Zhe; Burleyson, Casey D.; Lim, Kyo-Sun Sunny; Long, Charles N.] Pacific NW Natl Lab, Richland, WA 99352 USA. [Wu, Di] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Processes Lab, Greenbelt, MD 20771 USA. [Wu, Di] Sci Syst & Applicat Inc, Lanham, MD USA. [Thompson, Greg] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. RP Hagos, S (reprint author), Pacific NW Natl Lab, Richland, WA 99352 USA. EM samson.hagos@pnnl.gov RI Lim, Kyo-Sun/I-3811-2012; Burleyson, Casey/F-1833-2016; Feng, Zhe/E-1877-2015 OI Burleyson, Casey/0000-0001-6218-9361; Feng, Zhe/0000-0002-7540-9017 FU Office of Biological and Environmental Research of the U.S. Department of Energy (DOE) as part of the Regional and Global Climate Modeling Program; Office of Biological and Environmental Research of the U.S. Department of Energy (DOE) as part of the Atmospheric System Research Program; DOE by Battelle Memorial Institute [DE-AC06-76RLO 1830] FX The authors thank Yun Qian for his comments and suggestions. The data for this paper are available at NCAR's Earth Observing Laboratory's DYNAMO Data Catalogue https://www.eol.ucar.edu/field_projects/dynamo. The data set names are, R/V Roger Revelle Flux, Near-Surface Meteorology, and Navigation Data and S-PolKa Radar, fully corrected, merged, final moments data in cfRadial format. The S-Polka data were regridded by Stacy Brodzik (brodzik@atmos.washington.edu) at the University of Washington. This research is based on work supported by the Office of Biological and Environmental Research of the U.S. Department of Energy (DOE) as part of the Regional and Global Climate Modeling Program and Atmospheric System Research Program. Computing resources for the simulations are provided by the National Energy Research Scientific Computing Center (NERSC) and Oak Ridge Leadership Computing Facility (OLCF). The Pacific Northwest National Laboratory is operated for DOE by Battelle Memorial Institute under contract DE-AC06-76RLO 1830. NR 39 TC 11 Z9 11 U1 2 U2 6 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 NOV 16 PY 2014 VL 119 IS 21 BP 12052 EP 12068 DI 10.1002/2014JD022143 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AU6EQ UT WOS:000345696600031 ER PT J AU Halekas, JS Poppe, AR McFadden, JP Angelopoulos, V Glassmeier, KH Brain, DA AF Halekas, J. S. Poppe, A. R. McFadden, J. P. Angelopoulos, V. Glassmeier, K. -H. Brain, D. A. TI Evidence for small-scale collisionless shocks at the Moon from ARTEMIS SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SOLAR-WIND; LUNAR; THEMIS; PERTURBATIONS; MAGNETOMETER; INSTRUMENT; FIELDS; WAVE AB ARTEMIS observes structures near the Moon that display many properties commonly associated with collisionless shocks, including a discontinuity with downstream compression of magnetic field and density, heating and wave activity, and velocity deflections away from the Moon. The two-probe ARTEMIS measurements show that these features do not exist in the pristine solar wind and thus must result from lunar influences. Discontinuity analyses indicate mass flux and heating across the boundary, with the normal velocity dropping from supermagnetosonic to submagnetosonic across the discontinuity. The shock location with respect to crustal magnetic fields suggests a causal relationship, implying that solar wind protons reflected from crustal fields may produce the observed structures. These observations may indicate some of the smallest shocks in the solar system (in terms of plasma scales), driven by solar wind interaction with magnetic fields on the order of the ion gyroradius and inertial length. C1 [Halekas, J. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Poppe, A. R.; McFadden, J. P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Halekas, J. S.; Poppe, A. R.; Brain, D. A.] NASA Ames Res Ctr, Solar Syst Explorat Res Virtual Inst, Moffett Field, CA USA. [Angelopoulos, V.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA USA. [Glassmeier, K. -H.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterrestr Physik, D-38106 Braunschweig, Germany. [Brain, D. A.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. RP Halekas, JS (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. EM jasper-halekas@uiowa.edu OI Halekas, Jasper/0000-0001-5258-6128 FU Solar System Exploration Research Virtual Institute [SSERVI-2014-225]; NASA [NAS5-02099]; German Ministry for Economy and Energy; German Center for Aviation and Space (DLR) [50 OC 1001] FX We thank the Solar System Exploration Research Virtual Institute for supporting this study (SSERVI-2014-225). We acknowledge NASA contract NAS5-02099 for the use of ARTEMIS data and specifically J.W. Bonnell and F.S. Mozer for the EFI data and A. Roux and O. LeContel for the SCM data. All ARTEMIS data are publicly available at http://artemis.ssl.berkeley.edu and NASA's CDAWeb. K.H.G. was financially supported through the German Ministry for Economy and Energy and the German Center for Aviation and Space (DLR) under contract 50 OC 1001. NR 24 TC 4 Z9 4 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD NOV 16 PY 2014 VL 41 IS 21 BP 7436 EP 7443 DI 10.1002/2014GL061973 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AU3MT UT WOS:000345518300004 ER PT J AU Lambert, FH Taylor, PC AF Lambert, F. Hugo Taylor, Patrick C. TI Regional variation of the tropical water vapor and lapse rate feedbacks SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID GENERAL-CIRCULATION MODEL; OCEAN-ATMOSPHERE MODEL; CLIMATE FEEDBACKS; WARMING CONTRAST; TROPOSPHERIC ADJUSTMENT; RELATIVE-HUMIDITY; MEAN RESPONSE; PRECIPITATION; SIMULATIONS; TEMPERATURE AB The global and tropical mean water vapor and lapse rate radiative feedbacks are anticorrelated across contemporary climate models. Hence, despite substantial uncertainty in both, uncertainty in total clear-sky modeled radiative feedback is small compared with other sources of feedback spread. Previous work has demonstrated that no such correlation exists when grid point water vapor and lapse rate feedbacks are considered within one model. Here we show that robust physical processes nevertheless determine significant aspects of both the water vapor and particularly the lapse rate feedbacks within the tropics. The lapse rate feedback increases with surface temperature change because the tropical troposphere cannot maintain strong temperature gradients. The water vapor feedback increases weakly with surface temperature over tropical ocean but slightly decreases over land, associated with moisture availability. Water vapor feedback is more strongly related to precipitation changes, increasing most strongly in the heaviest precipitating regions and least in the weakest. C1 [Lambert, F. Hugo] Univ Exeter, Coll Engn Math & Phys Sci, Exeter, Devon, England. [Taylor, Patrick C.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Lambert, FH (reprint author), Univ Exeter, Coll Engn Math & Phys Sci, Exeter, Devon, England. EM f.h.lambert@exeter.ac.uk RI Taylor, Patrick/D-8696-2015 OI Taylor, Patrick/0000-0002-8098-8447 FU NERC PROBEC [NE/K016016/1] FX We thank Masakazu Yoshimori and Tokuta Yokohata for providing MIROC3.2 data (contact NIES, Japan), earthsystemgrid.org and PCMDI for CCSM3 data, Mark Webb for HadSM3 and QUMP data (contact the Met Office), Angus Ferraro for helpful discussions, and two anonymous reviewers for reviews that helped improve the manuscript. F.H.L. was partly supported by the NERC PROBEC project NE/K016016/1. NR 48 TC 3 Z9 3 U1 2 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD NOV 16 PY 2014 VL 41 IS 21 BP 7634 EP 7641 DI 10.1002/2014GL061987 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AU3MT UT WOS:000345518300030 ER PT J AU Yingst, RA Mest, SC Berman, DC Garry, WB Williams, DA Buczkowski, D Jaumann, R Pieters, CM De Sanctis, MC Frigeri, A Le Corre, L Preusker, E Raymond, CA Reddy, V Russell, CT Roatsch, T Schenk, PM AF Yingst, R. A. Mest, S. C. Berman, D. C. Garry, W. B. Williams, D. A. Buczkowski, D. Jaumann, R. Pieters, C. M. De Sanctis, M. C. Frigeri, A. Le Corre, L. Preusker, E. Raymond, C. A. Reddy, V. Russell, C. T. Roatsch, T. Schenk, P. M. TI Geologic mapping of Vesta SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Dawn; Vesta; Geologic mapping ID ASTEROID 4 VESTA; HUBBLE-SPACE-TELESCOPE; SOLAR-SYSTEM; DARK MATERIAL; PARENT BODY; 21 LUTETIA; IMPACT; DAWN; SURFACE; IMAGES AB We report on a preliminary global geologic map of Vesta, based on data from the Dawn spacecraft's HighAltitude Mapping Orbit (HAMO) and informed by Low-Altitude Mapping Orbit (LAMO) data. This map is part of an iterative mapping effort; the geologic map has been refined with each improvement in resolution. Vesta has a heavily-cratered surface, with large craters evident in numerous locations. The south pole is dominated by an impact structure identified before Dawn's arrival. Two large impact structures have been resolved: the younger, larger Rheasilvia structure, and the older, more degraded Veneneia structure. The surface is also characterized by a system of deep, globe-girdling equatorial troughs and ridges, as well as an older system of troughs and ridges to the north. Troughs and ridges are also evident cutting across, and spiraling arcuately from, the Rheasilvia central mound. However, no volcanic features have been unequivocally identified. Vesta can be divided very broadly into three terrains: heavily-cratered terrain; ridge-and-trough terrain (equatorial and northern); and terrain associated with the Rheasilvia crater. Localized features include bright and dark material and ejecta (some defined specifically by color); lobate deposits; and mass-wasting materials. No obvious volcanic features are evident. Stratigraphy of Vesta's geologic units suggests a history in which formation of a primary crust was followed by the formation of impact craters, including Veneneia and the associated Saturnalia Fossae unit. Formation of Rheasilvia followed, along with associated structural deformation that shaped the Divalia Fossae ridge-and-trough unit at the equator. Subsequent impacts and mass wasting events subdued impact craters, rims and portions of ridge-and-trough sets, and formed slumps and landslides, especially within crater floors and along crater rims and scarps. Subsequent to the formation of Rheasilvia, discontinuous low-albedo deposits formed or were emplaced; these lie stratigraphically above the equatorial ridges that likely were formed by Rheasilvia. The last features to be formed were craters with bright rays and other surface mantling deposits. Executed progressively throughout data acquisition, the iterative mapping process provided the team with geologic proto-units in a timely manner. However, interpretation of the resulting map was hampered by the necessity to provide the team with a standard nomenclature and symbology early in the process. With regard to mapping and interpreting units, the mapping process was hindered by the lack of calibrated mineralogic information. Topography and shadow played an important role in discriminating features and terrains, especially in the early stages of data acquisition. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Yingst, R. A.; Mest, S. C.; Berman, D. C.; Garry, W. B.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Williams, D. A.] Arizona State Univ, Tempe, AZ 85287 USA. [Buczkowski, D.] JHU APL, Laurel, MD USA. [Jaumann, R.; Preusker, E.; Roatsch, T.] DLR, Inst Planetary Res, Berlin, Germany. [Pieters, C. M.] Brown Univ, Providence, RI 02912 USA. [De Sanctis, M. C.; Frigeri, A.] Natl Inst Astrophys, Bologna, Italy. [Le Corre, L.; Reddy, V.] Max Planck Inst Solar Syst Res, Gottingen, Germany. [Raymond, C. A.] CALTECH, NASA JPL, Pasadena, CA 91125 USA. [Russell, C. T.] Univ Calif Los Angeles, Los Angeles, CA 90024 USA. [Schenk, P. M.] LPI, Houston, TX USA. RP Yingst, RA (reprint author), Planetary Sci Inst, 1700 E Ft Lowell,Suite 106, Tucson, AZ 85719 USA. EM yingst@psi.edu RI Frigeri, Alessandro/F-2151-2010; OI Frigeri, Alessandro/0000-0002-9140-3977; De Sanctis, Maria Cristina/0000-0002-3463-4437; Reddy, Vishnu/0000-0002-7743-3491; Le Corre, Lucille/0000-0003-0349-7932 FU NASA Dawn at Vesta Participating Scientist Program Grant [NNX1OAR19G]; Italian Space Agency (ASI) [1/004112/0] FX The authors are grateful to Corey Fortezzo, Trent Hare, Jenny Blue and other personnel at USGS for their invaluable discussions and for creating the ArcGIS base materials that greatly simplified the mapping process. Thanks go especially to the Dawn operations, engineering and science team. The authors also gratefully acknowledge the insightful comments of Drs. Jim Zimbelman and Jim Skinner, whose reviews greatly improved this manuscript. This work was funded through NASA Dawn at Vesta Participating Scientist Program Grant NNX1OAR19G to RAY. Italian co-authors were funded through the Italian Space Agency (ASI) Grant 1/004112/0. NR 75 TC 10 Z9 10 U1 1 U2 7 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 NOV 15 PY 2014 VL 103 BP 2 EP 23 DI 10.1016/j.pss.2013.12.014 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU2UD UT WOS:000345472000002 ER PT J AU Williams, DA O'Brien, DP Schenk, PM Denevi, BW Carsenty, U Marchi, S Scully, JEC Jaumann, R De Sanctis, MC Palomba, E Ammannito, E Longobardo, A Magni, G Frigeri, A Russell, CT Raymond, CA Davison, TM AF Williams, David A. O'Brien, David P. Schenk, Paul M. Denevi, Brett W. Carsenty, Uri Marchi, Simone Scully, Jennifer E. C. Jaumann, Ralf De Sanctis, Maria Cristina Palomba, Ernesto Ammannito, Eleonora Longobardo, Andrea Magni, Gianfranco Frigeri, Alessandro Russell, Christopher T. Raymond, Carol A. Davison, Thomas M. CA Dawn Sci Team TI Lobate and flow-like features on asteroid Vesta SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Asteroids; Vesta; Dawn; Impact cratering ID IMPACT MELT; DARK MATERIAL; CONSTRAINTS; CRATERS; DIOGENITES; EUCRITES; SURFACE; ORIGIN; IMAGES; CORE AB We studied high-resolution images of asteroid Vesta's surface (similar to 70 and 20-25 m/pixel) obtained during the High-and Low-Altitude Mapping Orbits (HAMO, LAMO) of NASA's Dawn mission to assess the formation mechanisms responsible for a variety of lobate, flow-like features observed across the surface. We searched for evidence of volcanic flows, based on prior mathematical modeling and the well-known basaltic nature of Vesta's crust, but no unequivocal morphologic evidence of ancient volcanic activity has thus far been identified. Rather, we find that all lobate, flow-like features on Vesta appear to be related either to impact or erosional processes. Morphologically distinct lobate features occur in and around impact craters, and most of these are interpreted as impact ejecta flows, or possibly flows of impact melt. Estimates of melt production from numerical models and scaling laws suggests that large craters like Marcia (similar to 60 km diameter) could have potentially produced impact melt volumes ranging from tens of millions of cubic meters to a few tens of cubic kilometers, which are relatively small volumes compared to similar-sized lunar craters, but which are consistent with putative impact melt features observed in Dawn images. There are also examples of lobate flows that trend downhill both inside and outside of crater rims and basin scarps, which are interpreted as the result of gravity-driven mass movements (slumps and landslides). (C) 2013 Elsevier Ltd. All rights reserved. C1 [Williams, David A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [O'Brien, David P.] Planetary Sci Inst, Tucson, AZ USA. [Schenk, Paul M.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Denevi, Brett W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Carsenty, Uri; Jaumann, Ralf] German Aerosp Ctr DLR, Berlin, Germany. [Marchi, Simone] NASA Lunar Sci Inst, Boulder, CO USA. [Scully, Jennifer E. C.; Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [De Sanctis, Maria Cristina; Palomba, Ernesto; Ammannito, Eleonora; Longobardo, Andrea; Magni, Gianfranco; Frigeri, Alessandro] Natl Inst Astrophys INAF, Rome, Italy. [Raymond, Carol A.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. [Davison, Thomas M.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. RP Williams, DA (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. EM David.Williams@asu.edu RI Denevi, Brett/I-6502-2012; Frigeri, Alessandro/F-2151-2010; OI Denevi, Brett/0000-0001-7837-6663; Frigeri, Alessandro/0000-0002-9140-3977; Davison, Thomas/0000-0001-8790-873X; De Sanctis, Maria Cristina/0000-0002-3463-4437; Palomba, Ernesto/0000-0002-9101-6774 FU NASA; NASA Dawn at Vesta Participating Scientists Program [NNX1OAR24, GNNX10AR21G] FX We thank Catherine Neish and Matteo Massironi for very helpful reviews that improved the quality of this paper. We would like to thank the Dawn Flight Team for their tireless work operating the spacecraft and returning the data used in this study: We also thank the Framing Camera teams at the Max Planck Institute (Katlenberg-Lindau) and the German Aerospace Center (DLR) and the VIR team at the National Institute of Astrophysics (Rome) for their work process the Dawn data. This work was funded by NASA through the Discovery Program and Dawn Project Office at the Jet Propulsion Laboratory, and by the NASA Dawn at Vesta Participating Scientists Program through grant NNX1OAR24G to DAW and grant NNX10AR21G to DPO. NR 65 TC 12 Z9 12 U1 2 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD NOV 15 PY 2014 VL 103 BP 24 EP 35 DI 10.1016/j.pss.2013.06.017 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU2UD UT WOS:000345472000003 ER PT J AU Krohn, K Jaumann, R Elbeshausen, D Kneissl, T Schmedemann, N Wagner, R Voigt, J Otto, K Matz, KD Preusker, F Roatsch, T Stephan, K Raymond, CA Russell, CT AF Krohn, K. Jaumann, R. Elbeshausen, D. Kneissl, T. Schmedemann, N. Wagner, R. Voigt, J. Otto, K. Matz, K. D. Preusker, F. Roatsch, T. Stephan, K. Raymond, C. A. Russell, C. T. TI Asymmetric craters on Vesta: Impact on sloping surfaces SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Vesta; Asymmetrical craters; Impact modeling; Crater formation on small bodies; Cratering; Processes ID INNER SOLAR-SYSTEM; COLLISIONAL HISTORY; FLOW SPEEDS; TARGETS; DISTRIBUTIONS; SIMULATIONS; MORPHOLOGY; DYNAMICS; VOLUME; BELT AB Cratering processes on planetary bodies happen continuously and cause the formation of a large variety of impact crater morphologies. On Vesta whose surface has been imaged at high resolution during a 14 months orbital mission by the Dawn spacecraft we identified a substantial number of craters with an asymmetrical shape. These craters, in total a number of 2892 ranging in diameter from 0.3 km to 43 km, are characterized by a sharp crater rim on the uphill side and a smooth one on the downhill side. The formation of these unusual asymmetric impact craters is controlled by Vesta's remarkable topographic relief. In order to understand the processes creating such unusual crater forms on a planetary body with a topography like Vesta we carried out the following work packages: (1) the asymmetric craters show various morphologies and therefore can be subdivided into distinct classes by their specific morphologic details; (2) using a digital terrain model (DTM), the craters are grouped into bins of slope angles for further statistical analysis; (3) for a subset of these asymmetric craters, the size-frequency distributions of smaller craters superimposed on their crater floors and continuous ejecta are measured in order to derive cratering model ages for the selected craters and to constrain possible post-impact processes; (4) three-dimensional hydrocode simulations using the iSALE-3D code are applied to the data set in order to quantify the effects of topography on crater shape and ejecta distribution. We identified five different classes (A-E) of asymmetric craters. Primarily, we focus on class A in this work. The global occurrence of these crater classes compared with a slope map clearly shows that these asymmetric crater types exclusively form on slopes. We found that slopes, especially slopes > 20, prevent the deposition of ejected material in the uphill direction, and slumping material superimposed the deposit of ejecta on the downhill side. The combination of these two processes explains the local accumulation of material in this direction. In the subset of asymmetric craters which we used for crater counts, our results show that no post-impact processes have taken place since floors and continuous ejecta in each crater show comparable cratering model ages within the uncertainties of the cratering chronology model. Therefore the formation, or modification, of the asymmetric crater forms by processes other than impact can be excluded with some certainty. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Krohn, K.; Jaumann, R.; Wagner, R.; Voigt, J.; Otto, K.; Matz, K. D.; Preusker, F.; Roatsch, T.; Stephan, K.] German Aerosp Ctr DLR, Inst Planetary Res, Berlin, Germany. [Jaumann, R.; Kneissl, T.; Schmedemann, N.] Free Univ Berlin, Inst Geosci Planetol & Remote Sensing, Berlin, Germany. [Elbeshausen, D.] Leibniz Inst Evolut & Biodiversitatsforsch, Museum Naturkunde, Berlin, Germany. [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys, Los Angeles, CA USA. RP Krohn, K (reprint author), German Aerosp Ctr DLR, Inst Planetary Res, Berlin, Germany. EM Katrin.Krohn@dlr.de FU Helmholtz-Gemeinschaft Deutscher Forschungszentren (HGF) FX We thank the Dawn team for the development, cruise, orbital insertion, and operations of the Dawn spacecraft at Vesta. Dawn data are archived with the NASA Planetary Data System. D. Elbeshausen has been 'supported by the Helmholtz-Alliance HA-203/"Planetary Evolution and Life" by the Helmholtz-Gemeinschaft Deutscher Forschungszentren (HGF). NR 57 TC 5 Z9 5 U1 2 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD NOV 15 PY 2014 VL 103 BP 36 EP 56 DI 10.1016/j.pss.2014.04.011 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU2UD UT WOS:000345472000004 ER PT J AU Vincent, JB Schenk, P Nathues, A Sierks, H Hoffmann, M Gaskell, RW Marchi, S O'Brien, DP Sykes, M Russell, CT Fulchignoni, M Kellerg, HU Raymond, C Palmer, E Preusker, F AF Vincent, J. -B. Schenk, P. Nathues, A. Sierks, H. Hoffmann, M. Gaskell, R. W. Marchi, S. O'Brien, D. P. Sykes, M. Russell, C. T. Fulchignoni, M. Kellerg, H. U. Raymond, C. Palmer, E. Preusker, F. TI Crater depth-to-diameter distribution and surface properties of (4) vesta SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Vesta; Asteroid; Craters morphology ID ASTEROID 433 EROS; IMPACT; MORPHOLOGY; GEOLOGY; DAWN AB Orbiting asteroid (4) Vesta from July 2011 to August 2012, the Framing Camera on board the Dawn spacecraft has acquired several tens of thousand images of the asteroid surface, revealing a complex landscape. The topography is dominated by craters of all sizes and shapes, from fresh, simple, bowlshaped craters to giant basins, as seen in the southern hemisphere. Craters of different ages or states of degradation can be seen all over the surface; some have very sharp rims and simple morphology, whereas others are highly eroded and have sometimes been filled by landslides and ejecta from nearby craters. The general depth/Diameter (d/D) distribution on Vesta is similar to what has been observed on other small rocky objects in the Solar System with a distribution peaking at 0.168 +/- 0.01 in the range 0.05-0.35. However, the global map of d/D reveals important geographic variations across the surface, unlike any other asteroid. The northern most regions of Vesta show d/D values comparable to other asteroid surfaces, with a mean d/D of 0.15 +/- 0.01, and a steep cumulative distribution. Craters in the regions affected by the giant southern impacts are deeper (mean d/D =0.19 +/- 0.01) and show less erosion. It can be interpreted as the southern surface being younger than the rest of the asteroid, or made of a material which either allows the formation of deeper features or prevents their erosion. This picture is consistent with the idea of a southern Vestan hemisphere resurfaced relatively recently by the giant impact that created the Rheasilvia basin. The analysis of depth-to-Diameter variations over the whole surface also brings some insight into the transition regions between different cratering regimes: about 20 km for the strength-to-gravity dominated regime, and 38 km for the beginning of the simple-tocomplex transition. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Vincent, J. -B.; Nathues, A.; Sierks, H.; Hoffmann, M.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Schenk, P.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Gaskell, R. W.; O'Brien, D. P.; Sykes, M.; Palmer, E.] Planetary Sci Inst, Tucson, AZ USA. [Marchi, S.] NASA Lunar Sci Inst, Boulder, CO USA. [Russell, C. T.] Univ Calif Los Angeles, Los Angeles, CA USA. [Fulchignoni, M.] Observ Paris, LESIA, Paris, France. [Kellerg, H. U.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, Braunschweig, Germany. [Raymond, C.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Preusker, F.] Deutsch Zentrum Luft & Raumfahrt, Berlin, Germany. RP Vincent, JB (reprint author), Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. EM vincent@mps.mpg.de NR 33 TC 8 Z9 9 U1 0 U2 9 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 NOV 15 PY 2014 VL 103 BP 57 EP 65 DI 10.1016/j.pss.2013.09.003 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU2UD UT WOS:000345472000005 ER PT J AU Schroder, SE Mottola, S Keller, HU Raymond, CA Russell, CT AF Schroeder, S. E. Mottola, S. Keller, H. U. Raymond, C. A. Russell, C. T. TI Resolved photometry of Vesta reveals physical properties of crater regolith (Reprinted from vol 85, pg 198-213, 2014) SO PLANETARY AND SPACE SCIENCE LA English DT Reprint DE Vesta; Photometry; Regolith; Surface; Reflectance; Space weathering ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; PARTICULATE SURFACES; GALILEO PHOTOMETRY; SCATTERING; DAWN; METEORITES; ASTEROIDS; ANALOGS; IMPACT; MOON AB During its year-long orbital mission, the Dawn spacecraft has mapped the surface of main-belt asteroid Vesta multiple times at different spatial resolutions and illumination and viewing angles. The onboard Framing Camera has acquired thousands of clear filter and narrow band images, which, with the availability of high-resolution global shape models, allows for a photometric characterization of the surface in unprecedented detail. We analyze clear filter images to retrieve the photometric properties of the regolith. In the first part of the paper we evaluate different photometric models for the global average. In the second part we use these results to study variations in albedo and steepness of the phase curve over the surface. Maps of these two photometric parameters show large scale albedo variations, which appear to be associated with compositional differences. They also reveal the location of photometrically extreme terrains, where the phase curve is unusually shallow or steep. We find that shallow phase curves are associated with steep slopes on crater walls and faults, as calculated from a shape model. On the other hand, the phase curve of ejecta associated with young impact craters is steep. We interpret these variations in phase curve slope in terms of physical roughness of the regolith. The lack of rough ejecta around older craters suggests that initially rough ejecta associated with impact craters on Vesta are smoothed over a relatively short time of several tens of Myr. We propose that this process is the result of impact gardening, and as such represents a previously unrecognized aspect of Vesta space weathering (Pieters et al., 2012). If this type of space weathering is common, we may expect to encounter this photometric phenomenon on other main belt asteroids. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Schroeder, S. E.; Mottola, S.] Deutsch Zentrum Luft & Raumfahrt DLR, D-12489 Berlin, Germany. [Keller, H. U.] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany. [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. RP Schroder, SE (reprint author), Deutsch Zentrum Luft & Raumfahrt DLR, D-12489 Berlin, Germany. EM stefanus.schroeder@dlr.de NR 48 TC 3 Z9 3 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD NOV 15 PY 2014 VL 103 BP 66 EP 81 DI 10.1016/j.pss.2014.08.001 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU2UD UT WOS:000345472000006 ER PT J AU Marchi, S Bottke, WF O'Brien, DP Schenk, P Mottola, S De Sanctis, MC Kring, DA Williams, DA Raymond, CA Russell, CT AF Marchi, S. Bottke, W. F. O'Brien, D. P. Schenk, P. Mottola, S. De Sanctis, M. C. Kring, D. A. Williams, D. A. Raymond, C. A. Russell, C. T. TI Small crater populations on Vesta SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Asteroid (4) Vesta; Asteroid cratering; Asteroid evolution; Main belt asteroids ID MAIN ASTEROID BELT; INNER SOLAR-SYSTEM; INDUCED SEISMIC ACTIVITY; NEAR-EARTH ASTEROIDS; COLLISIONAL HISTORY; IMPACT; SIZE; DISTRIBUTIONS; METEORITES; EVOLUTION AB The NASA Dawn mission has extensively examined the surface of asteroid Vesta, the second most massive body in the main belt. The high quality of the gathered data provides us with a unique opportunity to determine the surface and internal properties of one of the most important and intriguing main belt asteroids (MBAs). In this paper, we focus on the size frequency distributions (SFDs) of sub-kilometer impact craters observed at high spatial resolution on several selected young terrains on Vesta. These small crater populations offer an excellent opportunity to determine the nature of their asteroidal precursors (namely MBAs) at sizes that are not directly observable from ground-based telescopes (i.e., below similar to 100 m diameter). Moreover, unlike many other MBA surfaces observed by spacecraft thus far, the young terrains examined had crater spatial densities that were far from empirical saturation. Overall, we find that the cumulative power-law index (slope) of small crater SFDs on Vesta is fairly consistent with predictions derived from current collisional and dynamical models down to a projectile size of similar to 10 m diameter (e.g., Bottke et al., 2005a, b). The shape of the impactor SFD for small projectile sizes does not appear to have changed over the last several billions of years, and an argument can be made that the absolute number of small MBAs has remained roughly constant (within a factor of 2) over the same time period. The apparent steady state nature of the main belt population potentially provides us with a set of intriguing constraints that can be used to glean insights into the physical evolution of individual MBAs as well as the main belt as an ensemble. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Marchi, S.; Bottke, W. F.] Southwest Res Inst, NASA Lunar Sci Inst, Boulder, CO 80302 USA. [O'Brien, D. P.] Planetary Sci Inst, Tucson, AZ USA. [Schenk, P.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Mottola, S.] DLR Berlin, Inst Planetenforsch, Berlin, Germany. [De Sanctis, M. C.] Ist Nazl Astrofis, Rome, Italy. [Marchi, S.; Kring, D. A.] USRA Lunar & Planetary Inst, NASA Lunar Sci Inst, Houston, TX USA. [Williams, D. A.] Arizona State Univ, Tempe, AZ USA. [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Russell, C. T.] Univ Calif Los Angeles, Los Angeles, CA USA. RP Marchi, S (reprint author), Southwest Res Inst, NASA Lunar Sci Inst, Boulder, CO 80302 USA. EM marchi@boulder.swri.edu OI De Sanctis, Maria Cristina/0000-0002-3463-4437 FU NASA Lunar Science Institute (Center for Lunar Origin and Evolution at the Southwest Research Institute in Boulder, Colorado NASA) [NNA09DB32A]; NASA Lunar Science Institute (Center for Lunar Science and Exploration at the Lunar and Planetary Institute in Houston, Texas) FX We thank Nadine G. Barlow and an anonymous referee for valuable comments that improved the manuscript. D.P. O'Brien thanks NASA's Dawn at Vesta Participating Scientist Program. The contributions of Simone Marchi, William F. Bottke and David A. Kring were supported by the NASA Lunar Science Institute (Center for Lunar Origin and Evolution at the Southwest Research Institute in Boulder, Colorado NASA Grant NNA09DB32A; Center for Lunar Science and Exploration at the Lunar and Planetary Institute in Houston, Texas). NR 61 TC 5 Z9 5 U1 1 U2 7 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 NOV 15 PY 2014 VL 103 BP 96 EP 103 DI 10.1016/j.pss.2013.05.005 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU2UD UT WOS:000345472000008 ER PT J AU Schmedemann, N Kneissl, T Ivanov, BA Michael, GG Wagner, RJ Neukum, G Ruesch, O Hiesinger, H Krohn, K Roatsch, T Preusker, F Sierks, H Jaumann, R Reddy, V Nathues, A Walter, SHG Neesemann, A Raymond, CA Russell, CT AF Schmedemann, N. Kneissl, T. Ivanov, B. A. Michael, G. G. Wagner, R. J. Neukum, G. Ruesch, O. Hiesinger, H. Krohn, K. Roatsch, T. Preusker, F. Sierks, H. Jaumann, R. Reddy, V. Nathues, A. Walter, S. H. G. Neesemann, A. Raymond, C. A. Russell, C. T. TI The cratering record, chronology and surface ages of (4) Vesta in comparison to smaller asteroids and the ages of HED meteorites SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Vesta; Crater retention ages; Cratering chronology; Crater scaling; Rheasilvia; Veneneia ID TERMINAL LUNAR CATACLYSM; LATE HEAVY BOMBARDMENT; INNER SOLAR-SYSTEM; SIZE-FREQUENCY DISTRIBUTION; FRAMING CAMERA IMAGES; MAIN-BELT; TERRESTRIAL PLANETS; 21 LUTETIA; DYNAMICAL EVOLUTION; COLLISIONAL HISTORY AB We derived model functions for the crater production size-frequency distribution and chronology of the asteroids 951 Gaspra, 243 Ida, 21 Lutetia and 4 Vesta, based on a lunar-like crater production function and a lunar-like chronology with a smooth exponential decay in impact rate for the first similar to 1 Ga of Solar System history. For Gaspra, Ida and Lutetia we find surface ages roughly in agreement with published data. Using the same approach for Vesta leads to results with high correlation to Ar-Ar reset ages of HED meteorites, for which a strong dynamical and spectroscopic connection to Vesta has been found. In contrast to recently published young formation ages of the Rheasilvia and Veneneia basins of about 1 and 2 Ga, respectively, we find for Rheasilvia a formation age of 3.5 +/- 0.1 Ga and for the Veneneia formation a lower limit of 3.7 +/- 0.1 Ga. For comparison we also give surface model ages for a preliminary version of a chronology (pers. comm. D.P. O'Brien) based on the Late Heavy Bombardment theory. Error bars presented in our work stem only from statistical analysis of measured crater distributions and do not include the uncertainty of the used chronology model. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Schmedemann, N.; Kneissl, T.; Michael, G. G.; Neukum, G.; Jaumann, R.; Walter, S. H. G.; Neesemann, A.] Free Univ Berlin, Inst Geol Sci, D-12249 Berlin, Germany. [Ivanov, B. A.] Inst Dynam Geospheres, Moscow, Russia. [Wagner, R. J.; Krohn, K.; Roatsch, T.; Preusker, F.; Jaumann, R.] German Aerosp Ctr DLR, Inst Planetary Res, Berlin, Germany. [Ruesch, O.; Hiesinger, H.] Univ Munster, Inst Planetol, D-48149 Munster, Germany. [Sierks, H.; Nathues, A.] Max Planck Inst Solar Syst Res MPS, Gottingen, Germany. [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Reddy, V.] Planetary Sci Inst, Tucson, AZ 85719 USA. RP Schmedemann, N (reprint author), Free Univ Berlin, Inst Geol Sci, 74-100 Bldg D, D-12249 Berlin, Germany. EM nico.schmedemann@fu-berlin.de; thomas.kneissl@fu-berlin.de; boris_a_ivanov@mail.ru; gregory.michael@fu-berlin.de; roland.wagner@dlr.de; gerhard.neukum@fu-berlin.de; ottaviano.ruesch@uni-muenster.de; hiesinger@uni-muenster.de; katrin.krohn@dlr.de; Thomas.Roatsch@dlr.de; Frank.Preusker@dlr.de; sierks@mps.mpg.de; Ralf.jaumann@dlr.de; reddy@psi.edu; nathues@mps.mpg.de; sebastian.walter@fu-berlin.de; adrian.neesemann@fu-berlin.de; carol.a.raymond@jpl.nasa.gov; ctrussel@igpp.ucla.edu RI Ivanov, Boris/E-1413-2016; OI Ivanov, Boris/0000-0002-9938-9428; Reddy, Vishnu/0000-0002-7743-3491 FU German Space Agency (DLR) of Federal Ministry of Economics and Technology [50OW1101, 50QM1301] FX This work has been supported by the German Space Agency (DLR) on behalf of the Federal Ministry of Economics and Technology, grants 50OW1101 (NS, TK, AN) and 50QM1301 (GM). We thank D.P. O'Brien for providing his preliminary solution for a vestan chronology based on the Late Heavy Bombardment model. We would like to thank the Dawn Flight Team for their work operating the spacecraft and returning the data used in this study. We also thank the Framing Camera team at the Max Planck Institute for Solar System Research and the German Aerospace Center (DLR) for processing the Dawn data and Sharon Ui for proofreading. We thank the anonymous reviewer and C. R. Chapman for their constructive comments. NR 143 TC 13 Z9 13 U1 1 U2 9 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 NOV 15 PY 2014 VL 103 BP 104 EP 130 DI 10.1016/j.pss.2014.04.004 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU2UD UT WOS:000345472000009 ER PT J AU O'Brien, DP Marchi, S Morbidelli, A Bottke, WF Schenk, PM Russell, CT Raymond, CA AF O'Brien, David P. Marchi, Simone Morbidelli, Alessandro Bottke, William F. Schenk, Paul M. Russell, Christopher T. Raymond, Carol A. TI Constraining the cratering chronology of Vesta SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Vesta; Asteroids; Impact Cratering; Impact Chronology ID LATE HEAVY BOMBARDMENT; INNER SOLAR-SYSTEM; MAIN-BELT ASTEROIDS; EARTH-MOON SYSTEM; LUNAR CATACLYSM; SIZE DISTRIBUTION; PRIMORDIAL EXCITATION; COLLISIONAL HISTORY; PARENT BODY; RB-SR AB Vesta has a complex cratering history, with ancient terrains as well as recent large impacts that have led to regional resurfacing. Crater counts can help constrain the relative ages of different units on Vesta's surface, but converting those crater counts to absolute ages requires a chronology function. We present a cratering chronology based on the best current models for the dynamical evolution of asteroid belt, and calibrate it to Vesta using the record of large craters on its surface. While uncertainties remain, our chronology function is broadly consistent with an ancient surface of Vesta as well as other constraints such as the bombardment history of the rest of the inner Solar System and the Ar-Ar age distribution of howardite, eucrite and diogenite (HED) meteorites from Vesta. (C) 2014 Elsevier Ltd. All rights reserved. C1 [O'Brien, David P.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Marchi, Simone; Bottke, William F.] Southwest Res Inst, NASA Lunar Sci Inst, Boulder, CO USA. [Morbidelli, Alessandro] CNRS, Observ Cote Azur, F-06034 Nice, France. [Schenk, Paul M.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP O'Brien, DP (reprint author), Planetary Sci Inst, 1700 E Ft Lowell,Suite 106, Tucson, AZ 85719 USA. EM obrien@psi.edu FU NASA's Dawn at Vesta Participating Scientist Program [NNX10AR21G] FX D.P. O'Brien is supported by Grant NNX10AR21G from NASA's Dawn at Vesta Participating Scientist Program. The Dawn mission to asteroid Vesta and dwarf planet Ceres is managed by J.P.L., for NASA's Science Mission Directorate, Washington, DC. UCLA is responsible for overall Dawn mission science. We thank David Minton and an anonymous referee for their helpful reviews and comments. NR 97 TC 8 Z9 8 U1 1 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD NOV 15 PY 2014 VL 103 BP 131 EP 142 DI 10.1016/j.pss.2014.05.013 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU2UD UT WOS:000345472000010 ER PT J AU Brouet, Y Levasseur-Regourd, AC Encrenaz, P Gulkis, S AF Brouet, Y. Levasseur-Regourd, A. C. Encrenaz, P. Gulkis, S. TI Permittivity of porous granular matter, in relation with Rosetta cometary mission SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Rosetta mission; MIRO; Cometary nuclei; Permittivity; Porous matter ID INTERNAL STRUCTURE; 67P/CHURYUMOV-GERASIMENKO; DUST; INSTRUMENT; NUCLEUS; RADAR; MODEL; MILLIMETER; 1P/HALLEY; MIRO AB We report measurements in laboratory conditions of the relative complex permittivity (hereafter permittivity) of porous material on a large range of frequencies from 50 MHz to 190 GHz. Such measurements, developed in preparation of the Rosetta mission to comet 67P/Churyumov-Gerasimenko, specifically for the MIRO radiometric experiment, were obtained with different instrumentations in three frequency bands: 50-500 MHz, 2.45 - 12 GHz and 190 GHz (center-band frequency of the millimeter receiver of MIRO, specially developed for our purpose). Considering the expected properties of cometaly nuclei, they were carried out with porous granular materials of volcanic origin, with various sizes ranging from a few to 500 mu m, i.e. Etna's ashes and NASA JSC Mars-1 martian soil simulant. The samples were split into several sub-samples with different size ranges and bulk densities. The real part and the imaginary part of the permittivity remain respectively in the 2.1 - 4.0 range and in the 0.05 - 0.31 range. Volume scattering becomes significant for the measurements at 190 GHz when the mean grain size of sub-samples is greater than about 200 mu m and implies an increase of the real part and the imaginary part of the permittivity. Without this effect, for any sub-sample, the results are consistent over the frequency range. From 50 MHz to 190 GHz, evidence is provided for a slight decrease of the real part of the permittivity. Bulk densities of the sub-samples, being in the 800-1300 kg m(-3) range, were determined during the measurements at 190 GHz. Taking into account the expected bulk density of the nucleus (100-370 kg m(-3)), as well as temperature for the surface and subsurface (in the 30-300 K range) and its composition (consisting both of silica-rich dust and ices, mostly of water), these first series of results allow an estimate of the real part and the imaginary part of the permittivity of the near-surface of the cometary nucleus: the real part is likely to be lower than 1.6 for non-icy regions and lower than 1.4 for icy regions: the imaginary part is likely to be below 0.09. These estimates represent upper limits relevant for the interpretation of the future data of MIRO. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Brouet, Y.; Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Levasseur-Regourd, A. C.] Univ Paris 06, UMR 8190, LATMOS CNRS, F-75005 Paris, France. [Gulkis, S.] CALTECH, JPL, Pasadena, CA 91109 USA. RP Brouet, Y (reprint author), Observ Paris, LERMA, 61 Ave Observ, F-75014 Paris, France. EM yann.brouet@obspm.fr FU CNES; Universite Pierre et Marie Curie FX Support from CNES is acknowledged, as well as support from Universite Pierre et Marie Curie. We warmly acknowledge Valerie Ciarletti from the LATMOS laboratory (Paris, France) who gave us the Etna's ashes and Michel Cabane from the LATMOS laboratory who allowed us to make measurements on the JSC Mars-1 simulant sample. We also acknowledge Gilles Ruffle and Fabrice Bonnaudin from the IMS laboratory (Bordeaux, France) and Maurice Gheudin, Gerard Beaudin, Patrice Landry, Jean-Marie Munier and Michele Batrung from the LERMA laboratory (Paris, France) for their support to the measurements. We warmly thank Stefano Bertone (University of Bern, Switzerland) for his useful comments. We acknowledge the MIRO Team for its support to this work. And finally we acknowledge Jacques Thibieroz from the Sisyphe laboratory (Paris, France) for his support to the samples characterization. NR 32 TC 6 Z9 6 U1 2 U2 9 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 NOV 15 PY 2014 VL 103 BP 143 EP 152 DI 10.1016/j.pss.2014.08.012 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU2UD UT WOS:000345472000011 ER PT J AU Kereszturi, A Gobi, S AF Kereszturi, Akos Gobi, Sandor TI Possibility of H2O2 decomposition in thin liquid films on Mars SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Mars; Water; Oxidant; Regolith ID MARTIAN DUST DEVILS; HYDROGEN-PEROXIDE; INTERFACIAL WATER; MERIDIANI-PLANUM; OXIDANT ENHANCEMENT; LOW-LATITUDES; SURFACE; ICE; EVOLUTION; SOIL AB In this work the pathways and possibilities of H2O2 decomposition on Mars in microscopic liquid interfacial water were analyzed by kinetic calculations. Thermal and photochemical driven decomposition, just like processes catalyzed by various metal oxides, is too slow compared to the annual duration while such microscopic liquid layers exist on Mars today, to produce substantial decomposition. The most effective analyzed process is catalyzed by Fe ions, which could decompose H2O2 under pH <4.5 with a half life of 1-2 days. This process might be important during volcanically influenced periods when sulfur release produces acidic pH, and rotational axis tilt change driven climatic changes also influence the volatile circulation and spatial occurrence just like the duration of thin liquid layer. Under current conditions, using the value of 200 K as the temperature in interfacial water (at the southern hemisphere), and applying Phoenix lander's wet chemistry laboratory results, the pH is not favorable for Fe mobility and this kind of decomposition. Despite current conditions (especially pH) being unfavorable for H2O2 decomposition, microscopic scale interfacial liquid water still might support the process. By the reaction called heterogeneous catalysis, without acidic pH and mobile Fe, but with minerals surfaces containing Fe decomposition of H2O2 with half life of 20 days can happen. This duration is still longer but not several orders than the existence of springtime interfacial liquid water on Mars today. This estimation is relevant for activation energy controlled reaction rates. The other main parameter that may influence the reaction rate is the diffusion speed. Although the available tests and theoretical calculations do not provide firm values for the diffusion speed in such a "2-dimensional" environment, using relevant estimations this parameter in the interfacial liquid layer is smaller than in bulk water. But the 20 days' duration mentioned above is still relevant, as the activation energy driven reaction rate is the main limiting factor in the decomposition and not the diffusion speed. The duration of dozen(s) days is still longer but not with orders of magnitude than the expected duration for the existence of springtime interfacial liquid water on Mars today. The results suggest such decomposition may happen today, however, because of our limited knowledge on chemical processes in thin interfacial liquid layers, this possibility waits for confirmation and also points to the importance of conducting laboratory tests to validate the possible process. Although some tests were already realized for diffusion in an almost 2-dimensional liquid, the same is not true for activation energy, where only the value from the "normal" measurements was applied. Even if H2O2 decomposition is too slow today, the analysis of such a process is important, as under volcanic influence more effective decomposition might take place in thin interfacial liquids close to the climate of today if released sulfur produces pH <4.5. Large quantity and widespread occurrence of bulk liquid phase are not expected in the Amazonian period, but interfacial liquid water probably appeared regularly, and its locations, especially during volcanically active periods, might make certain sites than others more interesting for astrobiology with the lower concentration of oxidizing H2O2. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Kereszturi, Akos; Gobi, Sandor] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Thege Miklos Astron Inst, H-1121 Budapest, Hungary. [Kereszturi, Akos] NASA, Astrobiol Inst, TDE Focus Grp, Washington, DC USA. RP Kereszturi, A (reprint author), Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Thege Miklos Astron Inst, Konkoly Thege M 15-17, H-1121 Budapest, Hungary. EM kereszturi.akos@csfk.mta.hu RI Gobi, Sandor/A-2048-2015 FU OTKA; ESA ECS Co. [4000105405, 98076]; COST TD Projects [1308] FX This research work was realized under the Astrophysical and Geochemical Laboratory's activity at the Research Center for Astronomy and Earth Sciences, Hungary. The water-related issues of this work were supported by the OTKA PD 105970 fund, and the surface composition-related issues by the ESA ECS Co. 4000105405 (No. 98076) and COST TD 1308 Projects. NR 154 TC 4 Z9 4 U1 3 U2 29 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 NOV 15 PY 2014 VL 103 BP 153 EP 166 DI 10.1016/j.pss.2014.07.017 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU2UD UT WOS:000345472000012 ER PT J AU Jagota, S Kawai, J Deamer, D McKay, C Khare, B Beeler, D AF Jagota, Seema Kawai, Jun Deamer, David McKay, Christopher Khare, Bishun Beeler, David TI Surface-active substances in a laboratory simulated Titan's organic haze: Prebiotic microstructures SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Surface-active substances; Prebiotic; Self-assembled structures; Langmuir-Blodgett ID MURCHISON CARBONACEOUS CHONDRITE; CHEMISTRY; THOLINS; ACIDS; COMPONENTS; MONOLAYERS AB Titan, the largest satellite of Saturn, is a key planetary body for astrobiological studies due to its active organic chemistry, hydrocarbon lakes and possible subsurface water-ammonia liquids. We have investigated the physicochemical properties of organic compounds synthesized in a simulated Titan atmosphere. A laboratory analog of Titan's aerosols, called tholin, was produced by irradiation of a nitrogen/methane gas mixture. The primary aim was to determine whether tholin represent possible sources of surface-active substances that could have been involved in the formation of prebiotic structures. A tholin sample was extracted with chloroform-methanol and the chloroform soluble material was separated by two-dimensional thin layer chromatography. Fluorescence excited by UV light was used to identify the major components on the plates. After being scraped from the TLC plate, the components were eluted as specific fractions and investigated by surface chemical methods, FTIR, scanning electron microscopy and cyclic voltammetry. Fractions 1 and 2 were strongly fluorescent and surface active, producing films at air-water interfaces. When exposed to aqueous phases, components in fraction 1 form spherical microstructures resembling prebionts. The prebionts are precursor structures that might have evolved into the first living cells. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Jagota, Seema; McKay, Christopher; Khare, Bishun; Beeler, David] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Kawai, Jun] Yokohama Natl Univ, Dept Chem & Biotechnol, Hodogaya Ku, Yokohama, Kanagawa 2408501, Japan. [Deamer, David] Univ Calif Santa Cruz, Jack Baskin Sch Engn, Santa Cruz, CA 95064 USA. RP Jagota, S (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM seema.ames@gmail.com NR 19 TC 3 Z9 3 U1 1 U2 22 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 NOV 15 PY 2014 VL 103 BP 167 EP 173 DI 10.1016/j.pss.2014.09.003 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU2UD UT WOS:000345472000013 ER PT J AU Bouquet, A Baratoux, D Vaubaillon, J Gritsevich, MI Mimoun, D Mousis, O Bouley, S AF Bouquet, Alexis Baratoux, David Vaubaillon, Jeremie Gritsevich, Maria I. Mimoun, David Mousis, Olivier Bouley, Sylvain TI Simulation of the capabilities of an orbiter for monitoring the entry of interplanetary matter into the terrestrial atmosphere SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Meteors; Photometry ID CANADIAN CAMERA NETWORK; INNISFREE METEORITE; FIREBALL NETWORK; MISSION; RADIATION; BOLIDES; SCIENCE; PHYSICS; MOTION; EARTH AB In comparison with existing ground-based camera networks for meteors monitoring, a space-based optical system would escape dependency on weather and atmospheric conditions and would offer a wide spatial coverage and an unrestricted and extinction-free spectral domain. The potential rates of meteor detections by such systems are evaluated in this paper as a function of observations parameters (optical system capabilities, orbital parameters) and considering a reasonable range of meteoroids properties (e.g., mass, velocity, composition) determining their luminosity. A numerical tool called SWARMS (Simulator for Wide Area Recording of Meteors from Space) has been developed. SWARMS is also intended to be used in an operational phase to facilitate the comparison of observations with up-do-date constraints on the flux and characteristics of the interplanetary matter entering our planet's atmosphere. The laws governing the conversion of a fraction of the meteor kinetic energy into radiation during atmospheric entry have been revisited and evaluated based on an analysis of previously published meteor trajectories. Rates of detection were simulated for two different systems: the SPOSH (Smart Panoramic Optical Sensor Head) camera optimized for the observation of transient luminous events, and the JEM-EUSO (Japanese Experiment Module-Extreme Universe Space Observatory) experiment on the ISS (International Space Station). We conclude that up to 6 events per hour in the case of SPOSH, and up to 0.67 events in the case of JEM-EUSO may be detected. The optimal orbit for achieving such rates of detections depends on the mass index of the meteoroid populations. The determination of this parameter appears therefore critical before an optimal orbiting system might be designed for meteors monitoring. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Bouquet, Alexis] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX 78249 USA. [Bouquet, Alexis] Southwest Res Inst, Space Sci & Engn Div, San Antonio, TX USA. [Bouquet, Alexis; Baratoux, David] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Bouquet, Alexis; Mousis, Olivier] Univ Franche Comte, Inst UTINAM, CNRS INSU, Observ Sci Univers Besancon,UMR 6213, F-25030 Besancon, France. [Vaubaillon, Jeremie; Bouley, Sylvain] Inst Mecan Celeste & Calcul Ephemerides, UMR8028, F-75014 Paris, France. [Gritsevich, Maria I.] Finnish Geodet Inst, Masala, Finland. [Gritsevich, Maria I.] Ural Fed Univ, Inst Phys & Technol, Dept Phys Methods & Devices Qual Control, Ekaterinburg, Russia. [Gritsevich, Maria I.] Russian Acad Sci, Dorodnicyn Comp Ctr, Dept Computat Phys, Moscow, Russia. [Mimoun, David] Univ Toulouse, Inst Super Aeronaut & Espace, Toulouse, France. [Mimoun, David] Jet Prop Lab, Pasadena, CA USA. [Bouley, Sylvain] Univ Paris 11, CNRS, Lab IDES, UMR 8148, F-91405 Orsay, France. RP Bouquet, A (reprint author), Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX 78249 USA. EM alexis.bouquet@gmail.com RI MIMOUN, DAVID/M-7074-2016; Gritsevich, Maria/M-7311-2016 OI MIMOUN, DAVID/0000-0002-3427-2974; Gritsevich, Maria/0000-0003-4268-6277 FU CNES through the grant for the project METEOR; Partenariat Hubert Curien [MA/11/257]; IPPW Student Organizing Committee; Academy of Finland FX This research has been funded by CNES through the grant for the project METEOR. The Partenariat Hubert Curien MA/11/257 is also acknowledged for supporting the presentation of this work to OISA 2013 at Marrakech. IPPW Student Organizing Committee is acknowledged for supporting presentation of this work at IPPW 10. Maria Gritsevich is supported by the Academy of Finland. Thanks to Daria Kuznetsova and to two anonymous reviewers for useful corrections and comments. NR 33 TC 7 Z9 7 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD NOV 15 PY 2014 VL 103 BP 238 EP 249 DI 10.1016/j.pss.2014.09.001 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU2UD UT WOS:000345472000020 ER PT J AU El-Maarry, MR Heggy, E Dohm, JM AF El-Maarry, M. R. Heggy, E. Dohm, J. M. TI Radar investigations of Apollinaris Mons on Mars: Exploring the origin of the fan deposits SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Mars; Radar; Volcanology; Geomorphology ID ORBITER LASER ALTIMETER; FLUVIAL MEGAFANS; FORELAND BASIN; EVOLUTION; ERUPTION; ASH; SUBSURFACE; CHRONOLOGY; DISPERSAL; VOLCANOS AB Apollinaris Mons is an isolated volcano on Mars straddling the boundary between the southern highlands and the northern plains. One of its most distinctive features is its massive fan-shaped deposit that extends from a breach on its summit to distances of more than 150 km and drapes its entire southern flank. The composition and formation mechanism of these deposits remains controversial. We investigate the radar properties of the fan deposits (FD) of Apollinaris Mons using low-frequency sounding radar data in combination with high-resolution images and crater-size frequency analysis to constrain their inner shape and bulk composition. Our analysis indicates that the FD attains an irregular thickness and is gradually thinner towards their lateral margins. The crater-size frequency analysis shows that they may have undergone repeated resurfacing, which is suggestive of long-term evolution. Our analysis of Shallow Radar (SHARAD) radargrams traversing different sections of the FD reveals multiple and different subsurface interfaces among the radargrams crossing the thinnest part, which suggests a layered and complex inner shape. Our estimates for the bulk real part of the dielectric constant of the FD ranges from 3 to 5, which is consistent with an icy-silicate mixture or pyroclastic composition. Therefore, we conclude that lahars or pyroclastic flows are the most likely mechanism that created the FD, yet we cannot rule out additional contributions from lava flows. A combination of multiple processes is also possible since the deposits appear to have been modified by fluvial processes at a later stage of their formation. (C) 2014 Elsevier Ltd. All rights reserved. C1 [El-Maarry, M. R.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Heggy, E.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Dohm, J. M.] Tokyo Inst Technol, Earth Life Sci Inst, Meguro Ku, Tokyo, Japan. RP El-Maarry, MR (reprint author), Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland. EM mohamed.elmaarry@space.unibe.ch OI EL-MAARRY, MOHAMED RAMY/0000-0002-8262-0320 FU MPG-IMPRS Grant; Swiss National Science Foundation (SNSF); Berne University Research Foundation; NASA's Planetary Geology and Geophysics Program [NNXZ08AKA2G]; Earth-Life Science Institute FX The authors would like to thank Dr. Roberto Orosei and Dr. Nicholas Lang for their constructive reviews and inputs to this manuscript. M.R. El-M was initially supported by an MPG-IMPRS Grant and later a Swiss National Science Foundation (SNSF) grant. Parts of this research were additionally funded by the Berne University Research Foundation. JMD was supported by both NASA's Planetary Geology and Geophysics Program and the Earth-Life Science Institute. EH was supported in part by NASA Planetary Geology and Geophysics Program under Grant NNXZ08AKA2G. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 48 TC 0 Z9 0 U1 0 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD NOV 15 PY 2014 VL 103 BP 262 EP 272 DI 10.1016/j.pss.2014.09.007 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU2UD UT WOS:000345472000022 ER PT J AU Krot, AN Nagashima, K Wasserburg, GJ Huss, GR Papanastassiou, D Davis, AM Hutcheon, ID Bizzarro, M AF Krot, Alexander N. Nagashima, Kazuhide Wasserburg, Gerald J. Huss, Gary R. Papanastassiou, Dimitri Davis, Andrew M. Hutcheon, Ian D. Bizzarro, Martin TI Calcium-aluminum-rich inclusions with fractionation and unknown nuclear effects (FUN CAIs): I. Mineralogy, petrology, and oxygen isotopic compositions SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID UNUSUAL ALLENDE INCLUSION; EARLY SOLAR-SYSTEM; REFRACTORY INCLUSIONS; CARBONACEOUS CHONDRITES; PROTOPLANETARY DISK; MELILITE CRYSTALS; TRACE-ELEMENT; CV3 CHONDRITE; HETEROGENEOUS DISTRIBUTION; CAAL2SI2O8 POLYMORPHS AB We present a detailed characterization of the mineralogy, petrology, and oxygen isotopic compositions of twelve FUN CAIs, including C1 and EK1-4-1 from Allende (CV), that were previously shown to have large isotopic fractionation patterns for magnesium and oxygen, and large isotopic anomalies of several elements. The other samples show more modest patterns of isotopic fractionation and have smaller but significant isotopic anomalies. All FUN CAIs studied are coarse-grained igneous inclusions: Type B, forsterite-bearing Type B, compact Type A, and hibonite-rich. Some inclusions consist of two mineralogically distinct lithologies, forsterite-rich and forsterite-free/poor. All the CV FUN CAIs experienced postcrystallization open-system iron-alkali-halogen metasomatic alteration resulting in the formation of secondary minerals commonly observed in non-FUN CAIs from CV chondrites. The CR FUN CAI GG#3 shows no evidence for alteration. In all samples, clear evidence of oxygen isotopic fractionation was found. Most samples were initially O-16-rich. On a three-oxygen isotope diagram, various minerals in each FUN CAI (spinel, forsterite, hibonite, dmisteinbergite, most fassaite grains, and melilite (only in GG#3)), define mass-dependent fractionation lines with a similar slope of similar to 0.5. The different inclusions have different Delta O-17 values ranging from similar to-25 parts per thousand to similar to-16 parts per thousand. Melilite and plagioclase in the CV FUN CAIs have O-16-poor compositions (Delta O-17 similar to-3 parts per thousand) and plot near the intercept of the Allende CAI line and the terrestrial fractionation line. We infer that mass-dependent fractionation effects of oxygen isotopes in FUN CAI minerals are due to evaporation during melt crystallization. Differences in Delta O-17 values of mass-dependent fractionation lines defined by minerals in individual FUN CAIs are inferred to reflect differences in Delta O-17 values of their precursors. Differences in delta O-18 values of minerals defining the mass-dependent fractionation lines in several FUN CAIs are consistent with their inferred crystallization sequence, suggesting these minerals crystallized during melt evaporation. In other FUN CAIs, no clear correlation between delta O-18 values of individual minerals and their inferred crystallization sequence is observed, possibly indicating gas-melt back reaction and oxygen-isotope exchange in a O-16-rich gaseous reservoir. After oxygen-isotope fractionation, some FUN CAIs could have experienced partial melting and gas-melt oxygen-isotope exchange in a O-16-poor gaseous reservoir that resulted in crystallization of O-16-depleted fassaite, melilite and plagioclase. The final oxygen isotopic compositions of melilite and plagioclase in the CV FUN CAIs may have been established on the CV parent asteroid as a result of isotope exchange with a O-16-poor fluid during hydrothermal alteration. We conclude that FUN CAIs are part of a general family of refractory inclusions showing various degrees of fractionation effects due to evaporative processes superimposed on sampling of isotopically heterogeneous material. These processes have been experienced both by FUN and non-FUN igneous CAIs. Generally, the inclusions identified as FUN show larger isotope fractionation effects than non-FUN CAIs. There is a wide spread in UN isotopic anomalies in a large number of CAIs not exhibiting large fractionation effects in oxygen, magnesium, and silicon. The question of why some FUN CAIs show more extreme UN isotopic effects is attributed by us to limited sampling and not a special source of isotopically anomalous material. We consider the majority of igneous CAIs to be the result of several stages of thermal processing (evaporation, condensation, and melting) of aggregates of solid precursors composed of incompletely isotopically homogenized materials. The unknown nuclear effects in CAIs are common to both FUN and non-FUN CAIs, and are not a special characteristic of FUN inclusions but represent the spectrum of results from sampling a very heterogeneous medium in the accreting Solar System. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Krot, Alexander N.; Nagashima, Kazuhide; Wasserburg, Gerald J.; Huss, Gary R.] Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Wasserburg, Gerald J.; Papanastassiou, Dimitri] CALTECH, Lunat Asylum, Pasadena, CA 91125 USA. [Papanastassiou, Dimitri] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Davis, Andrew M.] Lawrence Livermore Natl Lab, Glenn Seaborg Inst, Livermore, CA 94551 USA. [Hutcheon, Ian D.] Univ Chicago, Enrico Fermi Inst, Dept Geophys Sci, Chicago, IL 60637 USA. [Hutcheon, Ian D.] Univ Chicago, Chicago Ctr Cosmochem, Chicago, IL 60637 USA. [Bizzarro, Martin] Univ Copenhagen, Ctr Star & Planet Format, Geol Museum, DK-1350 Copenhagen, Denmark. RP Krot, AN (reprint author), Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. EM sasha@higp.hawaii.edu RI Bizzarro, Martin/I-8701-2012 OI Bizzarro, Martin/0000-0001-9966-2124 FU NASA [NNX10AH76G, NNX12AJ01G, NNX08AG58G, NNH10AO48I]; Danish National Research Foundation [DNRF97] FX We thank Dr. Hisayoshi Yurimoto, the anonymous reviewer, and Dr. Sara S. Russell for useful comments and suggestions. Editorial handling of the manuscript by S. S. Russell is highly appreciated.. This work was supported by NASA grants NNX10AH76G and NNX12AJ01G (A. N. Krot, P. I.), NNX08AG58G (G. R. Huss, P. I.), and NNH10AO48I (I. D. Hutcheon, P. I.). The Centre for Star and Planet Formation is financed by the Danish National Research Foundation (Grant DNRF97). This is Hawai'i Institute of Geophysics and Planetology publication XXXX and School of Ocean and Earth Science and Technology publication XXXX. NR 110 TC 12 Z9 12 U1 3 U2 21 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD NOV 15 PY 2014 VL 145 BP 206 EP 247 DI 10.1016/j.gca.2014.09.027 PG 42 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AT4XO UT WOS:000344945800012 ER PT J AU Glaser, P Scholten, F De Rosa, D Figuera, RM Oberst, J Mazarico, E Neumann, GA Robinson, MS AF Glaeser, P. Scholten, F. De Rosa, D. Figuera, R. Marco Oberst, J. Mazarico, E. Neumann, G. A. Robinson, M. S. TI Illumination conditions at the lunar south pole using high resolution Digital Terrain Models from LOLA SO ICARUS LA English DT Article DE Moon, surface ID LANDING SITES; EXPLORATION; MISSION; LANDER; MOON; ICE AB The illumination conditions of the lunar south pole are investigated using a geometrically adjusted, 20 m/pixel Digital Terrain Model (DTM) from laser tracks of the Lunar Orbiter Laser Altimeter (LOLA). Several comparisons with Narrow Angle Camera (NAC) images have been made to cross-validate the results. Illumination conditions were first evaluated over a region of 20 x 20 km over a one-year period (October 22, 2018 - October 22, 2019) at surface level and 2 m above ground. Three potential landing sites are investigated in more detail. A 19-year study covering the lunar precessional cycle was carried out at surface level, 2 and 10 m above ground for a site found at "Connecting Ridge", the ridge connecting the Shackleton and de Gerlache crater. This area was found to be an ideal site for future landing missions with respect to illumination conditions. We identified locations receiving sunlight for 92.27% of the time at 2 m above ground and 95.65% of the time at 10 m above ground. At these locations the longest continuous periods in darkness are typically only 3-5 days. (C) 2014 Elsevier Inc. All rights reserved. C1 [Glaeser, P.; Figuera, R. Marco] Tech Univ Berlin, Dept Geodesy & Geoinformat Sci, D-10623 Berlin, Germany. [Scholten, F.; Oberst, J.] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany. [De Rosa, D.] European Space Agcy, Estec, NL-2200 AG Noordwijk, Netherlands. [Robinson, M. S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Mazarico, E.; Neumann, G. A.] NASA, Goddard Space Flight Ctr, Code 698, Greenbelt, MD 20771 USA. RP Glaser, P (reprint author), Tech Univ Berlin, Dept Geodesy & Geoinformat Sci, Str 17 Juni 135, D-10623 Berlin, Germany. EM philipp.glaeser@tu-berlin.de RI Neumann, Gregory/I-5591-2013; Mazarico, Erwan/N-6034-2014 OI Neumann, Gregory/0000-0003-0644-9944; Mazarico, Erwan/0000-0003-3456-427X FU German Research Foundation [FOR 1503, OB 124/8-1]; German Space Agency [FKZ 500W1202] FX P. Glaser was funded by a Grant of the German Research Foundation (FOR 1503, OB 124/8-1). Parts of this work were also supported by a Grant of the German Space Agency (FKZ 500W1202). We wish to thank the LOLA and LROC Science Team for releasing such great data products. NR 25 TC 3 Z9 3 U1 0 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD NOV 15 PY 2014 VL 243 BP 78 EP 90 DI 10.1016/j.icarus.2014.08.013 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT0OO UT WOS:000344635400008 ER PT J AU Hinson, DP Asmar, SW Kahan, DS Akopian, V Haberle, RM Spiga, A Schofield, JT Kleinbohl, A Abdou, WA Lewis, SR Paik, M Maalouf, SG AF Hinson, David P. Asmar, Sami W. Kahan, Daniel S. Akopian, Varoujan Haberle, Robert M. Spiga, Aymeric Schofield, John T. Kleinboehl, Armin Abdou, Wedad A. Lewis, Stephen R. Paik, Meegyeong Maalouf, Sami G. TI Initial results from radio occultation measurements with the Mars Reconnaissance Orbiter: A nocturnal mixed layer in the tropics and comparisons with polar profiles from the Mars Climate Sounder SO ICARUS LA English DT Article DE Mars, atmosphere; Mars, climate; Atmospheres, dynamics; Meteorology ID WATER ICE CLOUDS; CONVECTIVE BOUNDARY-LAYER; GENERAL-CIRCULATION MODEL; MIDDLE ATMOSPHERE; NORTHERN-HEMISPHERE; MARTIAN ATMOSPHERE; SURFACE PRESSURE; GLOBAL SURVEYOR; THERMAL TIDES; DUST STORMS AB The Mars Reconnaissance Orbiter (MRO) performs radio occultation (RO) measurements on selected orbits, generally once per day. We have retrieved atmospheric profiles from two subsets of data, yielding a variety of new results that illustrate the scientific value of the observations. One set of measurements sounded the tropics in northern summer at a local time similar to 1 h before sunrise. Some of these profiles contain an unexpected layer of neutral stability with a depth of similar to 4 km and a pressure at its upper boundary of similar to 160 Pa. The mixed layer is bounded above by a temperature inversion and below by another strong inversion adjacent to the surface. This type of structure is observed near Gale Crater, in the Tharsis region, and at a few other locations, whereas profiles in Amazonis Planitia and Elysium Planitia show no sign of a detached mixed layer with an overlying inversion. We supplemented the measurements with numerical simulations by the NASA Ames Mars General Circulation Model, which demonstrate that water ice clouds can generate this distinctive type of temperature structure through their influence on radiative transfer at infrared wavelengths. In particular, the simulations predict the presence of a nocturnal cloud layer in the Tharsis region at a pressure of similar to 150 Pa (similar to 10 km above the surface), and the nighttime radiative cooling at cloud level is sufficient to produce a temperature inversion above the cloud as well as convective instability below the cloud, consistent with the observations. The second set of measurements sounded mid-to-high northern latitudes in spring, when carefully coordinated observations by the MRO Mars Climate Sounder (MCS) are also available. The differences between the RO and MCS temperature profiles are generally consistent with the expected performance of the two instruments. Within this set of 21 comparisons the average temperature difference is less than 1 K where the aerosol opacities are smaller than 10(-3) km(-1), at pressures of 10-50 Pa, whereas it increases to similar to 2 K where the aerosol opacities exceed this threshold, at pressures of 50-300 Pa. The standard deviation of the temperature difference is similar to 2 K, independent of pressure. The second set of RO measurements also provides unique information about the stability of the annual CO2 cycle and the dynamics near the edge of the seasonal CO2 ice cap. (C) 2014 Elsevier Inc. All rights reserved. C1 [Hinson, David P.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Hinson, David P.] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA. [Asmar, Sami W.; Kahan, Daniel S.; Akopian, Varoujan; Schofield, John T.; Kleinboehl, Armin; Abdou, Wedad A.; Paik, Meegyeong; Maalouf, Sami G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Haberle, Robert M.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Spiga, Aymeric] UPMC, CNRS, IPSL, Lab Meteorol Dynam, F-75005 Paris, France. [Lewis, Stephen R.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. RP Hinson, DP (reprint author), SETI Inst, Carl Sagan Ctr, 189 Bernardo Ave, Mountain View, CA 94043 USA. EM dhinson@seti.org RI Spiga, Aymeric/O-4858-2014; OI Spiga, Aymeric/0000-0002-6776-6268; Lewis, Stephen/0000-0001-7237-6494 FU Mars Data Analysis Program [NNX12AL48G] FX This research was funded in part by Grant NNX12AL48G (Hinson) of the Mars Data Analysis Program. We are grateful to Reta Beebe, Jim Murphy, and Lyle Huber for their support and guidance in archiving the RO profiles at the PDS Atmospheres Node. NR 53 TC 4 Z9 4 U1 1 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD NOV 15 PY 2014 VL 243 BP 91 EP 103 DI 10.1016/j.icarus.2014.09.019 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT0OO UT WOS:000344635400009 ER PT J AU Anderson, CM Samuelson, RE Achterberg, RK Barnes, JW Flasar, FM AF Anderson, C. M. Samuelson, R. E. Achterberg, R. K. Barnes, J. W. Flasar, F. M. TI Subsidence-induced methane clouds in Titan's winter polar stratosphere and upper troposphere SO ICARUS LA English DT Article DE Titan, clouds; Atmosphere; Radiative transfer; Ices, IR spectroscopy ID ROTOTRANSLATIONAL ABSORPTION-SPECTRA; MOLECULAR SPECTROSCOPIC DATABASE; CASSINI RADIO OCCULTATIONS; ATMOSPHERE; PAIRS; DYNAMICS; TEMPERATURES; PROFILES; MODEL; HC3N AB Titan's atmospheric methane most likely originates from lakes at the surface and subsurface reservoirs. Accordingly, it has been commonly assumed that Titan's tropopause region, where the vertical temperature profile is a minimum, acts as a cold trap for convecting methane, leading to the expectation that the formation of methane clouds in Titan's stratosphere would be rare. The additional assumption that Titan's tropopause temperatures are independent of latitude is also required. However, Cassini Composite InfraRed Spectrometer (CIRS) and Radio Science Subsystem (RSS) data sets reveal colder temperatures in Titan's tropopause region near the winter pole than those at low latitudes and in the summer hemisphere. This, combined with the presence of a cross-equatorial meridional circulation with winter polar subsidence, as suggested by current general circulation models, implies the inevitable formation of Subsidence-Induced Methane Clouds (SIMCs) over Titan's winter pole. We verified this by retrieving the stratospheric methane mole fraction at 70 degrees N from the strength of the far infrared methane pure rotation lines observed by CIRS and by assuming the RSS-derived thermal profile at 74.1 degrees N. Our retrieved methane mole fraction of 1.50 +/- 0.15% allows for methane to condense and form SIMCs at altitudes between similar to 48 and similar to 20 km. Radiative transfer analyses of a color composite image obtained by the Cassini Visible and Infrared Mapping Spectrometer (VIMS) during northern winter appear to corroborate the existence of these clouds. Published by Elsevier Inc. C1 [Anderson, C. M.; Flasar, F. M.] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. [Samuelson, R. E.; Achterberg, R. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Barnes, J. W.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA. RP Anderson, CM (reprint author), NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. RI Flasar, F Michael/C-8509-2012; Barnes, Jason/B-1284-2009 OI Barnes, Jason/0000-0002-7755-3530 FU NASA FX The authors acknowledge funding support from NASA's Cassini Project and NASA's Cassini Data Analysis and Participating Scientist program. NR 46 TC 4 Z9 4 U1 0 U2 0 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 15 PY 2014 VL 243 BP 129 EP 138 DI 10.1016/j.icarus.2014.09.007 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT0OO UT WOS:000344635400012 ER PT J AU Hudson, RL Gerakines, PA Moore, MH AF Hudson, R. L. Gerakines, P. A. Moore, M. H. TI Infrared spectra and optical constants of astronomical ices: II. Ethane and ethylene SO ICARUS LA English DT Article DE Ices, IR spectroscopy; Trans-neptunian objects; Organic chemistry; Infrared observations ID CRYSTALLINE ACETYLENE; METHANE; PLUTO; INTENSITIES; ATMOSPHERE; TRITON; PHOTOCHEMISTRY; HYDROCARBONS; SPECTROSCOPY; IONOSPHERE AB Infrared spectroscopic observations have established the presence of hydrocarbon ices on Pluto and other TNOs, but the abundances of such molecules cannot be deduced without accurate optical constants (n, k) and reference spectra. In this paper we present our recent measurements of near- and mid-infrared optical constants for ethane (C2H6) and ethylene (C2H4) in multiple ice phases and at multiple temperatures. As in our recent work on acetylene (C2H2), we also report new measurements of the index of refraction of each ice at 670 nm. Comparisons are made to earlier work where possible, and electronic versions of our new results are made available. Published by Elsevier Inc. C1 [Hudson, R. L.; Gerakines, P. A.; Moore, M. H.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. RP Hudson, RL (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA. RI Gerakines, Perry/D-2226-2012 OI Gerakines, Perry/0000-0002-9667-5904 FU NASA; NASA Astrobiology Institute through the Goddard Center for Astrobiology FX NASA funding through the Outer Planets Research and Cassini Data Analysis programs is acknowledged. RLH and PAG received partial support from the NASA Astrobiology Institute through the Goddard Center for Astrobiology. Karen Smith (NPP, NASA-GSFC) is thanked for laboratory assistance. NR 34 TC 13 Z9 13 U1 0 U2 21 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 15 PY 2014 VL 243 BP 148 EP 157 DI 10.1016/j.icarus.2014.09.001 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT0OO UT WOS:000344635400014 ER PT J AU Hayne, PO McCord, TB Sotin, C AF Hayne, Paul O. McCord, Thomas B. Sotin, Christophe TI Titan's surface composition and atmospheric transmission with solar occultation measurements by Cassini VIMS SO ICARUS LA English DT Article DE Titan; Saturn, satellites; Titan, surface; Radiative transfer ID HUYGENS LANDING SITE; 5 MU-M; OPTICAL-CONSTANTS; METHANE CYCLE; SPECTRUM; MODEL; ICE; SPECTROSCOPY; SATELLITES; THOLINS AB Solar occultation measurements by the Cassini Visual and Infrared Mapping Spectrometer (VIMS) reveal the near-infrared transmission of Titan's atmosphere down to an altitude of similar to 40 km. By combining these observations with VIMS reflectance measurements of Titan's surface and knowledge of haze and gas opacity profiles from the Huygens probe, we constrain a simple model for the transfer of radiation in Titan's atmosphere in order to derive surface reflectance in the methane windows used for compositional analysis. The advantages of this model are twofold: (1) it is accurate enough to yield useful results, yet simple enough to be implemented in just a few lines of code, and (2) the model parameters are directly constrained by the VIMS occultation and on-planet measurements. We focus on the 2.0, 2.7, 2.8 and 5.0 mu m windows, where haze opacity is minimized, and diagnostic vibrational bands exist for water ice and other candidate surface species. A particularly important result is the strong atmospheric attenuation at 2.7 mu m compared to 2.8 mu m, resulting in a reversal of apparent spectral slope in a compositionally diagnostic wavelength range. These results show that Titan's surface reflectance is much "bluer" and more closely matched by water ice than the uncorrected spectra would indicate, although the majority of Titan's surface has a spectrum consistent with mixtures (either intimate or areal) of water ice and haze particles precipitated from the atmosphere. Compositions of geologic units can be accurately modeled as mixtures ranging from predominantly water ice (Sinlap crater ejecta and margins of dark equatorial terrain) to predominantly organic-rich (Tui Regio and Hotel Regio), with particles in the size range similar to 10-20 mu m. In distinguishing between hypothesized formation mechanisms for Tui and Hotei Regio, their organic-rich composition favors a process that concentrates precipitated haze particles, such as playa lake evaporite deposition (Barnes, J.W., Bow, J., Schwartz, J., Brown, R.H., Soderblom, J.M., Hayes, A.G., Vixie, G., Le Mouelic, S., Rodriguez, S., Sotin, C., Jaumann, R., Stephan, K, Soderblom, L.A., Clark, R.N., Buratti, B.J., Baines, K.H., Nicholson, P.D. [2011]. Icarus, 216, 136-140). In other places, kilometer-scale exposures of nearly pure water ice bedrock on Titan's surface indicate relatively locally rapid erosion compared to rates of accumulation of solid hydrocarbons precipitated from the atmosphere. Somewhat surprisingly, Titan's vast equatorial dune fields appear slightly enriched in water ice compared to the surrounding bright regions, but the spectrum of the dune material itself may nonetheless be consistent with a predominantly organic haze-derived composition. (C) 2014 Elsevier Inc. All rights reserved. C1 [Hayne, Paul O.; Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hayne, Paul O.; McCord, Thomas B.] Bear Fight Inst, Winthrop, WA 98862 USA. RP Hayne, PO (reprint author), CALTECH, Jet Prop Lab, MS 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Paul.O.Hayne@jpl.nasa.gov FU National Aeronautics and Space Administration FX We wish to thank K.H. Baines for valuable comments on an early version of this manuscript. During a large portion of this study, O. Aharonson, who also provided sanity checks on the compositional interpretations by comparison with Cassini RADAR data, supported P. Hayne as a postdoctoral fellow at Caltech. We also wish to thank F. Tosi and an anonymous reviewer for their thoughtful reviews. Part of this work was carried out at the Jet Propulsion Laboratory of the California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 67 TC 11 Z9 11 U1 1 U2 16 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 15 PY 2014 VL 243 BP 158 EP 172 DI 10.1016/j.icarus.2014.08.045 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT0OO UT WOS:000344635400015 ER PT J AU Cahill, JTS Thomson, BJ Patterson, GW Bussey, DBJ Neish, CD Lopez, NR Turner, FS Aldridge, T McAdam, M Meyer, HM Raney, RK Carter, LM Spudis, PD Hiesinger, H Pasckert, JH AF Cahill, Joshua T. S. Thomson, B. J. Patterson, G. Wesley Bussey, D. Benjamin J. Neish, Catherine D. Lopez, Norberto R. Turner, F. Scott Aldridge, T. McAdam, M. Meyer, H. M. Raney, R. K. Carter, L. M. Spudis, P. D. Hiesinger, H. Pasckert, J. H. TI The Miniature Radio Frequency instrument's (Mini-RF) global observations of Earth's Moon SO ICARUS LA English DT Article DE Moon; Radar observations; Cratering; Volcanism ID DIVINER LUNAR RADIOMETER; ORIENTALE BASIN; MARE BASALTS; OCEANUS-PROCELLARUM; WAVELENGTH RADAR; REGOLITH; AGES; STRATIGRAPHY; SURFACE; ANORTHOSITE AB Radar provides a unique means to analyze the surface and subsurface physical properties of geologic deposits, including their wavelength-scale roughness, the relative depth of the deposits, and some limited compositional information. The NASA Lunar Reconnaissance Orbiter's (LRO) Miniature Radio Frequency (Mini-RF) instrument has enabled these analyses on the Moon at a global scale. Mini-RF has accumulated similar to 67% coverage of the lunar surface in S-band (12.6 cm) radar with a resolution of 30 m/pixel. Here we present new Mini-RF global orthorectified uncontrolled S-band maps of the Moon and use them for analysis of lunar surface physical properties. Reported here are readily apparent global- and regional-scale differences in lunar surface physical properties that suggest three distinct terranes, namely: a (1) Nearside Radar Dark Region; (2) Orientale basin and continuous ejecta; and the (3) Highlands Radar Bright Region. Integrating these observations with new data from LRO's Diviner Radiometer rock abundance maps, as well Clementine and Lunar Prospector derived compositional values show multiple distinct lunar surface terranes and sub-terranes based upon both physical and compositional surface properties. Previous geochemical investigations of the Moon suggested its crust is best divided into three to four basic crustal provinces or terranes (Feldspathic Highlands Terrane (-An and -Outer), Procellarum KREEP Terrane, and South Pole Aitken Terrane) that are distinct from one another. However, integration of these geochemical data sets with new geophysical data sets allows us to refine these terranes. The result shows a more complex view of these same crustal provinces and provides valuable scientific and hazard perspectives for future targeted human and robotic exploration. (C) 2014 Elsevier Inc. All rights reserved. C1 [Cahill, Joshua T. S.; Patterson, G. Wesley; Bussey, D. Benjamin J.; Lopez, Norberto R.; Turner, F. Scott; Aldridge, T.; McAdam, M.; Meyer, H. M.; Raney, R. K.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Thomson, B. J.] Boston Univ, Boston, MA 02215 USA. [Neish, Catherine D.] Florida Inst Technol, Melbourne, FL 32901 USA. [McAdam, M.] Univ Maryland, College Pk, MD 20742 USA. [Meyer, H. M.] Arizona State Univ, Tempe, AZ 85287 USA. [Carter, L. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Spudis, P. D.] Lunar & Planetary Sci Inst, Houston, TX 77058 USA. [Hiesinger, H.; Pasckert, J. H.] Univ Munster, Munster, Germany. RP Cahill, JTS (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM Joshua.Cahill@jhuapl.edu RI Carter, Lynn/D-2937-2012; Cahill, Joshua/I-3656-2012; Patterson, Gerald/E-7699-2015 OI Cahill, Joshua/0000-0001-6874-5533; FU NASA LRO [NNN06AA01C, NNN10AA19T] FX We would like to acknowledge NASA's Lunar Reconnaissance Orbiter Mission and the Miniature Radio Frequency instrument science and engineering team. We would like to thank the NASA-APL Lunar Science Institute node. We would like to acknowledge the critiques of two anonymous reviewers. And finally, we would also like to acknowledge the Diviner Science Team for several insightful discussions relevant to this topic. NASA LRO contract NNN06AA01C, task order NNN10AA19T funded this work. This is NASA-APL Solar System Research Exploration Virtual Institute node publication SSERVI-2014-190. NR 63 TC 12 Z9 12 U1 0 U2 7 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD NOV 15 PY 2014 VL 243 BP 173 EP 190 DI 10.1016/j.icarus.2014.07.018 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT0OO UT WOS:000344635400016 ER PT J AU MacKenzie, SM Barnes, JW Sotin, C Soderblom, JM Le Mouelic, S Rodriguez, S Baines, KH Buratti, BJ Clark, RN Nicholson, PD McCord, TB AF MacKenzie, Shannon M. Barnes, Jason W. Sotin, Christophe Soderblom, Jason M. Le Mouelic, Stephane Rodriguez, Sebastien Baines, Kevin H. Buratti, Bonnie J. Clark, Roger N. Nicholson, Phillip D. McCord, Thomas B. TI Evidence of Titan's climate history from evaporite distribution SO ICARUS LA English DT Article DE Titan; Titan, surface; Spectroscopy; Infrared observations; Geological processes ID CASSINI RADAR; CHEMICAL-COMPOSITION; HUYGENS PROBE; ONTARIO LACUS; LANDING SITE; SURFACE; METHANE; LAKES; ATMOSPHERE; VIMS AB Water-ice-poor, 5-mu m-bright material on Saturn's moon Titan has previously been geomorphologically identified as evaporitic. Here we present a global distribution of the occurrences of the 5-mu m-bright spectral unit, identified with Cassini's Visual Infrared Mapping Spectrometer (VIMS) and examined with RADAR when possible. We explore the possibility that each of these occurrences are evaporite deposits. The 5-mu m-bright material covers 1% of Titan's surface and is not limited to the poles (the only regions with extensive, long-lived surface liquid). We find the greatest areal concentration to be in the equatorial basins Tui Regio and Hotel Regio. Our interpretations, based on the correlation between 5-mu m-bright material and lakebeds, imply that there was enough liquid present at some time to create the observed 5-mu m-bright material. We address the climate implications surrounding a lack of evaporitic material at the south polar basins: if the south pole basins were filled at some point in the past, then where is the evaporite? (C) 2014 Elsevier Inc. All rights reserved. C1 [MacKenzie, Shannon M.; Barnes, Jason W.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA. [Sotin, Christophe; Buratti, Bonnie J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Soderblom, Jason M.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Le Mouelic, Stephane] Univ Nantes, Lab Planetol & Geodynam, UMR6112, F-44322 Nantes 3, France. [Rodriguez, Sebastien] CEA Saclay, Ctr Orme Merisiers, DAPNIA Sap, Lab AIM, F-91191 Gif Sur Yvette, France. [Baines, Kevin H.] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA. [Clark, Roger N.] US Geol Survey, Denver, CO 80225 USA. [Nicholson, Phillip D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [McCord, Thomas B.] Bear Fight Inst, Winthrop, WA 98862 USA. RP MacKenzie, SM (reprint author), Univ Idaho, Dept Phys, Moscow, ID 83844 USA. EM mack3108@vandals.uidaho.edu RI Barnes, Jason/B-1284-2009; Rodriguez, Sebastien/H-5902-2016 OI Barnes, Jason/0000-0002-7755-3530; Rodriguez, Sebastien/0000-0003-1219-0641 FU NASA [NNX12AC28G]; NASA Astrobiology Institute FX The authors would like to thank an anonymous reviewer for constructive suggestions to the manuscript. This work was supported by NASA Cassini Data Analysts and Participating Scientists (CDAPS) Grant #NNX12AC28G to JWB. C.S. acknowledges support from the NASA Astrobiology Institute. Part of this work was conducted at JPL/Caltech under contract with NASA. NR 93 TC 13 Z9 13 U1 3 U2 16 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 15 PY 2014 VL 243 BP 191 EP 207 DI 10.1016/j.icarus.2014.08.022 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT0OO UT WOS:000344635400017 ER PT J AU Sciamma-O'Brien, E Ricketts, CL Salama, F AF Sciamma-O'Brien, Ella Ricketts, Claire L. Salama, Farid TI The Titan Haze Simulation experiment on COSmIC: Probing Titan's atmospheric chemistry at low temperature SO ICARUS LA English DT Article DE Titan, atmosphere; Atmospheres, chemistry; Experimental techniques; Organic chemistry ID POLYCYCLIC AROMATIC-HYDROCARBONS; MASS-SPECTROMETER MEASUREMENTS; CASSINI PLASMA SPECTROMETER; PULSED DISCHARGE NOZZLE; RING-DOWN SPECTROSCOPY; ION CHEMISTRY; AEROSOLS; BENZENE; MECHANISMS; ABUNDANCES AB The aim of the Titan Haze Simulation (THS) experiment is to contribute to a better understanding of aerosol formation in Titan's atmosphere through the study of the chemical formation pathways that link the simpler gas phase molecules resulting from the first steps of the N-2-CH4 chemistry, to the more complex gas phase precursors of aerosols; and more specifically, to investigate the role of polycyclic aromatic hydrocarbons (PAHs) and nitrogenated polycyclic aromatic hydrocarbons (PANHs), among other hydrocarbons, in this process. In the THS experiment developed at the NASA Ames Cosmic simulation facility (COSmIC), Titan's atmospheric chemistry is simulated by a pulsed plasma jet expansion at temperature conditions (similar to 150 K) close to those found in Titan's atmosphere in regions where aerosols are formed. In addition, because of the very short residence time of the gas in the plasma discharge, only the initial steps of the chemistry occur, making the COSmIC/THS a unique tool to study the first and intermediate (when adding heavier precursors to the initial N2-CH4 mixture) steps of Titan's atmospheric chemistry at low temperature as shown in the study presented here. We further illustrate the potential of COSmIC/THS for the simulation of Titan's atmospheric chemistry by presenting very promising results from a preliminary comparison of the laboratory data to data from the Cassini Plasma Spectrometer-Ion Beam Spectrometer (CAPS-IBS) instrument. (C) 2014 Elsevier Inc. All rights reserved. C1 [Sciamma-O'Brien, Ella; Ricketts, Claire L.; Salama, Farid] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Astrophys Branch, Moffett Field, CA 94035 USA. [Sciamma-O'Brien, Ella; Ricketts, Claire L.] Bay Area Environm Res Inst, Petaluma, CA 94952 USA. RP Sciamma-O'Brien, E (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Astrophys Branch, Mail Stop 245-6, Moffett Field, CA 94035 USA. EM ella.m.sciammaobrien@nasa.gov; claire.l.ricketts@gmail.com; farid.salama@nasa.gov RI Salama, Farid/A-8787-2009 OI Salama, Farid/0000-0002-6064-4401 FU NASA SMD (Planetary Atmospheres Program); NASA Postdoctoral Program (NPP) FX This research is supported by NASA SMD (Planetary Atmospheres Program). E. Sciamma-O'Brien and C.L. Ricketts acknowledge the support of the NASA Postdoctoral Program (NPP). The authors acknowledge fruitful discussions with C. Contreras, P. Bera, R. Fortenberry, J. Westlake, H. Waite, H. lmanaka, C. McKay, S. Lebonnois, D. Cruikshank and M. Smith. The authors are grateful to J. Westlake for providing the electronic data for CAPS-IBS. The authors also wish to acknowledge the outstanding technical support of R. Walker and E. Quigley (NASA ARC). NR 77 TC 2 Z9 2 U1 0 U2 17 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 15 PY 2014 VL 243 BP 325 EP 336 DI 10.1016/j.icarus.2014.08.004 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT0OO UT WOS:000344635400027 ER PT J AU Tyler, R AF Tyler, Robert TI Comparative estimates of the heat generated by ocean tides on icy satellites in the outer Solar System SO ICARUS LA English DT Article DE Satellites, dynamics; Europa; Enceladus; Titan ID TIDAL FRICTION; ROTATIONAL-DYNAMICS; GALILEAN SATELLITES; SUBSURFACE OCEAN; SOUTH-POLE; ENCELADUS; TITAN; CONSTRAINTS; OBLIQUITY; FRACTURES AB cant in the heat budgets maintaining liquid oceans on icy satellites in the outer Solar System. It has been shown in previous work that ocean tides, if resonantly forced, can supply heat at or exceeding the rates necessary for maintaining these oceans. It has also been shown that because of feedbacks these resonant configurations may be unavoidable under typical situations. This study extends from the previous work and seeks to examine the full set of dynamically-consistent ocean tidal solutions to describe the parameter dependencies that may cause one ocean to become trapped in such a vigorous ocean state while allowing another to freeze why do some of these satellites have oceans, and others do not? It is found that even with no other sources of heat, a liquid ocean on many of these satellites would be maintained by ocean tidal heat because the process of freezing (which changes the thickness of the remaining liquid ocean and thereby the eigenmodes) would push the ocean into a resonant configuration, with the associated increase in heat production preventing further freezing and stabilizing the configuration. An ocean on Io or Mimas would suffer extreme tides (with heat generated exceeding 1 W/m(2)) unless an implausibly large volume of water were present to lift the eigenmodes of the configuration out of resonance with the tidal forces. Europa can maintain a thick (similar to 100 km) ocean due to an obliquity-forced tidal resonance, while parameters for most other satellites suggest eccentricity-driven resonance scenarios involving much thinner ocean thicknesses (1-10s km). But these thin ocean thickness in the latter scenarios will be altered by ice cover: as the ice cover damps the ocean tidal response, significant heat is still generated which would stall freezing but the ocean thicknesses are modified to larger values than would be expected without ice cover. (C) 2014 Elsevier Inc. All rights reserved. C1 [Tyler, Robert] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Tyler, Robert] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Tyler, R (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Code 698, Greenbelt, MD 20771 USA. EM robert.h.tyler@nasa.gov FU NASA Outer Planets Research Program [NNX13AGO1G, NNX11AM38G] FX For helpful discussions on the dynamics and composition of the satellite oceans, the author wishes to thank Bruce Bills, Steve Vance, and Jason Goodman; and for discussions on solid tidal processes, Wade Henning, Michael Efroimsky, and Valeri Makarov. Finally, this study was supported by the NASA Outer Planets Research Program through Grants NNX13AGO1G, NNX11AM38G. NR 60 TC 7 Z9 7 U1 2 U2 13 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 15 PY 2014 VL 243 BP 358 EP 385 DI 10.1016/j.icarus.2014.08.037 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT0OO UT WOS:000344635400029 ER PT J AU Larson, EJL Toon, OB Friedson, AJ AF Larson, Erik J. L. Toon, Owen B. Friedson, Andrew J. TI Simulating Titan's aerosols in a three dimensional general circulation model SO ICARUS LA English DT Article DE Titan, atmosphere; Atmospheres, structure; Atmospheres, dynamics ID HUBBLE-SPACE-TELESCOPE; UPPER-ATMOSPHERE; PHYSICAL MODEL; DYNAMICS; HAZE; PHOTOCHEMISTRY; SURFACE; CLOUDS; WINDS; STRATOSPHERE AB We present results from a new three dimensional GCM with a complete microphysics treatment of the aerosols. We used the Titan Community Atmospheres Model (CAM), to which we have coupled the Community Aerosol and Radiation Model for Atmospheres (CARMA). This model was unable to reproduce superrotating winds without an ad hoc forcing of the zonal winds. Our model was validated by comparing the extinction, optical depth, phase functions, and number densities with data from Cassini and Huygens, as well as other space based and ground based observations. These comparisons allowed us to constrain the microphysical properties of Titan's haze in the tropics at the time of the Huygens descent. Our best fit of the free aerosol parameters include a haze production rate of 1 x 10(-14) g cm(-2) S-1 and a charge to radius ratio on the particles of 7.5 e(-)/mu m. Despite recent evidence of equatorial precipitation on Titan, we find the aerosols are only slowly removed by rainfall, less than once in 50 Earth years. One way to fit the wavelength dependence of the optical depth is to model the haze as fractal particles with a changing fractal dimension of 2 above 80 km that increases to 2.8 below 30 km. We investigate the spatial and seasonal variability of Titan's haze in our model. We find that the haze particle size and number density responds to the dynamics and creates a seasonal cycle in Titan's albedo.(C) 2014 Elsevier Inc. All rights reserved. C1 [Larson, Erik J. L.; Toon, Owen B.] Univ Colorado, Dept Atmospher & Ocean Sci, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Friedson, Andrew J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Larson, EJL (reprint author), Univ Colorado, Dept Atmospher & Ocean Sci, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. RI Larson, Erik/A-8668-2015 OI Larson, Erik/0000-0002-8994-1258 NR 62 TC 4 Z9 4 U1 1 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 15 PY 2014 VL 243 BP 400 EP 419 DI 10.1016/j.icarus.2014.09.003 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT0OO UT WOS:000344635400031 ER PT J AU Nuding, DL Rivera-Valentin, EG Davis, RD Gough, RV Chevrier, VF Tolbert, MA AF Nuding, D. L. Rivera-Valentin, E. G. Davis, R. D. Gough, R. V. Chevrier, V. F. Tolbert, M. A. TI Deliquescence and efflorescence of calcium perchlorate: An investigation of stable aqueous solutions relevant to Mars SO ICARUS LA English DT Article DE Mars; Mars, surface; Spectroscopy ID DEPOSITIONAL ICE NUCLEATION; BOUNDARY-LAYER; LANDING SITE; PARTICLES; SOIL AB Calcium perchlorate (Ca(ClO4)(2)) is a highly deliquescent salt that may exist on the surface of present-day Mars; however, its water uptake properties have not been well characterized at temperatures and relative humidity conditions relevant to Mars. Here, we quantify the deliquescent relative humidity (DRH) and efflorescent relative humidity (ERH) of Ca(ClO4)(2) as a function of temperature (223-273 K) to elucidate its behavior on the surface of Mars. A Raman microscope equipped with an environmental cell was used to simulate Mars relevant temperature and relative humidity conditions and monitor deliquescence (solid to aqueous) and efflorescence (aqueous to solid) phase transitions of Ca(ClO4)(2). Deliquescence and efflorescence were monitored visually using optical images and spectroscopically using Raman microscopy. We find that there is a wide range of deliquescence RH values between 5% and 55% RH. This range is due to the formation of hydrates in different temperatures regimes, with the higher DRH values occurring at the lowest temperatures. Experimental deliquescence results were compared to a thermodynamic model for three hydration states of Ca(ClO4)(2). The model predicts that the higher hydration states deliquesce at a higher RH than the lower hydration states. Calcium perchlorate was found to supersaturate, with lower ERH values than DRH values. The ERH results were less dependent on temperature with an average 15 +/- 4%, but values as low as 3 +/- 2% were measured at 273 K. Levitation experiments were performed on single particles of Ca(ClO4)(2) and Mg(ClO4)(2) at 298 K. While efflorescence was observed around 15% RH for Mg(ClO4)(2), the efflorescence of Ca(ClO4)(2) was not observed, even when exposed to 1% RH at 298 K. Additionally, a 17-h experiment was conducted to simulate a martian subsurface diurnal cycle. This demonstrated Ca(ClO4)(2) aqueous solutions can persist without efflorescing for the majority of a martian sol, up to 17 h under Mars temperature heating rates and RH conditions. We find that Ca(ClO4)(2) aqueous solutions could persist for most of the martian sol under present-day conditions. The aqueous phase stability and metastability quantified for Ca(ClO4)(2) under Mars relevant temperature and relative humidity conditions has important implications for the water cycle and the stability of liquid water on present day Mars. (C) 2014 Elsevier Inc. All rights reserved. C1 [Nuding, D. L.; Davis, R. D.; Gough, R. V.; Tolbert, M. A.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Nuding, D. L.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA. [Rivera-Valentin, E. G.] Natl Astron & Ionosphere Ctr, Arecibo Observ, USRA, Arecibo, PR 00612 USA. [Davis, R. D.; Gough, R. V.; Tolbert, M. A.] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA. [Chevrier, V. F.] Univ Arkansas, Arkansas Ctr Space & Planetary Sci, WM Keck Lab Space & Planetary Simulat, Fayetteville, AR 72701 USA. RP Nuding, DL (reprint author), Jet Prop Lab, Pasadena, CA 91106 USA. EM danielle.nuding@colorado.edu FU NASA Earth and Space Science Fellowship [NNX13A060H, NNX13AN69H]; NASA [NNX09AN19G]; NASA Data Analysis Program [NNX10AN81G] FX The authors would like to thank the reviewers for their time and valuable comments. The authors gratefully acknowledge the NASA Earth and Space Science Fellowship NNX13A060H and NNX13AN69H, NASA grant NNX09AN19G, and NASA Data Analysis Program Grant NNX10AN81G for supporting this work. NR 33 TC 13 Z9 13 U1 3 U2 37 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 15 PY 2014 VL 243 BP 420 EP 428 DI 10.1016/j.icarus.2014.08.036 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT0OO UT WOS:000344635400032 ER PT J AU Orton, GS Moses, JI Fletcher, LN Mainzer, AK Hines, D Hammel, HB Martin-Torres, J Burgdorf, M Merlet, C Line, MR AF Orton, Glenn S. Moses, Julianne I. Fletcher, Leigh N. Mainzer, Amy K. Hines, Dean Hammel, Heidi B. Martin-Torres, Javier Burgdorf, Martin Merlet, Cecile Line, Michael R. TI Mid-infrared spectroscopy of Uranus from the Spitzer infrared spectrometer: 2. Determination of the mean composition of the upper troposphere and stratosphere SO ICARUS LA English DT Article DE Uranus, atmosphere; Infrared observations; Atmospheres, structure ID DOUBLE-RESONANCE MEASUREMENTS; VIBRATIONAL-ENERGY-TRANSFER; RARE-GAS MIXTURES; MU-M; SATURNS ATMOSPHERE; THERMAL STRUCTURE; OUTER PLANETS; GIANT PLANETS; OCCULTATION MEASUREMENTS; BROADENING COEFFICIENT AB Mid-infrared spectral observations Uranus acquired with the Infrared Spectrometer (IRS) on the Spitzer Space Telescope are used to determine the abundances of C2H2, C2H6, CH3C2H, C4H2, CO2, and tentatively CH3 on Uranus at the time of the 2007 equinox. For vertically uniform eddy diffusion coefficients in the range 2200-2600 cm(2) s(-1), photochemical models that reproduce the observed methane emission also predict C2H6 profiles that compare well with emission in the 11.6-12.5 mu m wavelength region, where the upsilon(9) band of C2H6 is prominent. Our nominal model with a uniform eddy diffusion coefficient K-zz = 2430 cm(2) s(-1) and a CH4 tropopause mole fraction of 1.6 x 10(-5) provides a good fit to other hydrocarbon emission features, such as those of C2H2 and C4H2, but the model profile for CH3C2H must be scaled by a factor of 0.43, suggesting that improvements are needed in the chemical reaction mechanism for C3Hx species. The nominal model is consistent with a CH3D/CH4 ratio of 3.0 +/- 0.2 x 10(-4). From the best-fit scaling of these photochemical-model profiles, we derive column abundances above the 10-mbar level of 4.5 + 01.1/-0.8 x 10(9) molecule-cm(-2) for CH4, 6.2 +/- 1.0 x 10(16) molecule-cm(-2) for C2H2 (with a value 24% higher from a different longitudinal sampling), 3.1 +/- 0.3 x 10(16) molecule-cm(-2) for C2H6, 8.6 +/- 2.6 x 10(13) molecule-cm(-2) for CH3C2H, 1.8 +/- 0.3 x 10(13) molecule-cm(-2) for C4H2, and 1.7 +/- 0.4 x 10(13) molecule-cm(-2) for CO2 on Uranus. A model with K-zz increasing with altitude fits the observed spectrum and requires CH4 and C2H6 column abundances that are 54% and 45% higher than their respective values in the nominal model, but the other hydrocarbons and CO2 are within 14% of their values in the nominal model. Systematic uncertainties arising from errors in the temperature profile are estimated very conservatively by assuming an unrealistic "alternative" temperature profile that is nonetheless consistent with the observations; for this profile the column abundance of CH4 is over four times higher than in the nominal model, but the column abundances of the hydrocarbons and CO2 differ from their value in the nominal model by less than 22%. The CH3D/CH4 ratio is the same in both the nominal model with its uniform K-zz as in the vertically variable K-zz model, and it is 10% lower with the "alternative" temperature profile than the nominal model. There is no compelling evidence for temporal variations in global-average hydrocarbon abundances over the decade between Infrared Space Observatory and Spitzer observations, but we cannot preclude a possible large increase in the C2H2 abundance since the Voyager era. Our results have implications with respect to the influx rate of exogenic oxygen species and the production rate of stratospheric hazes on Uranus, as well as the C4H2 vapor pressure over C4H2 ice at low temperatures. (C) 2014 Elsevier Inc. All rights reserved. C1 [Orton, Glenn S.; Mainzer, Amy K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Moses, Julianne I.] Space Sci Inst, Boulder, CO 80301 USA. [Fletcher, Leigh N.; Merlet, Cecile] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. [Hines, Dean] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Hammel, Heidi B.] Assoc Univ Res Astron, Washington, DC 20005 USA. [Martin-Torres, Javier] CSIC, INTA, Inst Andaluz Ciencias Tierra, Granada 18100, Spain. [Burgdorf, Martin] HE Space Operat, D-28199 Bremen, Germany. [Line, Michael R.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Orton, GS (reprint author), CALTECH, Jet Prop Lab, MS 183-501,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM glenn.orton@jpl.nasa.gov RI Fletcher, Leigh/D-6093-2011; Martin-Torres, Francisco Javier/G-6329-2015; Moses, Julianne/I-2151-2013 OI Fletcher, Leigh/0000-0001-5834-9588; Martin-Torres, Francisco Javier/0000-0001-6479-2236; Moses, Julianne/0000-0002-8837-0035 FU Jet Propulsion Laboratory, California Institute of Technology; NASA [NNX13AH81G]; Spanish Economy and Competitivity Ministry [AYA2011-25720, AYA2012-38707]; JPL Office of the Chief Information Officer; [467] FX We thank NASA's Spitzer Space Telescope program for initial support of the data acquisition, reduction and its initial analysis, and we thank Tom Soifer for Director's Discretionary Time on Spitzer (Program #467). This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work from the Spitzer program was provided by NASA through an award issued by JPL/Caltech. Another portion of our support was provided to JPL/Caltech, from NASA's Planetary Atmospheres program. J. Moses acknowledges support from NASA Planetary Atmospheres Grant NNX13AH81G, as well as older grants from the NASA Planetary Atmospheres program. L. Fletcher acknowledges the Oak Ridge Association of Universities for its support during his tenure at the Jet Propulsion Laboratory in the NASA Postdoctoral Program (NPP), together with the Glasstone and Royal Society Research Fellowships during his current tenure at the University of Oxford. F.J. Martin-Torres was supported by the Spanish Economy and Competitivity Ministry (AYA2011-25720 and AYA2012-38707). During his contribution to this work, M. Line was supported by NASA's Undergraduate Student Research Program. The radiative-transfer calculations were primarily performed on JPL supercomputer facilities, which were provided by funding from the JPL Office of the Chief Information Officer. NR 116 TC 12 Z9 12 U1 1 U2 8 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD NOV 15 PY 2014 VL 243 BP 471 EP 493 DI 10.1016/j.icarus.2014.07.012 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT0OO UT WOS:000344635400036 ER PT J AU Orton, GS Fletcher, LN Moses, JI Mainzer, AK Hines, D Hammel, HB Martin-Torres, FJ Burgdorf, M Merlet, C Line, MR AF Orton, Glenn S. Fletcher, Leigh N. Moses, Julianne I. Mainzer, Amy K. Hines, Dean Hammel, Heidi B. Javier Martin-Torres, F. Burgdorf, Martin Merlet, Cecile Line, Michael R. TI Mid-infrared spectroscopy of Uranus from the Spitzer Infrared Spectrometer: 1. Determination of the mean temperature structure of the upper troposphere and stratosphere SO ICARUS LA English DT Article DE Uranus, atmosphere; Infrared observations; Atmospheres, structure ID SPACE-TELESCOPE; OUTER PLANETS; OCCULTATION MEASUREMENTS; BROADENING COEFFICIENT; VOYAGER MEASUREMENTS; RADIATIVE-TRANSFER; MODEL ATMOSPHERES; THERMAL STRUCTURE; HELIUM ABUNDANCE; NEAR-MILLIMETER AB On 2007 December 16-17, spectra were acquired of the disk of Uranus by the Spitzer Infrared Spectrometer (IRS), ten days after the planet's equinox, when its equator was close to the sub-Earth point. This spectrum provides the highest-resolution broad-band spectrum ever obtained for Uranus from space, allowing a determination of the disk-averaged temperature and molecule composition to a greater degree of accuracy than ever before. The temperature profiles derived from the Voyager radio occultation experiment by Lindal et al. (Lindal, G.F., Lyons, J.R., Sweetnam, D.N., Eshleman, V.R., Hinson, D.P. [1987]. J. Geophys. Res. 92, 14987-15001) and revisions suggested by Sromovsky et al. (Sromovslcy, LA., Fry, P.A., Kim, J.H. [2011]. Icarus 215, 292-312) that match these data best are those that assume a high abundance of methane in the deep atmosphere. However, none of these model profiles provides a satisfactory fit over the full spectral range sampled. This result could be the result of spatial differences between global and low-latitudinal regions, changes in time, missing continuum opacity sources such as stratospheric hazes or unknown tropospheric constituents, or undiagnosed systematic problems with either the Voyager radio-occultation or the Spitzer IRS data sets. The spectrum is compatible with the stratospheric temperatures derived from the Voyager ultraviolet occultations measurements by Herbert et al. (Herbert, F. et al. [1987]. J. Geophys. Res. 92, 15093-15109), but it is incompatible with the hot stratospheric temperatures derived from the same data by Stevens et al. (Stevens, M.H., Strobel, D.F., Herbert, F.H. [1993]. Icarus 101, 45-63). Thermospheric temperatures determined from the analysis of the observed H-2 quadrupole emission features are colder than those derived by Herbert et al. at pressures less than similar to 1 mu bar. Extrapolation of the nominal model spectrum to far-infrared through millimeter wavelengths shows that the spectrum arising solely from H-2 collision-induced absorption is too warm to reproduce observations between wavelengths of 0.8 and 3.3 mm. Adding an additional absorber such as H2S provides a reasonable match to the spectrum, although a unique identification of the responsible absorber is not yet possible with available data. An immediate practical use for the spectrum resulting from this model is to establish a high-precision continuum flux model for use as an absolute radiometric standard for future astronomical observations. (C) 2014 Elsevier Inc. All rights reserved. C1 [Orton, Glenn S.; Mainzer, Amy K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Fletcher, Leigh N.; Merlet, Cecile] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. [Moses, Julianne I.] Space Sci Inst, Boulder, CO 80301 USA. [Hines, Dean] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Hammel, Heidi B.] Assoc Univ Res Astron, Washington, DC 20005 USA. [Javier Martin-Torres, F.] CSIC, INTA, Inst Andaluz Ciencias Tierra, Granada 18100, Spain. [Burgdorf, Martin] HE Space Operat, D-28199 Bremen, Germany. [Line, Michael R.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Orton, GS (reprint author), CALTECH, Jet Prop Lab, MS 183-501,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM glenn.orton@jpl.nasa.gov RI Fletcher, Leigh/D-6093-2011; Martin-Torres, Francisco Javier/G-6329-2015; Moses, Julianne/I-2151-2013 OI Fletcher, Leigh/0000-0001-5834-9588; Martin-Torres, Francisco Javier/0000-0001-6479-2236; Moses, Julianne/0000-0002-8837-0035 FU Jet Propulsion Laboratory, California Institute of Technology; NASA [NNX13AH81G]; Spanish Economy and Competitivity Ministry [AYA2011-25720, AYA2012-38707]; [467] FX We thank NASA's Spitzer Space Telescope program for initial support of the data acquisition, reduction and its initial analysis, and we thank Tom Soifer for Director's Discretionary Time on Spitzer (Program #467). This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work from the Spitzer program was provided by NASA through an award issued by JPL/Caltech. Another portion of our support was provided to JPL/Caltech, from NASA's Planetary Atmospheres program. J. Moses acknowledges support from NASA Grants NNX13AH81G, as well as older grants from the NASA Planetary Atmospheres program. L. Fletcher acknowledges the Oak Ridge Association of Universities for its support during his tenure at the Jet Propulsion Laboratory in the NASA Postdoctoral Program (NPP), together with the Glasstone and Royal Society Research Fellowships during his current tenure at the University of Oxford. F.J. Martin-Torres acknowledges support from the Spanish Economy and Competitivity Ministry (AYA2011-25720 and AYA2012-38707). During his contribution to this work, M. Line was supported by NASA's Undergraduate Student Research Program (USRP).; This research made use of Tiny Tim/Spitzer, developed by John Krist for the Spitzer Science Center. The Center is managed by the California Institute of Technology under a contract with NASA.; The radiative-transfer calculations were primarily performed on JPL supercomputer facilities, which were provided by funding from the JPL Office of the Chief Information Officer. NR 72 TC 10 Z9 10 U1 1 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD NOV 15 PY 2014 VL 243 BP 494 EP 513 DI 10.1016/j.icarus.2014.07.010 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT0OO UT WOS:000344635400037 ER PT J AU Brown, AJ Piqueux, S Titus, TN AF Brown, Adrian J. Piqueux, Sylvain Titus, Timothy N. TI Interannual observations and quantification of summertime H2O ice deposition on the Martian CO2 ice south polar cap SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Mars; poles; H2O ice; CO2 ice; radiative transfer; snow ID GENERAL-CIRCULATION MODEL; SEASONAL WATER CYCLE; OPTICAL-PROPERTIES; SPECTRAL ALBEDO; CARBON-DIOXIDE; MARS; BEHAVIOR; VAPOR; SUBLIMATION; INSTABILITY AB The spectral signature of water ice was observed on Martian south polar cap in 2004 by the Observatoire pour l'Mineralogie, l'Eau les Glaces et l'Activite (OMEGA) (Bibring et al., 2004). Three years later, the OMEGA instrument was used to discover water ice deposited during southern summer on the polar cap (Langevin et al., 2007). However, temporal and spatial variations of these water ice signatures have remained unexplored, and the origins of these water deposits remains an important scientific question. To investigate this question, we have used observations from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) instrument on the Mars Reconnaissance Orbiter (MRO) spacecraft of the southern cap during austral summer over four Martian years to search for variations in the amount of water ice. We report below that for each year we have observed the cap, the magnitude of the H2O ice signature on the southern cap has risen steadily throughout summer, particularly on the west end of the cap. The spatial extent of deposition is in disagreement with the current best simulations of deposition of water ice on the south polar cap (Montmessin et al., 2007). This increase in water ice signatures is most likely caused by deposition of atmospheric H2O ice and a set of unusual conditions makes the quantification of this transport flux using CRISM close to ideal. We calculate a 'minimum apparent' amount of deposition corresponding to a thin H2O ice layer of 0.2 mm (with 70% porosity). This amount of H2O ice deposition is 0.6-6% of the total Martian atmospheric water budget. We compare our 'minimum apparent' quantification with previous estimates. This deposition process may also have implications for the formation and stability of the southern CO2 ice cap, and therefore play a significant role in the climate budget of modern day Mars. (C) 2014 Elsevier B.V. All rights reserved. C1 [Brown, Adrian J.] SETI Inst, Mountain View, CA 94043 USA. [Piqueux, Sylvain] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Titus, Timothy N.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. RP Brown, AJ (reprint author), SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA. EM abrown@seti.org FU NASA Mars Data Analysis Program [NNX11AN41G, NNX13AJ73G]; National Aeronautics and Space Administration FX We would like to thank the entire CRISM Team, particularly the Science Operations team at JHU APL. We also thank Ted Roush for supplying the palagonite optical constants and Franck Marchis and Peter Jenniskens and referees Yves Langevin and Francois Forget for helpful comments on the manuscript. This investigation was partially funded by NASA Mars Data Analysis Program Grants NNX11AN41G and NNX13AJ73G administered by Mitch Schulte. Piqueux' contribution was carried out at the Jet Propulsion Laboratory, under a contract with the National Aeronautics and Space Administration. NR 58 TC 4 Z9 4 U1 2 U2 11 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 NOV 15 PY 2014 VL 406 BP 102 EP 109 DI 10.1016/j.epsl.2014.08.039 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AS3YO UT WOS:000344211200011 ER PT J AU Norris, KJ Garrett, M Coleman, E Tompa, GS Zhang, J Kobayashi, NP AF Norris, Kate J. Garrett, Matthew Coleman, Elane Tompa, Gary S. Zhang, Junce Kobayashi, Nobuhiko P. TI Graphene mediated growth of polycrystalline indium phosphide nanowires and monocrystalline-core, polycrystalline-shell silicon nanowires on copper SO JOURNAL OF CRYSTAL GROWTH LA English DT Article DE Nanowirc; MOCVD; Polycrystalline; Indium phosphide; Silicon; Copper; Graphene ID DER-WAALS EPITAXY; FEW-LAYER GRAPHENE; RAMAN-SPECTROSCOPY; THERMOELECTRIC PERFORMANCE; SINGLE-LAYER; NETWORKS; GAN AB Two types of semiconductors, indium phosphide (InP) and silicon (Si), were separately grown on polycrystalline copper foils with the presence of gold colloidal particles. InP was grown with and without carbon deposition by metal organic chemical vapor deposition, and Si was grown with and without plasma enhanced chemical vapor deposition of carbon. While lnP and Si grew as films on untreated copper foils, they were found to grow in the form of nanowires when copper foils were pre-treated with carbon. Structural analysis revealed that the grown lnP nanowires were polycrystalline. In contrast, the grown Si nanowires were found to have core-shell structures with a monocrystalline core and a polycrystalline shell. Further analysis suggested that graphene was formed on the copper foils during the carbon deposition. Therefore, we concluded that the presence of graphene promoted the growth of lnP and Si in the form of nanowires. The demonstration of growing semiconductor nanowires on copper foils could be a new path to integrate semiconductor and metal to provide a unique material platform for a wide range of devices. (C) 2014 Elsevier B.V. All rights reserved. C1 [Norris, Kate J.; Garrett, Matthew; Zhang, Junce; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. [Norris, Kate J.; Garrett, Matthew; Zhang, Junce; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, NASA, Ames Res Ctr, NECTAR,Adc Studies Lab, Moffett Field, CA 94035 USA. [Coleman, Elane; Tompa, Gary S.] Struct Mat Ind Inc, Piscataway, NJ USA. RP Norris, KJ (reprint author), Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. EM katejeannenorris@gmail.com RI Kobayashi, Nobuhiko/E-3834-2012 FU Structured Materials industries, Inc.; NASA SBIR [NNX11CE14P]; National Science Foundation [DGE-0809125]; Semiconductor Research Corporation CSR fund FX We would like to thank Hewlett Packard labs and the UCSC Materials Analysis for Collaborative Science facility (Moffett Field, California) at Advanced Studies Laboratories, University of California Santa Cruz, and NASA Ames Research Center for continuous support on analytical equipment. This work was supported by Structured Materials industries, Inc. NASA SBIR NNX11CE14P and the National Science Foundation Graduate Research Fellowship under Grant no. DGE-0809125. Support by Semiconductor Research Corporation CSR fund (Dr. Victor Zhimov) is also highly appreciated. NR 33 TC 5 Z9 5 U1 2 U2 44 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0248 EI 1873-5002 J9 J CRYST GROWTH JI J. Cryst. Growth PD NOV 15 PY 2014 VL 406 BP 41 EP 47 DI 10.1016/j.jcrysgro.2014.08.016 PG 7 WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied SC Crystallography; Materials Science; Physics GA AQ8QC UT WOS:000343092800008 ER PT J AU Levitt, NP AF Levitt, Nicholas Paul TI Sample matrix effects on measured carbon and oxygen isotope ratios during continuous-flow isotope-ratio mass spectrometry SO RAPID COMMUNICATIONS IN MASS SPECTROMETRY LA English DT Article ID KEELING PLOT APPLICATIONS; RAPID O-18 ANALYSIS; HIGH-PRECISION; CO2 CONCENTRATIONS; ATMOSPHERIC CO2; STABLE-ISOTOPE; EXHALED BREATH; GAS SAMPLES; WATER; DELTA-C-13 AB RATIONALE: Continuous-flow isotope-ratio mass spectrometry (CF-IRMS) is frequently used to analyze CO2 found in media such as air, breath, and soil pore space gas with the aid of a sample preparation and transfer device such as a Gasbench II. This study investigated the effect that matrices other than helium (He) have on the measured C-13 and O-18 isotope ratios of CO2. METHODSIdentical CO2 was added to sample vials with matrices of pure He, pure N-2, or a 21:79 mixture of O-2/N-2 and analyzed by a ThermoFinnigan Delta(Plus) XP isotope-ratio mass spectrometer coupled to a ThermoFinnigan Gasbench II. Variables such as CO2 concentration, sample analysis sequence, and sample matrix removal ('blanking') through manipulation of an injection and dilution open split were tested to identify systematic isotope ratio offsets between the different matrix types. RESULTSThe process of blanking induced a C-13 and O-18 offset of 0.2 between otherwise identical populations of CO2 samples in He. The C-13/C-12 and O-18/O-16 isotope ratios of CO2 sampled from pure N-2 or a mixture of O-2/N-2 were found to be within 0.1 to 0.2 parts per thousand of those of an identical CO2 sampled from a He matrix when N-2 or O-2/N-2 was removed prior to transport to the mass spectrometer. The measured oxygen isotope ratios of CO2 sampled from N-2 and O-2/N-2 varied by as much as 0.6 parts per thousand and 4 parts per thousand, respectively, if matrix gas was not removed prior to ionization. CONCLUSIONSSampling CO2 from matrices similar to air does not significantly affect the measured C-13/C-12 and O-18/O-16 isotope ratios of CO2 when a gas-handling procedure that includes the removal of matrix gas is utilized. This procedure is much preferable to introducing matrix gas and potentially isobaric interference to the ion source. Copyright (c) 2014 John Wiley & Sons, Ltd. C1 [Levitt, Nicholas Paul] Univ Kentucky, NASA Astrobiol Inst, Dept Earth & Environm Sci, Lexington, KY 40506 USA. RP Levitt, NP (reprint author), Univ Wisconsin, NASA Astrobiol Inst, Dept Geosci, 1215 W Dayton St, Madison, WI 53706 USA. EM nlevitt@wisc.edu FU NASA Headquarters under the NASA Earth and Space Fellowship Program [NNX12AN84H]; NASA Astrobiology Institute FX The author thanks Dr Suvankar Chakraborty for instrument maintenance assistance and insightful discussions. Three anonymous reviewers are acknowledged for their helpful and constructive comments on an earlier version of this manuscript. This work was supported by NASA Headquarters under the NASA Earth and Space Fellowship Program - Grant NNX12AN84H - as well as the NASA Astrobiology Institute. NR 41 TC 2 Z9 2 U1 3 U2 26 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0951-4198 EI 1097-0231 J9 RAPID COMMUN MASS SP JI Rapid Commun. Mass Spectrom. PD NOV 15 PY 2014 VL 28 IS 21 BP 2259 EP 2274 DI 10.1002/rcm.7019 PG 16 WC Biochemical Research Methods; Chemistry, Analytical; Spectroscopy SC Biochemistry & Molecular Biology; Chemistry; Spectroscopy GA AQ6DM UT WOS:000342898700004 PM 25279739 ER PT J AU Shaygan, M Kheirabi, N Davami, K Mortazavi, B Lee, JS Cuniberti, G Meyyappan, M AF Shaygan, Mehrdad Kheirabi, Nazli Davami, Keivan Mortazavi, Bohayra Lee, Jeong-Soo Cuniberti, Gianaurelio Meyyappan, M. TI Annealing effect on the thermal conductivity of thermoelectric ZnTe nanowires SO MATERIALS LETTERS LA English DT Article DE Thermoelectric; ZnTe; Nanowire; Thermal conductivity ID SILICON NANOWIRES; MOLECULAR-DYNAMICS; DEFECTS AB We report here the effect of thermal annealing on the thermal conductivity of ZnTe nanowires measured on a microfabricated suspended device. Molecular dynamics simulation was used to calculate the effect of contacts on the measurements at different temperatures and to estimate the intrinsic nanowire thermal conductivity values. A decrease in thermal conductivity was observed after each thermal annealing step at all the measured temperatures. Thermal annealing can be a potential method to improve the thermoelectric efficiency of nanowires, not only by enhancing the electrical conduction as demonstrated before, but also by suppressing the thermal transport at the same time. (C) 2014 Elsevier B.V. All rights reserved. C1 [Shaygan, Mehrdad; Kheirabi, Nazli; Davami, Keivan; Lee, Jeong-Soo] Pohang Univ Sci & Technol POSTECH, Dept IT Convergence Engn, Pohang, South Korea. [Mortazavi, Bohayra; Cuniberti, Gianaurelio] Tech Univ Dresden, Inst Mat Sci, D-01062 Dresden, Germany. [Mortazavi, Bohayra; Cuniberti, Gianaurelio] Tech Univ Dresden, Max Bergmann Ctr Biomat, D-01062 Dresden, Germany. [Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Davami, K (reprint author), Pohang Univ Sci & Technol POSTECH, Dept IT Convergence Engn, Pohang, South Korea. EM keivandavami@yahoo.com; ljs6951@postech.ac.kr RI Cuniberti, Gianaurelio/B-7192-2008; Davami, Keivan/Q-5283-2016 OI Cuniberti, Gianaurelio/0000-0002-6574-7848; FU Ministry of Education, Science and Technology through the National Research Foundation of Korea [R31-10100] FX The World Class University program funded by the Ministry of Education, Science and Technology through the National Research Foundation of Korea (R31-10100) supported this research. Keivan Davami did the measurement part of this work during his visit at UT Austin and wishes to acknowledge Professor Shi and his group for their helpful support during the visit. Dr. T. Gemming at IFW Dresden is acknowledged for providing electron microscopy facilities. NR 24 TC 1 Z9 1 U1 3 U2 48 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0167-577X EI 1873-4979 J9 MATER LETT JI Mater. Lett. PD NOV 15 PY 2014 VL 135 BP 87 EP 91 DI 10.1016/j.matlet.2014.07.114 PG 5 WC Materials Science, Multidisciplinary; Physics, Applied SC Materials Science; Physics GA AQ1GF UT WOS:000342529200023 ER PT J AU Crespo-Medina, M Twing, KI Kubo, MDY Hoehler, TM Cardace, D McCollom, T Schrenk, MO AF Crespo-Medina, Melitza Twing, Katrina I. Kubo, Michael D. Y. Hoehler, Tori M. Cardace, Dawn McCollom, Tom Schrenk, Matthew O. TI Insights into environmental controls on microbial communities in a continental serpentinite aquifer using a microcosm-based approach SO FRONTIERS IN MICROBIOLOGY LA English DT Article DE serpentinization; subsurface; metabolism; nutrients; carbon ID DEEP-SEA; DIVERSITY; CEDARS; SITE AB Geochemical reactions associated with serpentinization alter the composition of dissolved organic compounds in circulating fluids and potentially liberate mantle-derived carbon and reducing power to support subsurface microbial communities. Previous studies have identified Betaproteobacteria from the order Burkholderiales and bacteria from the order Clostridiales as key components of the serpentinite-hosted microbiome, however there is limited knowledge of their metabolic capabilities or growth characteristics. In an effort to better characterize microbial communities, their metabolism, and factors limiting their activities, microcosm experiments were designed with fluids collected from several monitoring wells at the Coast Range Ophiolite Microbial Observatory (CROMO) in northern California during expeditions in March and August 2013. The incubations were initiated with a hydrogen atmosphere and a variety of carbon sources (carbon dioxide, methane, acetate, and formate), with and without the addition of nutrients and electron acceptors. Growth was monitored by direct microscopic counts; DNA yield and community composition was assessed at the end of the 3 month incubation. For the most part, results indicate that bacterial growth was favored by the addition of acetate and methane, and that the addition of nutrients and electron acceptors had no significant effect on microbial growth, suggesting no nutrient- or oxidant-limitation. However, the addition of sulfur amendments led to different community compositions. The dominant organisms at the end of the incubations were closely related to Dethiobacter sp. and to the family Comamonadaceae, which are also prominent in culture-independent gene sequencing surveys. These experiments provide one of first insights into the biogeochemical dynamics of the serpentinite subsurface environment and will facilitate experiments to trace microbial activities in serpentinizing ecosystems. C1 [Crespo-Medina, Melitza; Twing, Katrina I.; Schrenk, Matthew O.] Michigan State Univ, Dept Geol Sci, E Lansing, MI 48824 USA. [Crespo-Medina, Melitza] Inter Amer Puerto Rico, Ctr Environm Educ Conservat & Res, San Juan, PR USA. [Kubo, Michael D. Y.] SETI Inst, Mountain View, CA USA. [Hoehler, Tori M.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. [Cardace, Dawn] Univ Rhode Isl, Dept Geosci, Kingston, RI 02881 USA. [McCollom, Tom] Univ Colorado, Ctr Astrobiol, Boulder, CO 80309 USA. [McCollom, Tom] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. RP Schrenk, MO (reprint author), Michigan State Univ, Dept Geol Sci, Nat Sci Bldg, E Lansing, MI 48824 USA. EM mattoschrenk@gmail.com OI Twing, Katrina/0000-0002-5266-3397 FU NASA Astrobiology Institute Director's Discretionary Fund; Alfred P. Sloan Foundation Deep Carbon Observatory [2011-12-01] FX We thank the NASA Astrobiology Institute Director's Discretionary Fund and the Alfred P. Sloan Foundation Deep Carbon Observatory (2011-12-01) for the funding that made this research possible. We want to thank the staff of the UC-Davis McLaughlin Natural Reserve, particularly co-directors C. Koehler and P. Aigner, for their support and aid in the field and to S. Moore (Homestake Mining Co.) for his advice for sampling the CROMO wells. The 16S rRNA tag sequencing was performed at the Marine Biological Laboratory (Woods Hole, MA) and we are especially thankful to M. Sogin, S. Huse, J. Vineis, A. Voorhis, S. Grim, and H. Morrison for their expertise and technical assistance. We want to thank D. Carnevale for field assistance and W. Brazelton for his expert support and advice with the analysis of tag sequencing data. NR 24 TC 9 Z9 9 U1 4 U2 34 PU FRONTIERS RESEARCH FOUNDATION PI LAUSANNE PA PO BOX 110, LAUSANNE, 1015, SWITZERLAND SN 1664-302X J9 FRONT MICROBIOL JI Front. Microbiol. PD NOV 14 PY 2014 VL 5 AR 604 DI 10.3389/fmicb.2014.00604 PG 9 WC Microbiology SC Microbiology GA AU6FQ UT WOS:000345699500001 PM 25452748 ER PT J AU Zevalkink, A Swallow, J Ohno, S Aydemir, U Bux, S Snyder, GJ AF Zevalkink, Alex Swallow, Jessica Ohno, Saneyuki Aydemir, Umut Bux, Sabah Snyder, G. Jeffrey TI Thermoelectric properties of the Ca5Al2-xInxSb6 solid solution SO DALTON TRANSACTIONS LA English DT Article ID LATTICE THERMAL-CONDUCTIVITY; ZINTL PHASE; HIGH TEMPERATURES; EFFICIENCY; COMPOUND AB Zintl phases are attractive for thermoelectric applications due to their complex structures and bonding environments. The Zintl compounds Ca5Al2Sb6 and Ca5In2Sb6 have both been shown to have promising thermoelectric properties, with zT values of 0.6 and 0.7, respectively, when doped to control the carrier concentration. Alloying can often be used to further improve thermoelectric materials in cases when the decrease in lattice thermal conductivity outweighs reductions to the electronic mobility. Here we present the high temperature thermoelectric properties of the Ca5Al2-xInxSb6 solid solution. Undoped and optimally Zn-doped samples were investigated. X-ray diffraction confirms that a full solid solution exists between the Al and In end-members. We find that the Al: In ratio does not greatly influence the carrier concentration or Seebeck effect. The primary effect of alloying is thus increased scattering of both charge carriers and phonons, leading to significantly reduced electronic mobility and lattice thermal conductivity at room temperature. Ultimately, the figure of merit is unaffected by alloying in this system, due to the competing effects of reduced mobility and lattice thermal conductivity. C1 [Zevalkink, Alex; Bux, Sabah] Jet Prop Lab, Thermal Energy Convers Technol Grp, Pasadena, CA USA. [Swallow, Jessica; Ohno, Saneyuki; Aydemir, Umut; Snyder, G. Jeffrey] CALTECH, Dept Mat Sci, Pasadena, CA 91125 USA. [Aydemir, Umut] Koc Univ, Dept Chem, Sariyer, Turkey. RP Snyder, GJ (reprint author), CALTECH, Dept Mat Sci, Pasadena, CA 91125 USA. EM jsnyder@caltech.edu RI Snyder, G. Jeffrey/E-4453-2011; Snyder, G/I-2263-2015; Aydemir, Umut/P-8424-2015 OI Snyder, G. Jeffrey/0000-0003-1414-8682; Aydemir, Umut/0000-0003-1164-1973 FU NASA Science Missions Directorate's Radioisotope Power Systems Technology Advancement Program; Scientific and Technological Research Council of Turkey FX This work was performed at the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration. This work was supported by the NASA Science Missions Directorate's Radioisotope Power Systems Technology Advancement Program. We gratefully acknowledge Leslie D. Zoltan for performing high temperature Seebeck measurements. U. Aydemir greatly acknowledges the financial assistance of The Scientific and Technological Research Council of Turkey. NR 34 TC 5 Z9 6 U1 3 U2 27 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1477-9226 EI 1477-9234 J9 DALTON T JI Dalton Trans. PD NOV 14 PY 2014 VL 43 IS 42 BP 15872 EP 15878 DI 10.1039/c4dt02206h PG 7 WC Chemistry, Inorganic & Nuclear SC Chemistry GA AS0HP UT WOS:000343958900025 PM 25226576 ER PT J AU Heritier, KL Jaffe, RL Laporta, V Panesi, M AF Heritier, K. L. Jaffe, R. L. Laporta, V. Panesi, M. TI Energy transfer models in nitrogen plasmas: Analysis of N-2(X-1 Sigma(+)(g))-N(S-4(u))-e(-) interaction SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID II FLIGHT EXPERIMENT; VIBRATIONAL-EXCITATION; ELECTRON-IMPACT; RELAXATION; MOLECULES; FLOWS; SCATTERING; COLLISIONS; DYNAMICS; N-2 AB The relaxation of N-2(X-1 Sigma(+)(g)) molecules in a background gas composed of N(S-4(u)) atoms and free electrons is studied by using an ideal isochoric and isothermic chemical reactor. A rovibrational state-to-state model is developed to study energy transfer process induced by free electron and atomic collisions. The required cross sections and the corresponding rate coefficients are taken from two well-known kinetic databases: NASA Ames kinetic mechanism for the description of the N-2(X-1 Sigma(+)(g))-N(S-4(u)) processes and the Phys4Entry database for the electron driven processes, N-2(X-1 Sigma(+)(g))-e(-). The evolution of the population densities of each individual rovibrational level is explicitly determined via the numerical solution of the master equation for temperatures ranging from 10000 to 30 000 K. It was found that the distribution of the rovibrational energy levels of N-2(X-1 Sigma(+)(g)) is strongly influenced by the electron driven collisional processes, which promote the excitation of the low lying vibrational levels. The macroscopic vibrational energy relaxation is governed by the molecule-atom collisions, when free electrons, initially cold are relaxing to the final heat-bath temperature. Thus, the main role of the free electrons is to ensure the equilibration of vibrational and free electron excitation, thus validating the existence of the local equilibrium T-V-T-e. However, if electrons and heavy particles are assumed to be in equilibrium at the heat bath temperature, electron driven processes dominate the vibrational relaxation. Finally, we have assessed the validity of the Landau-Teller model for the description of the inelastic energy transfer between molecules and free electrons. In the case of free-electron temperatures lower than 10 000 K, Landau-Teller relaxation model gives an accurate description of the vibrational relaxation, while at higher temperatures the error in the predictions can be significant and the model should not be used. (C) 2014 AIP Publishing LLC. C1 [Heritier, K. L.; Panesi, M.] Univ Illinois, Dept Aerosp Engn, Urbana, IL 61801 USA. [Jaffe, R. L.] NASA, Ames Res Ctr, Aerothermodynam Branch, Moffett Field, CA 94035 USA. [Laporta, V.] CNR, Ist Metodol Inorgan & Plasmi, I-70126 Bari, Italy. [Laporta, V.] UCL, Dept Phys & Astron, London WC1E 6BT, England. RP Heritier, KL (reprint author), Univ Illinois, Dept Aerosp Engn, 104 S Wright St, Urbana, IL 61801 USA. EM mpanesi@illinois.edu RI Laporta, Vincenzo/O-4191-2015 OI Laporta, Vincenzo/0000-0003-4251-407X FU Department of Energy, National Nuclear Security Administration [DE-NA0002374]; Education Associates Program in the Entry Systems and Technology Division at Ames - Hypersonics EDL Project of the Space Technology Mission Directorate; NASA Space Technology Mission Directorate Entry Systems Modeling program; European Community [242311] FX The authors have benefited from numerous discussions with Dr. W. Huo and Dr. D. W. Schwenke at NASA Ames Research. This material is based upon work supported by the Department of Energy, National Nuclear Security Administration, under Award No. DE-NA0002374. K.L.H. was supported as summer intern under the Education Associates Program in the Entry Systems and Technology Division at Ames funded by the Hypersonics EDL Project of the Space Technology Mission Directorate. R.L.J. was supported by NASA Space Technology Mission Directorate Entry Systems Modeling program and V. L. was supported by the European Community's Seventh Framework Programme (FP72007-2013) under Grant Agreement No. 242311. NR 46 TC 3 Z9 3 U1 2 U2 15 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD NOV 14 PY 2014 VL 141 IS 18 AR 184302 DI 10.1063/1.4900508 PG 16 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA AT3PZ UT WOS:000344847600021 PM 25399142 ER PT J AU Shultz, MJ Bisson, P Vu, TH AF Shultz, Mary Jane Bisson, Patrick Tuan Hoang Vu TI Insights into hydrogen bonding via ice interfaces and isolated water SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID FREQUENCY VIBRATIONAL SPECTROSCOPY; SENSITIVE SUM-FREQUENCY; HYDROPHOBIC ENVIRONMENT; CARBON-TETRACHLORIDE; GENERATION SPECTRUM; VAPOR INTERFACE; AIR INTERFACE; SURFACE; DYNAMICS; LIQUID AB Water in a confined environment has a combination of fewer available configurations and restricted mobility. Both affect the spectroscopic signature. In this work, the spectroscopic signature of water in confined environments is discussed in the context of competing models for condensed water: (1) as a system of intramolecular coupled molecules or (2) as a network with intermolecular dipole-dipole coupled O-H stretches. Two distinct environments are used: the confined asymmetric environment at the ice surface and the near-isolated environment of water in an infrared transparent matrix. Both the spectroscopy and the environment are described followed by a perspective discussion of implications for the two competing models. Despite being a small molecule, water is relatively complex; perhaps not surprisingly the results support a model that blends inter-and intramolecular coupling. The frequency, and therefore the hydrogen-bond strength, appears to be a function of donor-acceptor interaction and of longer-range dipole-dipole alignment in the hydrogen-bonded network. The O-H dipole direction depends on the local environment and reflects intramolecular O-H stretch coupling. (C) 2014 AIP Publishing LLC. C1 [Shultz, Mary Jane; Bisson, Patrick] Tufts Univ, Dept Chem, Lab Water & Surface Studies, Medford, MA 02155 USA. [Tuan Hoang Vu] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Shultz, MJ (reprint author), Tufts Univ, Dept Chem, Lab Water & Surface Studies, Medford, MA 02155 USA. EM Mary.Shultz@Tufts.edu RI Vu, Tuan/F-5223-2017; OI Vu, Tuan/0000-0001-6839-9765; Bisson, Patrick/0000-0002-4985-3077 FU U.S. National Science Foundation [1306933, 0844986]; Petroleum Research Fund of American Chemical Society [PRF 46671-AC6] FX We would like to acknowledge the students who began this work, enabling this larger view of the spectral consequences of H-bonding and dipole-dipole interactions: Dr. Irene Barnett, Dr. Henning Groenzin, and Dr. Margaret Kuo. Financial support from the U.S. National Science Foundation (Grant Nos. 1306933 and 0844986) and the Petroleum Research Fund of the American Chemical Society (PRF 46671-AC6) is gratefully acknowledged. NR 82 TC 2 Z9 2 U1 3 U2 46 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD NOV 14 PY 2014 VL 141 IS 18 AR 18C521 DI 10.1063/1.4896603 PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA AT3PZ UT WOS:000344847600065 PM 25399186 ER PT J AU Wei, CY Pohorille, A AF Wei, Chenyu Pohorille, Andrew TI Flip-Flop of Oleic Acid in a Phospholipid Membrane: Rate and Mechanism SO JOURNAL OF PHYSICAL CHEMISTRY B LA English DT Article ID CHAIN FATTY-ACID; MOLECULAR-DYNAMICS SIMULATION; PROTON-HYDROXYL PERMEABILITY; LARGE UNILAMELLAR LIPOSOMES; LIPID-BILAYERS; MODEL PROTOCELLS; TRANSPORT; CHOLESTEROL; KINETICS; PERMEATION AB Flip-flop of protonated oleic acid molecules dissolved at two different concentrations in membranes made of 1-palmitoyl-2-oleoyl-sn-glycero-3-phosphocholine is studied with the aid of molecular dynamics simulations at a time scale of several microseconds. Direct, single-molecule flip-flop events are observed at this time scale, and the flip-flop rate is estimated at 0.20.3 mu s1. As oleic acid molecules move toward the center of the bilayer during flip-flop, they undergo gradual, correlated translational, and rotational motion. Rare, double-flipping events of two hydrogen-bonded oleic acid molecules are also observed. A two-dimensional free energy surface is obtained for the translational and rotational degree of freedom of the oleic acid molecule, and the minimum energy path on this surface is determined. A barrier to flip-flop of similar to 4.2 kcal/mol is found at the center of the bilayer. A two-dimensional diffusion model is found to provide a good description of the flip-flop process. The fast flip-flop rate lends support to the proposal that fatty acids permeate membranes without assistance of transport proteins. It also suggests that desorption rather than flip-flop is the rate-limiting step in fatty acid transport through membranes. The relation of flip-flop rates to the evolution of ancestral cellular systems is discussed. C1 [Wei, Chenyu; Pohorille, Andrew] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Wei, Chenyu; Pohorille, Andrew] Univ Calif San Francisco, Dept Pharmaceut Chem, San Francisco, CA 94143 USA. RP Wei, CY (reprint author), NASA, Ames Res Ctr, Mail Stop 229-1, Moffett Field, CA 94035 USA. EM chenyu.wei@nasa.gov; andrew.pohorille@nasa.gov FU NASA FX This work was supported by the NASA Exobiology Program. All simulations were performed at the NASA Advanced Supercomputing (NAS) Division and on the Anton computer at the Pittsburgh Supercomputer Center. NR 73 TC 8 Z9 8 U1 1 U2 22 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1520-6106 J9 J PHYS CHEM B JI J. Phys. Chem. B PD NOV 13 PY 2014 VL 118 IS 45 BP 12919 EP 12926 DI 10.1021/jp508163e PG 8 WC Chemistry, Physical SC Chemistry GA AT5IH UT WOS:000344976600012 PM 25319959 ER PT J AU Kim, JW Sauti, G Siochi, EJ Smith, JG Wincheski, RA Cano, RJ Connell, JW Wise, KE AF Kim, Jae-Woo Sauti, Godfrey Siochi, Emilie J. Smith, Joseph G. Wincheski, Russell A. Cano, Roberto J. Connell, John W. Wise, Kristopher E. TI Toward High Performance Thermoset/Carbon Nanotube Sheet Nanocomposites via Resistive Heating Assisted Infiltration and Cure SO ACS APPLIED MATERIALS & INTERFACES LA English DT Article DE thermoset/carbon nanotube; nanocomposite; resistive heating ID MULTIWALLED CARBON NANOTUBES; POLYMER COMPOSITES; MECHANICAL-PROPERTIES; SHEET/BISMALEIMIDE NANOCOMPOSITES; STRENGTH; FIBERS; FILMS; MATRIX; OPPORTUNITIES; CHALLENGES AB Thermoset/carbon nanotube (CNT) sheet nanocomposites were successfully fabricated by resistive heating assisted infiltration and cure (RHAIC) of the polymer matrix resin. Resistive heating takes advantage of the electrical and thermal conductivity of CNTs to rapidly and uniformly introduce heat into the CNT sheet. Heating the CNT sheet reduces the viscosity of the polymer resin due to localized temperature rise in close proximity to the resin, which enhances resin flow, penetration, and wetting of the CNT reinforcement. Once the resin infusion process is complete, the applied power is increased to raise the temperature of the CNT sheet, which rapidly cures the polymer matrix. Tensile tests were used to evaluate the mechanical properties of the processed thermoset/CNT sheet nanocomposites. The improved wetting and adhesion of the polymer resin to the CNT reinforcement yield significant improvement of thermoset/CNT nanocomposite mechanical properties. The highest specific tensile strength of bismaleimide(BMI)/CNT sheet nanocomposites was obtained to date was 684 MPa/(g/cm(3)), using 4 V (2 A) for resin infiltration, followed by precure at 10 V (6 A) for 10 min and post curing at 240 degrees C for 6 h in an oven. The highest specific Young's modulus of BMI/CNT sheet nanocomposite was 71 GPa/(g/cm(3)) using resistive heating infiltration at 8.3 V (4.7 A) for 3 min followed by resistive heating cure at 12.5 V (7 A) for 30 min. In both cases, the CNT sheets were stretched and held in tension to prevent relaxation of the aligned CNTs during the course of RHAIC. C1 [Kim, Jae-Woo; Sauti, Godfrey] Natl Inst Aerosp, Hampton, VA 23666 USA. [Siochi, Emilie J.; Smith, Joseph G.; Cano, Roberto J.; Connell, John W.; Wise, Kristopher E.] NASA Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. [Wincheski, Russell A.] NASA Langley Res Ctr, Nondestruct Evaluat Sci Branch, Hampton, VA 23681 USA. RP Kim, JW (reprint author), Natl Inst Aerosp, Hampton, VA 23666 USA. EM jae-woo.kim-1@nasa.gov; emilie.j.siochi@nasa.gov RI Kim, Jae-Woo/A-8314-2008 FU NASA FX This work was funded through the NASA Game Changing Development Program/Nanotechnology Project. NR 59 TC 7 Z9 8 U1 3 U2 45 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 NOV 12 PY 2014 VL 6 IS 21 BP 18832 EP 18843 DI 10.1021/am5046718 PG 12 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Science & Technology - Other Topics; Materials Science GA AT5IY UT WOS:000344978200060 PM 25325388 ER PT J AU van Haasteren, R Vallisneri, M AF van Haasteren, Rutger Vallisneri, Michele TI New advances in the Gaussian-process approach to pulsar-timing data analysis SO PHYSICAL REVIEW D LA English DT Article ID BLACK-HOLE BINARIES; GRAVITATIONAL-WAVES; GENERAL-RELATIVITY; LIMITS; ARRAY; DISPERSION; RADIATION; SYSTEMS; NOISE; PROBE AB In this work we review the application of the theory of Gaussian processes to the modeling of noise in pulsar-timing data analysis, and we derive various useful and optimized representations for the likelihood expressions that are needed in Bayesian inference on pulsar-timing-array data sets. The resulting viewpoint and formalism lead us to two improved parameter-sampling schemes inspired by Gibbs sampling. The new schemes have vastly lower chain autocorrelation lengths than the Markov-chain Monte Carlo methods currently used in pulsar-timing data analysis, potentially speeding up Bayesian inference by orders of magnitude. The new schemes can be used for a full-noise-model analysis of the large data sets currently being assembled by pulsar-timing-array collaborations, which generally present a serious computational challenge to existing methods. C1 [van Haasteren, Rutger; Vallisneri, Michele] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP van Haasteren, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM vhaasteren@gmail.com FU NASA Einstein Fellowship [PF3-140116]; Jet Propulsion Laboratory RTD program; National Aeronautics and Space Administration FX We are grateful to many NANOGrav and European Pulsar Timing Array colleagues for helpful discussions, to Scott Ransom for use of the NRAO Nimrod cluster, where our tests were run, and to Stephen Taylor and an anonymous referee for useful comments. R. v. H. is supported by NASA Einstein Fellowship Grant No. PF3-140116. M. V. is supported by the Jet Propulsion Laboratory RTD program. The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Government sponsorship is acknowledged. NR 73 TC 11 Z9 11 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD NOV 11 PY 2014 VL 90 IS 10 AR 104012 DI 10.1103/PhysRevD.90.104012 PG 21 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AU3SS UT WOS:000345534500009 ER PT J AU Elsaesser, A Quinn, RC Ehrenfreund, P Mattioda, AL Ricco, AJ Alonzo, J Breitenbach, A Chan, YK Fresneau, A Salama, F Santos, O AF Elsaesser, Andreas Quinn, Richard C. Ehrenfreund, Pascale Mattioda, Andrew L. Ricco, Antonio J. Alonzo, Jason Breitenbach, Alex Chan, Yee Kim Fresneau, Aurelien Salama, Farid Santos, Orlando TI Organics Exposure in Orbit (OREOcube): A Next-Generation Space Exposure Platform SO LANGMUIR LA English DT Article ID POLYCYCLIC AROMATIC-HYDROCARBONS; O/OREOS MISSION; ENVIRONMENT VIABILITY; COMET 81P/WILD-2; MARTIAN SOIL; UV; MOLECULES; ASTROBIOLOGY; ABSORPTION; METEORITES AB The OREOcube (ORganics Exposure in Orbit cube) experiment on the International Space Station (ISS) will investigate the effects of solar and cosmic radiation on organic thin films supported on inorganic substrates. Probing the kinetics of structural changes and photomodulated organicinorganic interactions with real-time in situ UVvisible spectroscopy, this experiment will investigate the role played by solid mineral surfaces in the (photo)chemical evolution, transport, and distribution of organics in our solar system and beyond. In preparation for the OREOcube ISS experiment, we report here laboratory measurements of the photostability of thin films of the 9,10-anthraquinone derivative anthrarufin (51 nm thick) layered upon ultrathin films of iron oxides magnetite and hematite (4 nm thick), as well as supported directly on fused silica. During irradiation with UV and visible light simulating the photon flux and spectral distribution on the surface of Mars, anthrarufin/iron oxide bilayer thin films were exposed to CO2 (800 Pa), the main constituent (and pressure) of the martian atmosphere. The time-dependent photodegradation of anthrarufin thin films revealed the inhibition of degradation by both types of underlying iron oxides relative to anthrarufin on bare fused silica. Interactions between the organic and inorganic thin films, apparent in spectral shifts of the anthrarufin bands, are consistent with presumed free-electron quenching of semiquinone anion radicals by the iron oxide layers, effectively protecting the organic compound from photodegradation. Combining such in situ real-time kinetic measurements of thin films in future space exposure experiments on the ISS with postflight sample return and analysis will provide time-course studies complemented by in-depth chemical analysis. This will facilitate the characterization and modeling of the chemistry of organic species associated with mineral surfaces in astrobiological contexts. C1 [Elsaesser, Andreas; Ehrenfreund, Pascale; Fresneau, Aurelien] Leiden Univ, Leiden Inst Chem, NL-2333 CC Leiden, Netherlands. [Quinn, Richard C.; Alonzo, Jason; Breitenbach, Alex; Chan, Yee Kim] NASA, Ames Res Ctr, SETI Inst, Carl Sagan Ctr, Moffett Field, CA 94035 USA. [Mattioda, Andrew L.; Ricco, Antonio J.; Salama, Farid; Santos, Orlando] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Alonzo, Jason] Calif State Polytech Univ Pomona, Dept Phys & Astron, Pomona, CA 91768 USA. [Breitenbach, Alex; Chan, Yee Kim] San Jose State Univ, San Jose, CA 95112 USA. RP Elsaesser, A (reprint author), Leiden Univ, Leiden Inst Chem, NL-2333 CC Leiden, Netherlands. EM a.elsaesser@umail.leidenuniv.nl; richard.c.quinn@nasa.gov; ajricco@stanford.edu RI Elsaesser, Andreas/K-2264-2014; Salama, Farid/A-8787-2009; OI Salama, Farid/0000-0002-6064-4401; Ricco, Antonio/0000-0002-2355-4984 FU Netherlands Organisation for Scientific Research; NASA Astrobiology Science and Technology Instrument Development (ASTID) program; San Jose State University; SETI Institute; National Science Foundation [AST-0847170]; PAARE grant for the California-Arizona Minority Partnership for Astronomy Research and Education FX We gratefully acknowledge helpful discussions regarding thin-film optical effects with Dr. Nathan Bramall of Los Gatos Research, Inc. The European participation in OREOcube is funded by The Netherlands Organisation for Scientific Research (Evolution of organics in space: OREOcube in situ spectroscopy). OREOcube was proposed to the International Research Announcement for Research in Space Life Sciences (ILSRA 2009) and selected for Definition Phase by the European Space Agency (ESA). U.S. participation in OREOcube is funded by the NASA Astrobiology Science and Technology Instrument Development (ASTID) program. We thank Dr. Monika Kress (San Jose State University) and Dr. Cynthia B. Phillips (SETI Institute) for providing partial funding for A.B. and Y.K.C. through the Undergraduate Research at SETI Institute in Astrobiology (URSA) Program (a NASA Education and Public Outreach in Earth and Space Science program award). Partial funding for J.A. was provided by National Science Foundation award no. AST-0847170, a PAARE grant for the California-Arizona Minority Partnership for Astronomy Research and Education (Dr. Alex Rudolph, Director). NR 60 TC 0 Z9 0 U1 2 U2 11 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0743-7463 J9 LANGMUIR JI Langmuir PD NOV 11 PY 2014 VL 30 IS 44 BP 13217 EP 13227 DI 10.1021/la501203g PG 11 WC Chemistry, Multidisciplinary; Chemistry, Physical; Materials Science, Multidisciplinary SC Chemistry; Materials Science GA AT4JG UT WOS:000344905100012 PM 24851720 ER PT J AU Hilker, T Lyapustin, AI Tucker, CJ Hall, FG Myneni, RB Wang, YJ Bi, J de Moura, YM Sellers, PJ AF Hilker, Thomas Lyapustin, Alexei I. Tucker, Compton J. Hall, Forrest G. Myneni, Ranga B. Wang, Yujie Bi, Jian de Moura, Yhasmin Mendes Sellers, Piers J. TI Vegetation dynamics and rainfall sensitivity of the Amazon SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Amazon; climate change; precipitation; NDVI; MODIS; MAIAC ID FORESTS GREEN-UP; CLIMATE-CHANGE; BRAZILIAN AMAZON; DRY-SEASON; INTERANNUAL VARIABILITY; ATMOSPHERIC CORRECTION; DROUGHT SENSITIVITY; DEFORESTATION; SATELLITE; INDEXES AB We show that the vegetation canopy of the Amazon rainforest is highly sensitive to changes in precipitation patterns and that reduction in rainfall since 2000 has diminished vegetation greenness across large parts of Amazonia. Large-scale directional declines in vegetation greenness may indicate decreases in carbon uptake and substantial changes in the energy balance of the Amazon. We use improved estimates of surface reflectance from satellite data to show a close link between reductions in annual precipitation, El Nino southern oscillation events, and photosynthetic activity across tropical and subtropical Amazonia. We report that, since the year 2000, precipitation has declined across 69% of the tropical evergreen forest (5.4 million km(2)) and across 80% of the subtropical grasslands (3.3 million km(2)). These reductions, which coincided with a decline in terrestrial water storage, account for about 55% of a satellite-observed widespread decline in the normalized difference vegetation index (NDVI). During El Nino events, NDVI was reduced about 16.6% across an area of up to 1.6 million km(2) compared with average conditions. Several global circulation models suggest that a rise in equatorial sea surface temperature and related displacement of the intertropical convergence zone could lead to considerable drying of tropical forests in the 21st century. Our results provide evidence that persistent drying could degrade Amazonian forest canopies, which would have cascading effects on global carbon and climate dynamics. C1 [Hilker, Thomas] Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA. [Lyapustin, Alexei I.; Tucker, Compton J.; Hall, Forrest G.; Wang, Yujie; Sellers, Piers J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hall, Forrest G.; Wang, Yujie] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. [Myneni, Ranga B.; Bi, Jian] Boston Univ, Dept Earth & Environm, Boston, MA 02215 USA. [de Moura, Yhasmin Mendes] Inst Nacl Pesquisas Espaciais, Div Sensoriamento Remoto, BR-12245970 Sao Jose Dos Campos, SP, Brazil. RP Hilker, T (reprint author), Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA. EM thomas.hilker@oregonstate.edu RI Myneni, Ranga/F-5129-2012; OI Moura, Yhasmin/0000-0001-8494-8787 FU Science of Terra and Aqua Program of NASA FX We thank Dr. Richard H. Waring (Oregon State University) for helpful discussions and comments and Dr. Lars Eklundh (Lund University) for help with the time-series algorithm. We also thank the NASA Center for Climate Simulation for computational support and access to their high-performance cluster. This work was supported by the Science of Terra and Aqua Program of NASA (A. I. L. and Y.W.). NR 65 TC 58 Z9 60 U1 13 U2 122 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD NOV 11 PY 2014 VL 111 IS 45 BP 16041 EP 16046 DI 10.1073/pnas.1404870111 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AS8WW UT WOS:000344526800051 PM 25349419 ER PT J AU van der Horst, AJ Paragi, Z de Bruyn, AG Granot, J Kouveliotou, C Wiersema, K Starling, RLC Curran, PA Wijers, RAMJ Rowlinson, A Anderson, GA Fender, RP Yang, J Strom, RG AF van der Horst, A. J. Paragi, Z. de Bruyn, A. G. Granot, J. Kouveliotou, C. Wiersema, K. Starling, R. L. C. Curran, P. A. Wijers, R. A. M. J. Rowlinson, A. Anderson, G. A. Fender, R. P. Yang, J. Strom, R. G. TI A comprehensive radio view of the extremely bright gamma-ray burst 130427A SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gamma-ray burst: individual: GRB 130427A ID GRB 130427A; INTERSTELLAR SCINTILLATION; CIRCULAR-POLARIZATION; COLLISIONLESS SHOCKS; QUASAR J1819+3845; OPTICAL AFTERGLOW; ORDINARY MONSTER; MAGNETIC-FIELD; EMISSION; STARS AB GRB130427A was extremely bright as a result of occurring at low redshift whilst the energetics were more typical of high-redshift gamma-ray bursts (GRBs). We collected well-sampled light curves at 1.4 and 4.8 GHz of GRB 130427A with the Westerbork Synthesis Radio Telescope (WSRT); and we obtained its most accurate position with the European Very Long Baseline Interferometry Network (EVN). Our flux density measurements are combined with all the data available at radio, optical and X-ray frequencies to perform broad-band modelling in the framework of a reverse-forward shock model and a two-component jet model, and we discuss the implications and limitations of both models. The low density inferred from the modelling implies that the GRB 130427A progenitor is either a very low metallicity Wolf-Rayet star, or a rapidly rotating, low-metallicity O star. We also find that the fraction of the energy in electrons is evolving over time, and that the fraction of electrons participating in a relativistic power-law energy distribution is less than 15 per cent. We observed intraday variability during the earliest WSRT observations, and the source sizes inferred from our modelling are consistent with this variability being due to interstellar scintillation effects. Finally, we present and discuss our limits on the linear and circular polarization, which are among the deepest limits of GRB radio polarization to date. C1 [van der Horst, A. J.; Wijers, R. A. M. J.; Rowlinson, A.] Univ Amsterdam, Anton Pannekoek Inst, NL-1098 XH Amsterdam, Netherlands. [Paragi, Z.; Yang, J.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [de Bruyn, A. G.; Strom, R. G.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [de Bruyn, A. G.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Granot, J.] Open Univ Israel, Dept Nat Sci, IL-43537 Raanana, Israel. [Kouveliotou, C.] NASA, Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. [Wiersema, K.; Starling, R. L. C.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Curran, P. A.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Anderson, G. A.; Fender, R. P.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Anderson, G. A.; Fender, R. P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Yang, J.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, SE-43992 Onsala, Sweden. RP van der Horst, AJ (reprint author), Univ Amsterdam, Anton Pannekoek Inst, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. EM A.J.vanderHorst@uva.nl OI Wijers, Ralph/0000-0002-3101-1808; Anderson, Gemma/0000-0001-6544-8007 FU Netherlands foundation for Scientific Research; European Commission [283393]; European Research Council [247295, 267697]; STFC; Royal Society; Australian Research Council [DP120102393]; European national research council; Chinese national research council; South African national research council FX AJvdH would like to thank Alex de Koter, Stan Woosley and Enrico Ramirez-Ruiz for helpful discussions. We greatly appreciate the support from the WSRT staff in their help with scheduling and obtaining the observations presented in this paper. The WSRT is operated by ASTRON (Netherlands Institute for Radio Astronomy) with support from the Netherlands foundation for Scientific Research. The EVN (http://www.evlbi.org) is a joint facility of European, Chinese, South African and other radio astronomy institutes funded by their national research councils. The research leading to these results has received funding from the European Commission Seventh Framework Programme (FP/2007-2013) under grant agreement no. 283393 (RadioNet3). AIPS is produced and maintained by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. AJvdH, RAMJW and AR acknowledge the support of the European Research Council Advanced Investigator Grant no. 247295. KW acknowledges support from STFC. RLCS is supported by a Royal Society Fellowship. PAC is supported by Australian Research Council grant DP120102393. GEA and RPF acknowledge the support of the European Research Council Advanced Investigator Grant no. 267697. NR 78 TC 14 Z9 14 U1 1 U2 8 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 11 PY 2014 VL 444 IS 4 BP 3151 EP 3163 DI 10.1093/mnras/stu1664 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR2FW UT WOS:000343400100012 ER PT J AU Zhu, XJ Hobbs, G Wen, L Coles, WA Wang, JB Shannon, RM Manchester, RN Bailes, M Bhat, NDR Burke-Spolaor, S Dai, S Keith, MJ Kerr, M Levin, Y Madison, DR Oslowski, S Ravi, V Toomey, L van Straten, W AF Zhu, X-J Hobbs, G. Wen, L. Coles, W. A. Wang, J-B Shannon, R. M. Manchester, R. N. Bailes, M. Bhat, N. D. R. Burke-Spolaor, S. Dai, S. Keith, M. J. Kerr, M. Levin, Y. Madison, D. R. Oslowski, S. Ravi, V. Toomey, L. van Straten, W. TI An all-sky search for continuous gravitational waves in the Parkes Pulsar Timing Array data set SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational waves; methods: data analysis; pulsars: general; galaxies: evolution ID BLACK-HOLE BINARIES; COALESCENCE RATE; 3C 66B; LIMITS; BAND; PACKAGE; SYSTEMS; TEMPO2; SIGNAL AB We present results of an all-sky search in the Parkes Pulsar Timing Array (PPTA) Data Release 1 data set for continuous gravitational waves (GWs) in the frequency range from 5 x 10(-9) to 2 x 10(-7) Hz. Such signals could be produced by individual supermassive binary black hole systems in the early stage of coalescence. We phase up the pulsar timing array data set to form, for each position on the sky, two data streams that correspond to the two GW polarizations and then carry out an optimal search for GW signals on these data streams. Since no statistically significant GWs were detected, we place upper limits on the intrinsic GW strain amplitude h(0) for a range of GW frequencies. For example, at 10(-8) Hz our analysis has excluded with 95 per cent confidence the presence of signals with h(0) >= 1.7 x 10(-14). Our new limits are about a factor of 4 more stringent than those of Yardley et al. based on an earlier PPTA data set and a factor of 2 better than those reported in the recent Arzoumanian et al. paper. We also present PPTA directional sensitivity curves and find that for the most sensitive region on the sky, the current data set is sensitive to GWs from circular supermassive binary black holes with chirp masses of 10(9) M-circle dot out to a luminosity distance of about 100 Mpc. Finally, we set an upper limit of 4 x 10(-3) Mpc(-3) Gyr(-1) at 95 per cent confidence on the coalescence rate of nearby (z less than or similar to 0.1) supermassive binary black holes in circular orbits with chirp masses of 10(10) M-circle dot. C1 [Zhu, X-J; Wen, L.] Univ Western Australia, Sch Phys, Crawley, WA 6009, Australia. [Zhu, X-J; Hobbs, G.; Wang, J-B; Shannon, R. M.; Manchester, R. N.; Dai, S.; Kerr, M.; Ravi, V.; Toomey, L.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Coles, W. A.] Univ Calif San Diego, Dept Elect & Comp Engn, La Jolla, CA 92093 USA. [Wang, J-B] Chinese Acad Sci, Xinjiang Astron Observ, Urumqi 830011, Xinjiang, Peoples R China. [Bailes, M.; van Straten, W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Bhat, N. D. R.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Burke-Spolaor, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Dai, S.] Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China. [Keith, M. J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Levin, Y.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Madison, D. R.] Cornell Univ, Dept Astron, Ithaca, NY 14850 USA. [Madison, D. R.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14850 USA. [Oslowski, S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Oslowski, S.] Univ Bielefeld, Dept Phys, D-33615 Bielefeld, Germany. [Ravi, V.] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia. RP Zhu, XJ (reprint author), Univ Western Australia, Sch Phys, Crawley, WA 6009, Australia. EM zhuxingjiang@gmail.com RI Zhu, Xingjiang/E-1501-2016; OI Zhu, Xingjiang/0000-0001-7049-6468; Shannon, Ryan/0000-0002-7285-6348; van Straten, Willem/0000-0003-2519-7375; Oslowski, Stefan/0000-0003-0289-0732 FU Commonwealth of Australia; University Postgraduate Award at UWA; UWA; Australian Research Council Future Fellowship; Australian Research Council; West Light Foundation of CAS [XBBS201322]; NSFC [11403086]; Science and Industry Endowment Fund FX We thank the anonymous referee for very useful comments on the manuscript. The Parkes radio telescope is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The work was supported by iVEC through the use of advanced computing resources located at iVEC@UWA. X-JZ thanks S. Chung and Y. Wang for useful discussions and acknowledges the support of an University Postgraduate Award at UWA. X-JZ additionally acknowledges the support for his attendance at the IPTA@Banff meeting in 2014 June from an University student travel award and a PSA travel award at UWA. GH is supported by an Australian Research Council Future Fellowship. LW acknowledges funding support from the Australian Research Council. J-BW is supported by West Light Foundation of CAS XBBS201322 and NSFC project No. 11403086. VR is a recipient of a John Stocker Postgraduate Scholarship from the Science and Industry Endowment Fund. NR 54 TC 24 Z9 25 U1 2 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 NOV 11 PY 2014 VL 444 IS 4 BP 3709 EP 3720 DI 10.1093/mnras/stu1717 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR2FW UT WOS:000343400100052 ER PT J AU Cohen, DH Li, ZQ Gayley, KG Owocki, SP Sundqvist, JO Petit, V Leutenegger, MA AF Cohen, David H. Li, Zequn Gayley, Kenneth G. Owocki, Stanley P. Sundqvist, Jon O. Petit, Veronique Leutenegger, Maurice A. TI Measuring the shock-heating rate in the winds of O stars using X-ray line spectra SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE hydrodynamics; line: profiles; shock waves; stars: massive; stars: winds,outflows; X-rays: stars ID DRIVEN STELLAR WINDS; ZETA-PUPPIS; MASS-LOSS; INTERSTELLAR-MEDIUM; EMISSION; PROFILES; SPECTROSCOPY; INSTABILITY; ABSORPTION; PARAMETERS AB We present a new method for using measured X-ray emission line fluxes from O stars to determine the shock-heating rate due to instabilities in their radiation-driven winds. The high densities of these winds means that their embedded shocks quickly cool by local radiative emission, while cooling by expansion should be negligible. Ignoring for simplicity any non-radiative mixing or conductive cooling, the method presented here exploits the idea that the cooling post-shock plasma systematically passes through the temperature characteristic of distinct emission lines in the X-ray spectrum. In this way, the observed flux distribution among these X-ray lines can be used to construct the cumulative probability distribution of shock strengths that a typical wind parcel encounters as it advects through the wind. We apply this new method to Chandra grating spectra from five O stars with X-ray emission indicative of embedded wind shocks in effectively single massive stars. The results for all the stars are quite similar: the average wind mass element passes through roughly one shock that heats it to at least 10(6) K as it advects through the wind, and the cumulative distribution of shock strengths is a strongly decreasing function of temperature, consistent with a negative power law of index n approximate to 3, implying a marginal distribution of shock strengths that scales as T-4, and with hints of an even steeper decline or cut-off above 10(7) K. C1 [Cohen, David H.; Li, Zequn] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [Gayley, Kenneth G.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Owocki, Stanley P.; Sundqvist, Jon O.; Petit, Veronique] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Sundqvist, Jon O.] Univ Munich, Inst Astron & Astrophys, D-81679 Munich, Germany. [Petit, Veronique] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Leutenegger, Maurice A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Leutenegger, Maurice A.] CRESST, Baltimore, MD 21250 USA. [Leutenegger, Maurice A.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. RP Cohen, DH (reprint author), Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. EM cohen@hven.astro.swarthmore.edu FU National Aeronautics and Space Administration through ADAP [NNX11AD26G]; National Aeronautics and Space Administration through Chandra grants [AR2-13001A, TM3-14001B]; National Aeronautics and Space Administration through ATP [NNX11AF83G, NNX11AC40G]; DFG [Pu117/8-1]; Physics and Astronomy Department; Provost's Office of Swarthmore College via a Vanderveld-Cheung Summer Research Fellowship FX Support for this work was provided by the National Aeronautics and Space Administration through ADAP grant NNX11AD26G and Chandra grants AR2-13001A and TM3-14001B to Swarthmore College, ATP grant NNX11AF83G to University of Iowa, and ATP grant NNX11AC40G to University of Delaware. JOS was supported by DFG grant Pu117/8-1. ZL was supported by the Physics and Astronomy Department and the Provost's Office of Swarthmore College via a Vanderveld-Cheung Summer Research Fellowship. We thank Randall Smith for his help and advice regarding ATOMDB, and we thank Marc Gagne for useful discussions about 9 Sgr. NR 43 TC 7 Z9 7 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 NOV 11 PY 2014 VL 444 IS 4 BP 3729 EP 3737 DI 10.1093/mnras/stu1661 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR2FW UT WOS:000343400100054 ER PT J AU Che, H Goldstein, ML AF Che, H. Goldstein, M. L. TI THE ORIGIN OF NON-MAXWELLIAN SOLAR WIND ELECTRON VELOCITY DISTRIBUTION FUNCTION: CONNECTION TO NANOFLARES IN THE SOLAR CORONA SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE acceleration of particles; instabilities; scattering; solar wind; Sun: corona; turbulence ID PARTICLE-ACCELERATION; MAGNETIC-FLUX; TEMPERATURE; FLARES; STRAHL; WAVES; LOOPS; HALO AB The formation of the observed core-halo feature in the solar wind electron velocity distribution function is a longtime puzzle. In this Letter, based on the current knowledge of nanoflares, we show that the nanoflare-accelerated electron beams are likely to trigger a strong electron two-stream instability that generates kinetic Alfven wave and whistler wave turbulence, as we demonstrated in a previous paper. We further show that the core-halo feature produced during the origin of kinetic turbulence is likely to originate in the inner corona and can be preserved as the solar wind escapes to space along open field lines. We formulate a set of equations to describe the heating processes observed in the simulation and show that the core-halo temperature ratio of the solar wind is insensitive to the initial conditions in the corona and is related to the core-halo density ratio of the solar wind and to the quasi-saturation property of the two-stream instability at the time when the exponential decay ends. This relation can be extended to the more general core-halo-strahl feature in the solar wind. The temperature ratio between the core and hot components is nearly independent of the heliospheric distance to the Sun. We show that the core-halo relative drift previously reported is a relic of the fully saturated two-stream instability. Our theoretical results are consistent with the observations while new tests for this model are provided. C1 [Che, H.; Goldstein, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Che, H (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. OI GOLDSTEIN, MELVYN/0000-0002-5317-988X; Che, Haihong/0000-0002-2240-6728 FU NASA Postdoctoral Program at NASA/GSFC; NASA [NNH11ZDA001N]; NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center FX H.C. is grateful to the helpful discussions with Drs. J. Klimchunk, B. Dennis, E. Marsch, and G. Gloeckler. The authors thank the anonymous referee whose comments helped make this manuscript more clear and readable. This research was supported by the NASA Postdoctoral Program at NASA/GSFC administered by Oak Ridge Associated Universities and NASA grant NNH11ZDA001N. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. NR 36 TC 13 Z9 13 U1 2 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 10 PY 2014 VL 795 IS 2 AR L38 DI 10.1088/2041-8205/795/2/L38 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU3FY UT WOS:000345499000014 ER PT J AU Cordiner, MA Nixon, CA Teanby, NA Irwin, PGJ Serigano, J Charnley, SB Milam, SN Mumma, MJ Lis, DC Villanueva, G Paganini, L Kuan, YJ Remijan, AJ AF Cordiner, M. A. Nixon, C. A. Teanby, N. A. Irwin, P. G. J. Serigano, J. Charnley, S. B. Milam, S. N. Mumma, M. J. Lis, D. C. Villanueva, G. Paganini, L. Kuan, Y. -J. Remijan, A. J. TI ALMA MEASUREMENTS OF THE HNC AND HC3N DISTRIBUTIONS IN TITAN'S ATMOSPHERE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planets and satellites: atmospheres; planets and satellites: individual (Titan); techniques: imaging spectroscopy; techniques: interferometric ID VIBRATIONALLY EXCITED-STATES; HYDROGEN ISOCYANIDE HNC; STRATOSPHERIC TEMPERATURE; ABUNDANCE; MILLIMETER; CHEMISTRY; HCN; CO AB We present spectrally and spatially resolved maps of HNC and HC3N emission from Titan's atmosphere, obtained using the Atacama Large Millimeter/submillimeter Array on 2013 November 17. These maps show anisotropic spatial distributions for both molecules, with resolved emission peaks in Titan's northern and southern hemispheres. The HC3N maps indicate enhanced concentrations of this molecule over the poles, consistent with previous studies of Titan's photochemistry and atmospheric circulation. Differences between the spectrally integrated flux distributions of HNC and HC3N show that these species are not co-spatial. The observed spectral line shapes are consistent with HNC being concentrated predominantly in the mesosphere and above (at altitudes z greater than or similar to 400 km), whereas HC3N is abundant at a broader range of altitudes (z approximate to 70-600 km). From spatial variations in the HC3N line profile, the locations of the HC3N emission peaks are shown to be variable as a function of altitude. The peaks in the integrated emission from HNC and the line core (upper atmosphere) component of HC3N (at z greater than or similar to 300 km) are found to be asymmetric with respect to Titan's polar axis, indicating that the mesosphere may be more longitudinally variable than previously thought. The spatially integrated HNC and HC3N spectra are modeled using the NEMESIS planetary atmosphere code and the resulting best-fitting disk-averaged vertical mixing ratio profiles are found to be in reasonable agreement with previous measurements for these species. Vertical column densities of the best-fitting gradient models for HNC and HC3N are 1.9 x 10(13) cm(-2) and 2.3 x 10(14) cm(-2), respectively. C1 [Cordiner, M. A.; Nixon, C. A.; Serigano, J.; Charnley, S. B.; Milam, S. N.; Mumma, M. J.; Villanueva, G.; Paganini, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cordiner, M. A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Teanby, N. A.] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England. [Irwin, P. G. J.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England. [Lis, D. C.] Univ Paris 06, Sorbonne Univ, CNRS, Observ Paris,LERMA,UMR 8112, F-75014 Paris, France. [Lis, D. C.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Kuan, Y. -J.] Natl Taiwan Normal Univ, Taipei 116, Taiwan. [Kuan, Y. -J.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Remijan, A. J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Cordiner, MA (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM martin.cordiner@nasa.gov RI Nixon, Conor/A-8531-2009; Milam, Stefanie/D-1092-2012; OI Nixon, Conor/0000-0001-9540-9121; Milam, Stefanie/0000-0001-7694-4129; Teanby, Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X; Mumma, Michael/0000-0003-4627-750X FU NASA; Leverhulme Trust; UK Science and Technology Facilities Council FX This research was supported by NASA's Planetary Atmospheres, Planetary Astronomy, and Astrobiology Programs, by The Leverhulme Trust and the UK Science and Technology Facilities Council. This Letter makes use of the following ALMA data: ADS/JAO.ALMA#2012.A.00033.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 24 TC 9 Z9 9 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 10 PY 2014 VL 795 IS 2 AR L30 DI 10.1088/2041-8205/795/2/L30 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU3FY UT WOS:000345499000006 ER PT J AU Awaki, H Kunieda, H Ishida, M Matsumoto, H Babazaki, Y Demoto, T Furuzawa, A Haba, Y Hayashi, T Iizuka, R Ishibashi, K Ishida, N Itoh, M Iwase, T Kosaka, T Kurihara, D Kuroda, Y Maeda, Y Meshino, Y Mitsuishi, I Miyata, Y Miyazawa, T Mori, H Nagano, H Namba, Y Ogasaka, Y Ogi, K Okajima, T Saji, S Shimasaki, F Sato, T Sato, T Sugita, S Suzuki, Y Tachibana, K Tachibana, S Takizawa, S Tamura, K Tawara, Y Torii, T Uesugi, K Yamashita, K Yamauchi, S AF Awaki, Hisamitsu Kunieda, Hideyo Ishida, Manabu Matsumoto, Hironori Babazaki, Yasunori Demoto, Tadatsugu Furuzawa, Akihiro Haba, Yoshito Hayashi, Takayuki Iizuka, Ryo Ishibashi, Kazunori Ishida, Naoki Itoh, Masayuki Iwase, Toshihiro Kosaka, Tatsuro Kurihara, Daichi Kuroda, Yuuji Maeda, Yoshitomo Meshino, Yoshifumi Mitsuishi, Ikuyuki Miyata, Yuusuke Miyazawa, Takuya Mori, Hideyuki Nagano, Housei Namba, Yoshiharu Ogasaka, Yasushi Ogi, Keiji Okajima, Takashi Saji, Shigetaka Shimasaki, Fumiya Sato, Takuro Sato, Toshiki Sugita, Satoshi Suzuki, Yoshio Tachibana, Kenji Tachibana, Sasagu Takizawa, Shunya Tamura, Keisuke Tawara, Yuzuru Torii, Tatsuharu Uesugi, Kentato Yamashita, Koujun Yamauchi, Shigeo TI Hard x-ray telescopes to be onboard ASTRO-H SO APPLIED OPTICS LA English DT Article ID SCATTERING; SPRING-8; ASCA AB The new Japanese x-ray astronomy satellite, ASTRO-H, will carry two identical hard x-ray telescopes (HXTs), which cover the energy range of 5 to 80 keV. The HXT mirrors employ tightly nested, conically approximated thin-foil Wolter-I optics, and the mirror surfaces are coated with Pt/C depth-graded multilayers to enhance the hard x-ray effective area by means of Bragg reflection. The HXT comprises foils 120-450 mm in diameter and 200 mm in length, with a focal length of 12 m. To obtain a large effective area, 213 aluminum foils 0.2 mm in thickness are tightly nested confocally. The requirements for HXT are a total effective area of >300 cm(2) at 30 keV and an angular resolution of <1.7' in half-power diameter (HPD). Fabrication of two HXTs has been completed, and the x-ray performance of each HXT was measured at a synchrotron radiation facility, SPring-8 BL20B2 in Japan. Angular resolutions (HPD) of 1.9' and 1.8' at 30 keV were obtained for the full telescopes of HXT-1 and HXT-2, respectively. The total effective area of the two HXTs at 30 keV is 349 cm(2). (C) 2014 Optical Society of America C1 [Awaki, Hisamitsu; Kurihara, Daichi; Ogi, Keiji; Sugita, Satoshi] Ehime Univ, Matsuyama, Ehime 7908577, Japan. [Kunieda, Hideyo; Matsumoto, Hironori; Babazaki, Yasunori; Demoto, Tadatsugu; Furuzawa, Akihiro; Ishibashi, Kazunori; Iwase, Toshihiro; Kuroda, Yuuji; Meshino, Yoshifumi; Mitsuishi, Ikuyuki; Miyata, Yuusuke; Miyazawa, Takuya; Mori, Hideyuki; Nagano, Housei; Saji, Shigetaka; Shimasaki, Fumiya; Tachibana, Kenji; Tachibana, Sasagu; Takizawa, Shunya; Tamura, Keisuke; Tawara, Yuzuru; Torii, Tatsuharu; Yamashita, Koujun] Nagoya Univ, Nagoya, Aichi 4648602, Japan. [Ishida, Manabu; Hayashi, Takayuki; Maeda, Yoshitomo; Sato, Takuro; Sato, Toshiki] ISAS JAXA, Sagamihara, Kanagawa 2298510, Japan. [Haba, Yoshito] Aichi Univ Educ, Kariya, Aichi 4488542, Japan. [Ishida, Naoki] Tamagawa Engn Co Ltd, Chifu Ku, Kasugai, Aichi 4800304, Japan. [Itoh, Masayuki] Kobe Univ, Kobe, Hyogo 6578501, Japan. [Kosaka, Tatsuro] Kochi Univ Technol, Kami, Kochi 7828502, Japan. [Namba, Yoshiharu] Chubu Univ, Kasugai, Aichi 4878501, Japan. [Ogasaka, Yasushi] Japan Sci & Technol Agcy, Chiyoda Ku, Tokyo 1020076, Japan. [Okajima, Takashi] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Sato, Takuro; Sato, Toshiki] Tokyo Metropolitan Univ, Hachioji, Tokyo 1920397, Japan. [Suzuki, Yoshio; Uesugi, Kentato; Yamashita, Koujun] JASRI SPring 8, Sayo, Hyogo 6795198, Japan. [Yamauchi, Shigeo] Nara Womens Univ, Nara 6308506, Japan. RP Awaki, H (reprint author), Ehime Univ, Bunkyo Cho, Matsuyama, Ehime 7908577, Japan. EM awaki@astro.phys.sci.ehime-u.ac.jp FU Japan Synchrotron Radiation Research Institute (JASRI) [2009A0088, 2009B0088, 2010A0088, 2010B0088, 2011A0088, 2011B0088, 2012A0088, 2012B0088, 2013A0088, 2013B0088] FX The authors are grateful to all full-time engineers and part-time workers at Nagoya University for support in the mass production of the HXT mirror reflectors. We thank Dr. Hans Krimm (NASA/GSFC) for his comments. We also thank the referee for the valuable comments. The x-ray measurement was performed at BL20B2 in SPring-8, with the approval of the Japan Synchrotron Radiation Research Institute (JASRI) (Proposal Nos. 2009A0088, 2009B0088, 2010A0088, 2010B0088, 2011A0088, 2011B0088, 2012A0088, 2012B0088, 2013A0088, and 2013B0088). NR 28 TC 13 Z9 13 U1 1 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 NOV 10 PY 2014 VL 53 IS 32 BP 7664 EP 7676 DI 10.1364/AO.53.007664 PG 13 WC Optics SC Optics GA AT7GF UT WOS:000345104100009 PM 25402988 ER PT J AU Hoglund, L Ting, DZ Soibel, A Fisher, A Khoshakhlagh, A Hill, CJ Keo, S Gunapala, SD AF Hoeglund, L. Ting, D. Z. Soibel, A. Fisher, A. Khoshakhlagh, A. Hill, C. J. Keo, S. Gunapala, S. D. TI Minority carrier lifetime in mid-wavelength infrared InAs/InAsSb superlattices: Photon recycling and the role of radiative and Shockley-Read-Hall recombination mechanisms SO APPLIED PHYSICS LETTERS LA English DT Article ID GAAS AB The influence of radiative recombination on the minority carrier lifetime in mid-wavelength InAs/InAsSb superlattices was investigated. From the lifetime's dependence on temperature, photon recycling, and carrier concentration, it was demonstrated that radiative lifetime dominates for carrier concentrations >5 x 10(14) cm(-3), and Shockley-Read-Hall recombination starts to dominate the minority carrier lifetime for carrier concentrations <5 x 10(14) cm(-3). An observed increase of the minority carrier lifetime with increasing superlattice thickness was attributed to photon recycling, and good agreement between measured and theoretical values of the photon recycling factor was obtained. (C) 2014 AIP Publishing LLC. C1 [Hoeglund, L.; Ting, D. Z.; Soibel, A.; Fisher, A.; Khoshakhlagh, A.; Hill, C. J.; Keo, S.; Gunapala, S. D.] CALTECH, Jet Prop Lab, Ctr Infrared Photodetectors, Pasadena, CA 91109 USA. RP Hoglund, L (reprint author), CALTECH, Jet Prop Lab, Ctr Infrared Photodetectors, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Soibel, Alexander/A-1313-2007 FU National Aeronautics and Space Administration FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 9 TC 10 Z9 10 U1 2 U2 39 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD NOV 10 PY 2014 VL 105 IS 19 AR 193510 DI 10.1063/1.4902022 PG 5 WC Physics, Applied SC Physics GA AT8YZ UT WOS:000345216100084 ER PT J AU Machacek, JR Mahapatra, DP Schultz, DR Ralchenko, Y Chutjian, A Simcic, J Mawhorter, RJ AF Machacek, J. R. Mahapatra, D. P. Schultz, D. R. Ralchenko, Yu. Chutjian, A. Simcic, J. Mawhorter, R. J. TI Measurement and calculation of absolute single- and double-charge-exchange cross sections for O6+ ions at 1.17 and 2.33 keV/u impacting He and H-2 SO PHYSICAL REVIEW A LA English DT Article ID ELECTRON-CAPTURE COLLISIONS; X-RAY-EMISSION; LOW-ENERGY COLLISIONS; FULLY STRIPPED IONS; SOLAR-WIND; INTERMEDIATE ENERGIES; MOLECULAR-HYDROGEN; SLOW COLLISIONS; KEV AMU-1; O-6+ AB Absolute single-and double-charge-exchange cross sections for the astrophysically prominent O6+ ion with the atomic and molecular targets He and H-2 are reported. These collisions give rise to x-ray emissions in the interplanetary medium, planetary atmospheres, and comets as they approach the sun. Measurements have been carried out using the Caltech Jet Propulsion Laboratory electron cyclotron resonance ion source with O6+ at energies of 1.17 and 2.33 keV/u characteristic of the slow and fast components of the solar wind. Absolute charge-exchange (CE) data are derived from knowledge of the target gas pressure, target path length, incident ion current, and charge-exchanged ion currents. These data are compared with results obtained using the n-electron classical trajectory Monte Carlo method. The radiative and Auger evolution of ion populations following one- and two-electron transfers is calculated with the time-dependent collisional-radiative code NOMAD using atomic data from the flexible atomic code. Calculated CE emission spectra for 100 angstrom < lambda < 1400 angstrom are reported as well and compared with experimental sublevel spectra and cross sections. C1 [Machacek, J. R.; Mahapatra, D. P.; Chutjian, A.] CALTECH, Jet Prop Lab, Atom & Mol Phys Grp, Pasadena, CA 91109 USA. [Schultz, D. R.] Univ N Texas, Dept Phys, Denton, TX 76203 USA. [Ralchenko, Yu.] NIST, Atom Spect Grp, Gaithersburg, MD 20899 USA. [Simcic, J.] CALTECH, Planetary Surface Instruments Grp, Jet Prop Lab, Pasadena, CA 91109 USA. [Mawhorter, R. J.] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA. RP Machacek, JR (reprint author), CALTECH, Jet Prop Lab, Atom & Mol Phys Grp, Pasadena, CA 91109 USA. RI Ralchenko, Yuri/E-9297-2016; Machacek, Joshua/A-5316-2011 OI Ralchenko, Yuri/0000-0003-0083-9554; FU NASA through the NASA Senior Research Associate Program; NASA; California Institute of Technology FX D.P.M. gratefully acknowledges support from NASA through the NASA Senior Research Associate Program managed by the Oak Ridge Associated Universities and Y.R. gratefully acknowledges partial support from NASA. The experimental work was carried out at the JPL, Caltech and was supported by NASA through an agreement with the California Institute of Technology. NR 54 TC 2 Z9 2 U1 0 U2 11 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD NOV 10 PY 2014 VL 90 IS 5 AR 052708 DI 10.1103/PhysRecA.90.052708 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AT4MW UT WOS:000344914400015 ER PT J AU Boersma, C Bregman, J Allamandola, LJ AF Boersma, C. Bregman, J. Allamandola, L. J. TI PROPERTIES OF POLYCYCLIC AROMATIC HYDROCARBONS IN THE NORTHWEST PHOTON DOMINATED REGION OF NGC 7023. II. TRADITIONAL PAH ANALYSIS USING k-MEANS AS A VISUALIZATION TOOL SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; infrared: ISM; ISM: individual objects (NGC 7023); techniques: spectroscopic ID INFRARED-EMISSION FEATURES; BLIND SIGNAL SEPARATION; SPITZER-SPACE-TELESCOPE; HERBIG AE/BE STARS; MU-M; SPECTROSCOPIC DATABASE; REFLECTION NEBULAE; PHOTODISSOCIATION REGIONS; BENDING MODES; ORION BAR AB Polycyclic aromatic hydrocarbon (PAH) emission in the Spitzer-IRS spectralmap of the northwest photon dominated region (PDR) in NGC 7023 is analyzed using the "traditional" approach in which the PAH bands and plateaus between 5.2-19.5 mu m are isolated by subtracting the underlying continuum and removing H-2 emission lines. The spectra are organized into seven spectroscopic bins by using k-means clustering. Each cluster corresponds to, and reveals, a morphological zone within NGC 7023. The zones self-organize parallel to the well-defined PDR front that coincides with an increase in intensity of the H-2 emission lines. PAH band profiles and integrated strengths are measured, classified, and mapped. The morphological zones revealed by the k-means clustering provides deeper insight into the conditions that drive variations in band strength ratios and evolution of the PAH population that otherwise would be lost. For example, certain band-band relations are bifurcated, revealing two limiting cases; one associated with the PDR, the other with the diffuse medium. Traditionally, PAH band strength ratios are used to gain insight into the properties of the emitting PAH population, i.e., charge, size, structure, and composition. Insights inferred from this work are compared and contrasted to those from Boersma et al. (first paper in this series), where the PAH emission in NGC 7023 is decomposed exclusively using the PAH spectra and tools made available through the NASA Ames PAH IR Spectroscopic Database. C1 [Boersma, C.; Bregman, J.; Allamandola, L. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Boersma, C (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA. EM Christiaan.Boersma@nasa.gov FU NASA [1407]; NASA's Laboratory Astrophysics, "Carbon in the Galaxy' consortium grant [NNH10ZDA001N]; NASA's Astrobiology; Astronomy + Physics Research and Analysis (APRA) [NNX07AH02G]; Spitzer Space Telescope Support Programs [50082]; San Jose State University Research Foundation [NNX11AJ33A] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. Support from NASA's Laboratory Astrophysics, "Carbon in the Galaxy' consortium grant (NNH10ZDA001N); and NASA's Astrobiology; Astronomy + Physics Research and Analysis (APRA; NNX07AH02G), and Spitzer Space Telescope Support Programs (50082) are greatly acknowledged. C.B. is grateful for an appointment at NASA's Ames Research Center through San Jose State University Research Foundation (NNX11AJ33A). Lastly, an anonymous referee is acknowledged for his/her careful reading and helpful suggestions that have significantly improved this paper. NR 55 TC 9 Z9 9 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2014 VL 795 IS 2 AR 110 DI 10.1088/0004-637X/795/2/110 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR8YT UT WOS:000343857900009 ER PT J AU Bouwens, RJ Bradley, L Zitrin, A Coe, D Franx, M Zheng, W Smit, R Host, O Postman, M Moustakas, L Labbe, I Carrasco, M Molino, A Donahue, M Kelson, DD Meneghetti, M Benitez, N Lemze, D Umetsu, K Broadhurst, T Moustakas, J Rosati, P Jouvel, S Bartelmann, M Ford, H Graves, G Grillo, C Infante, L Jimenez-Teja, Y Lahav, O Maoz, D Medezinski, E Melchior, P Merten, J Nonino, M Ogaz, S Seitz, S AF Bouwens, R. J. Bradley, L. Zitrin, A. Coe, D. Franx, M. Zheng, W. Smit, R. Host, O. Postman, M. Moustakas, L. Labbe, I. Carrasco, M. Molino, A. Donahue, M. Kelson, D. D. Meneghetti, M. Benitez, N. Lemze, D. Umetsu, K. Broadhurst, T. Moustakas, J. Rosati, P. Jouvel, S. Bartelmann, M. Ford, H. Graves, G. Grillo, C. Infante, L. Jimenez-Teja, Y. Lahav, O. Maoz, D. Medezinski, E. Melchior, P. Merten, J. Nonino, M. Ogaz, S. Seitz, S. TI A CENSUS OF STAR-FORMING GALAXIES IN THE Z similar to 9-10 UNIVERSE BASED ON HST plus SPITZER OBSERVATIONS OVER 19 CLASH CLUSTERS: THREE CANDIDATE Z similar to 9-10 GALAXIES AND IMPROVED CONSTRAINTS ON THE STAR FORMATION RATE DENSITY AT Z similar to 9.2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift ID ULTRA-DEEP-FIELD; LYMAN-BREAK GALAXIES; HIGH-REDSHIFT GALAXIES; ULTRAVIOLET LUMINOSITY DENSITY; SPECTRAL ENERGY-DISTRIBUTIONS; EARLY RELEASE SCIENCE; EXTRAGALACTIC LEGACY SURVEY; EMISSION-LINE GALAXIES; STELLAR MASS DENSITY; GOODS-SOUTH FIELD AB We utilize a two-color Lyman-break selection criterion to search for z similar to 9-10 galaxies over the first 19 clusters in the CLASH program. A systematic search yields three z similar to 9-10 candidates. While we have already reported the most robust of these candidates, MACS1149-JD, two additional z similar to 9 candidates are also found and have H-160- band magnitudes of similar to 26.2-26.9. A careful assessment of various sources of contamination suggests less than or similar to 1 contaminants for our z similar to 9-10 selection. To determine the implications of these search results for the luminosity function (LF) and star formation rate density at z similar to 9, we introduce a new differential approach to deriving these quantities in lensing fields. Our procedure is to derive the evolution by comparing the number of z similar to 9-10 galaxy candidates found in CLASH with the number of galaxies in a slightly lower-redshift sample (after correcting for the differences in selection volumes), here taken to be z similar to 8. This procedure takes advantage of the fact that the relative volumes available for the z similar to 8 and z similar to 9-10 selections behind lensing clusters are not greatly dependent on the details of the lensing models. We find that the normalization of the UV LF at z similar to 9 is just 0.28(-0.20)(+0.39) x that at z similar to 8, which is similar to 1.4(-0.8)(+3.0) x lower than extrapolating z similar to 4-8 LF results. While consistent with the evolution in the UV LF seen at z similar to 4-8, these results marginally favor a more rapid evolution at z > 8. Compared to similar evolutionary findings from the HUDF, our result is less insensitive to large-scale structure uncertainties, given our many independent sightlines on the high-redshift universe. C1 [Bouwens, R. J.; Franx, M.; Smit, R.; Labbe, I.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Bouwens, R. J.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Bradley, L.; Coe, D.; Postman, M.; Ogaz, S.] Space Telescope Sci Inst, Baltimore, MD 21208 USA. [Zitrin, A.; Carrasco, M.; Bartelmann, M.] Heidelberg Univ, D-69120 Heidelberg, Germany. [Zheng, W.; Lemze, D.; Ford, H.; Medezinski, E.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Host, O.; Grillo, C.] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Moustakas, L.; Merten, J.] CALTECH, JPL, Pasadena, CA 91109 USA. [Carrasco, M.; Infante, L.] Catholic Univ Chile, Santiago 22, Chile. [Molino, A.; Jimenez-Teja, Y.] Inst Astrofis Andalucia, Granada 18008, Spain. [Donahue, M.] Michigan State Univ, E Lansing, MI 48824 USA. [Kelson, D. D.] Carnegie Observ, Carnegie Inst Sci, Pasadena, CA 91101 USA. [Meneghetti, M.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Umetsu, K.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Broadhurst, T.] Univ Basque Country, Bilbao 48080, Spain. [Moustakas, J.] Siena Coll, Albany, NY 12211 USA. [Rosati, P.] European So Observ, D-85748 Garching, Germany. [Jouvel, S.] Inst Ciencies Espai IEEC CSIC, Barcelona 08034, Spain. [Graves, G.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Lahav, O.] UCL, London WC1E 6BT, England. [Maoz, D.] Tel Aviv Univ, IL-69978 Tel Aviv, Israel. [Melchior, P.] Ohio State Univ, Columbus, OH 43210 USA. [Nonino, M.] Osserv Astron Trieste, INAF, I-40131 Trieste, Italy. [Seitz, S.] Univ Sternwarte, D-81679 Munich, Germany. RP Bouwens, RJ (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. RI Jimenez-Teja, Yolanda/D-5933-2011; Grillo, Claudio/E-6223-2015; Meneghetti, Massimo/O-8139-2015; OI Grillo, Claudio/0000-0002-5926-7143; Meneghetti, Massimo/0000-0003-1225-7084; Umetsu, Keiichi/0000-0002-7196-4822; Moustakas, Leonidas/0000-0003-3030-2360; Benitez, Narciso/0000-0002-0403-7455 FU ERC [HIGHZ 227749]; NWO vrij competitie grant; NASA; DNRF FX We are grateful for extensive feedback on our manuscript from Pascal Oesch and Garth Illingworth. We thank Anton Koekemoer for providing us with high quality reductions of the available HST observations of our CLASH cluster fields. We acknowledge Dan Magee for assisting with the reductions of the IRAC data for our clusters using MOPEX. We are greatly appreciative to Ryan Quadri for sending us his results for the restframe V-band LF of red z similar to 2 galaxies based on a UKIDSS UDS search. Comments by the anonymous referee significantly improved this paper. We acknowledge support from ERC grant HIGHZ # 227749, an NWO vrij competitie grant, and the NASA grant for the CLASHMCT program. The dark cosmology center is funded by the DNRF. NR 135 TC 58 Z9 58 U1 1 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 NOV 10 PY 2014 VL 795 IS 2 AR 126 DI 10.1088/0004-637X/795/2/126 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR8YT UT WOS:000343857900025 ER PT J AU Crouzet, N McCullough, PR Deming, D Madhusudhan, N AF Crouzet, Nicolas McCullough, Peter R. Deming, Drake Madhusudhan, Nikku TI WATER VAPOR IN THE SPECTRUM OF THE EXTRASOLAR PLANET HD 189733b. II. THE ECLIPSE SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: observational; planets and satellites: atmospheres; planets and satellites: individual (HD 189733b); techniques: spectroscopic ID HUBBLE-SPACE-TELESCOPE; NICMOS TRANSMISSION SPECTROSCOPY; INFRARED-EMISSION-SPECTRUM; HOT JUPITERS; MU-M; ATMOSPHERIC CIRCULATION; SPITZER OBSERVATIONS; ABSORPTION; RETRIEVAL; HD189733B AB Spectroscopic observations of exoplanets are crucial to infer the composition and properties of their atmospheres. HD 189733b is one of the most extensively studied exoplanets and is a cornerstone for hot Jupiter models. In this paper, we report the dayside emission spectrum of HD 189733b in the wavelength range 1.1-1.7 mu m obtained with the Hubble Space Telescope Wide Field Camera 3 (WFC3) in spatial scan mode. The quality of the data is such that even a straightforward analysis yields a high-precision Poisson noise-limited spectrum: the median 1 sigma uncertainty is 57 ppm per 0.02 mu m bin. We also build a white-light curve correcting for systematic effects and derive an absolute eclipse depth of 96 +/- 39 ppm. The resulting spectrum shows marginal evidence for water vapor absorption, but can also be well explained by a blackbody spectrum. However, the combination of these WFC3 data with previous Spitzer photometric observations is best explained by a dayside atmosphere of HD 189733b with no thermal inversion and a nearly solar or subsolar H2O abundance in a cloud-free atmosphere. Alternatively, this apparent subsolar abundance may be the result of clouds or hazes that future studies need to investigate. C1 [Crouzet, Nicolas] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Crouzet, Nicolas; McCullough, Peter R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [McCullough, Peter R.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Deming, Drake] NASA, Astrobiol Inst, Virtual Planetary Lab, Seattle, WA 98195 USA. [Madhusudhan, Nikku] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Crouzet, N (reprint author), Univ Toronto, Dunlap Inst Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. EM crouzet@dunlap.utoronto.ca OI Crouzet, Nicolas/0000-0001-7866-8738 FU HST [GO-12881]; Origins of Solar Systems grant [NNX10AG30G] FX The authors gratefully acknowledge everyone who has contributed to the Hubble Space Telescope and the WFC3 and particularly those responsible for implementing the spatial scanning, which was critical to these observations. We thank, in particular, John MacKenty and Merle Reinhart. We acknowledge conversations with Suzanne Hawley, Leslie Hebb, Veselin Kostov, Rachel Osten, and Neill Reid. This research used NASA's Astrophysics Data System Bibliographic Services, the SIMBAD database operated at CDS, Strasbourg, France, and was funded in part by HST grant GO-12881 and Origins of Solar Systems grant NNX10AG30G. NR 56 TC 14 Z9 14 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2014 VL 795 IS 2 AR 166 DI 10.1088/0004-637X/795/2/166 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR8YT UT WOS:000343857900065 ER PT J AU Currie, T Burrows, A Girard, JH Cloutier, R Fukagawa, M Sorahana, S Kuchner, M Kenyon, SJ Madhusudhan, N Itoh, Y Jayawardhana, R Matsumura, S Pyo, TS AF Currie, Thayne Burrows, Adam Girard, Julien H. Cloutier, Ryan Fukagawa, Misato Sorahana, Satoko Kuchner, Marc Kenyon, Scott J. Madhusudhan, Nikku Itoh, Yoichi Jayawardhana, Ray Matsumura, Soko Pyo, Tae-Soo TI DEEP THERMAL INFRARED IMAGING OF HR 8799 bcde: NEW ATMOSPHERIC CONSTRAINTS AND LIMITS ON A FIFTH PLANET SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: atmospheres; planets and satellites: composition; stars: early-type; stars: individual (HR 8799); techniques: high angular resolution; techniques: image processing ID EXTRASOLAR GIANT PLANETS; DIRECTLY IMAGED PLANET; BETA-PICTORIS B; LOW-MASS STARS; BROWN DWARFS; MU-M; CANDIDATE COMPANION; ORBITING FOMALHAUT; DYNAMICAL MASS; UPPER SCORPIUS AB We present new L' (3.8 mu m) and Bra (4.05 mu m) data and reprocessed archival L' data for the young, planet-hosting star HR 8799 obtained with Keck/NIRC2, VLT/NaCo, and Subaru/IRCS. We detect all four HR 8799 planets in each data set at a moderate to high signal-to-noise ratio (S/N greater than or similar to 6-15). We fail to identify a fifth planet, "HR 8799 f," at r < 15 AU at a 5 sigma confidence level: one suggestive, marginally significant residual at 0 ''.2 is most likely a pointspread function artifact. Assuming companion ages of 30 Myr and the Baraffe planet cooling models, we rule out an HR 8799 f with a mass of 5 M-J (7 M-J), 7 M-J (10 M-J), or 12 M-J (13 M-J) at r(proj) similar to 12 AU, 9 AU, and 5 AU, respectively. All four HR 8799 planets have red early T dwarf-like L' - [4.05] colors, suggesting that their spectral energy distributions peak in between the L' and M' broadband filters. We find no statistically significant difference in HR 8799 cde's color. Atmosphere models assuming thick, patchy clouds appear to better match HR 8799 bcde's photometry than models assuming a uniform cloud layer. While non-equilibrium carbon chemistry is required to explain HR 8799 b and c's photometry/spectra, evidence for it from HR 8799 d and e's photometry is weaker. Future, deep-IR spectroscopy/spectrophotometry with the Gemini Planet Imager, SCExAO/CHARIS, and other facilities may clarify whether the planets are chemically similar or heterogeneous. C1 [Currie, Thayne; Cloutier, Ryan; Jayawardhana, Ray] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Currie, Thayne; Pyo, Tae-Soo] Natl Astron Observ Japan, Hilo, HI 96720 USA. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Girard, Julien H.] European So Observ, Santiago 19001, Chile. [Fukagawa, Misato] Osaka Univ, Grad Sch Sci, Toyonaka, Osaka 5600043, Japan. [Sorahana, Satoko] Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Kuchner, Marc] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Kenyon, Scott J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Madhusudhan, Nikku] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Itoh, Yoichi] Univ Hyago, Ctr Astron, Nishi Harima Astron Observ, Sayo, Hyogo 6795313, Japan. [Matsumura, Soko] Univ Dundee, Sch Engn Phys & Math, Dundee DD1 4HN, Scotland. RP Currie, T (reprint author), Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. OI Kenyon, Scott/0000-0003-0214-609X FU W.M. Keck Foundation; McLean Postdoctoral Fellowship FX We thank the anonymous referee for helpful comments. The NASA-Keck, ESO, and Subaru Time Allocation Committees supported this work through generous allotments of observing time. We thank Christian Marois and Laurent Pueyo for extensive discussions focused on advanced high-contrast image processing techniques, Stanimir Metchev for discussions on NIRC2 linearity corrections, Adam Burgasser for suggestions on comparing our data to field substellar objects, Ernst De Mooij for helpful discussions on flux calibration strategies, and Timothy Brandt for help regarding recent research results. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. This work is based on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This research has made use of the Keck Observatory Archive (KOA), which is operated by the W.M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration. We are extremely grateful to the NExScI/KOA staff for developing and maintaining the NIRC2 archive. T.C. is partially supported by a McLean Postdoctoral Fellowship. NR 77 TC 22 Z9 22 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2014 VL 795 IS 2 AR 133 DI 10.1088/0004-637X/795/2/133 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR8YT UT WOS:000343857900032 ER PT J AU Endl, M Caldwell, DA Barclay, T Huber, D Isaacson, H Buchhave, LA Brugamyer, E Robertson, P Cochran, WD MacQueen, PJ Havel, M Lucas, P Howell, SB Fischer, D Quintana, E Ciardi, DR AF Endl, Michael Caldwell, Douglas A. Barclay, Thomas Huber, Daniel Isaacson, Howard Buchhave, Lars A. Brugamyer, Erik Robertson, Paul Cochran, William D. MacQueen, Phillip J. Havel, Mathieu Lucas, Phillip Howell, Steve B. Fischer, Debra Quintana, Elisa Ciardi, David R. TI KEPLER-424 b: A "LONELY" HOT JUPITER THAT FOUND A COMPANION SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual ( KOI-22, KOI-127, KOI-135, KOI-183, KOI-214, Kepler-43, Kepler-77); techniques: radial velocities ID HOBBY-EBERLY TELESCOPE; TRANSITING EXTRASOLAR PLANETS; GIANT PLANETS; HOST STARS; CANDIDATES; EVOLUTION; MISSION; EXOPLANETS; I.; PERTURBATIONS AB Hot Jupiter systems provide unique observational constraints for migration models in multiple systems and binaries. We report on the discovery of the Kepler-424 (KOI-214) two-planet system, which consists of a transiting hot Jupiter (Kepler-424b) in a 3.31 day orbit accompanied by a more massive outer companion in an eccentric (e = 0.3) 223 day orbit. The outer giant planet, Kepler-424c, is not detected transiting the host star. The masses of both planets and the orbital parameters for the second planet were determined using precise radial velocity (RV) measurements from the Hobby-Eberly Telescope (HET) and its High Resolution Spectrograph (HRS). In stark contrast to smaller planets, hot Jupiters are predominantly found to be lacking any nearby additional planets; they appear to be "lonely". This might be a consequence of these systems having a highly dynamical past. The Kepler-424 planetary system has a hot Jupiter in a multiple system, similar to. Andromedae. We also present our results for Kepler-422 (KOI-22), Kepler-77 (KOI-127), Kepler-43 (KOI-135), and Kepler-423 (KOI-183). These results are based on spectroscopic data collected with the Nordic Optical Telescope (NOT), the Keck 1 telescope, and HET. For all systems, we rule out false positives based on various follow-up observations, confirming the planetary nature of these companions. We performed a comparison with planetary evolutionary models which indicate that these five hot Jupiters have heavy element contents between 20 and 120 M-circle plus. C1 [Endl, Michael; Cochran, William D.; MacQueen, Phillip J.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Caldwell, Douglas A.; Barclay, Thomas; Huber, Daniel; Havel, Mathieu; Howell, Steve B.; Quintana, Elisa] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Barclay, Thomas] Bay Area Environm Res Inst, Petaluma, CA 94952 USA. [Huber, Daniel] SETI Inst, Mountain View, CA 94043 USA. [Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Buchhave, Lars A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Brugamyer, Erik; Cochran, William D.; MacQueen, Phillip J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Robertson, Paul] Penn State Univ, Ctr Exoplanets & Habitable Worlds, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Lucas, Phillip] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Fischer, Debra] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. RP Endl, M (reprint author), Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. OI Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047 NR 56 TC 13 Z9 13 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2014 VL 795 IS 2 AR 151 DI 10.1088/0004-637X/795/2/151 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR8YT UT WOS:000343857900050 ER PT J AU Hamaguchi, K Corcoran, MF Takahashi, H Yuasa, T Ishida, M Gull, TR Pittard, JM Russell, CMP Madura, TI AF Hamaguchi, Kenji Corcoran, Michael F. Takahashi, Hiromitsu Yuasa, Takayuki Ishida, Manabu Gull, Theodore R. Pittard, Julian M. Russell, Christopher M. P. Madura, Thomas I. TI SUZAKU MONITORING OF HARD X-RAY EMISSION FROM eta CARINAE OVER A SINGLE BINARY ORBITAL CYCLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; stars: early-type; stars: individual (Eta Carinae); stars: winds, outflows; X-rays: stars ID COLLIDING WINDS; STARS; VARIABILITY; HOMUNCULUS; PERIASTRON; SPECTRUM; BEPPOSAX; COMPLEX; NEBULA AB The Suzaku X-ray observatory monitored the supermassive binary system. Carinae 10 times during the whole 5.5 yr orbital cycle between 2005 and 2011. This series of observations presents the first long-term monitoring of this enigmatic system in the extremely hard X-ray band between 15 and 40 keV. During most of the orbit, the 15-25 keV emission varied similarly to the 2-10 keV emission, indicating an origin in the hard energy tail of the kT similar to 4 keV wind-wind collision (WWC) plasma. However, the 15-25 keV emission declined only by a factor of three around periastron when the 2-10 keV emission dropped by two orders of magnitude due probably to an eclipse of the WWC plasma. The observed minimum in the 15-25 keV emission occurred after the 2-10 keV flux had already recovered by a factor of similar to 3. This may mean that the WWC activity was strong, but hidden behind the thick primary stellar wind during the eclipse. The 25-40 keV flux was rather constant through the orbital cycle, at the level measured with INTEGRAL in 2004. This result may suggest a connection of this flux component to the gamma-ray source detected in this field. The helium-like Fe K alpha line complex at similar to 6.7 keV became strongly distorted toward periastron as seen in the previous cycle. The 5-9 keV spectra can be reproduced well with a two-component spectral model, which includes plasma in collision equilibrium and a plasma in non-equilibrium ionization (NEI) with tau similar to 10(11) cm(-3) s(-1). The NEI plasma increases in importance toward periastron. C1 [Hamaguchi, Kenji; Corcoran, Michael F.] NASA, Goddard Space Flight Ctr, CRESST & Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Hamaguchi, Kenji] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. [Corcoran, Michael F.] Univ Space Res Assoc, Columbia, MD 21046 USA. [Takahashi, Hiromitsu] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Yuasa, Takayuki] RIKEN, Nishina Ctr, Wako, Saitama 3510198, Japan. [Ishida, Manabu] Inst Space & Astronaut Sci JAXA, Sagamihara, Kanagawa 2298510, Japan. [Gull, Theodore R.; Madura, Thomas I.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Pittard, Julian M.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Russell, Christopher M. P.] Univ Delaware, Bartol Res Inst, Dept Phys & Astron, Newark, DE 19716 USA. RP Hamaguchi, K (reprint author), NASA, Goddard Space Flight Ctr, CRESST & Xray Astrophys Lab, Greenbelt, MD 20771 USA. RI XRAY, SUZAKU/A-1808-2009 NR 45 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2014 VL 795 IS 2 AR 119 DI 10.1088/0004-637X/795/2/119 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR8YT UT WOS:000343857900018 ER PT J AU Lewis, NK Showman, AP Fortney, JJ Knutson, HA Marley, MS AF Lewis, Nikole K. Showman, Adam P. Fortney, Jonathan J. Knutson, Heather A. Marley, Mark S. TI ATMOSPHERIC CIRCULATION OF ECCENTRIC HOT JUPITER HAT-P-2B SO ASTROPHYSICAL JOURNAL LA English DT Article DE atmospheric effects; methods: numerical; planets and satellites: general; planets and satellites: individual (HAT-P-2b) ID TIDALLY LOCKED EXOPLANETS; PLANET HD 189733B; MASS DWARF STARS; EXTRASOLAR PLANET; GIANT PLANETS; NONHOMOGENEOUS ATMOSPHERES; HYDRODYNAMIC SIMULATIONS; HEAT REDISTRIBUTION; RADIATIVE-TRANSFER; INITIAL CONDITIONS AB The hot Jupiter HAT-P-2b has become a prime target for Spitzer Space Telescope observations aimed at understanding the atmospheric response of exoplanets on highly eccentric orbits. Here we present a suite of three-dimensional atmospheric circulation models for HAT-P-2b that investigate the effects of assumed atmospheric composition and rotation rate on global scale winds and thermal patterns. We compare and contrast atmospheric models for HAT-P-2b, which assume one and five times solar metallicity, both with and without TiO/VO as atmospheric constituents. Additionally we compare models that assume a rotation period of half, one, and two times the nominal pseudo-synchronous rotation period. We find that changes in assumed atmospheric metallicity and rotation rate do not significantly affect model predictions of the planetary flux as a function of orbital phase. However, models in which TiO/VO are present in the atmosphere develop a transient temperature inversion between the transit and secondary eclipse events that results in significant variations in the timing and magnitude of the peak of the planetary flux compared with models in which TiO/VO are omitted from the opacity tables. We find that no one single atmospheric model can reproduce the recently observed full orbit phase curves at 3.6, 4.5 and 8.0 mu m, which is likely due to a chemical process not captured by our current atmospheric models for HAT-P-2b. Further modeling and observational efforts focused on understanding the chemistry of HAT-P-2b's atmosphere are needed and could provide key insights into the interplay between radiative, dynamical, and chemical processes in a wide range of exoplanet atmospheres. C1 [Lewis, Nikole K.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Showman, Adam P.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Knutson, Heather A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Marley, Mark S.] NASA, Ames Res Ctr 245 3, Moffett Field, CA 94035 USA. RP Lewis, NK (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. EM nklewis@mit.edu OI Marley, Mark/0000-0002-5251-2943 FU California Institute of Technology (Caltech); NASA [NNX12AI79G]; NASA PATM FX This work was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. A.P.S. was supported by NASA Origins grant NNX12AI79G. M.S.M. acknowledges support from the NASA PATM program. N.K.L. wishes to thank C. Visscher for valuable discussions regarding possible chemical processes at work in HAT-P-2b's atmosphere. The authors thank the anonymous referee for their valuable comments on the manuscript. NR 58 TC 9 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2014 VL 795 IS 2 AR UNSP 150 DI 10.1088/0004-637X/795/2/150 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR8YT UT WOS:000343857900049 ER PT J AU Liu, C Deng, N Lee, J Wiegelmann, T Jiang, CW Dennis, BR Su, Y Donea, A Wang, HM AF Liu, Chang Deng, Na Lee, Jeongwoo Wiegelmann, Thomas Jiang, Chaowei Dennis, Brian R. Su, Yang Donea, Alina Wang, Haimin TI THREE-DIMENSIONAL MAGNETIC RESTRUCTURING IN TWO HOMOLOGOUS SOLAR FLARES IN THE SEISMICALLY ACTIVE NOAA AR 11283 SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: flares; Sun: helioseismology; Sun: magnetic fields; Sun: X-rays, gamma rays ID 2011 FEBRUARY 15; CORONAL MASS EJECTION; HIGH-RESOLUTION OBSERVATIONS; FLUX-ROPE; FIELD EXTRAPOLATIONS; VECTOR MAGNETOGRAMS; LORENTZ FORCE; RAPID CHANGES; X2.2 FLARE; ERUPTION AB We carry out a comprehensive investigation comparing the three-dimensional magnetic field restructuring, flare energy release, and the helioseismic response of two homologous flares, the 2011 September 6 X2.1 (FL1) and September 7 X1.8 (FL2) flares in NOAA AR 11283. In our analysis, (1) a twisted flux rope (FR) collapses onto the surface at a speed of 1.5 km s(-1) after a partial eruption in FL1. The FR then gradually grows to reach a higher altitude and collapses again at 3 km s(-1) after a fuller eruption in FL2. Also, FL2 shows a larger decrease of the flux-weighted centroid separation of opposite magnetic polarities and a greater change of the horizontal field on the surface. These imply a more violent coronal implosion with corresponding more intense surface signatures in FL2. (2) The FR is inclined northward and together with the ambient fields, it undergoes a southward turning after both events. This agrees with the asymmetric decay of the penumbra observed in the peripheral regions. (3) The amounts of free magnetic energy and nonthermal electron energy released during FL1 are comparable to those of FL2 within the uncertainties of the measurements. (4) No sunquake was detected in FL1; in contrast, FL2 produced two seismic emission sources S1 and S2 both lying in the penumbral regions. Interestingly, S1 and S2 are connected by magnetic loops, and the stronger source S2 has a weaker vertical magnetic field. We discuss these results in relation to the implosion process in the low corona and the sunquake generation. C1 [Liu, Chang; Deng, Na; Lee, Jeongwoo; Wang, Haimin] New Jersey Inst Technol, Space Weather Res Lab, Newark, NJ 07102 USA. [Lee, Jeongwoo] Chungnam Natl Univ, Dept Astron & Space Sci, Taejon 305764, South Korea. [Wiegelmann, Thomas] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany. [Jiang, Chaowei] Univ Alabama, Ctr Space Plasma & Aeronom Res, Huntsville, AL 35805 USA. [Jiang, Chaowei] Chinese Acad Sci, Ctr Space Sci & Appl Res, State Key Lab Space Weather, SIGMA Weather Grp, Beijing 100190, Peoples R China. [Dennis, Brian R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Su, Yang] Graz Univ, Inst Phys, IGAM Kanzelhole Observ, A-8010 Graz, Austria. [Donea, Alina] Monash Univ, Sch Math Sci, Ctr Stellar & Planetary Astrophys, Melbourne, Vic 3800, Australia. RP Liu, C (reprint author), New Jersey Inst Technol, Space Weather Res Lab, Newark, NJ 07102 USA. EM chang.liu@njit.edu RI Su, Yang/J-5381-2014; OI Deng, Na/0000-0001-8179-812X; Lee, Jeongwoo/0000-0002-5865-7924; Liu, Chang/0000-0002-6178-7471 FU Fermi GI program; NASA through LWS [NNX13AF76G, NNX13AG13, GNNX14AC12G]; NSF [AGS 1408703]; Brainpool Program of KOFST; DLR [50 OC 0904]; DFG [WI 3211/2-1]; National Natural Science Foundation of China [41204126]; Austrian Science Fund (FWF) [P24092-N16]; FWF [P27292-N20] FX We thank the SDO team for the magnetic and EUV/UV data. SDO is the first satellite under the Living with a Star (LWS) program at NASA. We acknowledge the use of the Fermi Solar Flare Observations facility funded by the Fermi GI program. We also thank the BBSO/NST team for the TiO image and the anonymous referee for helpful comments. C. L. is grateful to Dr. Yan Xu for helpful discussions on the thick-target heating. C. L., N.D., and H. W. were supported by NASA under grants NNX13AF76G and NNX13AG13G issued through the LWS program and NNX14AC12G, and by NSF under grant AGS 1408703. J. L. was supported by the Brainpool Program 2014 of KOFST. T. W. was supported by DLR grant 50 OC 0904 and DFG grant WI 3211/2-1. C. W. J was supported by the National Natural Science Foundation of China 41204126. Y.S. acknowledges the Austrian Science Fund (FWF) P24092-N16 and FWF P27292-N20. NR 87 TC 12 Z9 12 U1 8 U2 16 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 NOV 10 PY 2014 VL 795 IS 2 AR 128 DI 10.1088/0004-637X/795/2/128 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR8YT UT WOS:000343857900027 ER PT J AU Marelli, M Harding, A Pizzocaro, D De Luca, A Wood, KS Caraveo, P Salvetti, D Parkinson, PMS Acero, F AF Marelli, M. Harding, A. Pizzocaro, D. De Luca, A. Wood, K. S. Caraveo, P. Salvetti, D. Parkinson, P. M. Saz Acero, F. TI ON THE PUZZLING HIGH-ENERGY PULSATIONS OF THE ENERGETIC RADIO-QUIET gamma-RAY PULSAR J1813-1246 SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: stars; pulsars: general; pulsars: individual (PSR J1813-1246); stars: neutron; X-rays: stars ID BLIND FREQUENCY SEARCHES; ALL-SKY SURVEY; X-RAY; XMM-NEWTON; CURVATURE RADIATION; LIKELIHOOD RATIO; MAGNETIC-FIELD; NEUTRON-STARS; WIND NEBULAE; LIGHT CURVES AB We have analyzed the new deep XMM-Newton and Chandra observations of the energetic, radio-quiet pulsar J1813-1246. The X-ray spectrum is nonthermal, very hard, and absorbed. Based on spectral considerations, we propose that J1813 is located at a distance further than 2.5 kpc. J1813 is highly pulsed in the X-ray domain, with a light curve characterized by two sharp, asymmetrical peaks, separated by 0.5 in phase. We detected no significant X-ray spectral changes during the pulsar phase. We extended the available Fermi ephemeris to five years. We found two glitches. The gamma-ray light curve is characterized by two peaks, separated by 0.5 in phase, with a bridge in between and no off-pulse emission. The spectrum shows clear evolution in phase, being softer at the peaks and hardening toward the bridge. Surprisingly, both X-ray peaks lag behind the gamma-ray ones by a quarter of phase. We found a hint of detection in the 30-500 keV band with INTEGRAL, which is consistent with the extrapolation of both the soft X-ray and gamma-ray emission of J1813. The unique X-ray and gamma-ray phasing suggests a singular emission geometry. We discuss some possibilities within the current pulsar emission models. Finally, we develop an alternative geometrical model where the X-ray emission comes from polar cap pair cascades. C1 [Marelli, M.; Pizzocaro, D.; De Luca, A.; Caraveo, P.; Salvetti, D.] Ist Astrofis Spaziale Fis Cosm Milano, INAF, I-20133 Milan, Italy. [Harding, A.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Pizzocaro, D.] Univ Insubria, I-21100 Varese, Italy. [De Luca, A.; Caraveo, P.] Ist Nazl Fis Nucl, Sez Pavia, I-27100 Pavia, Italy. [Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Parkinson, P. M. Saz] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Parkinson, P. M. Saz] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Acero, F.] Univ Paris Diderot, CEA Saclay, CEA IRFU CNRS, Serv Astrophys,Lab AIM, F-91191 Gif Sur Yvette, France. RP Marelli, M (reprint author), Ist Astrofis Spaziale Fis Cosm Milano, INAF, Via E Bassini 15, I-20133 Milan, Italy. EM marelli@lambrate.inaf.it OI Caraveo, Patrizia/0000-0003-2478-8018; Marelli, Martino/0000-0002-8017-0338 FU NASA in the United States; DOE in the United States; CEA/Irfu in France; IN2P3/CNRS in France; ASI in Italy; INFN in Italy; MEXT in Japan; KEK in Japan; JAXA in Japan; K.A. Wallenberg Foundation; Swedish Research Council; National Space Board in Sweden; INAF in Italy; CNES in France; National Aeronautics and Space Administration through Chandra X-ray Observatory Center [GO3-14053X]; National Aeronautics Space Administration [NAS8-03060]; ASI-INAF [I/037/12/0, art.22 L.240/2010]; SWIFT [ASI-INAF I-004-11-0]; Fermi [ASI-INAF I-005-12-0] FX We warmly thank Paizis Adamantia, Andrea Giuliani, Fabio Gastaldelli, and Andrea Belfiore for discussions and help. We also thank Massimiliano Razzano and Marianne Lemoine-Goumard for their good work as Galactic Coordinators. The Fermi LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K.A. Wallenberg Foundation, the Swedish Research Council, and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO3-14053X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. This work was supported by the ASI-INAF contract I/037/12/0, art.22 L.240/2010 for the project "Calibrazione ed Analisi del satallite NuSTAR". This work was partially supported by the SWIFT contract ASI-INAF I-004-11-0 and the Fermi contract ASI-INAF I-005-12-0. NR 70 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2014 VL 795 IS 2 AR 168 DI 10.1088/0004-637X/795/2/168 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR8YT UT WOS:000343857900067 ER PT J AU Singer, LP Price, LR Farr, B Urban, AL Pankow, C Vitale, S Veitch, J Farr, WM Hanna, C Cannon, K Downes, T Graff, P Haster, CJ Mandel, I Sidery, T Vecchio, A AF Singer, Leo P. Price, Larry R. Farr, Ben Urban, Alex L. Pankow, Chris Vitale, Salvatore Veitch, John Farr, Will M. Hanna, Chad Cannon, Kipp Downes, Tom Graff, Philip Haster, Carl-Johan Mandel, Ilya Sidery, Trevor Vecchio, Alberto TI THE FIRST TWO YEARS OF ELECTROMAGNETIC FOLLOW-UP WITH ADVANCED LIGO AND VIRGO SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitational waves; stars: neutron; surveys ID NEUTRON-STAR MERGERS; GAMMA-RAY BURSTS; GRAVITATIONAL-WAVES; MASS-DISTRIBUTION; BLACK-HOLE; ASTRONOMY; DISCOVERY; EMISSION; SIGNALS; PROBE AB We anticipate the first direct detections of gravitational waves (GWs) with Advanced LIGO and Virgo later this decade. Though this groundbreaking technical achievement will be its own reward, a still greater prize could be observations of compact binary mergers in both gravitational and electromagnetic channels simultaneously. During Advanced LIGO and Virgo's first two years of operation, 2015 through 2016, we expect the global GW detector array to improve in sensitivity and livetime and expand from two to three detectors. We model the detection rate and the sky localization accuracy for binary neutron star (BNS) mergers across this transition. We have analyzed a large, astrophysically motivated source population using real-time detection and sky localization codes and higher-latency parameter estimation codes that have been expressly built for operation in the Advanced LIGO/Virgo era. We show that for most BNS events, the rapid sky localization, available about a minute after a detection, is as accurate as the full parameter estimation. We demonstrate that Advanced Virgo will play an important role in sky localization, even though it is anticipated to come online with only one-third as much sensitivity as the Advanced LIGO detectors. We find that the median 90% confidence region shrinks from similar to 500 deg(2) in 2015 to similar to 200 deg(2) in 2016. A few distinct scenarios for the first LIGO/Virgo detections emerge from our simulations. C1 [Singer, Leo P.; Price, Larry R.] CALTECH, LIGO Lab, Pasadena, CA 91125 USA. [Farr, Ben] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Farr, Ben] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Farr, Ben; Veitch, John; Farr, Will M.; Haster, Carl-Johan; Mandel, Ilya; Sidery, Trevor; Vecchio, Alberto] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Urban, Alex L.; Pankow, Chris; Downes, Tom] Univ Wisconsin, Leonard E Parker Ctr Gravitat Cosmol & Astrophys, Milwaukee, WI 53201 USA. [Vitale, Salvatore] MIT, Cambridge, MA 02139 USA. [Veitch, John] Nikhef, NL-1098 XG Amsterdam, Netherlands. [Hanna, Chad] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [Hanna, Chad] Penn State Univ, University Pk, PA 16802 USA. [Cannon, Kipp] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Graff, Philip] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. RP Singer, LP (reprint author), CALTECH, LIGO Lab, Pasadena, CA 91125 USA. EM lsinger@caltech.edu RI Vecchio, Alberto/F-8310-2015; OI Vecchio, Alberto/0000-0002-6254-1617; Farr, Ben/0000-0002-2916-9200; Singer, Leo/0000-0001-9898-5597; Mandel, Ilya/0000-0002-6134-8946; Veitch, John/0000-0002-6508-0713 FU National Science Foundation (NSF) [DGE-0824162, PHY-0969820, PHY-0923409, PHY-0600953, PHY-0757058]; NSF under University of Wisconsin-Milwaukee (UWM) Research Growth Initiative [PHY-0970074, PHY-1307429]; Foundation for Fundamental Research on Matter (FOM); Netherlands Organisation for Scientific Research (NWO); Science and Technology Facilities Council (STFC) [ST/K005014/1]; NASA FX L.P.S. and B.F. thank generous support from the National Science Foundation (NSF) in the form of Graduate Research Fellowships. B.F. acknowledges support through NSF grants DGE-0824162 and PHY-0969820. A.L.U. and C.P. gratefully acknowledge NSF support under grants PHY-0970074 and PHY-1307429 at the University of Wisconsin-Milwaukee (UWM) Research Growth Initiative. J.V. was supported by the research programme of the Foundation for Fundamental Research on Matter (FOM), which is partially supported by the Netherlands Organisation for Scientific Research (NWO), and by Science and Technology Facilities Council (STFC) grant ST/K005014/1. P.G. is supported by a NASA Postdoctoral Fellowship administered by the Oak Ridge Associated Universities.; GSTLAL analyses were produced on the NEMO computing cluster operated by the Center for Gravitation and Cosmology at UWM under NSF Grants PHY-0923409 and PHY-0600953. The bayestar analyses were performed on the LIGO-Caltech computing cluster. The MCMC computations were performed on Northwestern's CIERA High-Performance Computing cluster GRAIL.20; LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the NSF and operates under cooperative agreement PHY-0757058. NR 78 TC 70 Z9 71 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2014 VL 795 IS 2 AR 105 DI 10.1088/0004-637X/795/2/105 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR8YT UT WOS:000343857900004 ER PT J AU Stark, CC Roberge, A Mandell, A Robinson, TD AF Stark, Christopher C. Roberge, Aki Mandell, Avi Robinson, Tyler D. TI MAXIMIZING THE ExoEarth CANDIDATE YIELD FROM A FUTURE DIRECT IMAGING MISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: numerical; planetary systems; telescopes ID EXTRASOLAR PLANETS; OBSCURATIONAL COMPLETENESS; EARTH OBSERVATIONS; DUST; LIGHT; GLINT; DISK AB ExoEarth yield is a critical science metric for future exoplanet imaging missions. Here we estimate exoEarth candidate yield using single visit completeness for a variety of mission design and astrophysical parameters. We review the methods used in previous yield calculations and show that the method choice can significantly impact yield estimates as well as how the yield responds to mission parameters. We introduce a method, called Altruistic Yield Optimization, that optimizes the target list and exposure times to maximize mission yield, adapts maximally to changes in mission parameters, and increases exoEarth candidate yield by up to 100% compared to previous methods. We use Altruistic Yield Optimization to estimate exoEarth candidate yield for a large suite of mission and astrophysical parameters using single visit completeness. We find that exoEarth candidate yield is most sensitive to telescope diameter, followed by coronagraph inner working angle, followed by coronagraph contrast, and finally coronagraph contrast noise floor. We find a surprisingly weak dependence of exoEarth candidate yield on exozodi level. Additionally, we provide a quantitative approach to defining a yield goal for future exoEarth-imaging missions. C1 [Stark, Christopher C.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Roberge, Aki; Mandell, Avi] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Robinson, Tyler D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Stark, CC (reprint author), NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. EM christopher.c.stark@nasa.gov RI Roberge, Aki/D-2782-2012; OI Roberge, Aki/0000-0002-2989-3725; Robinson, Tyler/0000-0002-3196-414X FU NASA; GSFC's internal research and development fund FX The authors are thankful for enlightening conversations with Karl Stapelfeldt, Michael McElwain, Ruslan Belikov, and Stuart Shaklan, as well as the anonymous referee whose suggestions substantially improved the clarity of this manuscript. This research was supported by appointments to the NASA Postdoctoral Program at Goddard Space Flight Center and Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. A.R. and A.M. acknowledge support by GSFC's internal research and development fund. NR 32 TC 23 Z9 23 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2014 VL 795 IS 2 AR 122 DI 10.1088/0004-637X/795/2/122 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR8YT UT WOS:000343857900021 ER PT J AU Steidel, CC Rudie, GC Strom, AL Pettini, M Reddy, NA Shapley, AE Trainor, RF Erb, DK Turner, ML Konidaris, NP Kulas, KR Mace, G Matthews, K McLean, IS AF Steidel, Charles C. Rudie, Gwen C. Strom, Allison L. Pettini, Max Reddy, Naveen A. Shapley, Alice E. Trainor, Ryan F. Erb, Dawn K. Turner, Monica L. Konidaris, Nicholas P. Kulas, Kristin R. Mace, Gregory Matthews, Keith McLean, Ian S. TI STRONG NEBULAR LINE RATIOS IN THE SPECTRA of z similar to 2-3 STAR FORMING GALAXIES: FIRST RESULTS FROM KBSS-MOSFIRE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: abundances; galaxies: evolution; galaxies: formation; galaxies: fundamental parameters; galaxies: high-redshift; galaxies: starburst; instrumentation: spectrographs ID MASS-METALLICITY RELATION; ACTIVE GALACTIC NUCLEI; BARYONIC STRUCTURE SURVEY; GOODS-NORTH FIELD; GRAVITATIONALLY LENSED GALAXIES; REST-FRAME ULTRAVIOLET; HIGH-REDSHIFT GALAXIES; LYMAN BREAK GALAXIES; GREEN PEA GALAXIES; H-II REGIONS AB We present initial results of a deep near-IR spectroscopic survey covering the 15 fields of the Keck Baryonic Structure Survey using the recently commissioned MOSFIRE spectrometer on the Keck 1 telescope. We focus on a sample of 251 galaxies with redshifts 2.0 < z < 2.6, star formation rates (SFRs) 2 less than or similar to SFR less than or similar to 200 M-circle dot yr(-1), and stellar masses 8.6 < log(M-*/M-circle dot) < 11.4, with high-quality spectra in both H-and K-band atmospheric windows. We show unambiguously that the locus of z similar to 2.3 galaxies in the "BPT" nebular diagnostic diagram exhibits an almost entirely disjointed, yet similarly tight, relationship between the line ratios [N II] lambda 6585/H alpha and [O III]/H beta as compared to local galaxies. Using photoionization models, we argue that the offset of the z similar to 2.3 BPT locus relative to that at z similar to 0 is caused by a combination of harder stellar ionizing radiation field, higher ionization parameter, and higher N/O at a given O/H compared to most local galaxies, and that the position of a galaxy along the z similar to 2.3 star-forming BPT locus is surprisingly insensitive to gas-phase oxygen abundance. The observed nebular emission line ratios are most easily reproduced by models in which the net stellar ionizing radiation field resembles a blackbody with effective temperature T-eff = 50,000-60,000 K, the gas-phase oxygen abundances lie in the range 0.2 < Z/Z(circle dot) < 1.0, and the ratio of gas-phase N/O is close to the solar value. We critically assess the applicability at high redshift of commonly used strong line indices for estimating gas-phase metallicity, and consider the implications of the small intrinsic scatter of the empirical relationship between excitation-sensitive line indices and M-* (i.e., the "mass-metallicity" relation) at z less than or similar to 2.3. C1 [Steidel, Charles C.; Rudie, Gwen C.; Strom, Allison L.; Trainor, Ryan F.; Konidaris, Nicholas P.; Matthews, Keith] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Rudie, Gwen C.] Carnegie Observ, Pasadena, CA 91101 USA. [Pettini, Max] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Reddy, Naveen A.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Shapley, Alice E.; Kulas, Kristin R.; Mace, Gregory; McLean, Ian S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Erb, Dawn K.] Univ Wisconsin, Ctr Gravitat Cosmol & Astrophys, Dept Phys, Milwaukee, WI 53211 USA. [Turner, Monica L.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Kulas, Kristin R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Steidel, CC (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, 1216 East Calif Boulevard,MS 249-17, Pasadena, CA 91125 USA. OI Trainor, Ryan/0000-0002-6967-7322 FU US National Science Foundation [AST-0908805, AST-1313472]; NSF Graduate Student Research Fellowship; NSF Telescope System Instrumentation Program (TSIP) FX This work has been supported in part by the US National Science Foundation through grants AST-0908805 and AST-1313472 (CCS), as well as by an NSF Graduate Student Research Fellowship (ALS). The MOSFIRE instrument was made possible by grants to the W. M. Keck Observatory from the NSF Telescope System Instrumentation Program (TSIP) and by a generous donation from Gordon and Betty Moore. We thank our colleagues on the MOSFIRE instrument team, particularly Marcia Brown, Khan Bui, John Cromer, Jason Fucik, Hector Rodriguez, Bob Weber, and Jeff Zolkower at Caltech; Ted Aliado, George Brims, John Canfield, Chris Johnson, Ken Magnone, and Jason Weiss at UCLA; Harland Epps at UCO/Lick Observatory; and Sean Adkins at WMKO. Special thanks to the WMKO staff who helped make MOSFIRE commissioning successful, especially Marc Kassis, Allan Honey, Greg Wirth, Shui Kwok, Liz Chock, and Jim Lyke. We benefited significantly from an illuminating discussion on the subject of massive stars with Selma de Mink. Constructive comments from the anonymous referee, which led to significant improvements in the content and presentation of the results, are gratefully acknowledged. Finally, we wish to extend thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. NR 125 TC 138 Z9 138 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2014 VL 795 IS 2 AR 165 DI 10.1088/0004-637X/795/2/165 PG 40 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR8YT UT WOS:000343857900064 ER PT J AU Tendulkar, SP Furst, F Pottschmidt, K Bachetti, M Bhalerao, VB Boggs, SE Christensen, FE Craig, WW Hailey, CA Harrison, FA Stern, D Tomsick, JA Walton, DJ Zhang, W AF Tendulkar, Shriharsh P. Fuerst, Felix Pottschmidt, Katja Bachetti, Matteo Bhalerao, Varun B. Boggs, Steven E. Christensen, Finn E. Craig, William W. Hailey, Charles A. Harrison, Fiona A. Stern, Daniel Tomsick, John A. Walton, Dominic J. Zhang, William TI NuSTAR DISCOVERY OF A CYCLOTRON LINE IN THE BE/X-RAY BINARY RXJ0520.5-6932 DURING OUTBURST SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion,accretion disks; pulsars: general; pulsars: individual (RX J0520.5-6932); stars: neutron; X-rays: binaries; X-rays: bursts; X-rays: stars ID SPECTROSCOPIC-TELESCOPE-ARRAY; INTEGRAL OBSERVATION; RX J0520.5-6932; PULSE PROFILE; 4U 0115+63; LUMINOSITY; ENERGY; ABSORPTION; X-1; V-0332+53 AB We present spectral and timing analysis of NuSTAR observations of RXJ0520.5-6932 in the 3-79 keV band collected during its outburst in 2014 January. The target was observed on two epochs and we report the detection of a cyclotron resonant scattering feature with central energies of E-CRSF = 31.3(-0.7)(+0.8) keV and 31.5(0.6)(-)(+0.7) keV during the two observations, respectively, corresponding to a magnetic field of B approximate to 2 x 10(12) G. The 3-79 keV luminosity of the system during the two epochs, assuming a nominal distance of 50 kpc, was 3.667 +/- 0.007 x 10(38) erg s(-1) and 3.983 +/- 0.007 x 10(38) erg s(-1). Both values are much higher than the critical luminosity of approximate to 1.5 x 10(37) erg s(-1), above which a radiation-dominated shock front may be expected. This adds a new object to the sparse set of three systems that have a cyclotron line observed at luminosities in excess of 10(38) erg s(-1). A broad ( sigma approximate to 0.45 keV) Fe emission line is observed in the spectrum at a central energy of 6.58(-0.05)(+0.05) keV in both epochs. The pulse profile of the pulsar was observed to be highly asymmetric with a sharply rising and slowly falling profile of the primary peak. We also observed minor variations in the cyclotron line energy and width as a function of the rotation phase. C1 [Tendulkar, Shriharsh P.; Fuerst, Felix; Harrison, Fiona A.; Walton, Dominic J.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Pottschmidt, Katja] Univ Maryland, Ctr Res & Explorat Space Sci & Technol, Baltimore, MD 21250 USA. [Pottschmidt, Katja; Zhang, William] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Bachetti, Matteo] Univ Toulouse, UPS OMP, IRAP, F-31400 Toulouse, France. [Bachetti, Matteo] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France. [Bhalerao, Varun B.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Boggs, Steven E.; Tomsick, John A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, William W.; Hailey, Charles A.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Tendulkar, SP (reprint author), CALTECH, Space Radiat Lab, 1200 East Calif Blvd,MC 249-17, Pasadena, CA 91125 USA. EM spt@astro.caltech.edu RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Bhalerao, Varun/0000-0002-6112-7609; Bachetti, Matteo/0000-0002-4576-9337; Tendulkar, Shriharsh/0000-0003-2548-2926 FU NASA [NNG08FD60C] FX We thank the anonymous referee for detailed suggestions and comments. This work was supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). NR 44 TC 7 Z9 7 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2014 VL 795 IS 2 AR UNSP 154 DI 10.1088/0004-637X/795/2/154 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR8YT UT WOS:000343857900053 ER PT J AU Umetsu, K Medezinski, E Nonino, M Merten, J Postman, M Meneghetti, M Donahue, M Czakon, N Molino, A Seitz, S Gruen, D Lemze, D Balestra, I Benitez, N Biviano, A Broadhurst, T Ford, H Grillo, C Koekemoer, A Melchior, P Mercurio, A Moustakas, J Rosati, P Zitrin, A AF Umetsu, Keiichi Medezinski, Elinor Nonino, Mario Merten, Julian Postman, Marc Meneghetti, Massimo Donahue, Megan Czakon, Nicole Molino, Alberto Seitz, Stella Gruen, Daniel Lemze, Doron Balestra, Italo Benitez, Narciso Biviano, Andrea Broadhurst, Tom Ford, Holland Grillo, Claudio Koekemoer, Anton Melchior, Peter Mercurio, Amata Moustakas, John Rosati, Piero Zitrin, Adi TI CLASH: WEAK-LENSING SHEAR-AND-MAGNIFICATION ANALYSIS OF 20 GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; dark matter; galaxies: clusters: general; gravitational lensing: weak ID DARK-MATTER HALOS; STEEP MASS PROFILE; DIGITAL SKY SURVEY; X-RAY; DENSITY PROFILES; PHOTOMETRIC REDSHIFTS; GRAVITATIONAL DISTORTIONS; EMPIRICAL-MODELS; ADVANCED CAMERA; RICH CLUSTERS AB We present a joint shear-and-magnification weak-lensing analysis of a sample of 16 X-ray-regular and 4 high-magnification galaxy clusters at 0.19 less than or similar to z less than or similar to 0.69 selected from the Cluster Lensing And Supernova survey with Hubble (CLASH). Our analysis uses wide-field multi-color imaging, taken primarily with Suprime-Cam on the Subaru Telescope. From a stacked-shear-only analysis of the X-ray-selected subsample, we detect the ensemble-averaged lensing signal with a total signal-to-noise ratio of similar or equal to 25 in the radial range of 200-3500 kpc h(-1), providing integrated constraints on the halo profile shape and concentration-mass relation. The stacked tangential-shear signal is well described by a family of standard density profiles predicted for dark-matter-dominated halos in gravitational equilibrium, namely, the Navarro-Frenk-White (NFW), truncated variants of NFW, and Einasto models. For the NFW model, we measure a mean concentration of c(200c) = 4.01(-0.32)(+0.35) at an effective halo mass of M-200c = 1.34(-0.09)(+0.10) x 10(15) M-circle dot. We show that this is in excellent agreement with. cold dark matter (Lambda CDM) predictions when the CLASH X-ray selection function and projection effects are taken into account. The best-fit Einasto shape parameter is alpha(E) = 0.191(-0.068)(+0.071), which is consistent with the NFW-equivalent Einasto parameter of similar to 0.18. We reconstruct projected mass density profiles of all CLASH clusters from a joint likelihood analysis of shear-and-magnification data and measure cluster masses at several characteristic radii assuming an NFW density profile. We also derive an ensemble-averaged total projected mass profile of the X-ray-selected subsample by stacking their individual mass profiles. The stacked total mass profile, constrained by the shear+magnification data, is shown to be consistent with our shear-based halo-model predictions, including the effects of surrounding large-scale structure as a two-halo term, establishing further consistency in the context of the Lambda CDM model. C1 [Umetsu, Keiichi; Czakon, Nicole] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Medezinski, Elinor; Lemze, Doron; Ford, Holland] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Nonino, Mario; Balestra, Italo; Biviano, Andrea] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy. [Merten, Julian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Merten, Julian; Zitrin, Adi] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Postman, Marc; Koekemoer, Anton] Space Telescope Sci Inst, Baltimore, MD 21208 USA. [Meneghetti, Massimo] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Meneghetti, Massimo] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Meneghetti, Massimo] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy. [Donahue, Megan] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Molino, Alberto; Benitez, Narciso] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Seitz, Stella; Gruen, Daniel] Univ Sternwarte, D-81679 Munich, Germany. [Seitz, Stella; Gruen, Daniel] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Balestra, Italo] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Broadhurst, Tom] Ikerbasque Basque Fdn Sci, E-48011 Bilbao, Spain. [Grillo, Claudio; Koekemoer, Anton] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Melchior, Peter] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA. [Melchior, Peter] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Moustakas, John] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. [Rosati, Piero] Univ Ferrara, I-44122 Ferrara, Italy. RP Umetsu, K (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. EM keiichi@asiaa.sinica.edu.tw RI Grillo, Claudio/E-6223-2015; Meneghetti, Massimo/O-8139-2015; OI Koekemoer, Anton/0000-0002-6610-2048; Grillo, Claudio/0000-0002-5926-7143; Meneghetti, Massimo/0000-0003-1225-7084; Nonino, Mario/0000-0001-6342-9662; Balestra, Italo/0000-0001-9660-894X; Benitez, Narciso/0000-0002-0403-7455; Donahue, Megan/0000-0002-2808-0853; Umetsu, Keiichi/0000-0002-7196-4822; Biviano, Andrea/0000-0002-0857-0732 FU Academia Sinica Career Development Award; Ministry of Science and Technology of Taiwan [NSC100-2112-M-001-008-MY3, MOST 103-2112-M-001-030-MY3]; Jet Propulsion Laboratory, California Institute of Technology; National Aeronautics and Space Administration; Deutsche Forschungsgemeinschaft (DFG) [SFB-Transregio 33]; DFG cluster of excellence "Origin and Structure of the Universe"; NASA through Hubble Fellowship - STScI [HST-HF-51334.01-A]; Danish National Research Foundation FX We thank the anonymous referee for the careful reading of the manuscript and constructive suggestions. We acknowledge fruitful discussions with Nobuhiro Okabe, Masamune Oguri, Mauro Sereno, Jean Coupon, and Hitoshi Hanami. We thank Ole Host for providing very helpful comments on the manuscript. We are grateful to all members of the CLASH team who enabled us to carry out the work. We acknowledge the Subaru Support Astronomers, plus Justice Bruursema, Kai-Yang Lin, and Hiroaki Nishioka, for assistance with our Subaru observations. We thank Nick Kaiser and Masamune Oguri for making their IMCAT and GLAFIC packages publicly available. This work is partially supported by the Academia Sinica Career Development Award and by the Ministry of Science and Technology of Taiwan through grants NSC100-2112-M-001-008-MY3 and MOST 103-2112-M-001-030-MY3. J.M. acknowledges support from the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. D.G. and S.S. were supported by SFB-Transregio 33 "The Dark Universe" by the Deutsche Forschungsgemeinschaft (DFG) and the DFG cluster of excellence "Origin and Structure of the Universe." Support for A.Z. was provided by NASA through Hubble Fellowship grant #HST-HF-51334.01-A awarded by STScI. The Dark Cosmology Centre is funded by the Danish National Research Foundation. NR 136 TC 67 Z9 67 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2014 VL 795 IS 2 AR 163 DI 10.1088/0004-637X/795/2/163 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR8YT UT WOS:000343857900062 ER PT J AU Whitaker, KE Franx, M Leja, J van Dokkum, PG Henry, A Skelton, RE Fumagalli, M Momcheva, IG Brammer, GB Labbe, I Nelson, EJ Rigby, JR AF Whitaker, Katherine E. Franx, Marijn Leja, Joel van Dokkum, Pieter G. Henry, Alaina Skelton, Rosalind E. Fumagalli, Mattia Momcheva, Ivelina G. Brammer, Gabriel B. Labbe, Ivo Nelson, Erica J. Rigby, Jane R. TI CONSTRAINING THE LOW-MASS SLOPE OF THE STAR FORMATION SEQUENCE AT 0.5 < z < 2.5 SO ASTROPHYSICAL JOURNAL LA English DT Article ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; HIGH-REDSHIFT GALAXIES; LYMAN BREAK GALAXIES; DIGITAL SKY SURVEY; DEEP-FIELD-SOUTH; SIMILAR-TO 2; SPECTRAL ENERGY-DISTRIBUTION; EXTRAGALACTIC LEGACY SURVEY; EMISSION-LINE GALAXIES AB We constrain the slope of the star formation rate (SFR; log Psi) to stellar mass (logM(star)) relation down to log(M-star/M-circle dot) = 8.4 (log(M-star/M-circle dot) = 9.2) at z = 0.5 (z = 2.5) with a mass-complete sample of 39,106 starforming galaxies selected from the 3D-HST photometric catalogs, using deep photometry in the CANDELS fields. For the first time, we find that the slope is dependent on stellar mass, such that it is steeper at low masses (log Psi proportional to logM(star)) than at high masses (log Psi proportional to (0.3-0.6) logM(star)). These steeper low-mass slopes are found for three different star formation indicators: the combination of the ultraviolet (UV) and infrared (IR), calibrated from a stacking analysis of Spitzer/MIPS 24 mu m imaging; beta-corrected UV SFRs; and Ha SFRs. The normalization of the sequence evolves differently in distinct mass regimes as well: for galaxies less massive than log(M-star/M-circle dot) < 10 the specific SFR (Psi/M-star) is observed to be roughly self-similar with Psi/M-star proportional to (1 + z)(1.9), whereas more massive galaxies show a stronger evolution with Psi/M-star proportional to (1 + z)(2.2-3.5) for log(M-star/M-circle dot) = 10.2-11.2. The fact that we find a steep slope of the star formation sequence for the lower mass galaxies will help reconcile theoretical galaxy formation models with the observations. C1 [Whitaker, Katherine E.; Henry, Alaina; Rigby, Jane R.] Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Franx, Marijn; Fumagalli, Mattia; Labbe, Ivo] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Leja, Joel; van Dokkum, Pieter G.; Momcheva, Ivelina G.; Nelson, Erica J.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Skelton, Rosalind E.] S African Astron Observ, ZA-7935 Cape Town, South Africa. [Brammer, Gabriel B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Whitaker, KE (reprint author), Goddard Space Flight Ctr, Astrophys Sci Div, Code 665, Greenbelt, MD 20771 USA. EM kate.whitaker@nasa.gov RI Skelton, Rosalind/S-1845-2016; OI Skelton, Rosalind/0000-0001-7393-3336; Leja, Joel/0000-0001-6755-1315; Brammer, Gabriel/0000-0003-2680-005X FU NASA Post-doctoral Program at the Goddard Space Flight Center; NASA [NAS5-26555, HST-GO-12177, HST-GO-12328, N00181]; 3D-HST Treasury Program [GO 12177, 12328]; NWO Spinoza grant FX We thank the anonymous referee for insightful comments and a careful reading of the manuscript. The authors wish to acknowledge Kristian Finlator for helpful discussions. K.E.W. and A.H. are supported by appointments to the NASA Post-doctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. The authors are grateful to the many colleagues who have provided public data and catalogs in the five deep 3D-HST/CANDELS fields; high redshift galaxy science has thrived owing to this gracious mindset and the TACs and the Observatory Directors who have encouraged this. This work is based on observations taken by the 3D-HST Treasury Program (GO 12177 and 12328) with the NASA/ESA HST, which is operated by the Associations of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. M.F. acknowledges support from an NWO Spinoza grant. Support from NASA grants HST-GO-12177, HST-GO-12328, and N00181 is gratefully acknowledged. NR 109 TC 128 Z9 129 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 NOV 10 PY 2014 VL 795 IS 2 AR 104 DI 10.1088/0004-637X/795/2/104 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR8YT UT WOS:000343857900003 ER PT J AU Winebarger, AR Lionello, R Mok, Y Linker, JA Mikic, Z AF Winebarger, Amy R. Lionello, Roberto Mok, Yung Linker, Jon A. Mikic, Zoran TI VERIFICATION OF CORONAL LOOP DIAGNOSTICS USING REALISTIC THREE-DIMENSIONAL HYDRODYNAMIC MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: fundamental parameters; Sun: UV radiation; Sun: X-rays, gamma rays ID EMISSION MEASURE DISTRIBUTION; EUV IMAGING SPECTROMETER; TRANSITION REGION MOSS; SOLAR ACTIVE REGIONS; 3 DIMENSIONS; DYNAMICS; TRACE; HINODE; SOHO/CDS; EXPLORER AB Many different techniques have been used to characterize the plasma in the solar corona: density-sensitive spectral line ratios are used to infer the density, the evolution of coronal structures in different passbands is used to infer the temperature evolution, and the simultaneous intensities measured in multiple passbands are used to determine the emission measure distributions. All these analysis techniques assume that the intensity of the structures can be isolated through background subtraction. In this paper, we use simulated observations from a three-dimensional hydrodynamic simulation of a coronal active region to verify these diagnostics. The density and temperature from the simulation are used to generate images in several passbands and spectral lines. We identify loop structures in the simulated images and calculate the background. We then determine the density, temperature, and emission measure distribution as a function of time from the observations and compare these with the true temperature and density of the loop. We find that the overall characteristics of the temperature, density, and emission measure are recovered by the analysis methods, but the details are not. For instance, the emission measure curves calculated from the simulated observations are much broader than the true emission measure distribution, though the average temperature evolution is similar. These differences are due, in part, to a limitation of the analysis methods, but also to inadequate background subtraction. C1 [Winebarger, Amy R.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Lionello, Roberto; Linker, Jon A.; Mikic, Zoran] Predict Sci Inc, San Diego, CA 92121 USA. [Mok, Yung] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. RP Winebarger, AR (reprint author), NASA, Marshall Space Flight Ctr, ZP 13, Huntsville, AL 35812 USA. EM amy.r.winebarger@nasa.gov; lionel@predsci.com; ymok@uci.edu; linkerj@predsci.com; mikicz@predsci.com OI Lionello, Roberto/0000-0001-9231-045X FU NASA's LWS; Heliophysics Theory Programs; NSF's Strategic Capabilities Program; Center for Integrated Space Weather Modeling; AFOSR FX The authors thank Dr. Caroline Alexander for providing useful feedback on the manuscript. This work was supported by NASA's LWS and Heliophysics Theory Programs, NSF's Strategic Capabilities Program and the Center for Integrated Space Weather Modeling, and AFOSR. This paper is an outgrowth of the participation of A.W., Z.M., and R.L. in the 2011 "Loops Workshop." NR 40 TC 8 Z9 8 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2014 VL 795 IS 2 AR 138 DI 10.1088/0004-637X/795/2/138 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR8YT UT WOS:000343857900037 ER PT J AU Read, JS Winslow, LA Hansen, GJA Van den Hoek, J Hanson, PC Bruce, LC Markfort, CD AF Read, Jordan S. Winslow, Luke A. Hansen, Gretchen J. A. Van den Hoek, Jamon Hanson, Paul C. Bruce, Louise C. Markfort, Corey D. TI Simulating 2368 temperate lakes reveals weak coherence in stratification phenology SO ECOLOGICAL MODELLING LA English DT Article DE Limnology; Climate change; Water temperature; Lake temperature modeling; Coherence; Stratification ID NORTH-ATLANTIC OSCILLATION; FUTURE CLIMATE SCENARIOS; FRESH-WATER ECOSYSTEMS; ICE COVER; DISSOLVED-OXYGEN; UNITED-STATES; MODEL; HABITAT; QUALITY; CONSERVATION AB Changes in water temperatures resulting from climate warming can alter the structure and function of aquatic ecosystems. Lake-specific physical characteristics may play a role in mediating individual lake responses to climate. Past mechanistic studies of lake-climate interactions have simulated generic lake classes at large spatial scales or performed detailed analyses of small numbers of real lakes. Understanding the diversity of lake responses to climate change across landscapes requires a hybrid approach that couples site-specific lake characteristics with broad-scale environmental drivers. This study provides a substantial advancement in lake ecosystem modeling by combining open-source tools with freely available continental-scale data to mechanistically model daily temperatures for 2368 Wisconsin lakes over three decades (1979-2011). The model accurately predicted observed surface layer temperatures (RMSE: 1.74 degrees C) and the presence/absence of stratification (81.1% agreement). Among-lake coherence was strong for surface temperatures and weak for the timing of stratification, suggesting individual lake characteristics mediate some - but not all - ecologically relevant lake responses to climate. Published by Elsevier B.V. This is an open access article under the CC BY license. C1 [Read, Jordan S.] US Geol Survey, Ctr Integrated Data Analyt, Middleton, WI 53562 USA. [Winslow, Luke A.; Hansen, Gretchen J. A.; Hanson, Paul C.] Univ Wisconsin, Ctr Limnol, Madison, WI 53706 USA. [Hansen, Gretchen J. A.] Wisconsin Dept Nat Resources, Bur Sci Serv, Madison, WI USA. [Van den Hoek, Jamon] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Bruce, Louise C.] Univ Western Australia, Sch Earth & Environm, Perth, WA 6009, Australia. [Markfort, Corey D.] Univ Iowa, IIHR Hydrosci & Engn, Iowa City, IA USA. RP Read, JS (reprint author), US Geol Survey, Ctr Integrated Data Analyt, Middleton, WI 53562 USA. EM jread@usgs.gov RI Markfort, Corey/A-1217-2012; OI Markfort, Corey/0000-0003-3168-9149; Read, Jordan/0000-0002-3888-6631 FU U.S. Geological Survey NCCWSC [10909172]; NSF [DEB-0941510, DEB-0822700, IIS-1344272]; Wisconsin Department of Natural Resources Federal Aid in Sport Fish Restoration [F-95-P]; U.S. Geological Survey Center for Integrated Data Analytics FX This study was funded by U.S. Geological Survey NCCWSC grant 10909172, NSF grant DEB-0941510 (Global Lake Ecological Observatory Network), the Wisconsin Department of Natural Resources Federal Aid in Sport Fish Restoration (Project F-95-P), the U.S. Geological Survey Center for Integrated Data Analytics, and NSF grants DEB-0822700 (North Temperate Lakes Long-Term Ecological Research), and IIS-1344272 (INSPIRE). Mathew Hipsey and Casper Boon (the Aquatic Ecosystem Dynamics group at The University of Western Australia) shared modeling and development expertise for GLM. We thank Jereme Gaeta, Steven Greb, Matthew Diebel, Alex Latzka, Emily Stanley, Kevin Rose, Dale Robertson, Emily Read, David Blodgett, Ivan Suftin, Jordan Walker, Meredith Pavlick Warren, and Jake Vander Zanden for their contributions to this manuscript. Tim Kratz and Stephen Carpenter helped improve this article with thoughtful reviews. Two anonymous reviewers contributed substantially to the improvement of our original manuscript. We also thank the Ecological Modeling editorial staff. NR 66 TC 14 Z9 14 U1 7 U2 32 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3800 EI 1872-7026 J9 ECOL MODEL JI Ecol. Model. PD NOV 10 PY 2014 VL 291 BP 142 EP 150 DI 10.1016/j.ecolmodel.2014.07.029 PG 9 WC Ecology SC Environmental Sciences & Ecology GA AR2AU UT WOS:000343386500013 ER PT J AU Wang, AN Marashdeh, Q Motil, BJ Fan, LS AF Wang, Aining Marashdeh, Qussai Motil, Brian J. Fan, Liang-Shih TI Electrical capacitance volume tomography for imaging of pulsating flows in a trickle bed SO CHEMICAL ENGINEERING SCIENCE LA English DT Article DE Trickle bed; Pulsating flow; Capacitance tomography; Liquid pulse; Flow regime; Multiphase flow ID GAS-LIQUID DOWNFLOW; PULSING FLOW; PACKED-BED; HYDRODYNAMIC PROPERTIES; COCURRENT DOWNFLOW; PRESSURE-DROP; MASS-TRANSFER; REACTORS; TRANSITION; REGIME AB Experimental results of the air water pulsating flows in a trickle bed column were obtained using the electrical capacitance volume tomography (ECVT) system. Detailed 3-D pulse structures in both the fully developed and the transient conditions were illustrated. Pulse frequency, pulse traveling velocity, average liquid holdup and liquid holdup inside the gas rich and liquid rich regions, respectively, were measured. Based on a simplified model, the linear liquid velocities inside the gas rich and liquid rich regions were estimated. The results revealed that the gas flow rate was the most important parameter in controlling the pulsating flow properties. Discussion on the physical nature of the pulsating flow was also given. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Wang, Aining; Fan, Liang-Shih] Ohio State Univ, Dept Chem & Biomol Engn, Columbus, OH 43210 USA. [Marashdeh, Qussai] Tech4Imaging LLC, Columbus, OH 43220 USA. [Motil, Brian J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Fan, LS (reprint author), Ohio State Univ, Dept Chem & Biomol Engn, 140 West 19th Ave, Columbus, OH 43210 USA. EM wang.1954@osu.edu; marashdeh@tech4imaging.com; brian.j.motil@nasa.gov; fan.1@osu.edu OI Wang, Aining/0000-0002-2920-1338 NR 31 TC 7 Z9 7 U1 1 U2 26 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0009-2509 EI 1873-4405 J9 CHEM ENG SCI JI Chem. Eng. Sci. PD NOV 8 PY 2014 VL 119 BP 77 EP 87 DI 10.1016/j.ces.2014.08.011 PG 11 WC Engineering, Chemical SC Engineering GA AQ3GY UT WOS:000342680700008 ER PT J AU Struk, PM T'ien, JS Miller, FJ Dietrich, DL AF Struk, P. M. T'ien, J. S. Miller, F. J. Dietrich, D. L. TI Transient numerical modeling of catalytic channels using a quasi-steady gas phase SO CHEMICAL ENGINEERING SCIENCE LA English DT Article DE Catalysis; Mathematical modeling; Microreactor; Mass transfer; Heat transfer; Carbon monoxide ID DIFFERENTIAL-ALGEBRAIC SYSTEMS; MASS-TRANSFER; HEAT-TRANSFER; MONOLITH REACTORS; CARBON-MONOXIDE; LOW-TEMPERATURE; COMBUSTION; PLATINUM; OXIDATION; METHANE AB This paper presents a transient model of internal catalytic combustion suitable for isolated channels and monolith reactors. Due to time-scales in the problem, the model considers a quasi steady gas phase with a transient solid. The gas is described by axially varying bulk temperature and species. The gas includes lateral diffusion via transfer coefficients and the specification of a gas phase species concentration at the wall; axial diffusion is neglected. The solid phase is a thermally thin shell with axially varying temperature, surface species, and surface species concentrations. The solid includes axial heat conduction and external heat loss by convection and radiation. The combustion process utilizes detailed gas and surface reaction models. The gas-phase model becomes a system of stiff ordinary differential equations with respect to axial position; the upstream (inlet) boundary conditions are specified and the axially varying solid properties are parameters in integration. The solid phase discretizes into a system of stiff ordinary differential-algebraic equations with respect to time. The time evolution of the system comes from alternating integrations of the quasi-steady gas phase and transient solid. The model is compared to two experimental cases using CO fuel: (1) steady-state conversion in an isothermal platinum tube and (2) transient propagation of a catalytic reaction inside a small platinum tube and includes external tube temperature measurements. This work presents sensitivity studies on important parameters including internal transfer coefficients, catalytic surface site density, external heat-loss, and others. Under mass-transfer limited conditions, global transfer coefficients are adequate to predict fuel conversion. Near light-off, the model predictions improve for the first case after adjusting the surface kinetics such that the net rate of CO adsorption increases compared to O-2. For the second case, predictions of transient propagation speeds are good for equivalence ratios near unity and greater but require adjustment of external heat loss or kinetics to match under lean conditions. (C) 2014 Published by Elsevier Ltd. C1 [Struk, P. M.; Dietrich, D. L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [T'ien, J. S.] Case Western Reserve Univ, Cleveland, OH 44106 USA. [Miller, F. J.] San Diego State Univ, San Diego, CA 92182 USA. RP Struk, PM (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM Peter.M.Struk@nasa.gov FU NASA Office of Human Systems Research and Technology [NNC04AA29A]; NASA Glenn Research Center IRD Fund FX The authors gratefully acknowledge support from the NASA Office of Human Systems Research and Technology to the National Center for Space Exploration Research, and Cooperative Agreement NNC04AA29A to Case Western Reserve University. This work was also supported in part by the NASA Glenn Research Center IR&D Fund. Finally, the authors wish to thank Mr. Benjamin Mellish and Mr. Michael C. Johnston for their valuable contributions in the laboratory. NR 61 TC 1 Z9 1 U1 2 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0009-2509 EI 1873-4405 J9 CHEM ENG SCI JI Chem. Eng. Sci. PD NOV 8 PY 2014 VL 119 BP 158 EP 173 DI 10.1016/j.ces.2014.07.053 PG 16 WC Engineering, Chemical SC Engineering GA AQ3GY UT WOS:000342680700016 ER PT J AU Yu, SS Drouin, BJ Miller, CE AF Yu, Shanshan Drouin, Brian J. Miller, Charles E. TI High resolution spectral analysis of oxygen. IV. Energy levels, partition sums, band constants, RKR potentials, Franck-Condon factors involving the X-3 Sigma(-)(g), a(1) Delta(g) and b(1) Sigma(+)(g) states SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID A-BAND; MOLECULAR-OXYGEN; PART II; ABSORPTION; O-2; EMISSIONS; TRANSITIONS; INTENSITY; RETRIEVAL; NIGHTGLOW AB We have updated the isotopically invariant Dunham fit of O-2 with newly reported literature transitions to derive (1) the energy levels, partition sums, band-by-band molecular constants, and RKR potentials for the X-3 Sigma(-)(g), a(1) Delta(g), and b(1) Sigma(+)(g) states of the six O2 isotopologues: (OO)-O-16-O-16, (OO)-O-16-O-17, (OO)-O-16-O-18, (OO)-O-17-O-17, (OO)-O-17-O-18, and (OO)-O-18-O-18; (2) Franck-Condon factors for their a(1) Delta(g) - X-3 Sigma(-)(g), b(1) Sigma(+)(g) - X-3 Sigma(-)(g), and a(1) Delta(g) - b(1) Sigma(+)(g) band systems. This new spectroscopic parameterization characterizes all known transitions within and between the X-3 Sigma(-)(g), a(1) Sigma(-)(g), and b(1) Sigma(+)(g) states within experimental uncertainty and can be used for accurate predictions of as yet unmeasured transitions. All of these results are necessary to provide a consistent linelist of all transitions which will be reported in a followup paper. (C) 2014 AIP Publishing LLC. C1 [Yu, Shanshan; Drouin, Brian J.; Miller, Charles E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Yu, SS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM shanshan.yu@jpl.nasa.gov RI Yu, Shanshan/D-8733-2016 NR 37 TC 2 Z9 2 U1 2 U2 25 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD NOV 7 PY 2014 VL 141 IS 17 AR 174302 DI 10.1063/1.4900510 PG 12 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA AT2RL UT WOS:000344782200017 PM 25381509 ER PT J AU Moseley, SH AF Moseley, S. H. TI The other half of the universe? SO SCIENCE LA English DT Editorial Material ID BACKGROUND ANISOTROPIES; FLUCTUATIONS; GALAXIES; LIGHT C1 NASA, Goddard Space Flight Ctr, Lab Observat Cosmol, Greenbelt, MD 20771 USA. RP Moseley, SH (reprint author), NASA, Goddard Space Flight Ctr, Lab Observat Cosmol, Greenbelt, MD 20771 USA. EM harvey.moseley@nasa.gov NR 7 TC 0 Z9 0 U1 1 U2 5 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 NOV 7 PY 2014 VL 346 IS 6210 BP 696 EP 697 DI 10.1126/science.aaa1077 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AT1JT UT WOS:000344690100019 PM 25378605 ER PT J AU Zemcov, M Smidt, J Arai, T Bock, J Cooray, A Gong, Y Kim, MG Korngut, P Lam, A Lee, DH Matsumoto, T Matsuura, S Nam, UW Roudier, G Tsumura, K Wada, T AF Zemcov, Michael Smidt, Joseph Arai, Toshiaki Bock, James Cooray, Asantha Gong, Yan Kim, Min Gyu Korngut, Phillip Lam, Anson Lee, Dae Hee Matsumoto, Toshio Matsuura, Shuji Nam, Uk Won Roudier, Gael Tsumura, Kohji Wada, Takehiko TI On the origin of near-infrared extragalactic background light anisotropy SO SCIENCE LA English DT Article ID EXPERIMENT CIBER; POPULATION-III; FLUCTUATIONS; SKY; SPECTRUM; STARS; 2MASS AB Extragalactic background light (EBL) anisotropy traces variations in the total production of photons over cosmic history and may contain faint, extended components missed in galaxy point-source surveys. Infrared EBL fluctuations have been attributed to primordial galaxies and black holes at the epoch of reionization (EOR) or, alternately, intrahalo light (IHL) from stars tidally stripped from their parent galaxies at low redshift. We report new EBL anisotropy measurements from a specialized sounding rocket experiment at 1.1 and 1.6 micrometers. The observed fluctuations exceed the amplitude from known galaxy populations, are inconsistent with EOR galaxies and black holes, and are largely explained by IHL emission. The measured fluctuations are associated with an EBL intensity that is comparable to the background from known galaxies measured through number counts and therefore a substantial contribution to the energy contained in photons in the cosmos. C1 [Zemcov, Michael; Bock, James; Korngut, Phillip; Lam, Anson] CALTECH, Dept Phys Math & Astron, Pasadena, CA 91125 USA. [Zemcov, Michael; Bock, James; Korngut, Phillip; Roudier, Gael] NASA, JPL, Pasadena, CA 91109 USA. [Smidt, Joseph] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA. [Smidt, Joseph; Cooray, Asantha; Gong, Yan] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Arai, Toshiaki; Matsumoto, Toshio; Matsuura, Shuji; Wada, Takehiko] Japan Aerosp Explorat Agcy JAXA, ISAS, Dept Space Astron & Astrophys, Sagamihara, Kanagawa 2525210, Japan. [Arai, Toshiaki] Univ Tokyo, Grad Sch Sci, Dept Phys, Tokyo 1130033, Japan. [Kim, Min Gyu] Seoul Natl Univ, Dept Phys & Astron, Seoul 151742, South Korea. [Lam, Anson] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Lee, Dae Hee; Nam, Uk Won] Korea Astron & Space Sci Inst KASI, Taejon 305348, South Korea. [Matsumoto, Toshio] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Tsumura, Kohji] Tohoku Univ, Frontier Res Inst Interdisciplinary Sci, Sendai, Miyagi 9808578, Japan. RP Bock, J (reprint author), CALTECH, Dept Phys Math & Astron, Pasadena, CA 91125 USA. EM jjb@astro.caltech.edu RI Matsuura, Shuji/B-5658-2016 OI Matsuura, Shuji/0000-0002-5698-9634 FU NASA APRA [NNX07AI54G, NNG05WC18G, NNX07AG43G, NNX07AJ24G, NNX10AE12G]; Jet Propulsion Laboratory's Director's Research and Development Fund; KAKENHI from Japan Society for the Promotion of Science (JSPS) [20.34, 18204018, 19540250, 21340047, 21111004]; Ministry of Education, Culture, Sports, Science and Technology (MEXT); Pioneer Project from Korea Astronomy and Space Science Institute (KASI); NASA Postdoctoral Program; NSF CAREER [AST-0645427]; NSF [AST-1313319]; JSPS Research Fellowship for Young Scientists; National Aeronautics and Space Administration; National Science Foundation FX Our thanks to O. Dore, J. Filippini, and K. Ganga for useful conversations and comments throughout the course of this work and K. Helgason for kindly providing models of the statistics of the near-infrared CIB. The authors acknowledge the excellent support from the NASA sounding rockets program that was essential in developing, testing, qualifying, launching, and recovering our payloads. The CIBER auto-and cross-power spectra are available for public download at http://ciber.caltech.edu/zemcovetal. This work was supported by NASA APRA research grants NNX07AI54G, NNG05WC18G, NNX07AG43G, NNX07AJ24G, and NNX10AE12G. Initial support was provided by an award to J. B. from the Jet Propulsion Laboratory's Director's Research and Development Fund. Japanese participation in CIBER was supported by KAKENHI (20.34, 18204018, 19540250, 21340047, and 21111004) from Japan Society for the Promotion of Science (JSPS) and the Ministry of Education, Culture, Sports, Science and Technology (MEXT). Korean participation in CIBER was supported by the Pioneer Project from Korea Astronomy and Space Science Institute (KASI). M.Z. and P. K. acknowledge support from NASA Postdoctoral Program fellowships, A. C. acknowledges support from an NSF CAREER award AST-0645427 and NSF AST-1313319, and K. T. acknowledges support from the JSPS Research Fellowship for Young Scientists. This publication makes use of data products from the Two Micron All Sky Survey (2MASS), 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 work made use of images and/or data products provided by the National Optical Astronomy Observatory (NOAO) Deep Wide-Field Survey (NDWFS), which is supported by NOAO, operated by AURA, Inc., under a cooperative agreement with the National Science Foundation. NR 28 TC 24 Z9 24 U1 2 U2 19 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 NOV 7 PY 2014 VL 346 IS 6210 BP 732 EP 735 DI 10.1126/science.1258168 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AT1JT UT WOS:000344690100036 PM 25378620 ER PT J AU Mahieu, E Chipperfield, MP Notholt, J Reddmann, T Anderson, J Bernath, PF Blumenstock, T Coffey, MT Dhomse, SS Feng, W Franco, B Froidevaux, L Griffith, DWT Hannigan, JW Hase, F Hossaini, R Jones, NB Morino, I Murata, I Nakajima, H Palm, M Paton-Walsh, C Russell, JM Schneider, M Servais, C Smale, D Walker, KA AF Mahieu, E. Chipperfield, M. P. Notholt, J. Reddmann, T. Anderson, J. Bernath, P. F. Blumenstock, T. Coffey, M. T. Dhomse, S. S. Feng, W. Franco, B. Froidevaux, L. Griffith, D. W. T. Hannigan, J. W. Hase, F. Hossaini, R. Jones, N. B. Morino, I. Murata, I. Nakajima, H. Palm, M. Paton-Walsh, C. Russell, J. M., III Schneider, M. Servais, C. Smale, D. Walker, K. A. TI Recent Northern Hemisphere stratospheric HCl increase due to atmospheric circulation changes SO NATURE LA English DT Article ID INORGANIC CHLORINE; OZONE; EVOLUTION; SYSTEM; AIR; AGE AB The abundance of chlorine in the Earth's atmosphere increased considerably during the 1970s to 1990s, following large emissions of anthropogenic long-lived chlorine-containing source gases, notably the chlorofluorocarbons. The chemical inertness of chlorofluorocarbons allows their transport and mixing throughout the troposphere on a global scale(1), before they reach the stratosphere where they release chlorine atoms that cause ozone depletion(2). The large ozone loss over Antarctica(3) was the key observation that stimulated the definition and signing in 1987 of the Montreal Protocol, an international treaty establishing a schedule to reduce the production of the major chlorine-and bromine-containing halocarbons. Owing to its implementation, the near-surface total chlorine concentration showed a maximum in 1993, followed by a decrease of half a per cent to one per cent per year(4), in line with expectations. Remote-sensing data have revealed a peak in stratospheric chlorine after 1996(5), then a decrease of close to one per cent per year(6,7), in agreement with the surface observations of the chlorine source gases and model calculations(7). Here we present ground-based and satellite data that show a recent and significant increase, at the 2 sigma level, in hydrogen chloride (HCl), the main stratospheric chlorine reservoir, starting around 2007 in the lower stratosphere of the Northern Hemisphere, in contrast with the ongoing monotonic decrease of near-surface source gases. Using model simulations, we attribute this trend anomaly to a slow down in the Northern Hemisphere atmospheric circulation, occurring over several consecutive years, transporting more aged air to the lower stratosphere, and characterized by a larger relative conversion of source gases to HCl. This short-term dynamical variability will also affect other stratospheric tracers and needs to be accounted for when studying the evolution of the stratospheric ozone layer. C1 [Mahieu, E.; Franco, B.; Servais, C.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Chipperfield, M. P.; Dhomse, S. S.; Feng, W.; Hossaini, R.] Univ Leeds, Sch Earth & Environm, Natl Ctr Atmospher Sci, Leeds LS2 9JT, W Yorkshire, England. [Notholt, J.; Palm, M.] Univ Bremen, Dept Phys, D-28334 Bremen, Germany. [Reddmann, T.; Blumenstock, T.; Hase, F.; Schneider, M.] Karlsruhe Inst Technol KIT, Inst Meteorol & Climate Res IMK ASF, D-76021 Karlsruhe, Germany. [Anderson, J.; Russell, J. M., III] Hampton Univ, Dept Atmospher & Planetary Sci, Hampton, VA 23668 USA. [Bernath, P. F.] Old Dominion Univ, Dept Chem & Biochem, Norfolk, VA 23529 USA. [Bernath, P. F.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. [Bernath, P. F.; Walker, K. A.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. [Coffey, M. T.; Hannigan, J. W.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Froidevaux, L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Griffith, D. W. T.; Jones, N. B.; Paton-Walsh, C.] Univ Wollongong, Sch Chem, Wollongong, NSW 2522, Australia. [Morino, I.; Nakajima, H.] Natl Inst Environm Studies NIES, Tsukuba, Ibaraki 3058506, Japan. [Murata, I.] Tohoku Univ, Grad Sch Environm Studies, Sendai, Miyagi 9808578, Japan. [Smale, D.] Natl Inst Water & Atmospher Res NIWA, Lauder 9352, New Zealand. [Walker, K. A.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. RP Mahieu, E (reprint author), Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. EM emmanuel.mahieu@ulg.ac.be RI Chipperfield, Martyn/H-6359-2013; Morino, Isamu/K-1033-2014; Bernath, Peter/B-6567-2012; FENG, WUHU/B-8327-2008; Hossaini, Ryan/F-7134-2015; Jones, Nicholas/G-5575-2011; Dhomse, Sandip/C-8198-2011; Schneider, Matthias/B-1441-2013; Notholt, Justus/P-4520-2016; OI Mahieu, Emmanuel/0000-0002-5251-0286; Palm, Mathias/0000-0001-7191-6911; Chipperfield, Martyn/0000-0002-6803-4149; Morino, Isamu/0000-0003-2720-1569; Bernath, Peter/0000-0002-1255-396X; FENG, WUHU/0000-0002-9907-9120; Jones, Nicholas/0000-0002-0111-2368; Dhomse, Sandip/0000-0003-3854-5383; Notholt, Justus/0000-0002-3324-885X; Paton-Walsh, Clare/0000-0003-1156-4138 FU Belgian Science Policy Office (BELSPO), Brussels; Fonds de la Recherche Scientifique-FNRS, Brussels; MeteoSwiss (Global Atmospheric Watch); Federation Wallonie-Bruxelles; International Foundation High Altitude Research Stations Jungfraujoch and Gornergrat (HFSJG, Bern); NASA MEASURE's GOZCARDS programme; National Oceanic and Atmospheric Administration's Educational Partnership Program Cooperative Remote Sensing Science and Technology Center (NOAA EPP CREST); Canadian Space Agency; National Science Foundation; National Aeronautics and Space Administration (NASA); NSF Office of Polar Programs; Danish Meteorological Institute; Australian Research Council [DP110101948]; New Zealand's Ministry of Business, Innovation and Employment FX The University of Liege contribution was mainly supported by the Belgian Science Policy Office (BELSPO) and the Fonds de la Recherche Scientifique-FNRS, both in Brussels. Additional support was provided by MeteoSwiss (Global Atmospheric Watch) and the Federation Wallonie-Bruxelles. We thank the International Foundation High Altitude Research Stations Jungfraujoch and Gornergrat (HFSJG, Bern). We thank O. Flock and D. Zander (University of Liege). The SLIMCAT modelling work was supported by the UK Natural Environment Research Council (NCAS and NCEO). The FTIR measurements at Ny-Alesund, Spitsbergen, are supported by the AWI Bremerhaven. The work from Hampton University was partially funded under the NASA MEASURE's GOZCARDS programme and the National Oceanic and Atmospheric Administration's Educational Partnership Program Cooperative Remote Sensing Science and Technology Center (NOAA EPP CREST). The ACE mission is supported primarily by the Canadian Space Agency. We thank U. Raffalski and P. Voelger for technical support at IRF Kiruna. The National Center for Atmospheric Research is supported by the National Science Foundation. The observation programme at Thule, Greenland, is supported under contract by the National Aeronautics and Space Administration (NASA) and the site is also supported by the NSF Office of Polar Programs. We thank the Danish Meteorological Institute for support at Thule. Work at the Jet Propulsion Laboratory, California Institute of Technology, was performed under contract with NASA; we thank R. Fuller for help in producing the GOZCARDS data set, and work by many ACE-FTS, HALOE and MLS team members who helped to produce data towards the GOZCARDS data set is also acknowledged. We thank O. E. Garcia, E. Sepulveda, and the State Meteorological Agency (AEMET) of Spain for scientific and technical support at Izana. The Australian Research Council has provided notable support over the years for the NDACC site at Wollongong, most recently as part of project DP110101948. Measurements at Lauder are core funded through New Zealand's Ministry of Business, Innovation and Employment. We are grateful to all colleagues who have contributed to FTIR data acquisition. We thank ECMWF for providing the ERA-Interim reanalyses. NR 21 TC 20 Z9 20 U1 8 U2 57 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD NOV 6 PY 2014 VL 515 IS 7525 BP 104 EP 107 DI 10.1038/nature13857 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AS3OE UT WOS:000344187500038 PM 25373680 ER PT J AU Gao, F He, T Wang, ZS Ghimire, B Shuai, YM Masek, J Schaaf, C Williams, C AF Gao, Feng He, Tao Wang, Zhuosen Ghimire, Bardan Shuai, Yanmin Masek, Jeffrey Schaaf, Crystal Williams, Christopher TI Multiscale climatological albedo look-up maps derived from moderate resolution imaging spectroradiometer BRDF/albedo products SO JOURNAL OF APPLIED REMOTE SENSING LA English DT Article DE albedo; look-up table; radiative forcing; moderate resolution imaging spectroradi-ometer; climate change ID REFLECTANCE DISTRIBUTION FUNCTION; LAND-USE TRANSITIONS; SURFACE ALBEDO; SECONDARY LANDS; WOOD-HARVEST; IN-SITU; MODIS; RETRIEVALS; VEGETATION; MCD43A AB Surface albedo determines radiative forcing and is a key parameter for driving Earth's climate. Better characterization of surface albedo for individual land cover types can reduce the uncertainty in estimating changes to Earth's radiation balance due to land cover change. This paper presents albedo look-up maps (LUMs) using a multiscale hierarchical approach based on moderate resolution imaging spectroradiometer (MODIS) bidirectional reflectance distribution function (BRDF)/albedo products and Landsat imagery. Ten years (2001 to 2011) of MODIS BRDF/albedo products were used to generate global albedo climatology. Albedo LUMs of land cover classes defined by the International Geosphere-Biosphere Programme (IGBP) at multiple spatial resolutions were generated. The albedo LUMs included monthly statistics of white sky (diffuse) and black sky (direct) albedo for each IGBP class for visible, near infrared, and shortwave broadband under both snow free and snow covered conditions. The albedo LUMs were assessed by using the annual MODIS IGBP land cover map and the projected land use scenarios from the Intergovernmental Panel on Climate Change land use harmonization project. The comparisons between the reconstructed albedo and the MODIS albedo data product show good agreement. The LUMs provide high temporal and spatial resolution global albedo statistics without gaps for investigating albedo variations under different land cover scenarios and could be used for land surface modeling. (C) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. C1 [Gao, Feng] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. [He, Tao] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Wang, Zhuosen; Schaaf, Crystal] Univ Massachusetts, Sch Environm, Boston, MA 02125 USA. [Shuai, Yanmin; Masek, Jeffrey] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Ghimire, Bardan; Williams, Christopher] Clark Univ, Grad Sch Geog, Worcester, MA 01610 USA. RP Gao, F (reprint author), USDA ARS, Hydrol & Remote Sensing Lab, 10300 Baltimore Ave, Beltsville, MD 20705 USA. EM feng.gao@ars.usda.gov RI Masek, Jeffrey/D-7673-2012; He, Tao/H-5130-2012 OI He, Tao/0000-0003-2079-7988 FU NASA Science of Terra and Aqua award through the NASA Terrestrial Ecology Program; Landsat Science Team project through the U.S. Geological Survey FX This work was supported by a NASA Science of Terra and Aqua award through the NASA Terrestrial Ecology Program and a Landsat Science Team project through the U.S. Geological Survey. We would like to thank Demien Sulla-Menashe for providing MODIS climatology land cover data. USDA and NASA are an equal opportunity providers and employers. NR 24 TC 6 Z9 6 U1 1 U2 15 PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 1931-3195 J9 J APPL REMOTE SENS JI J. Appl. Remote Sens. PD NOV 5 PY 2014 VL 8 AR 083532 DI 10.1117/1.JRS.8.083532 PG 15 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA CA1MC UT WOS:000348675600001 ER PT J AU Adriani, O Akaike, Y Asaoka, Y Asano, K Bagliesi, MG Bigongiari, G Binns, WR Bongi, M Buckley, JH Cassese, A Castellini, G Cherry, ML Collazuol, G Ebisawa, K Di Felice, V Puke, H Guzik, TG Hams, T Hareyama, M Hibino, K Ichimura, M Ioka, K Israel, MH Javaid, A Kamioka, E Kasahara, K Katayose, Y Kataoka, J Kataoka, R Kawanaka, N Kitamura, H Kotani, T Krawczynski, HS Krizmanic, JF Kubota, A Kuramata, S Lomtadze, T Maestro, P Marcelli, L Marrocchesi, PS Mitchell, JW Miyake, S Mizutani, K Motz, HM Moiseev, AA Mori, K Mori, M Mori, N Munakata, K Murakami, H Nakagawa, YE Nakahira, S Nishimura, J Okuno, S Ormes, JF Ozawa, S Palma, F Papini, P Rauch, BF Ricciarini, S Sakamoto, T Sasaki, M Shibata, M Shimizu, Y Shiomi, A Sparvoli, R Spillantini, P Takahashi, I Takayanag, M Takita, M Tamura, T Tateyama, N Terasawa, T Tomid, H Torii, S Tunesada, Y Uchihori, Y Ueno, S Vannuccini, E Wefel, JP Yamaok, K Yanagita, S Yoshida, A Yoshida, K Yuda, T AF Adriani, O. Akaike, Y. Asaoka, Y. Asano, K. Bagliesi, M. G. Bigongiari, G. Binns, W. R. Bongi, M. Buckley, J. H. Cassese, A. Castellini, G. Cherry, M. L. Collazuol, G. Ebisawa, K. Di Felice, V. Puke, H. Guzik, T. G. Hasebe, N. Hareyama, M. Hibino, K. Ichimura, M. Ioka, K. Israel, M. H. Javaid, A. Kamioka, E. Kasahara, K. Katayose, Y. Kataoka, J. Kataoka, R. Kawanaka, N. Kitamura, H. Kotani, T. Krawczynski, H. S. Krizmanic, J. F. Kubota, A. Kuramata, S. Lomtadze, T. Maestro, P. Marcelli, L. Marrocchesi, P. S. Mitchell, J. W. Miyake, S. Mizutani, K. Motz, H. M. Moiseev, A. A. Mori, K. Mori, M. Mori, N. Munakata, K. Murakami, H. Nakagawa, Y. E. Nakahira, S. Nishimura, J. Okuno, S. Ormes, J. F. Ozawa, S. Palma, F. Papini, P. Rauch, B. F. Ricciarini, S. Sakamoto, T. Sasaki, M. Shibata, M. Shimizu, Y. Shiomi, A. Sparvoli, R. Spillantini, P. Takahashi, I. Takayanag, M. Takita, M. Tamura, T. Tateyama, N. Terasawa, T. Tomid, H. Torii, S. Tunesada, Y. Uchihori, Y. Ueno, S. Vannuccini, E. Wefel, J. P. Yamaok, K. Yanagita, S. Yoshida, A. Yoshida, K. Yuda, T. TI Status and performance of the CALorimetric Electron Telescope (CALET) on the International Space Station SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS LA English DT Proceedings Paper CT Frontier Research in Astrophysics Workshop CY MAY 26-31, 2014 CL Mondello, ITALY DE electrons; calorimeter; nearby sources; dark matter; ISS ID COSMIC-RAYS; ENERGY; ACCELERATION; ABUNDANCES AB The CALorimetric Electron Telescope (CALET) space experiment, currently under development by Japan in collaboration with Italy and the United States, will measure the flux of cosmic-ray electrons (including positrons) to 20 TeV, gamma rays to 10 TeV and nuclei with Z=1 to 40 up to 1,000 TeV during a two-year mission on the International Space Station (ISS), extendable to five years. These measurements are essential to search for dark matter signatures, investigate the mechanism of cosmic-ray acceleration and propagation in the Galaxy and discover possible astrophysical sources of high-energy electrons nearby the Earth. The instrument consists of two layers of segmented plastic scintillators for the cosmic-ray charge identification (CHD), a 3 radiation length thick tungsten-scintillating fiber imaging calorimeter (IMC) and a 27 radiation length thick lead-tungstate calorimeter (TASC). CALET has sufficient depth, imaging capabilities and excellent energy resolution to allow for a clear separation between hadrons and electrons and between charged particles and gamma rays. The instrument will be launched to the ISS within 2014 Japanese Fiscal Year (by the end of March 2015) and installed on the Japanese Experiment Module-Exposed Facility (JEM-EF). In this paper, we will review the status and main science goals of the mission and describe the instrument configuration and performance. C1 [Sakamoto, T.; Takahashi, I.; Yoshida, A.] Aoyama Gakuin Univ, Tokyo 150, Japan. [Ichimura, M.; Kuramata, S.; Miyake, S.] Hirosaki Univ, Hirosaki, Aomori, Japan. [Akaike, Y.; Takita, M.; Terasawa, T.] Univ Tokyo, ICRR, Tokyo 1138654, Japan. [Shimizu, Y.; Tamura, T.] JAXA SEUC, Tokyo, Japan. [Ebisawa, K.; Puke, H.; Mori, K.; Nakagawa, Y. E.; Nakahira, S.; Nishimura, J.; Takayanag, M.; Tomid, H.; Ueno, S.] JAXA ISAS, Sagamihara, Kanagawa, Japan. [Hibino, K.] St Marianna Univ, Sch Med, Kawasaki, Kanagawa, Japan. [Okuno, S.; Tamura, T.; Tateyama, N.] Kanagawa Univ, Yokohama, Kanagawa, Japan. [Cherry, M. L.; Guzik, T. G.; Wefel, J. P.] Louisiana State Univ, Baton Rouge, LA 70803 USA. [Mitchell, J. W.] NASA, GSFC, Washington, DC USA. [Kitamura, H.; Uchihori, Y.] Natl Inst Radiol Sci, Chiba, Japan. [Shiomi, A.] Nihon Univ, Tokyo 102, Japan. [Mori, M.] Ritsumeikan Univ, Kyoto, Japan. [Mizutani, K.] Saitama Univ, Saitama, Japan. [Kamioka, E.; Kubota, A.; Yoshida, K.] Shibaura Inst Technol, Tokyo, Japan. [Munakata, K.] Shinshu Univ, Nagano, Japan. [Asano, K.; Tunesada, Y.] Tokyo Inst Technol, Tokyo, Japan. [Ormes, J. F.] Univ Denver, Denver, CO 80208 USA. [Adriani, O.; Buckley, J. H.; Cassese, A.; Castellini, G.; Mori, N.; Papini, P.; Ricciarini, S.; Spillantini, P.; Vannuccini, E.] Univ Florence, CNR, IFAC, I-50121 Florence, Italy. [Adriani, O.; Bagliesi, M. G.; Bigongiari, G.; Binns, W. R.; Buckley, J. H.; Cassese, A.; Castellini, G.; Collazuol, G.; Di Felice, V.; Lomtadze, T.; Maestro, P.; Marcelli, L.; Marrocchesi, P. S.; Mori, N.; Palma, F.; Papini, P.; Ricciarini, S.; Sparvoli, R.; Spillantini, P.; Vannuccini, E.] Ist Nazl Fis Nucl, Milan, Italy. [Lomtadze, T.] Univ Pisa, I-56100 Pisa, Italy. [Di Felice, V.; Marcelli, L.; Palma, F.; Sparvoli, R.] Univ Roma Tor Vergata, I-00173 Rome, Italy. [Bagliesi, M. G.; Bigongiari, G.; Binns, W. R.; Maestro, P.; Marrocchesi, P. S.] Univ Siena, I-53100 Siena, Italy. [Asaoka, Y.; Hareyama, M.; Kasahara, K.; Kataoka, J.; Kotani, T.; Motz, H. M.; Mori, K.; Murakami, H.; Ozawa, S.; Torii, S.] Waseda Univ, Tokyo, Japan. [Bongi, M.; Israel, M. H.; Krawczynski, H. S.; Rauch, B. F.] Washington Univ, St Louis, MO USA. [Katayose, Y.; Shibata, M.] Yokohama Natl Univ, Yokohama, Kanagawa, Japan. [Collazuol, G.] Univ Padua, I-35100 Padua, Italy. [Yanagita, S.] Ibaraki Univ, Mito, Ibaraki, Japan. [Miyake, S.] Tokiwa Univ, Mito, Ibaraki, Japan. [Yamaok, K.] Nagoya Univ, Nagoya, Aichi 4648601, Japan. [Hasebe, N.; Moiseev, A. A.; Sasaki, M.] Univ Maryland, College Pk, MD USA. [Krizmanic, J. F.] Univ Space Res Assoc, College Pk, MD USA. [Kawanaka, N.] Univ Tokyo, Tokyo 1138654, Japan. RP Adriani, O (reprint author), Univ Florence, CNR, IFAC, I-50121 Florence, Italy. RI Palma, Francesco/K-3224-2015; Marrocchesi, Pier Simone/N-9068-2015; Bongi, Massimo/L-9417-2015; maestro, paolo/E-3280-2010; marcelli, laura/K-8860-2016; Di Felice, Valeria/L-2989-2016; Mori, Nicola/D-9459-2016; Cassese, Antonio/R-1713-2016; OI Sparvoli, Roberta/0000-0002-6314-6117; Bigongiari, Gabriele/0000-0003-3691-0826; Papini, Paolo/0000-0003-4718-2895; Palma, Francesco/0000-0001-7076-8830; Marrocchesi, Pier Simone/0000-0003-1966-140X; Bongi, Massimo/0000-0002-6050-1937; maestro, paolo/0000-0002-4193-1288; marcelli, laura/0000-0002-3180-1228; Mori, Nicola/0000-0003-2138-3787; Cassese, Antonio/0000-0003-3010-4516; Ricciarini, Sergio Bruno/0000-0001-6176-3368; Castellini, Guido/0000-0002-0177-0643 NR 16 TC 4 Z9 4 U1 2 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0920-5632 EI 1873-3832 J9 NUCL PHYS B-PROC SUP JI Nucl. Phys. B-Proc. Suppl. PD NOV-DEC PY 2014 VL 256 BP 225 EP 232 DI 10.1016/j.nuclphysbps.2014.10.026 PG 8 WC Physics, Particles & Fields SC Physics GA AY5FS UT WOS:000347599000026 ER PT J AU Bish, D Blake, D Vaniman, D Sarrazin, P Bristow, T Achilles, C Dera, P Chipera, S Crisp, J Downs, RT Farmer, J Gailhanou, M Ming, D Morookian, JM Morris, R Morrison, S Rampe, E Treiman, A Yen, A AF Bish, David Blake, David Vaniman, David Sarrazin, Philippe Bristow, Thomas Achilles, Cherie Dera, Przemyslaw Chipera, Steve Crisp, Joy Downs, R. T. Farmer, Jack Gailhanou, Marc Ming, Doug Morookian, John Michael Morris, Richard Morrison, Shaunna Rampe, Elizabeth Treiman, Allan Yen, Albert TI The first X-ray diffraction measurements on Mars SO IUCRJ LA English DT Article DE X-ray diffraction; Mars; extraterrestrial mineralogy; Curiosity rover ID GALE CRATER; SOFTWARE AB The Mars Science Laboratory landed in Gale crater on Mars in August 2012, and the Curiosity rover then began field studies on its drive toward Mount Sharp, a central peak made of ancient sediments. CheMin is one of ten instruments on or inside the rover, all designed to provide detailed information on the rocks, soils and atmosphere in this region. CheMin is a miniaturized X-ray diffraction/X-ray fluorescence (XRD/XRF) instrument that uses transmission geometry with an energy-discriminating CCD detector. CheMin uses onboard standards for XRD and XRF calibration, and beryl: quartz mixtures constitute the primary XRD standards. Four samples have been analysed by CheMin, namely a soil sample, two samples drilled from mudstones and a sample drilled from a sandstone. Rietveld and full-pattern analysis of the XRD data reveal a complex mineralogy, with contributions from parent igneous rocks, amorphous components and several minerals relating to aqueous alteration. In particular, the mudstone samples all contain one or more phyllosilicates consistent with alteration in liquid water. In addition to quantitative mineralogy, Rietveld refinements also provide unit-cell parameters for the major phases, which can be used to infer the chemical compositions of individual minerals and, by difference, the composition of the amorphous component. C1 [Bish, David; Achilles, Cherie] Indiana Univ, Geol Sci, Bloomington, IN 47405 USA. [Blake, David; Bristow, Thomas] NASA, Ames Res Ctr, Silicon Valley, CA USA. [Vaniman, David] Planetary Sci Inst, Tucson, AZ USA. [Sarrazin, Philippe] InXitu, Mountain View, CA USA. [Dera, Przemyslaw] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Chipera, Steve] Chesapeake Energy, Oklahoma City, OK USA. [Crisp, Joy; Morookian, John Michael; Yen, Albert] NASA, Jet Prop Lab, Pasadena, CA USA. [Downs, R. T.; Morrison, Shaunna] Univ Arizona, Tucson, AZ 85721 USA. [Farmer, Jack] Arizona State Univ, Tempe, AZ 85287 USA. [Gailhanou, Marc] CNRS, F-75700 Paris, France. [Ming, Doug; Morris, Richard; Rampe, Elizabeth] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Treiman, Allan] Lunar & Planetary Inst, Houston, TX 77058 USA. RP Bish, D (reprint author), Indiana Univ, Geol Sci, 1001 E 10th St, Bloomington, IN 47405 USA. EM bish@indiana.edu RI Gailhanou, Marc/F-8251-2014; Crisp, Joy/H-8287-2016 OI Gailhanou, Marc/0000-0002-7747-703X; Crisp, Joy/0000-0002-3202-4416 FU NASA Mars Science Laboratory Mission; National Aeronautics and Space Administration FX Support from the NASA Mars Science Laboratory Mission is gratefully acknowledged. Some of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. XRD data presented here are archived in the Planetary Data System (pds.nasa.gov). NR 26 TC 16 Z9 16 U1 3 U2 37 PU INT UNION CRYSTALLOGRAPHY PI CHESTER PA 2 ABBEY SQ, CHESTER, CH1 2HU, ENGLAND SN 2052-2525 J9 IUCRJ JI IUCrJ PD NOV PY 2014 VL 1 BP 514 EP 522 DI 10.1107/S2052252514021150 PN 6 PG 9 WC Chemistry, Multidisciplinary; Crystallography; Materials Science, Multidisciplinary SC Chemistry; Crystallography; Materials Science GA CL3QO UT WOS:000356865600015 PM 25485131 ER PT J AU Ade, PAR Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F 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 Bobin, J Bock, JJ Bonaldi, A Bond, JR Borrill, J Bouchet, FR Bridges, M Bucher, M Burigana, C Butler, RC Calabrese, E Cardoso, JF Catalano, A Challinor, A Chamballu, A Chiang, HC Chiang, LY Christensen, PR Church, S Clements, DL Colombi, S Colombo, LPL 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 Dunkley, J Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Gauthier, C Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hamann, J Hansen, FK Hanson, D Harrison, D Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leach, S Leahy, JP Leonardi, R Lesgourgues, J Lewis, A Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, 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 O'Dwyer, IJ Osborne, S Oxborrow, CA Paci, F Pagano, L Pajot, F Paladini, R Pandolfi, S Paoletti, D Partridge, B Pasian, F Patanchon, G Peiris, HV Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Rebolo, R Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C 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 Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sunyaev, R Sureau, F Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Tavagnacco, D Terenzi, L Toffolatti, L Tomasi, M Treguer-Goudineau, J Tristram, M Tucci, M Tuovinen, J Valenziano, L Valiviita, J Van Tent, B Varis, J Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD White, M Wilkinson, A Yvon, D Zacchei, A Zibin, JP Zonca, A AF Ade, P. A. R. Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. 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. Bobin, J. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Bridges, M. Bucher, M. Burigana, C. Butler, R. C. Calabrese, E. Cardoso, J.-F. Catalano, A. Challinor, A. Chamballu, A. Chiang, H. C. Chiang, L.-Y. Christensen, P. R. Church, S. Clements, D. L. Colombi, S. Colombo, L. P. L. 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. Dunkley, J. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Gauthier, C. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hamann, J. Hansen, F. K. Hanson, D. Harrison, D. 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. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Keihaenen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Laehteenmaeki, A. Lamarre, J.-M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leach, S. Leahy, J. P. Leonardi, R. Lesgourgues, J. Lewis, A. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, 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. O'Dwyer, I. J. Osborne, S. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paladini, R. Pandolfi, S. Paoletti, D. Partridge, B. Pasian, F. Patanchon, G. Peiris, H. V. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J.-L. Rachen, J. P. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. 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. Starck, J.-L. Stolyarov, V. Stompor, R. Sudiwala, R. Sunyaev, R. Sureau, F. Sutton, D. Suur-Uski, A.-S. Sygnet, J.-F. Tauber, J. A. Tavagnacco, D. Terenzi, L. Toffolatti, L. Tomasi, M. Treguer-Goudineau, J. Tristram, M. Tucci, M. Tuovinen, J. Valenziano, L. Valiviita, J. Van Tent, B. Varis, J. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. White, M. Wilkinson, A. Yvon, D. Zacchei, A. Zibin, J. P. Zonca, A. CA Planck Collaboration TI Planck 2013 results. XXII. Constraints on inflation SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmic background radiation; inflation; early Universe ID PROBE WMAP OBSERVATIONS; BARYON ACOUSTIC-OSCILLATIONS; ISOTHERMAL DENSITY PERTURBATIONS; MICROWAVE BACKGROUND ANISOTROPY; PRIMORDIAL POWER SPECTRUM; OBSERVATIONS COSMOLOGICAL INTERPRETATION; AXION-DOMINATED UNIVERSE; PARTICLE PHYSICS MODELS; HUBBLE-SPACE-TELESCOPE; LARGE-SCALE STRUCTURE AB We analyse the implications of the Planck data for cosmic inflation. The Planck nominal mission temperature anisotropy measurements, combined with the WMAP large-angle polarization, constrain the scalar spectral index to be n(s) = 0.9603 +/- 0:0073, ruling out exact scale invariance at over 5 sigma Planck establishes an upper bound on the tensor-to-scalar ratio of r < 0.11 (95% CL). The Planck data thus shrink the space of allowed standard inflationary models preferring potentials with V '' < 0. Exponential potential models, the simplest hybrid inflationary models, and monomial potential models of degree n >= 2 do not provide a good fit to the data. Planck does not find statistically significant running of the scalar spectral index, obtaining dn(s)/dln k = -0.0134 +/- 0.0090. We verify these conclusions through a numerical analysis, which makes no slowroll approximation, and carry out a Bayesian parameter estimation and model-selection analysis for a number of inflationary models including monomial, natural, and hilltop potentials. For each model, we present the Planck constraints on the parameters of the potential and explore several possibilities for the post-inflationary entropy generation epoch, thus obtaining nontrivial data-driven constraints. We also present a direct reconstruction of the observable range of the inflaton potential. Unless a quartic term is allowed in the potential, we find results consistent with second-order slow-roll predictions. We also investigate whether the primordial power spectrum contains any features. We find that models with a parameterized oscillatory feature improve the fit by delta 2 10; however, Bayesian evidence does not prefer these models. We constrain several single-field inflation models with generalized Lagrangians by combining power spectrum data with Planck bounds on fNL. Planck constrains with unprecedented accuracy the amplitude and possible correlation (with the adiabatic mode) of non-decaying isocurvature fluctuations. The fractional primordial contributions of cold dark matter (CDM) isocurvature modes of the types expected in the curvaton and axion scenarios have upper bounds of 0.25% and 3.9% (95% CL), respectively. In models with arbitrarily correlated CDM or neutrino isocurvature modes, an anticorrelated isocurvature component can improve the 2 by approximately 4 as a result of slightly lowering the theoretical prediction for the 40 multipoles relative to the higher multipoles. Nonetheless, the data are consistent with adiabatic initial conditions. C1 [Bartlett, J. G.; Bucher, M.; Cardoso, J.-F.; Delabrouille, J.; Ganga, K.; Gauthier, C.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Poutanen, T.; Remazeilles, M.; Rosset, C.; Roudier, G.; Stompor, R.; Treguer-Goudineau, J.] Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, CNRS IN2P3,CEA lrfu,APC, F-75205 Paris 13, France. [Laehteenmaeki, A.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Kunz, M.] African Inst Math Sci, ZA-7701 Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana, Sci Data Ctr, I-00133 Rome, Italy. [Mandolesi, N.] Agenzia Spaziale Italiana, I-00198 Rome, Italy. [Ashdown, M.; Bridges, M.; Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa. [Kneissl, R.] ALMA Santiago Cent Off, Vitacura 7630355, Casilla, Chile. [Bond, J. R.; Hanson, D.; Martin, P. G.; Miville-Deschenes, M.-A.] Univ Toronto, CITA, 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, F-31028 Toulouse 4, France. [Bock, J. J.; Dore, O.; Hildebrandt, S. R.; Prezeau, G.; Rocha, G.; Seiffert, M. D.] CALTECH, Pasadena, CA 91125 USA. [Challinor, A.; Shellard, E. 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R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, TRAP, F-31028 Toulouse 4, France. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, E-18071 Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Bucher, M (reprint author), Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, CNRS IN2P3,CEA lrfu,APC, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France. EM bucher@apc.univ-paris7.fr RI Barreiro, Rita Belen/N-5442-2014; Butler, Reginald/N-4647-2015; Herranz, Diego/K-9143-2014; Vielva, Patricio/F-6745-2014; Toffolatti, Luigi/K-5070-2014; bonavera, laura/E-9368-2017; Remazeilles, Mathieu/N-1793-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; White, Martin/I-3880-2015; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Lahteenmaki, Anne/L-5987-2013; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; Yvon, Dominique/D-2280-2015; OI Pierpaoli, Elena/0000-0002-7957-8993; Lilje, Per/0000-0003-4324-7794; Lopez-Caniego, Marcos/0000-0003-1016-9283; Masi, Silvia/0000-0001-5105-1439; Valenziano, Luca/0000-0002-1170-0104; Finelli, Fabio/0000-0002-6694-3269; Scott, Douglas/0000-0002-6878-9840; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Juvela, Mika/0000-0002-5809-4834; Villa, Fabrizio/0000-0003-1798-861X; Hivon, Eric/0000-0003-1880-2733; Starck, Jean-Luc/0000-0003-2177-7794; Franceschi, Enrico/0000-0002-0585-6591; Mitra, Sanjit/0000-0002-0800-4626; Galeotta, Samuele/0000-0002-3748-5115; Ricciardi, Sara/0000-0002-3807-4043; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Bouchet, Francois/0000-0002-8051-2924; TERENZI, LUCA/0000-0001-9915-6379; Matarrese, Sabino/0000-0002-2573-1243; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Frailis, Marco/0000-0002-7400-2135; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375; Herranz, Diego/0000-0003-4540-1417; Vielva, Patricio/0000-0003-0051-272X; Toffolatti, Luigi/0000-0003-2645-7386; bonavera, laura/0000-0001-8039-3876; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; De Zotti, Gianfranco/0000-0003-2868-2595; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; White, Martin/0000-0001-9912-5070; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; Burigana, Carlo/0000-0002-3005-5796; Zacchei, Andrea/0000-0003-0396-1192 FU ESA; CNES; CNRS/INSU-IN2P3-INP (France); ASI; CNR; INAF (Italy); NASA; DoE (USA); STFC; UKSA (UK); CSIC; MICINN; JA; RES (Spain); Tekes; AoF; CSC (Finland); DLR; MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); PRACE (EU) FX The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php? project=planck&page=Planck_Collaboration. We gratefully acknowledge CINECA (http://www.cineca.it/) under the agreement LFI/CINECA and IN2P3 Computer Center (http://cc.in2p3.fr) for providing a significant amount of the computing resources and services needed for this work. NR 332 TC 1126 Z9 1126 U1 23 U2 87 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 NOV PY 2014 VL 571 AR A22 DI 10.1051/0004-6361/201321569 PG 42 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600105 ER PT J AU Larabi, MC Triantaphillidou, S Watson, AB AF Larabi, Mohamed-Chaker Triantaphillidou, Sophie Watson, Andrew B. TI Image/Video Quality and System Performance SO JOURNAL OF ELECTRONIC IMAGING LA English DT Editorial Material C1 [Larabi, Mohamed-Chaker] Univ Poitiers, XLIM Signal Image & Commun Dept, F-86962 Poitiers, France. [Triantaphillidou, Sophie] Univ Westminster, Fac Media Arts & Design, Harrow HA1 3TP, Middx, England. [Watson, Andrew B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Larabi, MC (reprint author), Univ Poitiers, XLIM Signal Image & Commun Dept, Blvd Marie & Pierre Curie BP 30179, F-86962 Poitiers, France. EM chaker.larabi@univ-poitiers.fr; triants@westminster.ac.uk; andrew.b.watson@nasa.gov NR 0 TC 0 Z9 0 U1 1 U2 1 PU IS&T & SPIE PI BELLINGHAM PA 1000 20TH ST, BELLINGHAM, WA 98225 USA SN 1017-9909 EI 1560-229X J9 J ELECTRON IMAGING JI J. Electron. Imaging PD NOV-DEC PY 2014 VL 23 IS 6 AR 061101 DI 10.1117/1.JEI.23.6.061101 PG 2 WC Engineering, Electrical & Electronic; Optics; Imaging Science & Photographic Technology SC Engineering; Optics; Imaging Science & Photographic Technology GA CA8JJ UT WOS:000349164600001 ER PT J AU Phipps, WS Yin, ZZ Bae, C Sharpe, JZ Bishara, AM Nelson, ES Weaver, AS Brown, D Mckay, TL Griffin, D Chan, EY AF Phipps, William S. Yin, Zhizhong Bae, Candice Sharpe, Julia Z. Bishara, Andrew M. Nelson, Emily S. Weaver, Aaron S. Brown, Daniel Mckay, Terri L. Griffin, DeVon Chan, Eugene Y. TI Reduced-gravity Environment Hardware Demonstrations of a Prototype Miniaturized Flow Cytometer and Companion Microfluidic Mixing Technology (vol 93, e51743, 2014) SO JOVE-JOURNAL OF VISUALIZED EXPERIMENTS LA English DT Correction DE Cellular Biology; Point-of-care; prototype; diagnostics; spaceflight; reduced gravity; parabolic flight; flow cytometry; fluorescence; cell counting; micromixing; spiral-vortex; blood mixing C1 [Phipps, William S.; Yin, Zhizhong; Bae, Candice; Sharpe, Julia Z.; Chan, Eugene Y.] DNA Med Inst, Cambridge, MA 02139 USA. [Bishara, Andrew M.] Harvard Univ, Sch Med, Cambridge, MA 02138 USA. [Nelson, Emily S.; Weaver, Aaron S.; Mckay, Terri L.; Griffin, DeVon] NASA, Glenn Res Ctr, Cleveland, OH USA. [Brown, Daniel] ZIN Technol, Cleveland, OH USA. RP Phipps, WS (reprint author), DNA Med Inst, Cambridge, MA 02139 USA. NR 1 TC 0 Z9 0 U1 0 U2 2 PU JOURNAL OF VISUALIZED EXPERIMENTS PI CAMBRIDGE PA 1 ALEWIFE CENTER, STE 200, CAMBRIDGE, MA 02140 USA SN 1940-087X J9 JOVE-J VIS EXP JI J. Vis. Exp. PD NOV PY 2014 IS 93 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CB0JH UT WOS:000349311400086 ER PT J AU Phipps, WS Yin, ZZ Bae, C Sharpe, JZ Bishara, AM Nelson, ES Weaver, AS Brown, D McKay, TL Griffin, D Chan, EY AF Phipps, William S. Yin, Zhizhong Bae, Candice Sharpe, Julia Z. Bishara, Andrew M. Nelson, Emily S. Weaver, Aaron S. Brown, Daniel McKay, Terri L. Griffin, DeVon Chan, Eugene Y. TI Reduced-gravity Environment Hardware Demonstrations of a Prototype Miniaturized Flow Cytometer and Companion Microfluidic Mixing Technology SO JOVE-JOURNAL OF VISUALIZED EXPERIMENTS LA English DT Article DE Cellular Biology; Issue 93; Point-of-care; prototype; diagnostics; spaceflight; reduced gravity; parabolic flight; flow cytometry; fluorescence; cell counting; micromixing; spiral-vortex; blood mixing ID ELECTRONIC NUCLEAR VOLUME; PARABOLIC FLIGHT; ARABIDOPSIS-THALIANA; GENE-EXPRESSION; MICROGRAVITY; CELL; PROJECT; WEIGHTLESSNESS; SPACEFLIGHT; RESPONSES AB Until recently, astronaut blood samples were collected in-flight, transported to earth on the Space Shuttle, and analyzed in terrestrial laboratories. If humans are to travel beyond low Earth orbit, a transition towards space-ready, point-of-care (POC) testing is required. Such testing needs to be comprehensive, easy to perform in a reduced-gravity environment, and unaffected by the stresses of launch and spaceflight. Countless POC devices have been developed to mimic laboratory scale counterparts, but most have narrow applications and few have demonstrable use in an in-flight, reduced-gravity environment. In fact, demonstrations of biomedical diagnostics in reduced gravity are limited altogether, making component choice and certain logistical challenges difficult to approach when seeking to test new technology. To help fill the void, we are presenting a modular method for the construction and operation of a prototype blood diagnostic device and its associated parabolic flight test rig that meet the standards for flight-testing onboard a parabolic flight, reduced-gravity aircraft. The method first focuses on rig assembly for in-flight, reduced-gravity testing of a flow cytometer and a companion microfluidic mixing chip. Components are adaptable to other designs and some custom components, such as a microvolume sample loader and the micromixer may be of particular interest. The method then shifts focus to flight preparation, by offering guidelines and suggestions to prepare for a successful flight test with regard to user training, development of a standard operating procedure (SOP), and other issues. Finally, in-flight experimental procedures specific to our demonstrations are described. C1 [Phipps, William S.; Yin, Zhizhong; Bae, Candice; Sharpe, Julia Z.; Chan, Eugene Y.] DNA Med Inst, Cambridge, MA 02139 USA. [Bishara, Andrew M.] Harvard Univ, Sch Med, Cambridge, MA 02138 USA. [Nelson, Emily S.; Weaver, Aaron S.; McKay, Terri L.; Griffin, DeVon] NASA, Glenn Res Ctr, Cleveland, OH USA. [Brown, Daniel] ZIN Technol, Cleveland, OH USA. RP Chan, EY (reprint author), DNA Med Inst, Cambridge, MA 02139 USA. EM echan@dnamedinstitute.com FU NASA SBIR [NNX09CA44C, NNX10CA97C]; NASA Phase III [NNC11CA04C] FX Hardware development was supported by the NASA SBIR Contracts NNX09CA44C and NNX10CA97C. Data analysis for the optical block and sample loader demonstrations was supported by NASA Phase III Contract NNC11CA04C. The human blood collection was performed using NASA IRB Protocol # SA-10-008. Control/acquisition software provided through the National Instruments Medical Device Grant Program. Molds for the microchips were made at the Johns Hopkins microfabrication facility and the Harvard Center for Nanoscale Systems. Otto J. Briner and Luke Jaffe (DNA Medicine Institute) aided in rack assembly during summer 2010. NASA flight video staff provided video footage during flight week. Carlos Barrientos (DNA Medicine Institute) provided photograph and figure assistance. Special thanks to the Facilitated Access to the Space Environment for Technology 2010 Program, the NASA Reduced Gravity Office, the Human Adaptation and Countermeasures Division, NASA Glenn Research Center, ZIN Technologies, and the Human Research Program. NR 37 TC 0 Z9 0 U1 2 U2 6 PU JOURNAL OF VISUALIZED EXPERIMENTS PI CAMBRIDGE PA 1 ALEWIFE CENTER, STE 200, CAMBRIDGE, MA 02140 USA SN 1940-087X J9 JOVE-J VIS EXP JI J. Vis. Exp. PD NOV PY 2014 IS 93 AR e51743 DI 10.3791/51743 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CB0JH UT WOS:000349311400012 PM 25490614 ER PT J AU Abergel, A Ade, PAR Aghanim, N Alves, MIR Aniano, G Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bock, JJ Bonaldi, A Bond, JR Borrill, J Bouchet, FR Boulanger, F Bridges, M Bucher, M Burigana, C Butler, RC Cardoso, JF Catalano, A Chamballu, A Chary, RR Chiang, HC Chiang, LY Christensen, PR Church, S 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 Delouis, JM Desert, FX Dickinson, C Diego, JM Dole, H Donzelli, S Dore, O Douspis, M Draine, BT Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Falgarone, E Finelli, F Forni, O Frailis, M Fraisse, AA Franceschi, E Galeotta, S Ganga, K Ghosh, T Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Grenier, IA Gruppuso, A Guillet, V 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 Jaffe, AH Jaffe, TR Jewell, J Joncas, G Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leonardi, R Leon-Tavares, J Lesgourgues, J Levrier, F Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P McGehee, P Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S Oxborrow, CA Paci, F Pagano, L Pajot, F Paladini, R Paoletti, D Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Reach, WT Rebolo, R Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Roudier, G Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savini, G Scott, D Seiffert, MD Shellard, EPS Spencer, LD Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sunyaev, R Sureau, F 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 Verstraete, L Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Welikala, N Ysard, N Yvon, D Zacchei, A Zonca, A AF Abergel, A. Ade, P. A. R. Aghanim, N. Alves, M. I. R. Aniano, G. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bridges, M. Bucher, M. Burigana, C. Butler, R. C. Cardoso, J. -F. Catalano, A. Chamballu, A. Chary, R. -R. Chiang, H. C. Chiang, L. -Y Christensen, P. R. Church, S. 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. Delouis, J. -M. Desert, F. -X. Dickinson, C. Diego, J. M. Dole, H. Donzelli, S. Dore, O. Douspis, M. Draine, B. T. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Falgarone, E. Finelli, F. Forni, O. Frailis, M. Fraisse, A. A. Franceschi, E. Galeotta, S. Ganga, K. Ghosh, T. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Grenier, I. A. Gruppuso, A. Guillet, V. 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. Jaffe, A. H. Jaffe, T. R. Jewell, J. Joncas, G. Jones, W. C. Juvela, M. Keihaenen, E. Keskitalo, R. Kisner, T. S. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Laehteenmaeki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. 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. Maffei, B. Maino, D. Mandolesi, N. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. McGehee, P. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Osborne, S. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paladini, R. Paoletti, D. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Reach, W. T. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sunyaev, R. Sureau, F. 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. Tuerler, M. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Verstraete, L. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Welikala, N. Ysard, N. Yvon, D. Zacchei, A. Zonca, A. TI Planck 2013 results. XI. All-sky model of thermal dust emission SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: data analysis; ISM: general; dust, extinction; infrared: ISM; submillimeter: ISM; opacity ID INTERSTELLAR MOLECULAR-HYDROGEN; SPECTRAL ENERGY-DISTRIBUTIONS; HIGH GALACTIC LATITUDES; 7TH DATA RELEASE; INFRARED-EMISSION; ULTRAVIOLET EXTINCTION; CIRRUS CLOUDS; H-I; PROTOPLANETARY DISKS; SOLAR NEIGHBORHOOD AB This paper presents an all-sky model of dust emission from the Planck 353, 545, and 857 GHz, and IRAS 100 mu m data. Using a modified blackbody fit to the data we present all-sky maps of the dust optical depth, temperature, and spectral index over the 353-3000 GHz range. This model is a good representation of the IRAS and Planck data at 5 0 between 353 and 3000 GHz (850 and 100 mu m). It shows variations of the order of 30% compared with the widely-used model of Finkbeiner, Davis, and Schlegel. The Planck data allow us to estimate the dust temperature uniformly over the whole sky, down to an angular resolution of 5 0, providing an improved estimate of the dust optical depth compared to previous all-sky dust model, especially in high-contrast molecular regions where the dust temperature varies strongly at small scales in response to dust evolution, extinction, and/or local production of heating photons. An increase of the dust opacity at 353 GHz, tau(353)/N-H, from the diffuse to the denser interstellar medium (ISM) is reported. It is associated with a decrease in the observed dust temperature, T-obs, that could be due at least in part to the increased dust opacity. We also report an excess of dust emission at HI column densities lower than 10(20) cm(-2) that could be the signature of dust in the warm ionized medium. In the diffuse ISM at high Galactic latitude, we report an anticorrelation between tau(353)/N-H and T-obs while the dust specific luminosity, i.e., the total dust emission integrated over frequency (the radiance) per hydrogen atom, stays about constant, confirming one of the Planck Early Results obtained on selected fields. This e ff ect is compatible with the view that, in the diffuse ISM, Tobs responds to spatial variations of the dust opacity, due to variations of dust properties, in addition to (small) variations of the radiation field strength. The implication is that in the di ff use high-latitude ISM tau(353) is not as reliable a tracer of dust column density as we conclude it is in molecular clouds where the correlation of tau(353) with dust extinction estimated using colour excess measurements on stars is strong. To estimate Galactic E(B-V) in extragalactic fields at high latitude we develop a new method based on the thermal dust radiance, instead of the dust optical depth, calibrated to E(B-V) using reddening measurements of quasars deduced from Sloan Digital Sky Survey data. C1 [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Gorski, K. M.; Patanchon, G.; Piat, M.; Remazeilles, M.; Rosset, C.; Roudier, G.; Stompor, R.; Welikala, N.] Univ Paris Diderot, CNRS IN2P3, Observ Paris, Sorbonne Paris Cite,CEA Irfu,APC, F-75205 Paris 13, France. [Laehteenmaeki, A.; Leon-Tavares, J.; Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Aalto 00076, Finland. [Laehteenmaeki, A.; Leon-Tavares, J.; Poutanen, T.] Aalto Univ, Dept Radio Sci & Engn, Aalto 00076, Finland. [Kunz, M.] African Inst Math Sci, Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy. [Mandolesi, N.] Agenzia Spaziale Italiana, Rome, Italy. [Ashdown, M.; Bridges, M.; Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa. [Bond, J. R.; Hanson, D.; Martin, P. G.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, 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, F-31028 Toulouse 4, France. [Battaner, E.; Bock, J. J.; Dore, O.; Gorski, K. M.; Helou, G.; Hildebrandt, S. R.; Prezeau, G.; Rocha, G.; Seiffert, M. D.] CALTECH, Pasadena, CA 91125 USA. [Shellard, E. P. S.] Univ Cambridge, DAMTP, Ctr Theoret Cosmol, Cambridge CB3 0WA, England. [Hernandez-Monteagudo, C.] CEFCA, 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, DK-2800 Lyngby, Denmark. [Kunz, M.; Tucci, M.] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland. [Joncas, G.] Univ Laval, Dept Phys Gen Phys & Opt, Quebec City, PQ, Canada. [Atrio-Barandela, F.] Univ Salamanca, Fac Ciencias, Dept Fis Fundamental, E-37008 Salamanca, Spain. [Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain. [Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada. [Rachen, J. 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D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Sunyaev, R.] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia. 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.; Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Armitage-Caplan, C.] Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England. [Lesgourgues, J.] CERN, PH TH, Div Theory, CH-1211 Geneva 23, Switzerland. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UPMC, UMR7095, F-75014 Paris, France. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, IRAP, UPS OMP, F-31028 Toulouse 4, France. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Miville-Deschenes, MA (reprint author), Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, Batiment 121, F-91405 Orsay, France. EM mamd@ias.u-psud.fr RI Kurki-Suonio, Hannu/B-8502-2016; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Martinez-Gonzalez, Enrique/E-9534-2015; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Ghosh, Tuhin/E-6899-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; Remazeilles, Mathieu/N-1793-2015; Barreiro, Rita Belen/N-5442-2014; Butler, Reginald/N-4647-2015; OI Kurki-Suonio, Hannu/0000-0002-4618-3063; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; De Zotti, Gianfranco/0000-0003-2868-2595; Matarrese, Sabino/0000-0002-2573-1243; Lopez-Caniego, Marcos/0000-0003-1016-9283; Umana, Grazia/0000-0002-6972-8388; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Galeotta, Samuele/0000-0002-3748-5115; Ricciardi, Sara/0000-0002-3807-4043; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Reach, William/0000-0001-8362-4094; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993 FU ESA; CNES FX The development of Planck has been supported by: ESA; CNES and CNRS /INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collabora tion. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7 /2007-2013) /ERC grant agreement No. 267934. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbuk agakusho, 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-PlanckInstitute 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. Some of the results in this paper have been derived using the HEALPix package. NR 142 TC 126 Z9 124 U1 4 U2 23 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 NOV PY 2014 VL 571 AR A11 DI 10.1051/0004-6361/201323195 PG 37 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600034 ER PT J AU Ade, PAR Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Battaner, E Benabed, K Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bond, JR Borrill, J Bouchet, FR Burigana, C Cardoso, JF Catalano, A Challinor, A Chamballu, A Chiang, HC Christensen, PR Clements, DL Colombi, S Colombo, LPL 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 Dupac, X Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Fraisse, AA Franceschi, E Galeotta, S Ganga, K Giard, M Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A 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 Jaffe, AH Jaffe, TR Jones, WC Keihanen, E Keskitalo, R Knoche, J Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Lawrence, CR Leonardi, R Leon-Tavares, J Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maino, D Mandolesi, N Maris, M Martin, PG Martinez-Gonzalez, E Masi, S Matarrese, S Mazzotta, 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 Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Oxborrow, CA Pagano, L Pajot, F Paoletti, D Partridge, B Pasian, F Patanchon, G Pearson, D Pearson, TJ Perdereau, O Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Pratt, GW Prunet, S Puget, JL Rachen, JP Reinecke, M Remazeilles, M Renault, C Ricciardi, S Ristorcelli, I Rocha, G Roudier, G Rubino-Martin, JA Rusholme, B Sandri, M Scott, D Stolyarov, V Sudiwala, R Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Valenziano, L Valiviita, J Van Tent, B Vielva, P Villa, F Wade, LA Wandelt, BD Wehus, IK White, SDM Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Battaner, E. Benabed, K. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bond, J. R. Borrill, J. Bouchet, F. R. Burigana, C. Cardoso, J. -F. Catalano, A. Challinor, A. Chamballu, A. Chiang, H. C. Christensen, P. R. Clements, D. L. Colombi, S. Colombo, L. P. L. 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. Dupac, X. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Fraisse, A. A. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. 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. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Keihaenen, E. Keskitalo, R. Knoche, J. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Lawrence, C. R. Leonardi, R. Leon-Tavares, J. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maino, D. Mandolesi, N. Maris, M. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Mazzotta, 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. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Oxborrow, C. A. Pagano, L. Pajot, F. Paoletti, D. Partridge, B. Pasian, F. Patanchon, G. Pearson, D. Pearson, T. J. Perdereau, O. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Pratt, G. W. Prunet, S. Puget, J. -L. Rachen, J. P. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Ristorcelli, I. Rocha, G. Roudier, G. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Scott, D. Stolyarov, V. Sudiwala, R. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Tucci, M. Valenziano, L. Valiviita, J. Van Tent, B. Vielva, P. Villa, F. Wade, L. A. Wandelt, B. D. Wehus, I. K. White, S. D. M. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. XXXI. Consistency of the Planck data SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology: observations; cosmic background radiation; instrumentation: detectors ID MICROWAVE; MAPS AB The Planck design and scanning strategy provide many levels of redundancy that can be exploited to provide tests of internal consistency. One of the most important is the comparison of the 70 GHz (amplifier) and 100 GHz (bolometer) channels. Based on different instrument technologies, with feeds located differently in the focal plane, analysed independently by different teams using different software, and near the minimum of diffuse foreground emission, these channels are in effect two different experiments. The 143 GHz channel has the lowest noise level on Planck, and is near the minimum of unresolved foreground emission. In this paper, we analyse the level of consistency achieved in the 2013 Planck data. We concentrate on comparisons between the 70, 100, and 143 GHz channel maps and power spectra, particularly over the angular scales of the first and second acoustic peaks, on maps masked for diffuse Galactic emission and for strong unresolved sources. Difference maps covering angular scales from 8 degrees to 15 ' are consistent with noise, and show no evidence of cosmic microwave background structure. Including small but important corrections for unresolved-source residuals, we demonstrate agreement (measured by deviation of the ratio from unity) between 70 and 100 GHz power spectra averaged over 70 <= l <= 390 at the 0.8% level, and agreement between 143 and 100 GHz power spectra of 0.4% over the same l range. These values are within and consistent with the overall uncertainties in calibration given in the Planck 2013 results. We also present results based on the 2013 likelihood analysis showing consistency at the 0.35% between the 100, 143, and 217 GHz power spectra. We analyse calibration procedures and beams to determine what fraction of these differences can be accounted for by known approximations or systematic errors that could be controlled even better in the future, reducing uncertainties still further. Several possible small improvements are described. Subsequent analysis of the beams quantifies the importance of asymmetry in the near sidelobes, which was not fully accounted for initially, affecting the 70/100 ratio. Correcting for this, the 70, 100, and 143 GHz power spectra agree to 0.4% over the first two acoustic peaks. The likelihood analysis that produced the 2013 cosmological parameters incorporated uncertainties larger than this. We show explicitly that correction of the missing near sidelobe power in the HFI channels would result in shifts in the posterior distributions of parameters of less than 0.3 sigma except for As, the amplitude of the primordial curvature perturbations at 0.05 Mpc(-1), which changes by about 1 sigma. We extend these comparisons to include the sky maps from the complete nine-year mission of the Wilkinson Microwave Anisotropy Probe (WMAP), and find a roughly 2% difference between the Planck and WMAP power spectra in the region of the first acoustic peak. 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[Melchiorri, A.; Pagano, L.] Univ Roma La Sapienza, INFN, Sez Roma 1, I-00185 Rome, Italy. [Gregorio, A.] Ist Nazl Fis Nucl, Natl Inst Nucl Phys, I-34127 Trieste, Italy. [Desert, F. -X.; Ponthieu, N.] Univ Grenoble 1, IPAG, CNRS INSU, UMR 5274, F-38041 Grenoble, France. [Mitra, S.] IUCAA, Pune 411007, Maharashtra, India. [Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Pearson, T. J.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Dole, H.] Inst Univ France, F-75005 Paris, France. [Aumont, J.; Chamballu, A.; Dole, H.; Douspis, M.; Kunz, M.; Lagache, G.; Miville-Deschenes, M. -A.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Remazeilles, M.] Univ Paris 11, Inst Astrophys Spatiale, CNRS, UMR 8617, F-91405 Orsay, France. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Popa, L.] Inst Space Sci, Bucharest, Romania. [Challinor, A.; Gratton, S.; Harrison, D. L.; Migliaccio, M.; Sutton, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Eriksen, H. K.; Hansen, F. K.; Lilje, P. B.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Leon-Tavares, J.] INAOE, Puebla 72000, Mexico. [Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife 38200, Spain. [Barreiro, R. 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, E-39005 Santander, Spain. [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.; Pearson, D.; Pietrobon, D.; Rocha, G.; Roudier, G.; Wade, L. A.; Wehus, I. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Davies, R. D.; Davis, R. J.; Dickinson, C.; Noviello, F.; Remazeilles, M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Challinor, A.; Gratton, S.; Harrison, D. L.; Lasenby, A.; Migliaccio, M.; Stolyarov, V.; Sutton, D.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Couchot, F.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.; Tucci, M.] Univ Paris 11, CNRS, IN2P3, LAL, Orsay, France. [Catalano, A.; Coulais, A.; Lamarre, J. -M.; Roudier, G.] CNRS, Observ Paris, LERMA, F-75014 Paris, France. [Arnaud, M.; Chamballu, A.; Pratt, G. W.] Univ Paris Diderot, CEA Saclay, IRFU Serv Astrophys, CEA DSM CNRS,Lab AIM, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France. [Catalano, A.; Macias-Perez, J. F.; Renault, C.] Univ Grenoble 1, Inst Natl Polytech Grenoble, CNRS IN2P3, Lab Phys Subatom & Cosmol, F-38026 Grenoble, France. [Van Tent, B.] Univ Paris 11, Lab Phys Theor, CNRS, F-91405 Orsay, France. [Ensslin, T. A.; Hovest, W.; Knoche, J.; Rachen, J. P.; Reinecke, M.; White, S. D. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Hanson, D.] McGill Univ, McGill Phys, Montreal, PQ H3A 2T8, Canada. [Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Co Kildare, Ireland. [Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Crill, B. P.] CALTECH, Observ Cosmol, Pasadena, CA 91125 USA. [Lesgourgues, J.] Ecole Polytech Fed Lausanne, SB ITP LPPC, CH-1015 Lausanne, Switzerland. [Baccigalupi, C.; Bielewicz, P.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Perrotta, F.] SISSA, Astrophys Sector, I-34136 Trieste, Italy. [Ade, P. A. R.; Munshi, D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, The Parade, Cardiff CF24 3AA, S Glam, Wales. [Moss, A.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [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. [Lesgourgues, J.] CERN, PH TH, Div Theory, CH-1211 Geneva 23, Switzerland. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Colombi, S.; Hivon, E.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UMR7095, F-75014 Paris, France. [Banday, A. J.; Bernard, J. -P.; Bielewicz, 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, Dept Fis Teor & Cosmos, Fac Ciencias, E-18071 Granada, Spain. [Battaner, E.] Univ Granada, Inst Carlos Fis Teor & Computac I, E-18071 Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Lawrence, CR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM charles.lawrence@jpl.nasa.gov RI Remazeilles, Mathieu/N-1793-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Stolyarov, Vladislav/C-5656-2017; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Martinez-Gonzalez, Enrique/E-9534-2015; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Pearson, Timothy/N-2376-2015; Barreiro, Rita Belen/N-5442-2014; OI de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Stolyarov, Vladislav/0000-0001-8151-828X; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Matarrese, Sabino/0000-0002-2573-1243; De Zotti, Gianfranco/0000-0003-2868-2595; Lopez-Caniego, Marcos/0000-0003-1016-9283; Masi, Silvia/0000-0001-5105-1439; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Pearson, Timothy/0000-0001-5213-6231; Pierpaoli, Elena/0000-0002-7957-8993; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Sandri, Maura/0000-0003-4806-5375 FU ESA; CNES (France) [CNRS/INSU-IN2P3-INP]; ASI (Italy); CNR (Italy); INAF (Italy); NASA and DoE (USA); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); DEISA (EU); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany) FX The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.rssd.esa.int/Planck. Some of the results in this paper have been derived using the HEALPix package. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis ( LAMBDA), part of the High Energy Astrophysics Science Archive Center (HEASARC); HEASARC/LAMBDA is a service of the Astrophysics Science Division at the NASA Goddard Space Flight Center. NR 35 TC 40 Z9 39 U1 3 U2 15 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 NOV PY 2014 VL 571 AR A31 DI 10.1051/0004-6361/201423743 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600045 ER PT J AU Ade, PAR Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bethermin, M Bielewicz, P Blagrave, K Bobin, J Bock, JJ Bonaldi, A Bond, JR Borrill, J Bouchet, FR Boulanger, F Bridges, M Bucher, M Burigana, C Butler, RC Cardoso, JF Catalano, A Challinor, A Chamballu, A Chen, X Chiang, HC Chiang, LY Christensen, PR Church, S Clements, DL Colombi, S Colombo, LPL 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 Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Ghosh, T Giard, M Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Hanson, D Harrison, D Helou, G Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Jaffe, AH Jaffe, TR Jones, WC Juvela, M Kalberla, P Keihanen, E Kerp, J Keskitalo, R Kisner, TS Kneissl, R Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lacasa, F Lagache, G Lahteenmaki, A Lamarre, JM Langer, M Lasenby, A Laureijs, RJ Lawrence, CR Leonardi, R Leon-Tavares, J Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S Oxborrow, CA Paci, F Pagano, L Pajot, F Paladini, R Paoletti, D Partridge, B Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Reach, WT Rebolo, R Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Roudier, G Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savini, G Scott, D Seiffert, MD Serra, P Shellard, EPS Spencer, LD Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sunyaev, R Sureau, F 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 Valenziano, L Valiviita, J Van Tent, B Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Welikala, N White, M White, SDM Winkel, B Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bethermin, M. Bielewicz, P. Blagrave, K. Bobin, J. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bridges, M. Bucher, M. Burigana, C. Butler, R. C. Cardoso, J. -F. Catalano, A. Challinor, A. Chamballu, A. Chen, X. Chiang, H. C. Chiang, L. -Y Christensen, P. R. Church, S. Clements, D. L. Colombi, S. Colombo, L. P. L. 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. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Ghosh, T. Giard, M. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Hanson, D. Harrison, D. Helou, G. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Kalberla, P. Keihanen, E. Kerp, J. Keskitalo, R. Kisner, T. S. Kneissl, R. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lacasa, F. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Langer, M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leonardi, R. Leon-Tavares, J. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Osborne, S. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paladini, R. Paoletti, D. Partridge, B. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Reach, W. T. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Serra, P. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sunyaev, R. Sureau, F. 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. Tuerler, M. Valenziano, L. Valiviita, J. Van Tent, B. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Welikala, N. White, M. White, S. D. M. Winkel, B. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology: observations; large-scale structure of Universe; galaxies: star formation; infrared: diffuse background ID FORMATION RATE DENSITY; SOUTH-POLE TELESCOPE; DARK-MATTER HALOES; CONDITIONAL LUMINOSITY FUNCTION; SPECTRAL ENERGY-DISTRIBUTIONS; ANGULAR POWER SPECTRA; SIMILAR-TO 2; 100 MU-M; SUBMILLIMETER GALAXIES; FORMING GALAXIES AB We present new measurements of cosmic infrared background (CIB) anisotropies using Planck. Combining HFI data with IRAS, the angular auto-and cross-frequency power spectrum is measured from 143 to 3000 GHz, and the auto-bispectrum from 217 to 545 GHz. The total areas used to compute the CIB power spectrum and bispectrum are about 2240 and 4400 deg(2), respectively. After careful removal of the contaminants (cosmic microwave background anisotropies, Galactic dust, and Sunyaev-Zeldovich emission), and a complete study of systematics, the CIB power spectrum is measured with unprecedented signal to noise ratio from angular multipoles l similar to 150 to 2500. The bispectrum due to the clustering of dusty, star-forming galaxies is measured from l similar to 130 to 1100, with a total signal to noise ratio of around 6, 19, and 29 at 217, 353, and 545 GHz, respectively. Two approaches are developed for modelling CIB power spectrum anisotropies. The first approach takes advantage of the unique measurements by Planck at large angular scales, and models only the linear part of the power spectrum, with a mean bias of dark matter haloes hosting dusty galaxies at a given redshift weighted by their contribution to the emissivities. The second approach is based on a model that associates star-forming galaxies with dark matter haloes and their subhaloes, using a parametrized relation between the dust-processed infrared luminosity and (sub-) halo mass. The two approaches simultaneously fit all auto-and cross-power spectra very well. We find that the star formation history is well constrained up to redshifts around 2, and agrees with recent estimates of the obscured star-formation density using Spitzer and Herschel. However, at higher redshift, the accuracy of the star formation history measurement is strongly degraded by the uncertainty in the spectral energy distribution of CIB galaxies. We also find that the mean halo mass which is most efficient at hosting star formation is log (M-eff/ M-circle dot) = 12.6 and that CIB galaxies have warmer temperatures as redshift increases. The CIB bispectrum is steeper than that expected from the power spectrum, although well fitted by a power law; this gives some information about the contribution of massive haloes to the CIB bispectrum. Finally, we show that the same halo occupation distribution can fit all power spectra simultaneously. The precise measurements enabled by Planck pose new challenges for the modelling of CIB anisotropies, indicating the power of using CIB anisotropies to understand the process of galaxy formation. 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.; Welikala, N.] Univ Paris Diderot, Sorbonne Paris Cite, APC, CNRS IN2P3,CEA Lrfu,Observ Paris, F-75205 Paris 13, France. [Lahteenmaki, A.; Leon-Tavares, J.; Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Kunz, M.] African Inst Math Sci, ZA-7945 Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy. [Mandolesi, N.] Agenzia Spaziale Italiana, Rome, Italy. [Kalberla, P.; Kerp, J.; Winkel, B.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Ashdown, M.; Bridges, M.; Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa. [Kneissl, R.] ALMA Santiago Cent Off, Atacama Large Millimeter Submillimeter Array, Santiago 0355, Chile. [Blagrave, K.; Bond, J. R.; Hanson, D.; Martin, P. G.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. 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EM guilaine.lagache@ias.u-psud.fr RI Remazeilles, Mathieu/N-1793-2015; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Ghosh, Tuhin/E-6899-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Langer, Mathieu/C-5100-2013; Martinez-Gonzalez, Enrique/E-9534-2015; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; White, Martin/I-3880-2015; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Butler, Reginald/N-4647-2015; Barreiro, Rita Belen/N-5442-2014; SERRA, PAOLO/G-9678-2014; OI Lopez-Caniego, Marcos/0000-0003-1016-9283; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; De Zotti, Gianfranco/0000-0003-2868-2595; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; Langer, Mathieu/0000-0002-9088-2718; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; White, Martin/0000-0001-9912-5070; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Bethermin, Matthieu/0000-0002-3915-2015; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Reach, William/0000-0001-8362-4094; Butler, Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; SERRA, PAOLO/0000-0002-7609-3931; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196 FU ESA; CNES FX The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP-PNCG (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members with the technical or scientific activities they have been involved into, can be found at http://www.rssd.esa.int/index.php?project=PLANCK&page=PlanckCollaboratio n. The Parkes radio telescope is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. Some Hi data used in this paper are based on observations with the 100 m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at Effelsberg. NR 162 TC 74 Z9 73 U1 3 U2 14 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2014 VL 571 AR A30 DI 10.1051/0004-6361/201322093 PG 39 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600030 ER PT J AU Ade, PAR Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bock, JJ Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Boulanger, F Bridges, M Bucher, M Burigana, C Butler, RC Cardoso, JF Castex, G Catalano, A Challinor, A Chamballu, A Chary, RR Chen, X Chiang, HC Chiang, LY Christensen, PR Church, S Clements, DL Colombi, S Colombo, LPL 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 Dickinson, C Diego, JM Dobler, G Dole, H Donzelli, S Dore, O Douspis, M Dunkley, J Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Falgarone, E Finelli, F Forni, O Frailis, M Fraisse, AA Franceschi, E Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK 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 Huey, G Huffenberger, KM Jaffe, AH Jaffe, TR Jewell, J Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Le Jeune, M Leach, S Leahy, JP Leonardi, R Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Marcos-Caballero, A Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, 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 O'Dwyer, IJ Osborne, S 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 Platania, P Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Reach, WT Rebolo, R Reinecke, M Remazeilles, M Renault, C Renzi, A Ricciardi, S Riller, T Ristorcelli, I Rocha, G Roman, M Rosset, C Roudier, G Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Salerno, E Sandri, M Santos, D Savini, G Schiavon, F Scott, D Seiffert, MD Shellard, EPS Spencer, LD Starck, JL Stompor, R Sudiwala, R Sunyaev, R Sureau, F 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 Varis, J Viel, M Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Wehus, IK Wilkinson, A Xia, JQ Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bock, J. J. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bridges, M. Bucher, M. Burigana, C. Butler, R. C. Cardoso, J. -F. Castex, G. Catalano, A. Challinor, A. Chamballu, A. Chary, R. -R. Chen, X. Chiang, H. C. Chiang, L. -Y Christensen, P. R. Church, S. Clements, D. L. Colombi, S. Colombo, L. P. L. 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. Dickinson, C. Diego, J. M. Dobler, G. Dole, H. Donzelli, S. Dore, O. Douspis, M. Dunkley, J. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Falgarone, E. Finelli, F. Forni, O. Frailis, M. Fraisse, A. A. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. 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. Huey, G. Huffenberger, K. M. Jaffe, A. H. Jaffe, T. R. Jewell, J. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Le Jeune, M. Leach, S. Leahy, J. P. Leonardi, R. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Marcos-Caballero, A. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, 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. O'Dwyer, I. J. Osborne, S. 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. Platania, P. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Reach, W. T. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Renzi, A. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Roman, M. Rosset, C. Roudier, G. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Salerno, E. Sandri, M. Santos, D. Savini, G. Schiavon, F. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stompor, R. Sudiwala, R. Sunyaev, R. Sureau, F. 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. Tuerler, M. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Varis, J. Viel, M. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Wehus, I. K. Wilkinson, A. Xia, J. -Q. Yvon, D. Zacchei, A. Zonca, A. TI Planck 2013 results. XII. Diffuse component separation SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmic background radiation ID MICROWAVE-ANISOTROPY-PROBE; INTERSTELLAR-MEDIUM EMISSION; TEMPERATURE POWER SPECTRUM; SPINNING DUST; FOREGROUND EMISSION; FULL-SKY; GALACTIC EMISSION; WMAP OBSERVATIONS; POLARIZATION DATA; LIKELIHOOD AB Planck has produced detailed all-sky observations over nine frequency bands between 30 and 857 GHz. These observations allow robust reconstruction of the primordial cosmic microwave background (CMB) temperature fluctuations over nearly the full sky, as well as new constraints on Galactic foregrounds, including thermal dust and line emission from molecular carbon monoxide (CO). This paper describes the component separation framework adopted by Planck for many cosmological analyses, including CMB power spectrum determination and likelihood construction on large angular scales, studies of primordial non-Gaussianity and statistical isotropy, the integrated Sachs-Wolfe effect, gravitational lensing, and searches for topological defects. We test four foreground-cleaned CMB maps derived using qualitatively different component separation algorithms. The quality of our reconstructions is evaluated through detailed simulations and internal comparisons, and shown through various tests to be internally consistent and robust for CMB power spectrum and cosmological parameter estimation up to l = 2000. The parameter constraints on ACDM cosmologies derived from these maps are consistent with those presented in the cross-spectrum based Planck likelihood analysis. We choose two of the CMB maps for specific scientific goals. We also present maps and frequency spectra of the Galactic low-frequency, CO, and thermal dust emission. The component maps are found to provide a faithful representation of the sky, as evaluated by simulations, with the largest bias seen in the CO component at 3%. For the low-frequency component, the spectral index varies widely over the sky, ranging from about beta = 4 to -2. Considering both morphology and prior knowledge of the low frequency components, the index map allows us to associate a steep spectral index (beta < -3.2) with strong anomalous microwave emission, corresponding to a spinning dust spectrum peaking below 20 GHz, a flat index of beta > -2.3 with strong free-free emission, and intermediate values with synchrotron emission. C1 [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Castex, G.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Le Jeune, M.; Patanchon, G.; Piat, M.; Remazeilles, M.; Roman, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, Univ Paris 04, APC, CNRS IN2P3,CEA Lrfu,Observ Paris, F-75205 Paris 13, France. [Lahteenmaki, A.; Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Aalto 00076, Finland. [Lahteenmaki, A.; Poutanen, T.] Aalto Univ, Dept Radio Sci & Engn, Aalto 00076, Finland. [Kunz, M.] African Inst Math Sci, ZA-7945 Cape Town, South Africa. 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EM maja1@mrao.cam.ac.uk RI Renzi, Alessandro/K-4114-2015; Barreiro, Rita Belen/N-5442-2014; Remazeilles, Mathieu/N-1793-2015; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; bonavera, laura/E-9368-2017; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Cruz, Marcos/N-3429-2014; Martinez-Gonzalez, Enrique/E-9534-2015; Salerno, Emanuele/A-2137-2010; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Pearson, Timothy/N-2376-2015; Butler, Reginald/N-4647-2015; OI Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Renzi, Alessandro/0000-0001-9856-1970; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Viel, Matteo/0000-0002-2642-5707; Galeotta, Samuele/0000-0002-3748-5115; Ricciardi, Sara/0000-0002-3807-4043; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; De Zotti, Gianfranco/0000-0003-2868-2595; Lopez-Caniego, Marcos/0000-0003-1016-9283; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; bonavera, laura/0000-0001-8039-3876; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Reach, William/0000-0001-8362-4094; Juvela, Mika/0000-0002-5809-4834; Molinari, Diego/0000-0002-7799-3915; Zacchei, Andrea/0000-0003-0396-1192; Gruppuso, Alessandro/0000-0001-9272-5292; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; Cruz, Marcos/0000-0002-4767-530X; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Salerno, Emanuele/0000-0002-3433-3634; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Pearson, Timothy/0000-0001-5213-6231; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Villa, Fabrizio/0000-0003-1798-861X; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099 FU ESA; CNES; CNRS/INSU-IN2P3-INP (France); ASI; CNR; INAF (Italy); NASA; DoE (USA); STFC; UKSA (UK); CSIC; MICINN; JA; RES (Spain); Tekes; AoF; CSC (Finland); DLR; MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); PRACE (EU); Advanced Computing and e-Science team at IFCA FX The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php? project=planck&page=Planck_Collaboration. The authors acknowledge the support provided by the Advanced Computing and e-Science team at IFCA. This work made use of the COSMOS supercomputer, part of the STFC DiRAC HPC Facility. Some of the results in this paper have been derived using the HEALPix package. NR 90 TC 136 Z9 136 U1 10 U2 24 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 NOV PY 2014 VL 571 AR A12 DI 10.1051/0004-6361/201321580 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600026 ER PT J AU Ade, PAR Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bock, JJ Bond, JR Borrill, J Bouchet, FR Bridges, M Bucher, M Burigana, C Cardoso, JF Catalano, A Challinor, A Chamballu, A Chiang, HC Chiang, LY Christensen, PR Church, S Clements, DL Colombi, S Colombo, LPL Couchot, F Coulais, A Crill, P Curto, A Cuttaia, F Danese, L Davies, RD 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 Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Gana, K Giard, M Girard, D Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Hanson, D Harrison, D Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leonardi, R Leroy, C Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Mandolesi, N Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P McGehee, P Melchiorri, A Mendes, L Mennella, A Migliaccio, M Miniussi, A Mitra, A Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Mottet, S Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S Oxborrow, CA Paci, F Pagano, L Pajot, F Paoletti, D Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Racine, B Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Roudier, G Rusholme, B Sanselme, L Santos, D Sauve, A Savini, G Scott, D Shellard, EPS Spencer, LD Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sureau, F Sutton, D 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 Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bock, J. J. Bond, J. R. Borrill, J. Bouchet, F. R. Bridges, M. Bucher, M. Burigana, C. Cardoso, J. -F. Catalano, A. Challinor, A. Chamballu, A. Chiang, H. C. Chiang, L. -Y. Christensen, P. R. Church, S. Clements, D. L. Colombi, S. Colombo, L. P. L. Couchot, F. Coulais, A. Crill, P. Curto, A. Cuttaia, F. Danese, L. Davies, R. D. 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. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Gana, K. Giard, M. Girard, D. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Hanson, D. Harrison, D. 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. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leonardi, R. Leroy, C. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Mandolesi, N. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. McGehee, P. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Miniussi, A. Mitra, A. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. 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. Osborne, S. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paoletti, D. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Racine, B. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rusholme, B. Sanselme, L. Santos, D. Sauve, A. Savini, G. Scott, D. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sureau, F. Sutton, D. 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. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. X. HFI energetic particle effects: characterization, removal, and simulation SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmic background radiation; cosmology: observations; instrumentation: detectors; space vehicles: instruments; methods: data analysis ID INSTRUMENT; ANISOTROPY; BOOMERANG; FLIGHT AB We describe the detection, interpretation, and removal of the signal resulting from interactions of high energy particles with the Planck High Frequency Instrument (HFI). There are two types of interactions: heating of the 0.1 K bolometer plate; and glitches in each detector time stream. The transient responses to detector glitch shapes are not simple single- pole exponential decays and fall into three families. The glitch shape for each family has been characterized empirically in flight data and these shapes have been used to remove glitches from the detector time streams. The spectrum of the count rate per unit energy is computed for each family and a correspondence is made to the location on the detector of the particle hit. Most of the detected glitches are from Galactic protons incident on the die frame supporting the micro- machined bolometric detectors. In the Planck orbit at L2, the particle flux is around 5 cm 2 s 1 and is dominated by protons incident on the spacecraft with energy > 39 MeV, at a rate of typically one event per second per detector. Di ff erent categories of glitches have di ff erent signatures in the time stream. Two of the glitch types have a low amplitude component that decays over nearly 1 s. This component produces excess noise if not properly removed from the time- ordered data. We have used a glitch detection and subtraction method based on the joint fit of population templates. The application of this novel glitch subtraction method removes excess noise from the time streams. 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[McGehee, P.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, F-38042 Grenoble, France. [Dole, H.] Inst Univ France, F-75005 Paris, France. [Aghanim, N.; Aumont, J.; Chamballu, A.; Dole, H.; Douspis, M.; Kunz, M.; Lagache, G.; Leroy, C.; Miniussi, A.; Miville-Deschenes, M. -A.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Remazeilles, M.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Moneti, A.; Mottet, S.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Popa, L.] Inst Space Sci, Bucharest 077125, Romania. [Chiang, L. -Y.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Bridges, M.; Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Migliaccio, M.; Sutton, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Eriksen, H. K.; Hansen, F. K.; Lilje, P. B.; Valiviita, J.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Barreiro, R. 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, Santander 39005, Spain. [Bock, J. J.; Colombo, L. P. L.; Crill, P.; Dore, O.; Gorski, K. M.; Hanson, D.; Holmes, W. A.; Lawrence, C. R.; Mitra, A.; Pietrobon, D.; Prezeau, G.; Rocha, G.; Roudier, G.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Davies, R. D.; Noviello, F.; Remazeilles, M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Bridges, M.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; Migliaccio, M.; Stolyarov, V.; Sutton, D.] Cosmol Cambridge, Kavli Inst, Cambridge CB3 0HA, England. [Couchot, F.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.; Tucci, M.] Univ Paris 11, CNRS, IN2P3, LAL, Orsay, France. [Catalano, A.; Coulais, A.; Lamarre, J. -M.; Roudier, G.] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Arnaud, M.; Bobin, J.; Chamballu, A.; Marshall, D. J.; Pratt, G. W.; Starck, J. -L.; Sureau, F.] Univ Paris Diderot, CEA Saclay, CNRS, CEA DSM,IRFU,Serv Astrophys,Lab AIM, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom Paris Tech, F-75634 Paris 13, France. [Catalano, A.; Girard, D.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Sanselme, L.; Santos, D.] Univ Grenoble 1, CNRS, IN2P3, Inst Natl Polytech Grenoble,Lab Phys Subatom & Co, F-38026 Grenoble, France. [Van Tent, B.] Univ Paris 11, CNRS, Phys Theor Lab, F-91405 Orsay, France. [Kisner, T. S.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Knoche, J.; Matthai, F.; Reinecke, M.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Hanson, D.] McGill Univ, McGill Phys, Montreal, PQ H3A 2T8, Canada. [Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Co Kildare, Ireland. [Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Crill, P.] CALTECH, Pasadena, CA 91125 USA. [Savini, G.] UCL, Opt Sci Lab, London, England. [Lesgourgues, J.] Ecole Polytech Fed Lausanne, SB ITP LPPC, CH-1015 Lausanne, Switzerland. [Baccigalupi, C.; Bielewicz, P.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Paci, F.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Ade, P. A. R.; Munshi, D.; Spencer, L. D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Karachai Cherkessian Rep 369167, Zelenchukskiy R, Russia. [Church, S.; Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Armitage-Caplan, C.] Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England. [Lesgourgues, J.] CERN, PH TH, Div Theory, CH-1211 Geneva, Switzerland. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UMR 7095, F-75014 Paris, France. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Leroy, C.; 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, Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Patanchon, G (reprint author), Univ Paris Diderot, Sorbonne Paris Cite, CNRS, IN2P3,CEA Irfu,Observ Paris,APC, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France. EM patanchon@apc.univ-paris-Diderot.fr RI Barreiro, Rita Belen/N-5442-2014; Remazeilles, Mathieu/N-1793-2015; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; Martinez-Gonzalez, Enrique/E-9534-2015; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Toffolatti, Luigi/K-5070-2014; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; OI Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; De Zotti, Gianfranco/0000-0003-2868-2595; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; Pierpaoli, Elena/0000-0002-7957-8993; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794 FU ESA FX Planck is a project of the European Space Agency ESA -with instruments provided by two scientific Consortia funded by ESA member states (in particular the lead countries: France and Italy) with contributions from NASA (USA), and telescope reflectors provided in a collaboration between ESA and a scientific Consortium led and funded by Denmark. The development of Planck has been supported by: ESA; CNES and CNRS / INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at h t t p : / / w w w. s c i o p s. e s a. i n t / i n d e x. p h p ? p r o j e c t = p l a n c k & p a g e = P l a n c k _ C o l l a b o r a t i o n NR 54 TC 40 Z9 39 U1 3 U2 12 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2014 VL 571 AR A10 DI 10.1051/0004-6361/201321577 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600025 ER PT J AU Ade, PAR Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bock, JJ Bond, JR Borrill, J Bouchet, FR Boulanger, F Bowyer, JW Bridges, M Bucher, M Burigana, C Cardoso, JF Catalano, A Chamballu, A Chary, RR Chen, X Chiang, HC Chiang, LY 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 Rose, A de Zotti, G Delabrouille, J Delouis, JM Desert, FX Dickinson, C Diego, JM Dole, H Donzelli, S Dore, O Douspis, M Dunkley, J Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Fraisse, AA Franceschi, E Galeotta, S Ganga, K Giard, M Giardino, G Girard, D Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Gudmundsson, JE Hansen, FK Hanson, D Harrison, D Helou, G Henrot-Versille, S Herent, O Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hou, Z Hovest, W Huffenberger, KM Hurier, G Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Le Jaune, M Leonardi, R Leroy, C Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF MacTavish, CJ Maffei, B Mandolesi, N Maris, M Marleau, F Marshall, J Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P McGehee, P Meinhold, PR Melchiorri, A Melot, F Mendes, L Mennella, A Migliaccio, M Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Mottet, S Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU North, C Noviello, F Novikov, D Novikov, I Orieux, F Osborne, S Oxborrow, CA Paci, F Pagano, L Pajot, F Paladini, R Paoletti, D Pasian, F Patanchon, G Perdereaun, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Racine, B Reach, WT Rebolo, R Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Roudier, G Rowan-Robinson, M Rusholme, B Sanselme, L Santos, D Sauve, A Savini, G Scott, D Shellard, EPS Spencer, LD Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sureae, F Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Tavagnacco, D Techene, S Terenzi, L Tomasi, M Tristram, M Tucci, M Umana, G Valenziano, L Valiviita, J Van Tent, B Vibert, L Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD White, SDM Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bock, J. J. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bowyer, J. W. Bridges, M. Bucher, M. Burigana, C. Cardoso, J. -F. Catalano, A. Chamballu, A. Chary, R. -R. Chen, X. Chiang, H. C. Chiang, L. -Y 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 Rose, 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. Dunkley, J. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Fraisse, A. A. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Girard, D. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Gudmundsson, J. E. Hansen, F. K. Hanson, D. Harrison, D. Helou, G. Henrot-Versille, S. Herent, O. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hou, Z. 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. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Le Jaune, M. Leonardi, R. Leroy, C. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. MacTavish, C. J. Maffei, B. Mandolesi, N. Maris, M. Marleau, F. Marshall, J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. McGehee, P. Meinhold, P. R. Melchiorri, A. Melot, F. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Mottet, S. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. North, C. Noviello, F. Novikov, D. Novikov, I. Orieux, F. Osborne, S. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paladini, R. Paoletti, D. Pasian, F. Patanchon, G. Perdereaun, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. 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. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rowan-Robinson, M. Rusholme, B. Sanselme, L. Santos, D. Sauve, A. Savini, G. Scott, D. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sureae, F. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Tavagnacco, D. Techene, S. Terenzi, L. Tomasi, M. Tristram, M. Tucci, M. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Vibert, L. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. White, S. D. M. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. VI. High Frequency Instrument data processing SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: data analysis; cosmic background radiation; cosmology: observations; surveys ID PRE-LAUNCH STATUS; MODEL; CALIBRATION; BEAMS AB We describe the processing of the 531 billion raw data samples from the High Frequency Instrument (HFI), which we performed to produce six temperature maps from the first 473 days of Planck-HFI survey data. These maps provide an accurate rendition of the sky emission at 100, 143, 217, 353, 545, and 857 GHz with an angular resolution ranging from 9. 0 7 to 4. 0 6. The detector noise per (effective) beam solid angle is respectively, 10, 6, 12, and 39 K in the four lowest HFI frequency channels (100-353 GHz) and 13 and 14 kJy sr 1 in the 545 and 857 GHz channels. Relative to the 143 GHz channel, these two high frequency channels are calibrated to within 5% and the 353 GHz channel to the percent level. The 100 and 217 GHz channels, which together with the 143 GHz channel determine the high-multipole part of the CMB power spectrum (50 < l < 2500), are calibrated relative to 143 GHz to better than 0.2%. C1 [Bucher, M.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Le Jaune, M.; Patanchon, G.; Piat, M.; Racine, B.; Remazeilles, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, APC, CNRS IN2P3, CEA Irfu,Observ Paris,Sorbonne Paris Cite, F-75205 Paris 13, France. [Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Kunz, M.] African Inst Math Sci, ZA-7945 Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy. [Mandolesi, N.] Agenzia Spaziale Italiana, Rome, Italy. [Ashdown, M.; Bridges, M.; Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 OHE, England. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa. [Kneissl, R.] ALMA, Santiago Cent Off, Santiago 7630355, Chile. [Bond, J. R.; Hanson, D.; Martin, P. G.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Leroy, C.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.; Sauve, A.] CNRS, IRAP, F-31028 Toulouse 4, France. [Bock, J. J.; Dore, O.; Helou, G.; Hildebrandt, S. R.; Prezeau, G.; Rocha, G.] CALTECH, Pasadena, CA 91125 USA. [Shellard, E. P. S.] Univ Cambridge, DAMTP, Ctr Theoret Cosmol, Cambridge CB3 0WA, England. [Hernandez-Monteagudo, C.] CEFCA, Teruel 44001, Spain. [Borrill, J.; Keskitalo, R.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Rebolo, R.] CSIC, 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, DK-2800 Lyngby, Denmark. [Kunz, M.; Tucci, M.] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland. [Atrio-Barandela, F.] Univ Salamanca, Fac Ciencias, Dept Fis Fundamental, E-37008 Salamanca, Spain. [Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada. [Rachen, J. P.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Keskitalo, R.] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Colombo, L. P. L.; Pierpaoli, E.] Univ So Calif, Dana & David Dornsife Coll Letter Arts & Sci, Dept Phys & Astron, Los Angeles, CA 90089 USA. [Benoit-Levy, A.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Huffenberger, K. M.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Juvela, M.; Keihanen, E.; Kurki-Suonio, H.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland. [Chiang, H. C.; Fraisse, A. A.; Gudmundsson, J. E.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Hou, Z.; Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 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, Urbana, IL USA. [Liguori, M.; Matarrese, S.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Burigana, C.; Mandolesi, N.; Natoli, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Nati, F.; Pagano, L.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Bersanelli, M.; Mennella, A.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy. [Gregorio, A.; Tavagnacco, D.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark. [Rebolo, R.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Kneissl, R.] ESO Vitacura, European So Observ, Santiago 19001, Chile. [Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Madrid 28692, Spain. [Frailis, M.; Giardino, G.; Laureijs, R. J.; Tauber, J. A.] Estec, European Space Agcy, NL-2201 AZ Noordwijk, Netherlands. [Kurki-Suonio, H.; Poutanen, T.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Helsinki Inst Phys, FIN-00014 Helsinki, Finland. [Umana, G.] INAF Osservatorio Astrofis Catania, Catania, Italy. [de Zotti, G.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Polenta, G.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Galeotta, S.; Gregorio, A.; Maris, M.; Pasian, F.; Tavagnacco, D.; Zacchei, A.] INAF Osservatorio Astron Trieste, Trieste, Italy. [Massardi, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Burigana, C.; Cuttaia, F.; de Rose, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Paoletti, D.; Ricciardi, S.; Terenzi, L.; Valenziano, L.; Villa, F.] INAF IASF Bologna, I-40129 Bologna, Italy. [Bersanelli, M.; Donzelli, S.; Mennella, A.; Tomasi, M.] INAF IASF Milano, I-20133 Milan, Italy. [Finelli, F.; Paoletti, D.] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy. [Melchiorri, A.; Pagano, L.] Univ Roma La Sapienza, Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy. Univ Joseph Fourier Grenoble 1, CNRS INSU, IPAG, UMR 5274, F-38041 Grenoble, France. [Mitra, S.] IUCAA, Pune 411007, Maharashtra, India. [Bowyer, J. W.; Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Chary, R. -R.; Chen, X.; Desert, F. -X.; McGehee, P.; Paladini, R.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Benoit, A.] Univ Joseph Fourier Grenoble I, CNRS, Inst Neel, F-38042 Grenoble, France. [Dole, H.] Inst Univ France, F-75005 Paris, France. [Aghanim, N.; Aumont, J.; Boulanger, F.; Chamballu, A.; Dole, H.; Douspis, M.; Hurier, G.; Kunz, M.; Lagache, G.; Leroy, C.; Miville-Deschenes, M. -A.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Remazeilles, M.; Vibert, L.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Herent, O.; Hivon, E.; Moneti, A.; Mottet, S.; Orieux, F.; Prunet, S.; Sygnet, J. -F.; Techene, S.; Wandelt, B. D.] CNRS, Inst Astrophys Paris, UMR7095, F-75014 Paris, France. [Popa, L.] Inst Space Sci, Bucharest, Romania. [Marleau, F.] Univ Innsbruck, Inst Astro & Particle Phys, A-6020 Innsbruck, Austria. [Chiang, L. -Y] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Bridges, M.; Efstathiou, G.; Gratton, S.; Harrison, D.; Migliaccio, M.; Sutton, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Eriksen, H. K.; Hansen, F. K.; Lilje, P. B.; Valiviita, J.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway. [Rebolo, R.] Inst Astrofis Canarias, Tenerife, Spain. [Barreiro, R. B.; Curto, A.; Diego, J. M.; Gonzalez-Nuevo, J.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain. [Bock, J. J.; Colombo, L. P. L.; Crill, B. P.; Dore, O.; Gorski, K. M.; Hanson, D.; Holmes, W. A.; Lawrence, C. R.; Mitra, S.; Pietrobon, D.; Prezeau, G.; Rocha, G.; Roudier, G.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Davies, R. D.; Davis, R. J.; Dickinson, C.; Maffei, B.; Noviello, F.; Remazeilles, M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Bridges, M.; Gratton, S.; Harrison, D.; Lasenby, A.; MacTavish, C. J.; Migliaccio, M.; Stolyarov, V.; Sutton, D.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Couchot, F.; Henrot-Versille, S.; Perdereaun, O.; Plaszczynski, S.; Tristram, M.; Tucci, M.] Univ Paris 11, CNRS IN2P3, LAL, F-91405 Orsay, France. [Catalano, A.; Coulais, A.; Lamarre, J. -M.; Roudier, G.] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Arnaud, M.; Bobin, J.; Chamballu, A.; Marshall, J.; Pratt, G. W.; Starck, J. -L.; Sureae, F.] Univ Paris Diderot, CEA Saclay, CEA DSM CNRS, Lab AIM,IRFU,Serv Astrophys, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, UMR 5141, Lab Traitement & Commun Informat, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom Paris Tech, F-75634 Paris 13, France. [Catalano, A.; Combet, C.; Girard, D.; Hurier, G.; Macias-Perez, J. F.; Melot, F.; Perotto, L.; Renault, C.; Sanselme, L.; Santos, D.] Univ Joseph Fourier Grenoble I, CNRS IN2P3, Inst Natl Polytech Grenoble, Lab Phys Subatom & Cosmol, F-38026 Grenoble, France. [Van Tent, B.] Univ Paris 11, Phys Theor Lab, F-91405 Orsay, France. [Van Tent, B.] CNRS, F-91405 Orsay, France. [Kisner, T. S.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Knoche, J.; Matthai, F.; Rachen, J. P.; Reinecke, M.; Riller, T.; White, S. D. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Hanson, D.] McGill Univ, McGill Phys, Montreal, PQ H3A 2T8, Canada. [Murphy, J. A.] Natl Univ Ireland, Maynooth, Kildare, Ireland. [Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Crill, B. P.] CALTECH, Observ Cosmol, Pasadena, CA 91125 USA. [Savini, G.] UCL, Opt Sci Lab, London, England. [Lesgourgues, J.] Ecole Polytech Fed Lausanne, SB ITP LPPC, CH-1015 Lausanne, Switzerland. [Baccigalupi, C.; Bielewicz, P.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; North, C.; Paci, F.; Perrotta, F.] SISSA, Astrophys Sector, I-34136 Trieste, Italy. [Ade, P. A. R.; Munshi, D.; Spencer, L. D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz 369167, Zelenchukskiy R, Russia. [Church, S.; Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA USA. [Armitage-Caplan, C.; Dunkley, J.] Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England. [Lesgourgues, J.] CERN, PH TH, Div Theory, CH-1211 Geneva 23, Switzerland. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UMR7095, Paris, France. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Leroy, C.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.; Sauve, A.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, E-18071 Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Bouchet, FR (reprint author), CNRS, Inst Astrophys Paris, UMR7095, 98bis Blvd Arago, F-75014 Paris, France. EM bouchet@iap.fr RI Barreiro, Rita Belen/N-5442-2014; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; Remazeilles, Mathieu/N-1793-2015; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Martinez-Gonzalez, Enrique/E-9534-2015; OI Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; De Zotti, Gianfranco/0000-0003-2868-2595; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Vielva, Patricio/0000-0003-0051-272X; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Reach, William/0000-0001-8362-4094; Hurier, Guillaume/0000-0002-1215-0706; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794 FU ESA FX The development of Planck has been supported by: ESA; CNES and CNRS / INSU- IN2P3- INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at h t t p : / / w w w. s c i o p s. e s a. i n t / i n d e x. p h p ? p r o j e c t = p l a n c k & p a g e = P l a n c k _ C o l l a b o r a t i o n. NR 57 TC 66 Z9 65 U1 3 U2 16 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 NOV PY 2014 VL 571 AR A6 DI 10.1051/0004-6361/201321570 PG 44 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600022 ER PT J AU Ade, PAR Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bock, JJ Bonaldi, A Bond, JR Borrill, J Bouchet, FR Boulanger, F Bridges, M Bucher, M Burigana, C Butler, RC Cardoso, JF Catalano, A Chamballu, A Chary, RR Chen, X Chiang, HC Chiang, LY Christensen, PR Church, S Clements, DL Colley, JM Colombi, S Colombo, LPL Couchot, F Coulais, A Crill, BP Curto, A Cuttaia, F Danese, L Davies, RD 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 Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Fraisse, AA Franceschi, E Galeotta, S Ganga, K Giard, M Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Hanson, D Harrison, D Helou, G Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leonardi, R Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Mottet, S Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S O'Sullivan, C Oxborrow, CA Paci, F Pagano, L Pajot, F Paladini, R Paoletti, D Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polegre, AM Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Reach, WT Rebolo, R Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Roudier, G Rowan-Robinson, M Rusholme, B Sandri, M Santos, D Savini, G Scott, D Seiffert, MD Shellard, EPS Smoot, GF Spencer, LD Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sureau, F Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Tavagnacco, D Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Tuovinen, J Umana, G Valenziano, L Valiviita, J Van Tent, B Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bridges, M. Bucher, M. Burigana, C. Butler, R. C. Cardoso, J. -F. Catalano, A. Chamballu, A. Chary, R. -R. Chen, X. Chiang, H. C. Chiang, L. -Y Christensen, P. R. Church, S. Clements, D. L. Colley, J. -M. Colombi, S. Colombo, L. P. L. Couchot, F. Coulais, A. Crill, B. P. Curto, A. Cuttaia, F. Danese, L. Davies, R. D. 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. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Fraisse, A. A. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Hanson, D. Harrison, D. Helou, G. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leonardi, R. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, 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. 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. Osborne, S. O'Sullivan, C. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paladini, R. Paoletti, D. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polegre, A. M. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Reach, W. T. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rowan-Robinson, M. Rusholme, B. Sandri, M. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Smoot, G. F. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sureau, F. 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. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. XIV. Zodiacal emission SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE zodiacal dust; interplanetary medium; cosmic background radiation ID SYSTEM DUST BANDS; SOLAR-SYSTEM; INFRARED-EMISSION; IRAS OBSERVATIONS; ORIGIN; CLOUD; COBE; MODEL; COMETARY; SPECTRUM AB The Planck satellite provides a set of all-sky maps at nine frequencies from 30 GHz to 857 GHz. Planets, minor bodies, and di ff use interplanetary dust emission (IPD) are all observed. The IPD can be separated from Galactic and other emissions because Planck views a given point on the celestial sphere multiple times, through di ff erent columns of IPD. We use the Planck data to investigate the behaviour of zodiacal emission over the whole sky at sub-millimetre and millimetre wavelengths. We fit the Planck data to find the emissivities of the various components of the COBE zodiacal model -a di ff use cloud, three asteroidal dust bands, a circumsolar ring, and an Earth-trailing feature. The emissivity of the diffuse cloud decreases with increasing wavelength, as expected from earlier analyses. The emissivities of the dust bands, however, decrease less rapidly, indicating that the properties of the grains in the bands are di ff erent from those in the di ff use cloud. We fit the small amount of Galactic emission seen through the telescope's far sidelobes, and place limits on possible contamination of the cosmic microwave background (CMB) results from both zodiacal and far-sidelobe emission. When necessary, the results are used in the Planck pipeline to make maps with zodiacal emission and far sidelobes removed. We show that the zodiacal correction to the CMB maps is small compared to the Planck CMB temperature power spectrum and give a list of flux densities for small solar system bodies. C1 [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Colley, J. -M.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Remazeilles, M.; Rosset, C.; Roudier, G.; Smoot, G. F.; Stompor, R.] Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, CNRS IN2P3 CEA Irfu,APC, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France. [Lahteenmaki, A.; Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Kunz, M.] African Inst Math Sci, ZA-7945 Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana, Sci Data Ctr, I-00133 Rome, Italy. [Mandolesi, N.] Agenzia Spaziale Italiana, I-00198 Rome, Italy. [Ashdown, M.; Bridges, M.; Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. 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EM ganga@apc.univ-paris-diderot.fr RI Butler, Reginald/N-4647-2015; Barreiro, Rita Belen/N-5442-2014; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; Remazeilles, Mathieu/N-1793-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; OI Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; De Zotti, Gianfranco/0000-0003-2868-2595; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Starck, Jean-Luc/0000-0003-2177-7794; Reach, William/0000-0001-8362-4094; Valiviita, Jussi/0000-0001-6225-3693; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379 FU NASA FX This paper benefited from exchanges with Dale Fixsen, Tom Kelsall and Janet Weiland. We acknowledge the IN2P3 Computer Center ( h t t p : / / c c. i n 2 p 3. f r) for providing a significant amount of the computing resources and services needed for this work. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis ( LAMBDA). Support for LAMBDA is provided by the NASA O ffi ce of Space Science. The development of Planck has been supported by: ESA; CNES and CNRS / INSUIN2P3- INP ( France); ASI, CNR, and INAF ( Italy); NASA and DoE ( USA); STFC and UKSA ( UK); CSIC, MICINN, 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); and PRACE ( EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at h t t p : / / w w w. s c i o p s. e s a. i n t / i n d e x. p h p ? p r o j e c t = p l a n c k & p a g e = P l a n c k _ C o l l a b o r a t i o n NR 75 TC 49 Z9 48 U1 3 U2 15 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 NOV PY 2014 VL 571 AR A14 DI 10.1051/0004-6361/201321562 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600020 ER PT J AU Ade, PAR Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bock, JJ Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Bridges, M Bucher, M Burigana, C Butler, RC Cardoso, JF Catalano, A Challinor, A Chamballu, A Chiang, HC Chiang, LY Christensen, PR Church, S Clements, DL Colombi, S Colombo, LPL 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 Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Fabre, O Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK 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 Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leahy, JP Leonardi, R Leroy, C Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P McEwen, JD 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 Osborne, S Oxborrow, CA Paci, F Pagano, L Pajot, F Paoletti, D Pasian, F Patanchon, G Peiris, HV Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pogosyan, D Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Rebolo, R Reinecke, M Remazeilles, M Renault, C Riazuelo, A Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Roudier, G Rowan-Robinson, M Rusholme, B Sandri, M Santos, D Savini, G Scott, D Seiffert, MD Shellard, EPS Spencer, LD Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sureau, F Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Tavagnacco, D Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Tuovinen, J Valenziano, L Valiviita, J Van Tent, B Varis, J Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bock, J. J. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Bridges, M. Bucher, M. Burigana, C. Butler, R. C. Cardoso, J. -F. Catalano, A. Challinor, A. Chamballu, A. Chiang, H. C. Chiang, L. -Y. Christensen, P. R. Church, S. Clements, D. L. Colombi, S. Colombo, L. P. L. 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. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Fabre, O. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. 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. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leahy, J. P. Leonardi, R. Leroy, C. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. McEwen, J. D. 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. Osborne, S. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paoletti, D. Pasian, F. Patanchon, G. Peiris, H. V. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pogosyan, D. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Riazuelo, A. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rowan-Robinson, M. Rusholme, B. Sandri, M. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sureau, F. 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. Valenziano, L. Valiviita, J. Van Tent, B. Varis, J. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. XXVI. Background geometry and topology of the Universe SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology: observations; cosmic background radiation; cosmological parameters; gravitation; methods: data analysis; methods: statistical ID MICROWAVE-ANISOTROPY-PROBE; DODECAHEDRAL SPACE TOPOLOGY; BIANCHI-VIIH MODELS; WMAP OBSERVATIONS; COBE-DMR; SKY MAPS; COSMIC CRYSTALLOGRAPHY; PARAMETER-ESTIMATION; COSMOLOGICAL MODELS; SPHERICAL WAVELETS AB The new cosmic microwave background (CMB) temperature maps from Planck provide the highest-quality full-sky view of the surface of last scattering available to date. This allows us to detect possible departures from the standard model of a globally homogeneous and isotropic cosmology on the largest scales. We search for correlations induced by a possible non-trivial topology with a fundamental domain intersecting, or nearly intersecting, the last scattering surface (at comoving distance chi(rec)), both via a direct search for matched circular patterns at the intersections and by an optimal likelihood search for specific topologies. For the latter we consider flat spaces with cubic toroidal (T3), equal-sided chimney (T2) and slab (T1) topologies, three multi-connected spaces of constant positive curvature (dodecahedral, truncated cube and octahedral) and two compact negative-curvature spaces. These searches yield no detection of the compact topology with the scale below the diameter of the last scattering surface. For most compact topologies studied the likelihood maximized over the orientation of the space relative to the observed map shows some preference for multi-connected models just larger than the diameter of the last scattering surface. Since this effect is also present in simulated realizations of isotropic maps, we interpret it as the inevitable alignment of mild anisotropic correlations with chance features in a single sky realization; such a feature can also be present, in milder form, when the likelihood is marginalized over orientations. Thus marginalized, the limits on the radius R-i of the largest sphere inscribed in topological domain (at log-likelihood-ratio Delta ln L > -5 relative to a simply-connected flat Planck best-fit model) are: in a flat Universe, R-i > 0.92 chi(rec) for the T3 cubic torus; R-i > 0.71 chi(rec) for the T2 chimney; R-i > 0.50 chi(rec) for the T1 slab; and in a positively curved Universe, R-i > 1.03 chi(rec) for the dodecahedral space; R-i > 1.0 chi(rec) for the truncated cube; and R-i > 0.89 chi(rec) for the octahedral space. The limit for a wider class of topologies, i. e., those predicting matching pairs of back-to-back circles, among them tori and the three spherical cases listed above, coming from the matched-circles search, is R-i > 0.94 chi(rec) at 99% confidence level. Similar limits apply to a wide, although not exhaustive, range of topologies. 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 data favour the inclusion of a Bianchi component with a Bayes factor of at least 1.5 units of log-evidence. Indeed, the Bianchi pattern is quite efficient at accounting for some of the large-scale anomalies found in Planck data. However, the cosmological parameters that generate this pattern are in strong disagreement with those found from CMB anisotropy data alone. 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) < 8.1 x 10(-10) (95% confidence level). 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, Sorbonne Paris Cite, Observ Paris, CNRS,IN2P3,CEA,Irfu,APC, F-75205 Paris 13, France. [Lahteenmaki, A.; Poutanen, T.] Aalto Univ Metsahovi Radio Observ, Aalto 00076, Finland. [Lahteenmaki, A.; Poutanen, T.] Dept Radio Sci & Engn, Aalto 00076, Finland. [Kunz, M.] African Inst Math Sci, ZA-7945 Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy. [Mandolesi, N.] Agenzia Spaziale Italiana, Rome, Italy. 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[Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Zelenchukskiy Region 369167, Karachai Cherke, Russia. [Church, S.; Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Armitage-Caplan, C.] Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England. [Lesgourgues, J.] CERN, Div Theory, PH TH, CH-1211 Geneva 23, Switzerland. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Prunet, S.; Riazuelo, A.; Wandelt, B. D.] Univ Paris 06, UMR 7095, F-75014 Paris, France. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Leroy, C.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Battaner, E.] Univ Granada, Dept Fis Teor & Cosmos, Fac Ciencias, E-18071 Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Jaffe, AH (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, Prince Consort Rd, London SW7 2AZ, England. EM a.jaffe@imperial.ac.uk RI Remazeilles, Mathieu/N-1793-2015; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; bonavera, laura/E-9368-2017; Kurki-Suonio, Hannu/B-8502-2016; Toffolatti, Luigi/K-5070-2014; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Martinez-Gonzalez, Enrique/E-9534-2015; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Lahteenmaki, Anne/L-5987-2013; Barreiro, Rita Belen/N-5442-2014; Butler, Reginald/N-4647-2015; OI Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Ricciardi, Sara/0000-0002-3807-4043; Pasian, Fabio/0000-0002-4869-3227; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; bonavera, laura/0000-0001-8039-3876; De Zotti, Gianfranco/0000-0003-2868-2595; Lopez-Caniego, Marcos/0000-0003-1016-9283; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Kurki-Suonio, Hannu/0000-0002-4618-3063; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Starck, Jean-Luc/0000-0003-2177-7794; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375 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); MICINN (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); PRACE (EU); Canada Foundation for Innovation under the auspices of Compute Canada; Government of Ontario; Ontario Research Fund - Research Excellence; University of Toronto FX The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collabora tion. The authors thank the anonymous referee for helpful comments and acknowledge the use of the UCL Legion High Performance Computing Facility (Legion@UCL), and associated support services, in the completion of this work. Part of the computations were performed on the Andromeda cluster of the University of Geneve, the Hopper Cray XE6 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 124 TC 82 Z9 81 U1 4 U2 13 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2014 VL 571 AR A26 DI 10.1051/0004-6361/201321546 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600015 ER PT J AU Ade, PAR Aghanim, N Alves, MIR Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bock, JJ Bonaldi, A Bond, JR Borrill, J Bouchet, FR Boulanger, F Bridges, M Bucher, M Burigana, C Butler, RC Cardos, JF Catalano, A Chamballu, A Chary, RR Chen, X Chiang, HC Chiang, LY 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 de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Dempsey, JT Desert, FX Dickinson, C Diego, JM Dole, H Donzelli, S Dore, O Douspis, M Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Falgarone, E Finelli, F Forni, O Frailis, M Franceschi, E Fukui, Y Galeotta, S Ganga, K Giard, M Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Handa, T Hansen, FK Hanson, D Harrison, D Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hily-Blant, P Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Hurier, G Jaffe, AH Jaffe, TR Jewell, J Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leonardi, R Leon-Tavares, J Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffein, B Mandolesi, N Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P McGehee, P Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Moore, TJT Morgante, G Morino, J Mortlock, D Munshi, D Murphy, JA Nakajima, T Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviellon, F Novikov, D Novikov, I Okuda, T Osborne, S Oxborrow, CA Paci, F Pagano, L Pajot, F Paladini, R Paoletti, D Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Reach, WT Rebolo, R Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Roudier, G Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savini, G Scott, D Seiffert, MD Shellard, EPS Spencer, LD Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sunyaev, R Sureau, F Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Tavagnacco, D Terenzi, L Thomas, HS Toffolatti, L Tomasi, M Torii, K Tristram, M Tucci, M Tuovinen, J Umana, G Valenziano, L Valiviita, J Van Tent, B Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Wehus, IK Yamamoto, H Yoda, T Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Alves, M. I. R. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bridges, M. Bucher, M. Burigana, C. Butler, R. C. Cardos, J. -F. Catalano, A. Chamballu, A. Chary, R. -R. Chen, X. Chiang, H. C. Chiang, L. -Y. 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. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J. -M. Dempsey, J. T. Desert, F. -X. Dickinson, C. Diego, J. M. Dole, H. Donzelli, S. Dore, O. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Falgarone, E. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Fukui, Y. Galeotta, S. Ganga, K. Giard, M. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Handa, T. Hansen, F. K. Hanson, D. Harrison, D. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hily-Blant, P. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Hurier, G. Jaffe, A. H. Jaffe, T. R. Jewell, J. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leonardi, R. Leon-Tavares, J. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffein, B. Mandolesi, N. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. McGehee, P. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Moore, T. J. T. Morgante, G. Morino, J. Mortlock, D. Munshi, D. Murphy, J. A. Nakajima, T. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviellon, F. Novikov, D. Novikov, I. Okuda, T. Osborne, S. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paladini, R. Paoletti, D. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Reach, W. T. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sunyaev, R. Sureau, F. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Tavagnacco, D. Terenzi, L. Thomas, H. S. Toffolatti, L. Tomasi, M. Torii, K. Tristram, M. Tucci, M. Tuovinen, J. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Wehus, I. K. Yamamoto, H. Yoda, T. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. XIII. Galactic CO emission SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: molecules ID LATITUDE MOLECULAR GAS; (CO)-C-13 J=2-1; CARBON-MONOXIDE; MAPPING SURVEY; MILKY-WAY; CLOUDS; REGION; GALAXY; ORION; HEMISPHERE AB Rotational transition lines of CO play a major role in molecular radio astronomy as a mass tracer and in particular in the study of star formation and Galactic structure. Although a wealth of data exists for the Galactic plane and some well-known molecular clouds, there is no available high sensitivity all-sky survey of CO emission to date. Such all-sky surveys can be constructed using the Planck HFI data because the three lowest CO rotational transition lines at 115, 230 and 345 GHz significantly contribute to the signal of the 100, 217 and 353 GHz HFI channels, respectively. Two different component separation methods are used to extract the CO maps from Planck HFI data. The maps obtained are then compared to one another and to existing external CO surveys. From these quality checks the best CO maps, in terms of signal to noise ratio and/or residual contamination by other emission, are selected. Three different sets of velocity-integrated CO emission maps are produced with different trade-offs between signal-to-noise, angular resolution, and reliability. Maps for the CO J = 1 -> 0, J = 2 -> 1, and J = 3 -> 2 rotational transitions are presented and described in detail. They are shown to be fully compatible with previous surveys of parts of the Galactic plane as well as with undersampled surveys of the high latitude sky. The Planck HFI velocity-integrated CO maps for the J = 1 -> 0, J = 2 -> 1, and J = 3 -> 2 rotational transitions provide an unprecedented all-sky CO view of the Galaxy. These maps are also of great interest to monitor potential CO contamination of the Planck studies of the cosmological microwave background. C1 [Bartlett, J. G.; Bucher, M.; Cardos, J. -F.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Remazeilles, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, CNRS IN2P3,CEA Irfu,APC, F-75205 Paris 13, France. [Lahteenmaki, A.; Leon-Tavares, J.; Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Kunz, M.] African Inst Math Sci, ZA-7701 Rondebosch, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana, Sci Data Ctr, I-00133 Rome, Italy. [Mandolesi, N.] Agenzia Spaziale Italiana, Rome, Italy. 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[Bersanelli, M.; Donzelli, S.; Mennella, A.; Tomasi, M.] INAF IASF Milano, I-20133 Milan, Italy. [Finelli, F.; Paoletti, D.] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy. [Melchiorri, A.; Pagano, L.] Univ Roma La Sapienza, Ist Nazl Fis Nucl, Sez Roma 1, I-00185 Rome, Italy. [Desert, F. -X.; Hily-Blant, P.; Ponthieu, N.] Univ Grenoble 1, CNRS INSU, Inst Planetol & Astrophys Grenoble, UMR 5274, F-38041 Grenoble, France. [Mitra, S.] IUCAA, Pune 411007, Maharashtra, India. [Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Chary, R. -R.; Chen, X.; McGehee, P.; Paladini, R.; Rusholme, B.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, F-38042 Grenoble, France. [Dole, H.] Inst Univ France, F-75005 Paris, France. [Aghanim, N.; Alves, M. I. R.; Aumont, J.; Boulanger, F.; Chamballu, A.; Dole, H.; Douspis, M.; Hurier, G.; Kunz, M.; Lagache, G.; Miville-Deschenes, M. -A.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Remazeilles, M.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France. [Benabed, K.; Benoit-Levy, A.; Boulanger, F.; Cardos, J. -F.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Popa, L.] Inst Space Sci, Bucharest 077125, Romania. [Chiang, L. -Y.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Bridges, M.; Efstathiou, G.; Gratton, S.; Harrison, D.; Migliaccio, M.; Sutton, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Yoda, T.] Univ Tokyo, Inst Astron, Mitaka, Tokyo 181, Japan. [Eriksen, H. K.; Hansen, F. K.; Lilje, P. B.; Valiviita, J.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife 38200, Spain. [Barreiro, R. 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, E-39005 Santander, Spain. [Bartlett, J. G.; Bock, J. J.; Colombo, L. P. L.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Jewell, J.; 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, Pasadena, CA USA. [Bonaldi, A.; Davies, R. D.; Maffein, B.; Noviellon, F.; Remazeilles, M.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Dempsey, J. T.; Thomas, H. S.] Joint Astron Ctr, Hilo, HI 96720 USA. [Couchot, F.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.; Tucci, M.] Kavli Inst Cosmol Cambridge, Cambridge, England. [Catalano, A.; Coulais, A.; Falgarone, E.; Lamarre, J. -M.; Roudier, G.] Univ Paris 11, CNRS, IN2P3, LAL, F-91898 Orsay, France. [Arnaud, M.; Bobin, J.; Chamballu, A.; Marshall, D. J.; Pratt, G. W.; Starck, J. -L.; Sureau, F.] CNRS, Observ Paris, LERMA, F-75014 Paris, France. [Cardos, J. -F.] Univ Paris Diderot, CNRS, CEA DSM, Lab AIM,IRFU Serv Astrophys, F-91191 Gif Sur Yvette, France. [Cardos, J. -F.] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris 13, France. [Cardos, J. -F.] Telecom Paris Tech, F-75634 Paris 13, France. [Catalano, A.; Combet, C.; Hurier, G.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble 1, Inst Natl Polytech Grenoble, CNRS IN2P3, Lab Phys Subatom & Cosmol, F-38026 St Martin Dheres, France. [Van Tent, B.] Univ Paris 11, Phys Theor Lab, F-91405 Orsay, France. [Kisner, T. S.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Knoche, J.; Matthai, F.; Rachen, J. P.; Reinecke, M.; Riller, T.; Sunyaev, R.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Hanson, D.] McGill Univ, McGill Phys, Montreal H3A 2T8, PQ, Canada. [Tuovinen, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo 02044, Finland. [Morino, J.] Natl Astron Observ Japan, Tokyo 1818588, Japan. [Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Nakajima, T.] Natl Astron Observ Japan, Nobeyama Radio Observ, Minamisa Ku, Minamimaki, Nagano 3841305, Japan. [Crill, B. P.] CALTECH, Observat Cosmol, Pasadena, CA 91125 USA. [Savini, G.] UCL, Opt Sci Lab, London, England. [Lesgourgues, J.] Ecole Polytech Fed Lausanne, SB ITP LPPC, CH-1015 Lausanne, Switzerland. [Baccigalupi, C.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Paci, F.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Ade, P. A. R.; Munshi, D.; Spencer, L. D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Sunyaev, R.] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Karachai Cherkessian 369167, Russia. [Church, S.; Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Armitage-Caplan, C.] Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England. [Lesgourgues, J.] CERN, Div Theory, PH TH, CH-1211 Geneva 23, Switzerland. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Colombi, S.; Delouis, J. -M.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UMR 7095, F-75014 Paris, France. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Reach, W. T.] Univ Space Res Assoc, Observ Infrared Astron, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Dept Fis Teor & Cosmos, Fac Ciencias, E-18071 Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Macias-Perez, JF (reprint author), Univ Grenoble 1, Inst Natl Polytech Grenoble, CNRS IN2P3, Lab Phys Subatom & Cosmol, 53 Rue Martyrs, F-38026 St Martin Dheres, France. EM macias@lpsc.in2p3.fr RI Barreiro, Rita Belen/N-5442-2014; Remazeilles, Mathieu/N-1793-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; Martinez-Gonzalez, Enrique/E-9534-2015; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Butler, Reginald/N-4647-2015; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; OI Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Ricciardi, Sara/0000-0002-3807-4043; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; De Zotti, Gianfranco/0000-0003-2868-2595; Masi, Silvia/0000-0001-5105-1439; Pierpaoli, Elena/0000-0002-7957-8993; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Butler, Reginald/0000-0003-4366-5996; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Reach, William/0000-0001-8362-4094; Hurier, Guillaume/0000-0002-1215-0706; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Villa, Fabrizio/0000-0003-1798-861X FU ESA FX The development of Planck has been supported by: ESA; CNES and CNRS /INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at h t t p : //w w w. s c i o p s. e s a. i n t /i n d e x. p h p ? p r o j e c t = P l a n c k \ & p a g e = P l a n c k _ C o l l a b o r a t i o n. We acknowledge the use of the H E A L P i x software. NR 77 TC 77 Z9 76 U1 3 U2 19 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 NOV PY 2014 VL 571 AR A13 DI 10.1051/0004-6361/201321553 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600017 ER PT J AU Ade, PAR Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartlett, JG Basak, S Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bethermin, M Bielewicz, P Bobin, J Bock, JJ Bonaldi, A Bond, JR Borrill, J Bouchet, FR Boulanger, F Bridges, M Bucher, M Burigana, C Butler, RC Cardoso, JF Catalano, A Challinor, A Chamballu, A Chiang, HC Chiang, LY Christensen, PR Church, S Clements, DL Colombi, S Colombo, LPL Couchot, F Coulais, A Crill, BP Curto, A Cuttaia, F Danese, L Davies, RD 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 Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Gudmundsson, JE Hansen, FK Hanson, D Harrison, D Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lacasa, F Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leonardi, R Leon-Tavares, J Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S Oxborrow, CA Paci, F Pagano, L Pajot, F Paoletti, D Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Rebolo, R Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Roudier, G Rowan-Robinson, M Rusholme, B Sandri, M Santos, D Savini, G Scott, D Seiffert, MD Serra, P Shellard, EPS Spencer, LD Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sunyaev, R Sureau, F Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Tavagnacco, D Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Tuovinen, J Valenziano, L Valiviita, J Van Tent, B Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD White, SDM Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Basak, S. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bethermin, M. Bielewicz, P. Bobin, J. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bridges, M. Bucher, M. Burigana, C. Butler, R. C. Cardoso, J. -F. Catalano, A. Challinor, A. Chamballu, A. Chiang, H. C. Chiang, L. -Y Christensen, P. R. Church, S. Clements, D. L. Colombi, S. Colombo, L. P. L. Couchot, F. Coulais, A. Crill, B. P. Curto, A. Cuttaia, F. Danese, L. Davies, R. D. 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. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Gudmundsson, J. E. Hansen, F. K. Hanson, D. Harrison, D. 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. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lacasa, F. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leonardi, R. Leon-Tavares, J. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Osborne, S. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paoletti, D. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rowan-Robinson, M. Rusholme, B. Sandri, M. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Serra, P. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sunyaev, R. Sureau, F. 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. Valenziano, L. Valiviita, J. Van Tent, B. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. White, S. D. M. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. XVIII. The gravitational lensing-infrared background correlation SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gravitational lensing: weak; cosmic background radiation; large-scale structure of Universe; dark matter; galaxies: star formation ID STAR-FORMING GALAXIES; SOUTH-POLE TELESCOPE; PRE-LAUNCH STATUS; ANISOTROPY POWER SPECTRUM; SENSITIVITY HI SURVEY; DARK-MATTER HALOES; FINAL DATA RELEASE; DUST EMISSION; FORMATION HISTORY; DISTANT GALAXIES AB The multi-frequency capability of the Planck satellite provides information both on the integrated history of star formation (via the cosmic infrared background, or CIB) and on the distribution of dark matter (via the lensing effect on the cosmic microwave background, or CMB). The conjunction of these two unique probes allows us to measure directly the connection between dark and luminous matter in the high redshift (1 <= z <= 3) Universe. We use a three-point statistic optimized to detect the correlation between these two tracers, using lens reconstructions at 100, 143, and 217 GHz, together with CIB measurements at 100-857 GHz. Following a thorough discussion of possible contaminants and a suite of consistency tests, we report the first detection of the correlation between the CIB and CMB lensing. The well matched redshift distribution of these two signals leads to a detection significance with a peak value of 42/19 sigma (statistical/statistical + systematics) at 545 GHz and a correlation as high as 80% across these two tracers. Our full set of multi-frequency measurements (both CIB auto-and CIB-lensing cross-spectra) are consistent with a simple halo-based model, with a characteristic mass scale for the halos hosting CIB sources of log(10)(M/M-circle dot) = 10.5 +/- 0.6. Leveraging the frequency dependence of our signal, we isolate the high redshift contribution to the CIB, and constrain the star formation rate (SFR) density at z >= 1. We measure directly the SFR density with around 2 sigma significance for three redshift bins between z = 1 and 7, thus opening a new window into the study of the formation of stars at early times. C1 [Ade, P. A. R.; Bartlett, J. G.; Bucher, M.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, Sorbonne Paris Cite, Observ Paris, CNRS,IN2P3,CEA,lrfu,APC, F-75205 Paris 13, France. [Aghanim, N.; Lahteenmaki, A.] Aalto Univ Metsahovi Radio Observ, Kylmala 02540, Finland. [Armitage-Caplan, C.] African Inst Math Sci, ZA-7701 Muizenberg, Rondebosch Cape, South Africa. [Armitage-Caplan, C.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy. [Arnaud, M.] Agenzia Spaziale Italiana, I-00198 Rome, Italy. [Ashdown, M.; Atrio-Barandela, F.; Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Aumont, J.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa. [Baccigalupi, C.] Atacama Large Millimeter submillimeter Array, ALMA Santiago Cent Off, Santiago 7630355, Chile. [Arnaud, M.; Banday, A. J.; Bond, J. R.; Martin, P. G.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Barreiro, R. B.; Bartlett, J. G.; Basak, S.; Battaner, E.; Benabed, K.; Benoit, A.; Benoit-Levy, A.; Bernard, J. -P.; Bersanelli, M.] CNRS, IRAP, F-31028 Toulouse 4, France. [Bethermin, M.; Bielewicz, P.; Bobin, J.; Bock, J. J.; Hildebrandt, S. 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EM olivier.p.dore@jpl.nasa.gov RI Barreiro, Rita Belen/N-5442-2014; Butler, Reginald/N-4647-2015; Remazeilles, Mathieu/N-1793-2015; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Martinez-Gonzalez, Enrique/E-9534-2015; OI Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; De Zotti, Gianfranco/0000-0003-2868-2595; Lopez-Caniego, Marcos/0000-0003-1016-9283; Masi, Silvia/0000-0001-5105-1439; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; Bethermin, Matthieu/0000-0002-3915-2015 FU ESA; CNES (France); CNRS/INSU-IN2P3INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MICINN (Spain); JA (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); PRACE (EU); ESA Member State, NASA; ESA Member State, Canada FX Based on observations obtained with Planck (http://www.esa.int/Planck), an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA, and Canada. The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http : //www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. We acknowledge the use of the HEALPix package, and the LAMBDA archive (http://lambda.gsfc.nasa.gov). NR 113 TC 65 Z9 64 U1 3 U2 9 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2014 VL 571 AR A18 DI 10.1051/0004-6361/201321540 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600012 ER PT J AU Ade, PAR Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bertincourt, B Bielewicz, P Bobin, J Bock, JJ Bond, JR Borrill, J Bouchet, FR Boulanger, F Bridges, M Bucher, M Burigana, C Cardoso, JF Catalano, A Challinor, A Chamballu, A Chary, RR Chen, X Chiang, HC Chiang, LY 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 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 Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Filliard, C Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Hanson, D Harrison, D Helou, G Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Le Jeune, M Lellouch, E Leonardi, R Leroy, C Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Mandolesi, N Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Maurin, L Mazzotta, P McGehee, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Moreno, R Morgante, G Mortlock, D Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S 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 Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Roudier, G Rusholme, B Santos, D Savini, G Scott, D Shellard, EPS Spencer, LD Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sunyaev, R Sureau, F Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Tavagnacco, D Techene, S Terenzi, L Tomasi, M Tristram, M Tucci, M Umana, G Valenziano, L Valiviita, J Van Tent, B Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bertincourt, B. Bielewicz, P. Bobin, J. Bock, J. J. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bridges, M. Bucher, M. Burigana, C. Cardoso, J. -F. Catalano, A. Challinor, A. Chamballu, A. Chary, R. -R. Chen, X. Chiang, H. C. Chiang, L. -Y 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. 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. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Filliard, C. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Hanson, D. Harrison, D. Helou, G. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Le Jeune, M. Lellouch, E. Leonardi, R. Leroy, C. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Mandolesi, N. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Maurin, L. Mazzotta, P. McGehee, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Moreno, R. Morgante, G. Mortlock, D. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Osborne, S. 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. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rusholme, B. Santos, D. Savini, G. Scott, D. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sunyaev, R. Sureau, F. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Tavagnacco, D. Techene, S. Terenzi, L. Tomasi, M. Tristram, M. Tucci, M. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. VIII. HFI photometric calibration and mapmaking SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmic background radiation; cosmology: observations; surveys; methods: data analysis ID IN-FLIGHT PERFORMANCE; PRE-LAUNCH STATUS; DUST EMISSION; 1ST DETECTION; COBE FIRAS; ATMOSPHERE; ANISOTROPY; SPECTRUM; DESIGN; DIRBE AB This paper describes the methods used to produce photometrically calibrated maps from the Planck High Frequency Instrument (HFI) cleaned, time-ordered information. HFI observes the sky over a broad range of frequencies, from 100 to 857 GHz. To obtain the best calibration accuracy over such a large range, two different photometric calibration schemes have to be used. The 545 and 857 GHz data are calibrated by comparing flux-density measurements of Uranus and Neptune with models of their atmospheric emission. The lower frequencies (below 353 GHz) are calibrated using the solar dipole. A component of this anisotropy is time-variable, owing to the orbital motion of the satellite in the solar system. Photometric calibration is thus tightly linked to mapmaking, which also addresses low-frequency noise removal. By comparing observations taken more than one year apart in the same configuration, we have identified apparent gain variations with time. These variations are induced by non-linearities in the read-out electronics chain. We have developed an effective correction to limit their effect on calibration. We present several methods to estimate the precision of the photometric calibration. We distinguish relative uncertainties (between detectors, or between frequencies) and absolute uncertainties. Absolute uncertainties lie in the range from 0.54% to 10% from 100 to 857 GHz. We describe the pipeline used to produce the maps from the HFI timelines, based on the photometric calibration parameters, and the scheme used to set the zero level of the maps a posteriori. We also discuss the cross-calibration between HFI and the SPIRE instrument on board Herschel. Finally we summarize the basic characteristics of the set of HFI maps included in the 2013 Planck data release. C1 [Ade, P. A. R.; Bucher, M.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Le Jeune, M.; Maurin, L.; Patanchon, G.; Piat, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, APC, Sorbonne Paris Cite, CNRS,IN2P3,CEA,Irfu,Observ Paris, F-75205 Paris 13, France. [Aghanim, N.] Aalto Univ, Metsahovi Radio Observ, Aalto 00076, Finland. [Aghanim, N.] Dept Radio Sci & Engn, Aalto 00076, Finland. [Armitage-Caplan, C.] African Inst Math Sci, ZA-7701 Cape Town, Rondebosh, South Africa. [Aghanim, N.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy. 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[Bertincourt, B.; Frailis, M.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.; Giardino, G.; Giraud-Heraud, Y.] Univ Paris 06, UMR7095, F-75014 Paris, France. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Gonzalez-Nuevo, J.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Battaner, E.] Univ Granada, Dept Fis Teer & Cosmos, E-18071 Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Perdereau, O (reprint author), Univ Paris 11, CNRS, IN2P3, LAL, Bat 425, F-91898 Orsay, France. EM guilaine.lagache@ias.u-psud.fr; perdereau@lal.in2p3.fr RI Remazeilles, Mathieu/N-1793-2015; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Martinez-Gonzalez, Enrique/E-9534-2015; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Pearson, Timothy/N-2376-2015; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Barreiro, Rita Belen/N-5442-2014; OI de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; De Zotti, Gianfranco/0000-0003-2868-2595; Lopez-Caniego, Marcos/0000-0003-1016-9283; Masi, Silvia/0000-0001-5105-1439; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Vielva, Patricio/0000-0003-0051-272X; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Pearson, Timothy/0000-0001-5213-6231; Gruppuso, Alessandro/0000-0001-9272-5292; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099 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); MICINN (Spain); JA (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); PRACE (EU) FX The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members with the technical or scientific activities they have been involved into, can be found at http://www.rssd.esa.int/index.php?project=PLANCK&page=PlanckCollaboratio n NR 67 TC 70 Z9 69 U1 5 U2 14 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2014 VL 571 AR A8 DI 10.1051/0004-6361/201321538 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600011 ER PT J AU Ade, PAR Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, E Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bock, JJ Bond, JR Borrill, J Bouchet, FR Bowyer, JW Bridges, M Bucher, M Burigana, C Cardoso, JE Catalano, A Challinor, A Chamballu, A Chary, RR Chiang, HC Chiang, LY Christensen, PR Church, S Clements, DL Colombi, S Colombo, LPL Couchot, F Coulais, A Crill, BP Curto, A Cuttaia, E Danese, L Davies, RD 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 Dunkley, J Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Fraisse, AA Franceschi, E Galeotta, S Ganga, K Giard, M Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Gudmundsson, JE Haissinski, J Hansen, FK Hanson, D Harrison, D Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hou, Z Hovest, W Huffenberger, KM Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneiss, R Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leonardi, R Leroy, C Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF MacTavish, CJ Maffei, B Mandolesi, N Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matsumura, T Matthai, E Mazzotta, P McGehee, P Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, JA Naselsky, P Nati, E Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S Oxborrow, CA Paci, F Pagano, L Pajot, F Paoletti, D Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polegre, AM Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Roudier, G Rowan-Robinson, M Rusholme, B Sandri, M Santos, D Sauve, A Savini, G Scott, D Shellard, EPS Spencer, LD Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sureau, E Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Tavagnacco, D Terenzi, L Tomasi, M Tristram, M Tucci, M Umana, G Valenziano, L Valiviita, J Van Tent, B Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, E. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bock, J. J. Bond, J. R. Borrill, J. Bouchet, F. R. Bowyer, J. W. Bridges, M. Bucher, M. Burigana, C. Cardoso, J. -E Catalano, A. Challinor, A. Chamballu, A. Chary, R. -R. Chiang, H. C. Chiang, L. -Y Christensen, P. R. Church, S. Clements, D. L. Colombi, S. Colombo, L. P. L. Couchot, F. Coulais, A. Crill, B. P. Curto, A. Cuttaia, E. Danese, L. Davies, R. D. 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. Dunkley, J. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Fraisse, A. A. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Gudmundsson, J. E. Haissinski, J. Hansen, F. K. Hanson, D. Harrison, D. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hou, Z. Hovest, W. Huffenberger, K. M. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneiss, R. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leonardi, R. Leroy, C. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. MacTavish, C. J. Maffei, B. Mandolesi, N. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matsumura, T. Matthai, E. Mazzotta, P. McGehee, P. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, J. A. Naselsky, P. Nati, E. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Osborne, S. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paoletti, D. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polegre, A. M. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rowan-Robinson, M. Rusholme, B. Sandri, M. Santos, D. Sauve, A. Savini, G. Scott, D. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sureau, E. Sutton, D. Suur-Uski, A-S. Sygnet, J. -F. Tauber, J. A. Tavagnacco, D. Terenzi, L. Tomasi, M. Tristram, M. Tucci, M. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. VII. HFI time response and beams SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmic background radiation; cosmology: observations; instrumentation: detectors; surveys ID PRE-LAUNCH STATUS; POWER SPECTRUM; MAP-MAKING; MICROWAVE; CALIBRATION; PLANETS; CMB AB This paper characterizes the effective beams, the effective beam window functions and the associated errors for the Planck High Frequency Instrument (HFI) detectors. The effective beam is the angular response including the effect of the optics, detectors, data processing and the scan strategy. The window function is the representation of this beam in the harmonic domain which is required to recover an unbiased measurement of the cosmic microwave background angular power spectrum. The HFI is a scanning instrument and its effective beams are the convolution of: a) the optical response of the telescope and feeds; b) the processing of the time-ordered data and deconvolution of the bolometric and electronic transfer function; and c) the merging of several surveys to produce maps. The time response transfer functions are measured using observations of Jupiter and Saturn and by minimizing survey difference residuals. The scanning beam is the post-deconvolution angular response of the instrument, and is characterized with observations of Mars. The main beam solid angles are determined to better than 0.5% at each HFI frequency band. Observations of Jupiter and Saturn limit near sidelobes (within 5 degrees) to about 0.1% of the total solid angle. Time response residuals remain as long tails in the scanning beams, but contribute less than 0.1% of the total solid angle. The bias and uncertainty in the beam products are estimated using ensembles of simulated planet observations that include the impact of instrumental noise and known systematic effects. The correlation structure of these ensembles is well-described by five errors eigenmodes that are sub-dominant to sample variance and instrumental noise in the harmonic domain. A suite of consistency tests provide confidence that the error model represents a sufficient description of the data. The total error in the effective beam window functions is below 1% at 100 GHz up to multiple l similar to 1500, below 0.5% at 143 and 217 GHz up to l similar to 2000. C1 [Bucher, M.; Cardoso, J. -E; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Remazeilles, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, CNRS IN2P3,CEA lrfu,APC, F-75205 Paris 13, France. [Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Kunz, M.] African Inst Math Sci, Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana, Sci Data Ctr, I-00133 Rome, Italy. [Mandolesi, N.] Agenzia Spaziale Italiana, I-00198 Rome, Italy. [Ashdown, M.; Bridges, M.; Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa. [Kneiss, R.] ALMA Santiago Cent Off, Santiago 0355, Chile. [Bond, J. R.; Hanson, D.; Martin, P. G.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Leroy, C.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.; Sauve, A.] CNRS, TRAP, F-31028 Toulouse 4, France. [Bock, J. J.; Dore, O.; Hildebrandt, S. R.; Matsumura, T.; Prezeau, G.; Rocha, G.] CALTECH, Pasadena, CA 91125 USA. [Challinor, A.; Shellard, E. 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[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Colombo, L. P. L.; Pierpaoli, E.] Univ So Calif, Dept Phys & Astron, Dana & David Dornsife Coll Letter Arts & Sci, Los Angeles, CA 90089 USA. [Benoit-Levy, A.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Huffenberger, K. M.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Juvela, M.; Keihanen, E.; Kurki-Suonio, H.; Poutanen, T.; Suur-Uski, A-S.; Valiviita, J.] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland. [Chiang, H. C.; Fraisse, A. A.; Gudmundsson, J. E.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Hou, Z.; Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lubin, P. M.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wandelt, B. D.] Univ Illinois UrbanaChampaign, Dept Phys, Urbana, IL USA. [Liguori, M.; Matarrese, S.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. 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[Melchiorri, A.; Pagano, L.] Univ Roma La Sapienza, Ist Nazl Fis Nucl, Sez Roma 1, I-00185 Rome, Italy. [Desert, F. -X.; Ponthieu, N.] Univ Grenoble 1, CNRS INSU, UMR 5274, Inst Planetol & Astrophys Grenoble, F-38041 Grenoble, France. [Mitra, S.] IUCAA, Pune 411007, Maharashtra, India. [Bowyer, J. W.; Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England. [Chary, R. -R.; McGehee, P.; Rusholme, B.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, F-38042 Grenoble, France. [Dole, H.] Inst Univ France, F-75005 Paris, France. [Aghanim, N.; Aumont, J.; Chamballu, A.; Dole, H.; Douspis, M.; Kunz, M.; Lagache, G.; Leroy, C.; Miville-Deschenes, M. -A.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Remazeilles, M.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Cardoso, J. -E; Delouis, J. -M.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Popa, L.] Inst Space Sci, Bucharest 077125, Romania. [Chiang, L. -Y] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Bridges, M.; Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Migliaccio, M.; Sutton, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Eriksen, H. K.; Hansen, F. K.; Lilje, P. B.; Valiviita, J.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Barreiro, R. B.; Curto, A.; Diego, J. M.; Gonzalez-Nuevo, J.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain. [Bock, J. J.; Colombo, L. P. L.; Crill, B. P.; Dore, O.; Gorski, K. M.; Hanson, D.; Holmes, W. A.; Lawrence, C. R.; Mitra, S.; Pietrobon, D.; Prezeau, G.; Rocha, G.; Roudier, G.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Davies, R. D.; Maffei, B.; Noviello, F.; Remazeilles, M.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Bridges, M.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; MacTavish, C. J.; Migliaccio, M.; Stolyarov, V.; Sutton, D.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Couchot, F.; Haissinski, J.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.; Tucci, M.] Univ Paris 11, CNRS, IN2P3, LAL, F-91898 Orsay, France. [Catalano, A.; Coulais, A.; Lamarre, J. -M.; Roudier, G.] CNRS, Observ Paris, LERMA, F-75014 Paris, France. [Arnaud, M.; Bobin, J.; Chamballu, A.; Marshall, D. J.; Pratt, G. W.; Starck, J. -L.; Sureau, E.] Univ Paris Diderot, CNRS, CEA DSM, Lab AIM,IRFU Serv Astrophys, F-91191 Gif Sur Yvette, France. [Cardoso, J. -E] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris 13, France. [Cardoso, J. -E] Telecom Paris Tech, F-75634 Paris 13, France. [Catalano, A.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble 1, Inst Natl Polytech Grenoble, Lab Phys Subatom & Cosmol, CNRS IN2P3, F-38026 Grenoble, France. [Van Tent, B.] Univ Paris 11, Phys Theor Lab, F-91405 Orsay, France. [Van Tent, B.] CNRS, F-91405 Orsay, France. [Kisner, T. S.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Knoche, J.; Matthai, E.; Rachen, J. P.; Reinecke, M.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Hanson, D.] McGill Univ, McGill Phys, Montreal, PQ H3A 2T8, Canada. [Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Crill, B. P.] CALTECH, Observat Cosmol, Pasadena, CA 91125 USA. [Savini, G.] UCL, Opt Sci Lab, London, England. [Lesgourgues, J.] Ecole Polytech Fed Lausanne, SB ITP LPPC, CH-1015 Lausanne, Switzerland. [Baccigalupi, C.; Bielewicz, P.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Paci, F.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Ade, P. A. R.; Munshi, D.; Spencer, L. D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Karachai Cherkessian 369167, Russia. [Church, S.; Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA USA. [Armitage-Caplan, C.; Dunkley, J.] Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England. [Lesgourgues, J.] CERN, Div Theory, PH TH, CH-1211 Geneva 23, Switzerland. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Delouis, J. -M.; Hivon, E.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UMR7095, F-75014 Paris, France. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Leroy, C.; 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. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Crill, BP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM bcrill@jpl.nasa.gov RI Barreiro, Rita Belen/N-5442-2014; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; Remazeilles, Mathieu/N-1793-2015; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Martinez-Gonzalez, Enrique/E-9534-2015; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; OI Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; De Zotti, Gianfranco/0000-0003-2868-2595; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Vielva, Patricio/0000-0003-0051-272X; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794 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); MICINN (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); PRACE (EU) FX The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck-Collabora tion. NR 68 TC 57 Z9 56 U1 3 U2 11 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2014 VL 571 AR A7 DI 10.1051/0004-6361/201321535 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600010 ER PT J AU Ade, PAR Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, E Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartlett, JG Basak, S Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bock, JJ Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Bridges, M Bucher, M Burigana, C Butler, RC Cardoso, JF Catalano, A Challinor, A Chamballu, A Chiang, HC Chiang, LY Christensen, PR Church, S Clements, DL Colombi, S Colombo, LPL 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 Dechelette, T Delabrouille, J Delouis, JM Desert, FX Dickinson, C Diego, JM Dole, H Donzelli, S Dore, O Douspis, M Dunkley, J Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Gudmundsson, JE Hansen, EK Hanson, D Harrison, D Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Ho, S Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lavabre, A Lawrence, CR Leahy, JP Leonardi, R Leon-Tavares, J Lesgourgues, J Lewis, A Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Mangilli, A Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, E Mazzotta, P 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 Osborne, S Oxborrow, CA Paci, F Pagano, L Pajot, F Paoletti, D Partridge, B Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeaul, G Prunet, S Puget, JL Pullen, AR Rachen, JP Rebolo, R Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Roudier, G Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savini, G Scott, D Seiffert, MD Shellard, EPS Smith, K Spencer, LD Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sunyaev, R Sureau, E Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Tavagnacco, D Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Tuovinen, J Umana, G Valenziano, L Valiviita, J Van Tent, B Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD White, M White, SDM Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, E. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Basak, S. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bock, J. J. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Bridges, M. Bucher, M. Burigana, C. Butler, R. C. Cardoso, J. -F. Catalano, A. Challinor, A. Chamballu, A. Chiang, H. C. Chiang, L. -Y Christensen, P. R. Church, S. Clements, D. L. Colombi, S. Colombo, L. P. L. 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. Dechelette, T. Delabrouille, J. Delouis, J. -M. Desert, F. -X. Dickinson, C. Diego, J. M. Dole, H. Donzelli, S. Dore, O. Douspis, M. Dunkley, J. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Gudmundsson, J. E. Hansen, F. K. Hanson, D. Harrison, D. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Ho, S. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lavabre, A. Lawrence, C. R. Leahy, J. P. Leonardi, R. Leon-Tavares, J. Lesgourgues, J. Lewis, A. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Mangilli, A. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. 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. Osborne, S. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paoletti, D. Partridge, B. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeaul, G. Prunet, S. Puget, J. -L. Pullen, A. R. Rachen, J. P. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Smith, K. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sunyaev, R. Sureau, E. 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. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. White, M. White, S. D. M. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. XVII. Gravitational lensing by large-scale structure SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gravitational lensing: weak; methods: data analysis; cosmic background radiation; large-scale structure of Universe ID MICROWAVE BACKGROUND ANISOTROPIES; SOUTH-POLE TELESCOPE; PROBE WMAP OBSERVATIONS; DIGITAL SKY SURVEY; POWER SPECTRUM; CROSS-CORRELATION; GALAXY CLUSTERS; NON-GAUSSIANITY; DAMPING TAIL; MAPS AB On the arcminute angular scales probed by Planck, the cosmic microwave background (CMB) anisotropies are gently perturbed by gravitational lensing. Here we present a detailed study of this effect, detecting lensing independently in the 100, 143, and 217 GHz frequency bands with an overall significance of greater than 25 sigma. We use the temperature-gradient correlations induced by lensing to reconstruct a (noisy) map of the CMB lensing potential, which provides an integrated measure of the mass distribution back to the CMB last-scattering surface. Our lensing potential map is significantly correlated with other tracers of mass, a fact which we demonstrate using several representative tracers of large-scale structure. We estimate the power spectrum of the lensing potential, finding generally good agreement with expectations from the best-fitting ACDM model for the Planck temperature power spectrum, showing that this measurement at z = 1100 correctly predicts the properties of the lower-redshift, later-time structures which source the lensing potential. When combined with the temperature power spectrum, our measurement provides degeneracy-breaking power for parameter constraints; it improves CMB-alone constraints on curvature by a factor of two and also partly breaks the degeneracy between the amplitude of the primordial perturbation power spectrum and the optical depth to reionization, allowing a measurement of the optical depth to reionization which is independent of large-scale polarization data. Discarding scale information, our measurement corresponds to a 4% constraint on the amplitude of the lensing potential power spectrum, or a 2% constraint on the root-mean-squared amplitude of matter fluctuations at z similar to 2. 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, Observ Paris, Sorbonne Paris Cite, CNRS,IN2P3,CEA,lrfu,APC, F-75205 Paris 13, France. [Lahteenmaki, A.; Leon-Tavares, J.; Poutanen, T.] Aalto Univ Metsahovi Radio Observ, Kylmala 02540, Finland. [Kunz, M.] African Inst Math Sci, Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy. [Mandolesi, N.] Agenzia Spaziale Italiana, Rome, Italy. [Ashdown, M.; Bridges, M.; Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa. [Kneissl, R.] Atacama Large Millimeter Submillimeter Array, ALMA Santiago Cent Off, Santiago 7630355, Chile. [Bond, J. R.; Hanson, D.; Martin, P. G.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, 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, F-31028 Toulouse 4, France. [Bock, J. J.; Dore, O.; Hildebrandt, S. R.; Prezeaul, G.; Rocha, G.; Seiffert, M. D.] CALTECH, Pasadena, CA 91125 USA. [Challinor, A.; Shellard, E. P. S.] Univ Cambridge, Ctr Theoret Cosmol, DAMTP, Cambridge CB3 0WA, England. [Hernandez-Monteagudo, C.] Ctr Estudios Fis Cosmos Aragon, Teruel 44001, Spain. [Borrill, J.; Keskitalo, R.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Rebolo, R.] CSIC, Madrid, Spain. [Chamballu, A.; Yvon, D.] CEA Saclay, DMS, SPP, Irfu, 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, DK-2800 Lyngby, Denmark. [Kunz, M.; Tucci, M.] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland. [Atrio-Barandela, E.] Univ Salamanca, Dept Fis Fundamental, Fac Ciencias, E-37008 Salamanca, Spain. [Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain. [Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada. [Rachen, J. P.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Keskitalo, R.] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Colombo, L. P. L.; Pierpaoli, E.] Univ So Calif, Dept Phys & Astron, Dana & David Dornsife Coll Letter Arts & Sci, Los Angeles, CA 90089 USA. [Benoit-Levy, A.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Lewis, A.] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Ho, S.] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Huffenberger, K. M.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Juvela, M.; Keihanen, E.; Kurki-Suonio, H.; Poutanen, T.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Dept Phys, Helsinki, Finland. [Chiang, H. C.; Gudmundsson, J. E.; Jones, W. 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EM benabed@iap.fr; dhanson@physics.mcgill.ca RI Butler, Reginald/N-4647-2015; Remazeilles, Mathieu/N-1793-2015; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; bonavera, laura/E-9368-2017; White, Martin/I-3880-2015; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Martinez-Gonzalez, Enrique/E-9534-2015; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Pullen, Anthony/I-7007-2015; Barreiro, Rita Belen/N-5442-2014; OI Galeotta, Samuele/0000-0002-3748-5115; Frailis, Marco/0000-0002-7400-2135; De Zotti, Gianfranco/0000-0003-2868-2595; Polenta, Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996; Lopez-Caniego, Marcos/0000-0003-1016-9283; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; bonavera, laura/0000-0001-8039-3876; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Maris, Michele/0000-0001-9442-2754; White, Martin/0000-0001-9912-5070; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Pullen, Anthony/0000-0002-2091-8738; Pierpaoli, Elena/0000-0002-7957-8993; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Gregorio, Anna/0000-0003-4028-8785; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840 FU ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); INAF (Italy); CNR (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MICINN (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); PRACE (EU); Office of Science of the US Department of Energy [DE-AC02-05CH11231]; IN2P3 Computer Center; CNES; Science and Technology Facilities Council [ST/I000976/1] FX The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.soirees.esa.int/index.php?project=planck&pagess-Planck_Collab oration. Some of the results in this paper have been derived using the HEALPix package (Gorski et al. 2005). This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the US Department of Energy under Contract No. DE-AC02-05CH11231, as well as of the IN2P3 Computer Center (http://cc.in2p3.fr) and the Planck-HFI data processing center infrastructures hosted at the Institut d'Astrophysique de Paris (France) and financially supported by CNES. We acknowledge support from the Science and Technology Facilities Council [grant number ST/I000976/1]. NR 120 TC 198 Z9 197 U1 4 U2 20 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2014 VL 571 AR A17 DI 10.1051/0004-6361/201321543 PG 39 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600013 ER PT J AU Ade, PAR Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandelals, E Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartlett, JG Bartlett, JG Bartolo, N Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bock, JJ Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Bridges, M Bucher, M Burigana, C Butler, RC Cardoso, JF Catalano, A Challinor, A Chamballu, A Chiang, HC Chiang, LY Christensen, PR Church, S Clements, DL Colombi, S Colombo, LPL Couchot, E Coulais, A Crill, BP Curto, A Cuttaia, E 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 Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Fergusson, J Finelli, F Fomi, O Fosalba, P Frailis, M Franceschi, E Frommert, M Galeotta, S Ganga, K Genova-Santos, RT Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, EK Hanson, D Harrison, D Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Ho, S Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Ilic, S Jaffe, AH Jaffe, TR Jasche, J Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Langer, M Lasenby, A Laureijs, RJ Lawrence, CR Leahy, JP Leonardi, R Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Mangilli, A Marcos-Caballero, A Maris, M Marshall, DJ Martins, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthais, E Mazzotta, 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 Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S Oxborrow, CA Paci, E Pagano, L Pajot, F Paoletti, D Partridge, B Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Racine, B Rebolo, R Reinecke, M Remazeilles, M Renault, C Renzi, A Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Roudier, G Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savini, G Schaefer, BM Schiavon, F Scott, D Seiffert, MD Shellard, EPS Spencer, LD Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sunyaev, R Sureau, F Sutter, P Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Tavagnacco, D Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Tuovinen, J Umana, G Valenziano, L Valiviita, J Van Tent, B Varis, J Viel, M Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD White, M Xia, JQ Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandelals, E. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Bartlett, J. G. Bartolo, N. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bock, J. J. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Bridges, M. Bucher, M. Burigana, C. Butler, R. C. Cardoso, J. -F. Catalano, A. Challinor, A. Chamballu, A. Chiang, H. C. Chiang, L. -Y. Christensen, P. R. Church, S. Clements, D. L. Colombi, S. Colombo, L. P. L. Couchot, E. Coulais, A. Crill, B. P. Curto, A. Cuttaia, E. 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. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Fergusson, J. Finelli, F. Fomi, O. Fosalba, P. Frailis, M. Franceschi, E. Frommert, M. Galeotta, S. Ganga, K. Genova-Santos, R. T. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, E. K. Hanson, D. Harrison, D. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Ho, S. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Ilic, S. Jaffe, A. H. Jaffe, T. R. Jasche, J. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Laehteenmaeki, A. Lamarre, J. -M. Langer, M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leahy, J. P. Leonardi, R. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Mangilli, A. Marcos-Caballero, A. Maris, M. Marshall, D. J. Martins, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthais, E. Mazzotta, 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. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Osborne, S. Oxborrow, C. A. Paci, E. Pagano, L. Pajot, F. Paoletti, D. Partridge, B. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Racine, B. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Renzi, A. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savini, G. Schaefer, B. M. Schiavon, F. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sunyaev, R. Sureau, F. Sutter, P. 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. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Varis, J. Viel, M. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. White, M. Xia, J. -Q. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. XIX. The integrated Sachs-Wolfe effect SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmic background radiation; large-scale structure of Universe; dark energy; galaxies: clusters: general; methods: data analysis ID DIGITAL SKY SURVEY; PRIMORDIAL NON-GAUSSIANITY; DARK ENERGY CONSTRAINTS; PROBE WMAP OBSERVATIONS; ANGULAR POWER SPECTRUM; CROSS-CORRELATION; RADIO-SOURCES; SPHERICAL WAVELETS; GALAXY SURVEY; DATA RELEASE AB Based on cosmic microwave background (CMB) maps from the 2013 Planck Mission data release, this paper presents the detection of the integrated Sachs-Wolfe (ISW) effect, that is, the correlation between the CMB and large-scale evolving gravitational potentials. The significance of detection ranges from 2 to 4 sigma, depending on which method is used. We investigated three separate approaches, which essentially cover all previous studies, and also break new ground. (i) We correlated the CMB with the Planck reconstructed gravitational lensing potential (for the first time). This detection was made using the lensing-induced bispectrum between the low-l and high-l temperature anisotropies; the correlation between lensing and the ISW effect has a significance close to 2.5 sigma. (ii) We cross-correlated with tracers of large-scale structure, which yielded a significance of about 3 sigma, based on a combination of radio (NVSS) and optical (SDSS) data. (iii) We used aperture photometry on stacked CMB fields at the locations of known large-scale structures, which yielded and confirms a 4 sigma signal, over a broader spectral range, when using a previously explored catalogue, but shows strong discrepancies in amplitude and scale when compared with expectations. More recent catalogues give more moderate results that range from negligible to 2.5 sigma at most, but have a more consistent scale and amplitude, the latter being still slightly higher than what is expected from numerical simulations within Lambda CMD. Where they can be compared, these measurements are compatible with previous work using data from WMAP, where these scales have been mapped to the limits of cosmic variance. Planck's broader frequency coverage allows for better foreground cleaning and confirms that the signal is achromatic, which makes it preferable for ISW detection. As a final step we used tracers of large-scale structure to filter the CMB data, from which we present maps of the ISW temperature perturbation. These results provide complementary and independent evidence for the existence of a dark energy component that governs the currently accelerated expansion of the Universe. C1 [Bartlett, J. 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[Schaefer, B. M.] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Barreiro, R. B.; Bernard, J. -P.; Bielewicz, P.; Fomi, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse, France. [Dolag, K.] Univ Munich, Univ Observ, D-81679 Munich, Germany. [Battaner, E.] Univ Granada, Dept Fis Teor & Cosmos, Granada 18071, Spain. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Vielva, P (reprint author), Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain. EM vielva@ifca.unican.es RI Remazeilles, Mathieu/N-1793-2015; Renzi, Alessandro/K-4114-2015; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Fosalba Vela, Pablo/I-5515-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; bonavera, laura/E-9368-2017; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Langer, Mathieu/C-5100-2013; Martinez-Gonzalez, Enrique/E-9534-2015; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; White, Martin/I-3880-2015; Gruppuso, Alessandro/N-5592-2015; Butler, Reginald/N-4647-2015; Barreiro, Rita Belen/N-5442-2014; OI Pierpaoli, Elena/0000-0002-7957-8993; Masi, Silvia/0000-0001-5105-1439; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; De Zotti, Gianfranco/0000-0003-2868-2595; Lopez-Caniego, Marcos/0000-0003-1016-9283; Scott, Douglas/0000-0002-6878-9840; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Renzi, Alessandro/0000-0001-9856-1970; Franceschi, Enrico/0000-0002-0585-6591; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; bonavera, laura/0000-0001-8039-3876; de Bernardis, Paolo/0000-0001-6547-6446; Valiviita, Jussi/0000-0001-6225-3693; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; Langer, Mathieu/0000-0002-9088-2718; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; White, Martin/0000-0001-9912-5070; Gruppuso, Alessandro/0000-0001-9272-5292; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Viel, Matteo/0000-0002-2642-5707; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Frailis, Marco/0000-0002-7400-2135 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); MICINN (Spain); J.A. (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); PRACE (EU); Advanced Computing and e-Sciance team at IFCA FX The development of Planck has been supported by: ESA; CNES and CNRS/INSU- IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, J.A. 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); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found athttp://www.sciops.esa.int/index.php?project=planck&page=Planck_Collabo ration. The modal and KSW bispectrum estimator analysis was performed on the COSMOS supercomputer, part of the STFC DiRAC HPC Facility. We acknowledge the computer resources, technical expertise and assistance provided by the Spanish Supercomputing Network (RES) node at Universidad de Cantarbria, and the support provided by the Advanced Computing and e-Sciance team at IFCA. NR 133 TC 105 Z9 104 U1 5 U2 13 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2014 VL 571 AR A19 DI 10.1051/0004-6361/201321526 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600005 ER PT J AU Ade, PAR Aghanim, N Argueso, F Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Beelen, A Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bock, JJ Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Bridges, M Bucher, M Burigana, C Butler, RC Cardoso, JF Carvalho, P Catalano, A Challinor, A Chamballu, A Chen, X Chiang, HC Chiang, LY Christensen, PR Church, S Clemens, M Clements, DL Colombi, S Colombo, LPL 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 Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK 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 Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Kneissl, R Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leahy, JP Leonardi, R Leon-Tavares, J Leroy, C Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P 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 Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Negrello, M Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I O'Dwyer, IJ Osborne, S 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 Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Reach, WT Rebolo, R Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Roudier, G Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savini, G Scott, D Seiffert, MD Shellard, EPS Spencer, LD Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sunyaev, R Sureau, F 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 Varis, J Vielva, P Villa, F Vittorio, N Wade, LA Walter, B Wandelt, BD Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Argueeso, F. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Beelen, A. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bock, J. J. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Bridges, M. Bucher, M. Burigana, C. Butler, R. C. Cardoso, J. -F. Carvalho, P. Catalano, A. Challinor, A. Chamballu, A. Chen, X. Chiang, H. C. Chiang, L. -Y Christensen, P. R. Church, S. Clemens, M. Clements, D. L. Colombi, S. Colombo, L. P. L. 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. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. 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. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneissl, R. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leahy, J. P. Leonardi, R. Leon-Tavares, J. Leroy, C. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. 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. 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. O'Dwyer, I. J. Osborne, S. 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. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Reach, W. T. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sunyaev, R. Sureau, F. 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. Tuerler, M. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Varis, J. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Walter, B. Wandelt, B. D. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. XXVIII. The Planck Catalogue of Compact Sources SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology: observations; radio continuum: general; submillimeter: general ID COEVAL OBSERVATIONS PROJECT; EXTRAGALACTIC POINT SOURCES; MICROWAVE BACKGROUND MAPS; STAR-FORMING GALAXIES; HERSCHEL-ATLAS; RADIO-SOURCES; NEARBY GALAXIES; NUMBER COUNTS; SAMPLE; RELEASE AB The Planck Catalogue of Compact Sources (PCCS) is the catalogue of sources detected in the first 15 months of Planck operations, the "nominal" mission. It consists of nine single-frequency catalogues of compact sources, both Galactic and extragalactic, detected over the entire sky. The PCCS covers the frequency range 30-857 GHz with higher sensitivity (it is 90% complete at 180 mJy in the best channel) and better angular resolution (from 32.88' to 4.33') than previous all-sky surveys in this frequency band. By construction its reliability is >80% and more than 65% of the sources have been detected in at least two contiguous Planck channels. In this paper we present the construction and validation of the PCCS, its contents and its statistical characterization. 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.] Sorbonne Paris Cite, Univ Paris Diderot, Observ Paris, CNRS IN2P3 CEA lrfu,APC, F-75205 Paris 13, France. [Lahteenmaki, A.; Leon-Tavares, J.; Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Aalto 00076, Finland. [Lahteenmaki, A.; Leon-Tavares, J.; Poutanen, T.] Dept Radio Sci & Engn, Aalto 00076, Finland. 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[Kisner, T. S.] CNRS, F-91405 Orsay, France. [Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Knoche, J.; Matthai, F.; Rachen, J. P.; Reinecke, M.; Riller, T.; Sunyaev, R.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Hanson, D.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Tuovinen, J.; Varis, J.] McGill Univ, Montreal, PQ H3A 2T8, Canada. [Tuovinen, J.; Varis, J.] VTT Tech Res Ctr Finland, Milli Lab, Espoo 02044, Finland. [Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Crill, B. P.] CALTECH, Observ Cosmol, Pasadena, CA 91125 USA. [Savini, G.] UCL, Opt Sci Lab, London, England. [Lesgourgues, J.] Ecole Polytech Fed Lausanne, SB ITP LPPC, CH-1015 Lausanne, Switzerland. [Baccigalupi, C.; Bobin, J.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Paci, F.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Ade, P. A. R.; Munshi, D.; Spencer, L. D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Sunyaev, R.] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz 369167, Russia. [Church, S.; Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Armitage-Caplan, C.] Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England. [Lesgourgues, J.] CERN, PH TH, Div Theory, CH-1211 Geneva 23, Switzerland. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UMR7095, F-75014 Paris, France. [Banday, A. J.; Beelen, A.; Bernard, J. -P.; Bobin, J.; Forni, O.; Giard, M.; Jaffe, T. R.; Leroy, C.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, E-18071 Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Gonzalez-Nuevo, J (reprint author), Univ Cantabria, CSIC, Inst Fis Cantabria, Avda Castros S-N, E-39005 Santander, Spain. EM gnuevo@ifca.unican.es RI Barreiro, Rita Belen/N-5442-2014; Remazeilles, Mathieu/N-1793-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; bonavera, laura/E-9368-2017; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Pearson, Timothy/N-2376-2015; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Martinez-Gonzalez, Enrique/E-9534-2015; Butler, Reginald/N-4647-2015; OI Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; bonavera, laura/0000-0001-8039-3876; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; De Zotti, Gianfranco/0000-0003-2868-2595; Pierpaoli, Elena/0000-0002-7957-8993; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Pearson, Timothy/0000-0001-5213-6231; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Reach, William/0000-0001-8362-4094; Butler, Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043 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); MICINN (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); PRACE (EU) FX The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collabora tion. This research has made use of Aladin. We are deeply grateful to Rick Perley and the U.S. National Radio Astronomy Observatory for participating in the joint Planck-VLA observations. We also thank Steve Eales and the H-ATLAS team (Eales et al, 2010 PASP 122 499E) for sharing their SPIRE catalogs prior to publication, allowing a comparison of flux densities between HFI and SPIRE. NR 91 TC 77 Z9 76 U1 3 U2 9 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2014 VL 571 AR A28 DI 10.1051/0004-6361/201321524 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600004 ER PT J AU Ade, PAR Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bock, JJ Bond, JR Bonrrill, J Bouchet, FR Boulanger, F Bridges, M Bucher, M Burigana, C Cardoso, JF Catalano, A Challinor, A Chamballu, A Chary, RR Chen, X Chiang, HC Chiang, LY 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 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 Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Falgarone, E Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Ciard, M Giraud-Heraud, Y Gonzadlez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Hanson, D Harrison, D 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 Kneiss, R Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leahy, JP Leonardi, R Leroy, C Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Mandolesi, N Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P McGehee, P Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU North, C Noviello, F Novikov, D Novikov, I Osborne, S Oxborrow, CA Paci, F Pagano, L Pajot, F Paoletti, D Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Roudier, G Rusholme, B Santos, D Savini, G Scott, D Shellard, EPS Spencer, LD Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sureau, F Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Tavagnacco, D Terenzi, L Tomasi, M Tristram, M Tucci, M Umana, G Valenziano, L Valiviita, J Van Tent, B Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bock, J. J. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bridges, M. Bucher, M. Burigana, C. Cardoso, J. -F. Catalano, A. Challinor, A. Chamballu, A. Chary, R. -R. Chen, X. Chiang, H. C. Chiang, L. -Y 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. 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. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Falgarone, E. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Ciard, M. Giraud-Heraud, Y. Gonzadlez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Hanson, D. Harrison, D. 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. Kneiss, R. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leahy, J. P. Leonardi, R. Leroy, C. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Mandolesi, N. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. McGehee, P. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. North, C. Noviello, F. Novikov, D. Novikov, I. Osborne, S. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paoletti, D. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rusholme, B. Santos, D. Savini, G. Scott, D. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sureau, F. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Tavagnacco, D. Terenzi, L. Tomasi, M. Tristram, M. Tucci, M. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. IX. HFI spectral response SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE instrumentation: detectors; instrumentation: photometers; space vehicles: instruments; cosmology: observations; cosmic background radiation ID HIGH-FREQUENCY INSTRUMENT; COBE FIRAS INSTRUMENT; MOLECULAR CLOUDS; MICROWAVE; SPECTROSCOPY; CALIBRATION AB The Planck High Frequency Instrument (HFI) spectral response was determined through a series of ground based tests conducted with the HFI focal plane in a cryogenic environment prior to launch. The main goal of the spectral transmission tests was to measure the relative spectral response (including the level of out-of-band signal rejection) of all HFI detectors to a known source of electromagnetic radiation individually. This was determined by measuring the interferometric output of a continuously scanned Fourier transform spectrometer with all HFI detectors. As there is no on-board spectrometer within HFI, the ground-based spectral response experiments provide the definitive data set for the relative spectral calibration of the HFI. Knowledge of the relative variations in the spectral response between HFI detectors allows for a more thorough analysis of the HFI data. The spectral response of the HFI is used in Planck data analysis and component separation, this includes extraction of CO emission observed within Planck bands, dust emission, Sunyaev-Zeldovich sources, and intensity to polarization leakage. The HFI spectral response data have also been used to provide unit conversion and colour correction analysis tools. While previous papers describe the pre-flight experiments conducted on the Planck HFI, this paper focusses on the analysis of the pre-flight spectral response measurements and the derivation of data products, e.g. band-average spectra, unit conversion coefficients, and colour correction coefficients, all with related uncertainties. Verifications of the HFI spectral response data are provided through comparisons with photometric HFI flight data. This validation includes use of HFI zodiacal emission observations to demonstrate out-of-band spectral signal rejection better than 10(8). The accuracy of the HFI relative spectral response data is verified through comparison with complementary flight-data based unit conversion coefficients and colour correction coefficients. These coefficients include those based upon HFI observations of CO, dust, and Sunyaev-Zeldovich emission. General agreement is observed between the ground-based spectral characterization of HFI and corresponding in-flight observations, within the quoted uncertainty of each; explanations are provided for any discrepancies. 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, Observ Paris, Sorbonne Paris Cite, CNRS IN2P3,CEA lrfu,APC, F-75205 Paris 13, France. [Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Kunz, M.] African Inst Math Sci, ZA-7701 Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci, Ctr Data, I-00133 Rome, Italy. [Mandolesi, N.] Agenzia Spaziale Italiana, Rome, Italy. [Ashdown, M.; Bridges, M.; Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 OHE, England. [Chiang, H. 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[Battaner, E.] Univ Toulouse, UPS OMP, TRAP, F-31028 Toulouse 4, France. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, E-18071 Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, Warsaw, Poland. RP Spencer, LD (reprint author), Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales. EM Locke.Spencer@astro.cf.ac.uk RI Barreiro, Rita Belen/N-5442-2014; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; Remazeilles, Mathieu/N-1793-2015; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Martinez-Gonzalez, Enrique/E-9534-2015; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; OI Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; De Zotti, Gianfranco/0000-0003-2868-2595; Lopez-Caniego, Marcos/0000-0003-1016-9283; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Vielva, Patricio/0000-0003-0051-272X; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Hurier, Guillaume/0000-0002-1215-0706; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796 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); MICINN (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); PRACE (EU); NSERC (Canada) FX The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collabora tion. The authors thank Emmanuel Lellouch, Raphael Moreno, and Matt Griffin for the provision of the planet model spectra used to generate HFI planet colour correction coefficients. L. Spencer acknowledges support from NSERC (Canada) and STFC (UK). NR 70 TC 60 Z9 59 U1 3 U2 11 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2014 VL 571 AR A9 DI 10.1051/0004-6361/201321531 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600008 ER PT J AU Ade, PAR Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Aussel, H Baccigalupi, C Banday, AJ Barreiro, RB Barrena, R Bartelinann, M Bartlett, JG Battaner, E Benabed, K Benoit, A Benoit-Ley, A Bernard, J Bersanelli, M Bielewicz, P Bikmaev, I Bobin, J Bock, JJ Bohringer, H Bonaldi, A Bond, JR Borrill, J Bouchet, FR Bridges, M Bucher, M Burenin, R Burigana, C Butier, RC Cardoso, JF Carvalho, P Catalano, A Challinor, A Chamballu, A Chary, RR Chen, X Chiang, HC Chiang, LY Chon, G Christensen, PR Churazov, E Church, S Clements, DL Colombi, S Colombo, LPL Comis, B Couchot, F Coulais, A Crill, BP Curto, A Cuttaia, F Da Silva, A Dahle, H Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouilie, J Delouis, JM Democles, J Desert, FX Dickinson, C Diego, IM Dolag, K Dole, H Donzelli, S Dore, O Douspis, M Dupac, X Efstathiou, G Eisenhardt, PRM Ensslin, TA Eriksen, HK Feroz, F Finelli, F Flores-Cacho, I Forni, O Frailis, M Franceschi, E Fromenteau, S Galeotta, S Ganga, K Genova-Santos, RT Giard, M Giardino, G Gilfanov, M Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Grainge, KJB Gratton, S Gregorio, A Groeneboom, NE Gruppuso, A Hansen, FK Hanson, D Harrison, D Hempel, A Elenrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Homstrup, A Hovest, W Huffenberger, KM Hurier, G Hurley-Walker, N Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihanen, E Keskitalo, R Khamitov, I Kisner, TS Kneissl, R Knoche, J Knox, L Kunz, M Kurki-Suonio, H Laeache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leahy, JP Leonardi, R Leon-Tavares, J Lesgourgues, J Li, C Liddle, A Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF MacTavish, CJ Maffei, B Maino, D Mandolesi, N Maris, M Marshal, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P Mei, S Meinhold, PR Meichiorri, A Melin, JB Mendes, L Mennelia, A Migliaccio, M Mikkeisen, K Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Nesvadba, NPH Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novilov, I O'Dwyer, IJ Olamaie, M Osborne, S Oxborrow, CA Paci, F Pagano, L Pajot, F Paoletti, D Pasian, F Patanchon, G Pearson, TJ Perdereau, O Perotto, L Perrott, YC Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pletrobon, D Plaszczynski, S Pointecouteau, E Polenta, O Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Reach, WT Rebolo, R Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Roudier, G Rowan-Robinson, M Rubino-Martin, JA Rumsey, C Rusholme, B Sandri, M Santos, D Saunders, RDE Savini, G Schammel, MP Scott, D Seiffert, MD Shellard, EPS Shimwell, TW Spencer, LD Stanford, SA Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sunyaev, R Sureau, F 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 Vibert, L Vielva, P Vilia, F Vittorio, N Wade, LA Wandelt, BD White, M White, SDM Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Aussel, H. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Barrena, R. Bartelinann, M. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. . Bersanelli, M. Bielewicz, P. Bikmaev, I. Bobin, J. Bock, J. J. Boehringer, H. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Bridges, M. Bucher, M. Burenin, R. Burigana, C. Butier, R. C. Cardoso, J. -F. Carvalho, P. Catalano, A. Challinor, A. Chamballu, A. Chary, R. -R. Chen, X. Chiang, H. C. Chiang, L. -Y. Chon, G. Christensen, P. R. Churazov, E. Church, S. Clements, D. L. Colombi, S. Colombo, L. P. L. Comis, B. Couchot, F. Coulais, A. Crill, B. P. Curto, A. Cuttaia, F. Da Silva, A. Dahle, H. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouilie, J. Delouis, J. -M. Democles, J. Desert, F. -X. Dickinson, C. Diego, I. M. Dolag, K. Dole, H. Donzelli, S. Dore, O. Douspis, M. Dupac, X. Efstathiou, G. Eisenhardt, P. R. M. Ensslin, T. A. Eriksen, H. K. Feroz, F. Finelli, F. Flores-Cacho, I. Forni, O. Frailis, M. Franceschi, E. Fromenteau, S. Galeotta, S. Ganga, K. Genova-Santos, R. T. Giard, M. Giardino, G. Gilfanov, M. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Grainge, K. J. B. Gratton, S. Gregorio, A. Groeneboom, N. E. Gruppuso, A. Hansen, F. K. Hanson, D. Harrison, D. Hempel, A. Elenrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Homstrup, A. Hovest, W. Huffenberger, K. M. Hurier, G. Hurley-Walker, N. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Khamitov, I. Kisner, T. S. Kneissl, R. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Laeache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leahy, J. P. Leonardi, R. Leon-Tavares, J. Lesgourgues, J. Li, C. Liddle, A. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. MacTavish, C. J. Maffei, B. Maino, D. Mandolesi, N. Maris, M. Marshal, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. Mei, S. Meinhold, P. R. Meichiorri, A. Melin, J. -B. Mendes, L. Mennelia, A. Migliaccio, M. Mikkeisen, K. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Nesvadba, N. P. H. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novilov, I. O'Dwyer, I. J. Olamaie, M. Osborne, S. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paoletti, D. Pasian, F. Patanchon, G. Pearson, T. J. Perdereau, O. Perotto, L. Perrott, Y. C. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pletrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, O. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Reach, W. T. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rowan-Robinson, M. Rubino-Martin, J. A. Rumsey, C. Rusholme, B. Sandri, M. Santos, D. Saunders, R. D. E. Savini, G. Schammel, M. P. Scott, D. Seiffert, M. D. Shellard, E. P. S. Shimwell, T. W. Spencer, L. D. Stanford, S. A. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sunyaev, R. Sureau, F. 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. Tuerler, M. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Vibert, L. Vielva, P. Vilia, F. Vittorio, N. Wade, L. A. Wandelt, B. D. White, M. White, S. D. M. Yvon, D. Zacchei, A. Zonca, A. TI Planck 2013 results. XXIX. The Planck catalogue of Sunyaev-Zeldovich sources SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE large-scale structure of Universe; galaxies: clusters: general; catalogs ID GALAXY CLUSTER SURVEY; SOUTH-POLE TELESCOPE; DIGITAL SKY SURVEY; X-RAY-PROPERTIES; LUMINOSITY-TEMPERATURE RELATION; MICROWAVE BACKGROUND-RADIATION; ARCMINUTE MICROKELVIN IMAGER; DISCRETE OBJECT DETECTION; ADAPTIVE MATCHED-FILTER; ASTRONOMICAL DATA SETS AB We describe the all-sky Planck catalogue of clusters and cluster candidates derived from Sunyaev-Zeldovich (SZ) effect detections using the first 15.5 months of Planck satellite observations. The catalogue contains 1227 entries, making it over six times the size of the Planck Early SZ (ESZ) sample and the largest SZ-selected catalogue to date. It contains 861 confirmed clusters, of which 178 have been confirmed as clusters, mostly through follow-up observations, and a further 683 are previously-known clusters. The remaining 366 have the status of cluster candidates, and we divide them into three classes according to the quality of evidence that they are likely to be true clusters. The Planck SZ catalogue is the deepest all-sky cluster catalogue, with redshifts up to about one, and spans the broadest cluster mass range from (0.1 to 1.6) x 10(15) M-circle dot. Confirmation of cluster candidates through comparison with existing surveys or cluster catalogues is extensively described, as is the statistical characterization of the catalogue in terms of completeness and statistical reliability. The outputs of the validation process are provided as additional information. This gives, in particular, an ensemble of 813 cluster redshifts, and for all these Planck clusters we also include a mass estimated from a newly-proposed SZ-mass proxy. 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EM nabila.aghanim@ias.u-psud.fr RI Barreiro, Rita Belen/N-5442-2014; Remazeilles, Mathieu/N-1793-2015; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; Martinez-Gonzalez, Enrique/E-9534-2015; Churazov, Eugene/A-7783-2013; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; White, Martin/I-3880-2015; Pearson, Timothy/N-2376-2015; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Hurley-Walker, Natasha/B-9520-2013; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Butler, Reginald/N-4647-2015; OI Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; De Zotti, Gianfranco/0000-0003-2868-2595; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; White, Martin/0000-0001-9912-5070; Pearson, Timothy/0000-0001-5213-6231; Gruppuso, Alessandro/0000-0001-9272-5292; Hurley-Walker, Natasha/0000-0002-5119-4808; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; Hurier, Guillaume/0000-0002-1215-0706; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Reach, William/0000-0001-8362-4094; Butler, Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924 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); MICINN (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); PRACE (EU); BTA 6-m telescope Time Allocation Committee (TAC); CCI International Time Programme; Alfred P. Sloan Foundation; Participating Institutions; National Science Foundation; DoE; NASA; CNES; CNRS FX The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collabora tion. The authors thank N. Schartel, ESA XMM-Newton project scientist, for granting the Director Discretionary Time used for confirmation of SZ Planck candidates. The authors thank TUBITAK, IKI, KFU and AST for support in using RTT150 (Russian-Turkish 1.5-m telescope, Bakyrlytepe, Turkey); in particular we thank KFU and IKI for providing significant amount of their observing time at RTT150. We also thank BTA 6-m telescope Time Allocation Committee (TAC) for support of optical follow-up project. The authors acknowledge the use of the INT and WHT telescopes operated on the island of La Palma by the Isaac Newton Group of Telescopes at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias (IAC); the Nordic Optical Telescope, operated on La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, at the Spanish Observatorio del Roque de los Muchachos of the IAC; the TNG telescope, operated on La Palma by the Fundacion Galileo Galilei of the INAF at the Spanish Observatorio del Roque de los Muchachos of the IAC; the GTC telescope, operated on La Palma by the IAC at the Spanish Observatorio del Roque de los Muchachos of the IAC; and the IAC80 telescope operated on the island of Tenerife by the IAC at the Spanish Observatorio del Teide of the IAC. Part of this research has been carried out with telescope time awarded by the CCI International Time Programme. The authors thank the TAC of the MPG/ESO-2.2m telescope for support of optical follow-up with WFI under Max Planck time. Observations were also conducted with ESO NTT at the La Silla Paranal Observatory. This research has made use of SDSS-III data. Funding for SDSS-III http://www.sdss3.org/ has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and DoE. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration. This research has made use of the following databases: the NED and IRSA databases, operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the NASA; SIMBAD, operated at CDS, Strasbourg, France; SZ cluster database operated by Integrated Data and Operation Center (IDOC) operated by IAS under contract with CNES and CNRS. The authors acknowledge the use of software provided by the US National Virtual Observatory. NR 160 TC 179 Z9 178 U1 5 U2 24 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 NOV PY 2014 VL 571 AR A29 DI 10.1051/0004-6361/201321523 PG 41 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600003 ER PT J AU Ade, PAR Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, B Bartlett, JG Battanerioo, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bock, JJ Bonaldi, A Bond, JR Borrill, J Bouchet, FR Bridges, M Bucher, M Burigana, C Butler, RC Cardoso, JF Carvalho, P Catalano, A Challinor, A Chamballu, A Chiang, HC Chiang, LY Christensen, PR Church, S Clements, DL Colombi, S Colombo, LPL Comis, B Couchot, F Coulais, A Crill, BP Curto, A Cuttaia, F Da Silva, A 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, A Douspis, M Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Flores-Cacho, I Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Genova-Santos, RT Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Hanson, D Harrison, D 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 Knox, L Kunz, M Kurki-Suonio, H Lacasa, F Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leahy, JP Leonardi, R Loen-Tavares, J Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Marcos-Caballero, A Maris, M Marshall, DJ Martin, G Macinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P 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 Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S Oxborrow, CA Paci, F Pagano, L Pajot, F Paoletti, D Partridge, B Pasian, F Patanchonl, G Perdereau, . Perotto, L Perrotta, F Piacentini, F Mae, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Rebolo, R Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rossetl, C Rossetti, M Roudier, G Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Savini, G Scott, D Seiffert, MD Shellard, EPS Spencer, LD Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sunyaev, R Sureau, F Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Tavagnacco, D Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Tuovinen, J Umana, G Valenziano, L Valiviita, J Van Tent, B Varis, J Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD White, SDM Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, B. Bartlett, J. G. Battanerioo, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Bridges, M. Bucher, M. Burigana, C. Butler, R. C. Cardoso, J. -F. Carvalho, P. Catalano, A. Challinor, A. Chamballu, A. Chiang, H. C. Chiang, L. -Y Christensen, P. R. Church, S. Clements, D. L. Colombi, S. Colombo, L. P. L. Comis, B. Couchot, F. Coulais, A. Crill, B. P. Curto, A. Cuttaia, F. Da Silva, A. 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, A. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Flores-Cacho, I. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Genova-Santos, R. T. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Hanson, D. Harrison, D. 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. Knox, L. Kunz, M. Kurki-Suonio, H. Lacasa, F. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leahy, J. P. Leonardi, R. Loen-Tavares, J. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Marcos-Caballero, A. Maris, M. Marshall, D. J. Martin, G. Macinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. 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. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Osborne, S. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paoletti, D. Partridge, B. Pasian, F. Patanchonl, G. Perdereau, . Perotto, L. Perrotta, F. Piacentini, F. Mae, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rossetl, C. Rossetti, M. Roudier, G. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sunyaev, R. Sureau, F. 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. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Varis, J. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. White, S. D. M. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. XXI. Power spectrum and high-order statistics of the Planck all-sky Compton parameter map SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmological parameters; large-scale structure of Universe; galaxies: clusters: general ID SUNYAEV-ZELDOVICH CLUSTERS; MICROWAVE BACKGROUND MAPS; POLE TELESCOPE SURVEY; POINT SOURCES; COSMOLOGICAL PARAMETERS; DATA SETS; COUNTS; CMB; EXTRACTION; GALAXIES AB We have constructed the first all-sky map of the thermal Sunyaev-Zeldovich (tSZ) effect by applying specifically tailored component separation algorithms to the 100 to 857 GHz frequency channel maps from the Planck survey. This map shows an obvious galaxy cluster tSZ signal that is well matched with blindly detected clusters in the Planck SZ catalogue. To characterize the signal in the tSZ map we have computed its angular power spectrum. At large angular scales (l < 60), the major foreground contaminant is the diffuse thermal dust emission. At small angular scales (l > 500) the clustered cosmic infrared background and residual point sources are the major contaminants. These foregrounds are carefully modelled and subtracted. We thus measure the tSZ power spectrum over angular scales 0.17 degrees less than or similar to theta less than or similar to 3.0 degrees that were previously unexplored. The measured tSZ power spectrum is consistent with that expected from the Planck catalogue of SZ sources, with clear evidence of additional signal from unresolved clusters and, potentially, diffuse warm baryons. Marginalized band-powers of the Planck tSZ power spectrum and the best-fit model are given. The non-Gaussianity of the Compton parameter map is further characterized by computing its 1D probability distribution function and its bispectrum. The measured tSZ power spectrum and high order statistics are used to place constraints on sigma(8). C1 [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchonl, G.; Mae, M.; Remazeilles, M.; Rossetl, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, Sorbonne Paris Cite, CNRS, IN2P3,CEA Irfu,Observ Paris,APC, F-75205 Paris 13, France. [Lahteenmaki, A.; Loen-Tavares, J.; Poutanen, T.] Aalto Univ Metsahovi Radio Observ, Kylmala 02540, Finland. [Kunz, M.] African Inst Math Sci, Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana, Sci Data Ctr, I-00133 Rome, Italy. [Mandolesi, N.] Agenzia Spaziale Italiana, Rome, Italy. [Ashdown, M.; Bridges, M.; Carvalho, P.; Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa. [Kneissl, R.] ALMA Santiago Cent Offices, Santiago 0355, Chile. [Bond, J. R.; Hanson, D.; Martin, G.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Flores-Cacho, I.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] CNRS, IRAP, F-31028 Toulouse 4, France. [Bock, J. J.; Dore, A.; Hildebrandt, S. R.; Prezeau, G.; Rocha, G.; Seiffert, M. D.] CALTECH, Pasadena, CA USA. [Challinor, A.; Shellard, E. P. S.] Univ Cambridge, Ctr Theoret Cosmol, DAMTP, Cambridge CB3 0WA, England. [Da Silva, A.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Hernandez-Monteagudo, C.] CEFCA, Teruel 44001, Spain. [Borrill, J.; Keskitalo, R.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. CSIC, Madrid, Spain. [Chamballu, A.; Melin, J. -B.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Kunz, M.; Tucci, M.] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland. [Atrio-Barandela, F.] Univ Salamanca, Fac Ciencias, Dept Fis Fundamental, E-37008 Salamanca, Spain. [Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain. [Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada. [Rachen, J. P.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Keskitalo, R.] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Colombo, L. P. L.; Pierpaoli, E.] Univ So Calif, Dana & David Dornsife Coll Letter Arts & Sci, Dept Phys & Astron, Los Angeles, CA 90089 USA. [Benoit-Levy, A.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Huffenberger, K. M.] Florida State Univ, Dept Phys, Tallahassee, FL USA. [Juvela, M.; Keihanen, E.; Kurki-Suonio, H.; Poutanen, T.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland. [Chiang, H. C.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lubin, P. M.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wandelt, B. D.] Univ Illinois, Dept Phys, Urbana, IL USA. [Liguori, M.; Matarrese, S.] Univ Padua, Dipartimento Fis Astron G Galilei, I-35131 Padua, Italy. [Burigana, C.; Mandolesi, N.; Natoli, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy. [de Bernardis, P.; Melchiorri, A.; Nati, F.; Pagano, L.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Bersanelli, M.; Maino, D.; Mennella, A.; Rossetti, M.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy. [Gregorio, A.; Tavagnacco, D.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark. [Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain. [Kneissl, R.] ESO Vitacura, Santiago, Chile. [Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain. [Giardino, G.; Laureijs, R. J.; Tauber, J. A.] Estec, European Space Agcy, NL-2201 AZ Noordwijk, Netherlands. [Loen-Tavares, J.] Univ Turku, Finnish Ctr Astron ESO FINCA, Piikkio 21500, Finland. [Partridge, B.] Haverford Coll, Dept Astron, Haverford, PA 19041 USA. [Kurki-Suonio, H.; Lahteenmaki, A.; Poutanen, T.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Helsinki Inst Phys, FIN-00014 Helsinki, Finland. [Umana, G.] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [de Zotti, G.; Villa, F.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. 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[Clements, D. L.; Jaffe, A. H.; Mortlock, D.; Novikov, D.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Benoit, A.] Univ Grenoble 1, CNRS, Inst Neel, F-38042 Grenoble, France. [Dole, H.] Inst Univ France, F-75005 Paris, France. [Aghanim, N.; Aumont, J.; Chamballu, A.; Dole, H.; Douspis, M.; Hurier, G.; Kunz, M.; Lacasa, F.; Lagache, G.; Masi, S.; Miville-Deschenes, M. -A.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Remazeilles, M.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Moneti, A.; Prunet, S.; Sygnet, J. -F.; Wandelt, B. D.] CNRS, Inst Astrophys Paris, UMR 7095, Paris, France. [Popa, L.] Inst Space Sci, Bucharest 077125, Romania. [Chiang, L. -Y] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Bridges, M.; Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Migliaccio, M.; Sutton, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Eriksen, H. K.; Hansen, F. K.; Lilje, P. B.; Valiviita, J.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Genova-Santos, R. T.; Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife 38205, Spain. [Barreiro, B.; Curto, A.; Diego, J. M.; Gonzalez-Nuevo, J.; Herranz, D.; Lopez-Caniego, M.; Marcos-Caballero, A.; Macinez-Gonzalez, E.; Toffolatti, L.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain. [Bartlett, J. G.; Bock, J. J.; Colombo, L. P. L.; Crill, B. P.; Dore, A.; Gorski, K. M.; Hanson, D.; Holmes, W. A.; Lawrence, C. R.; Mitra, S.; Pietrobon, D.; Prezeau, G.; Rocha, G.; Roudier, G.; Seiffert, M. D.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Bonaldi, A.; Davies, R. D.; Davis, R. J.; Dickinson, C.; Leahy, J. P.; Maffei, B.; Noviello, F.; Remazeilles, M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Bridges, M.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; Migliaccio, M.; Stolyarov, V.; Sutton, D.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Couchot, F.; Dore, A.; Henrot-Versille, S.; Perdereau, .; Plaszczynski, S.; Tristram, M.; Tucci, M.] Univ Paris 11, CNRS, IN2P3, LAL, F-91898 Orsay, France. [Catalano, A.; Coulais, A.; Lamarre, J. -M.; Roudier, G.] CNRS, Observ Paris, LERMA, F-75014 Paris, France. [Arnaud, M.; Bobin, J.; Chamballu, A.; Marshall, D. J.; Pratt, G. W.; Starck, J. -L.; Sureau, F.] Univ Paris Diderot, CEA Saclay, CNRS, CEA CSM,IRFU,Serv Astrophys,Lab AIM, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, Lab Traitement & Commun Informat, UMR 51541, F-75634 Paris 13, France. [Catalano, A.; Comis, B.; Hurier, G.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble 1, CNRS, IN2P3, Inst Natl Polytech Grenoble,Lab Phys Subatom & Co, F-38026 Grenoble 13, France. [Van Tent, B.] Univ Paris 11, Phys Theor Lab, F-91405 Orsay, France. [Van Tent, B.] CNRS, F-91405 Orsay, France. [Kisner, T. S.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Dolag, K.; Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Knoche, J.; Matthai, F.; Rachen, J. P.; Reinecke, M.; Riller, T.; Sunyaev, R.; White, S. D. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Hanson, D.] McGill Univ, Montreal, PQ H3A 2T8, Canada. [Tuovinen, J.; Varis, J.] VTT Tech Res Ctr Finland, Milli Lab, Espoo 02044, Finland. [Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Crill, B. P.] CALTECH, Observ Cosmol, Pasadena, CA 91125 USA. [Savini, G.] UCL, Opt Sci Lab, London, England. [Lesgourgues, J.] Ecole Polytech Fed Lausanne, SB ITP LPPC, CH-1015 Lausanne, Switzerland. [Baccigalupi, C.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Paci, F.; Perrotta, F.] SISSA, Astrophys Sector, I-34136 Trieste, Italy. [Ade, P. A. R.; Munshi, D.; Spencer, L. D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Moss, A.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Sunyaev, R.] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia. [Borrill, J.; Stolyarov, V.] 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.; Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Armitage-Caplan, C.] Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England. [Lesgourgues, J.] CERN, PH TH, Div Theory, CH-1211 Geneva 23, Switzerland. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Colombi, S.; Delouis, J. -M.; Hivon, E.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UMR7095, F-75014 Paris, France. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Flores-Cacho, I.; 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.] Univ Munich, Univ Observ, D-81679 Munich, Germany. [Battanerioo, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, E-18071 Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Macias-Perez, JF (reprint author), Univ Grenoble 1, CNRS, IN2P3, Inst Natl Polytech Grenoble,Lab Phys Subatom & Co, 53 Rue Martyrs, F-38026 Grenoble 13, France. EM macias@lpsc.in2p3.fr RI Remazeilles, Mathieu/N-1793-2015; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Barreiro, Rita Belen/N-5442-2014; Butler, Reginald/N-4647-2015 OI Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Ricciardi, Sara/0000-0002-3807-4043; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; WANDELT, Benjamin/0000-0002-5854-8269; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; De Zotti, Gianfranco/0000-0003-2868-2595; Lopez-Caniego, Marcos/0000-0003-1016-9283; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Starck, Jean-Luc/0000-0003-2177-7794; Hurier, Guillaume/0000-0002-1215-0706; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Pasian, Fabio/0000-0002-4869-3227; Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996 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); MICINN (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); PRACE (EU) FX The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=Planck&page=Planck_Collabora tion. We acknowledge the use of the HEALPix software. NR 87 TC 77 Z9 76 U1 3 U2 12 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2014 VL 571 AR A21 DI 10.1051/0004-6361/201321522 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600002 ER PT J AU Ade, PAR Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Barrena, R Bartlett, JG Battaner, E Battye, R Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bikmaev, I Blanchard, A Bobin, J Bock, JJ Bohringer, H Bonaldi, A Bond, JR Borrill, J Bouchet, FR Bourdin, H Bridges, M Brown, ML Bucher, M Burenin, R Burigana, C Butler, RC Cardoso, JF Carvalho, P Catalano, A Challinor, A Chamballu, A Chary, RR Chiang, LY Chiang, HC Chon, G Christensen, PR Church, S Clements, DL Colombi, S Colombo, LPL Couchot, F Coulais, A Crill, BP Curto, A Cuttaia, F Da Silva, A Dahle, H Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Delouis, JM Democles, J Desert, FX Dickinson, C Diego, JM Dolag, K Dole, H Donzelli, S Dore, O Douspis, M Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Flores-Cacho, I Forni, O Frailis, M Franceschi, E Fromenteau, S Galeotta, S Ganga, K Genova-Santos, RT Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Hanson, D Harrison, D 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, TR Jaffe, AH Jones, WC Juvela, M Keihanen, E Keskitalo, R Khamitov, I Kisner, TS Kneissl, R Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leahy, JP Leonardi, R Leon-Tavares, J Lesgourgues, J Liddle, A Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Marcos-Caballero, A Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Matarrese, S Matthai, F Mazzotta, 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 Naselsky, P Nati, F Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S Oxborrow, CA Paci, F Pagano, L Pajot, F Paoletti, D Partridge, B Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Rebolo, R Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Roman, M Rosset, C Roudier, G Rowan-Robinson, M Rubino-Martin, A Rusholme, B Sandri, M Santos, D Savini, G Scott, D Seiffert, MD Shellard, EPS Spencer, LD Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sunyaev, R Sureau, F 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 Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Weller, J White, M White, SDM Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Barrena, R. Bartlett, J. G. Battaner, E. Battye, R. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bikmaev, I. Blanchard, A. Bobin, J. Bock, J. J. Boehringer, H. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Bourdin, H. Bridges, M. Brown, M. L. Bucher, M. Burenin, R. Burigana, C. Butler, R. C. Cardoso, J. -F. Carvalho, P. Catalano, A. Challinor, A. Chamballu, A. Chary, R. -R. Chiang, L. -Y Chiang, H. C. Chon, G. Christensen, P. R. Church, S. Clements, D. L. Colombi, S. Colombo, L. P. L. Couchot, F. Coulais, A. Crill, B. P. Curto, A. Cuttaia, F. Da Silva, A. Dahle, H. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J. -M. Democles, J. Desert, F. -X. Dickinson, C. Diego, J. M. Dolag, K. Dole, H. Donzelli, S. Dore, O. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Flores-Cacho, I. Forni, O. Frailis, M. Franceschi, E. Fromenteau, S. Galeotta, S. Ganga, K. Genova-Santos, R. T. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Hanson, D. Harrison, D. 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, T. R. Jaffe, A. H. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Khamitov, I. Kisner, T. S. Kneissl, R. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leahy, J. P. Leonardi, R. Leon-Tavares, J. Lesgourgues, J. Liddle, A. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Marcos-Caballero, A. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Matthai, F. Mazzotta, 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. Naselsky, P. Nati, F. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Osborne, S. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paoletti, D. Partridge, B. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Roman, M. Rosset, C. Roudier, G. Rowan-Robinson, M. Rubino-Martin, A. Rusholme, B. Sandri, M. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sunyaev, R. Sureau, F. 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. Tuerler, M. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Weller, J. White, M. White, S. D. M. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. XX. Cosmology from Sunyaev-Zeldovich cluster counts SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmological parameters; large-scale structure of Universe; galaxies: clusters: general ID BARYON ACOUSTIC-OSCILLATIONS; SOUTH-POLE TELESCOPE; MASSIVE GALAXY CLUSTERS; LARGE-SCALE STRUCTURE; DIGITAL SKY SURVEY; X-RAY-PROPERTIES; SPT-SZ SURVEY; XMM-NEWTON; HYDRODYNAMIC SIMULATIONS; NONTHERMAL PRESSURE AB We present constraints on cosmological parameters using number counts as a function of redshift for a sub-sample of 189 galaxy clusters from the Planck SZ (PSZ) catalogue. The PSZ is selected through the signature of the Sunyaev-Zeldovich (SZ) effect, and the sub-sample used here has a signal-to-noise threshold of seven, with each object confirmed as a cluster and all but one with a redshift estimate. We discuss the completeness of the sample and our construction of a likelihood analysis. Using a relation between mass M and SZ signal Y calibrated to X-ray measurements, we derive constraints on the power spectrum amplitude sigma(8) and matter density parameter Omega(m) in a flat Lambda CDM model. We test the robustness of our estimates and find that possible biases in the Y-M relation and the halo mass function are larger than the statistical uncertainties from the cluster sample. Assuming the X-ray determined mass to be biased low relative to the true mass by between zero and 30%, motivated by comparison of the observed mass scaling relations to those from a set of numerical simulations, we find that sigma(8) = 0.75 +/- 0.03, Omega(m) = 0.29 +/- 0.02, and sigma(8)(Omega(m)/0.27)(0.3) = 0.764 +/- 0.025. The value of sigma(8) is degenerate with the mass bias; if the latter is fixed to a value of 20% (the central value from numerical simulations) we find sigma(8)(Omega(m)/0.27)(0.3) = 0.78 +/- 0.01 and a tighter one-dimensional range sigma(8) = 0.77 +/- 0.02. We find that the larger values of sigma(8) and Omega(m) preferred by Planck's measurements of the primary CMB anisotropies can be accommodated by a mass bias of about 40%. Alternatively, consistency with the primary CMB constraints can be achieved by inclusion of processes that suppress power on small scales relative to the Lambda CDM model, such as a component of massive neutrinos. We place our results in the context of other determinations of cosmological parameters, and discuss issues that need to be resolved in order to make further progress in this field. C1 [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Delabrouille, J.; Fromenteau, S.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Remazeilles, M.; Roman, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, Sorbonne Paris Cite, Observ Paris, CEA lrfu,APC,CNRS IN2P3, F-75205 Paris 13, France. [Lahteenmaki, A.; Leon-Tavares, J.; Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. 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EM marian.douspis@ias.u-psud.fr RI Remazeilles, Mathieu/N-1793-2015; Barreiro, Rita Belen/N-5442-2014; da Silva, Antonio/A-2693-2010; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Lopez-Caniego, Marcos/M-4695-2013; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Lahteenmaki, Anne/L-5987-2013; Valiviita, Jussi/A-9058-2016; Toffolatti, Luigi/K-5070-2014; Mazzotta, Pasquale/B-1225-2016; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Martinez-Gonzalez, Enrique/E-9534-2015; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; White, Martin/I-3880-2015; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Stolyarov, Vladislav/C-5656-2017; Butler, Reginald/N-4647-2015; OI Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; da Silva, Antonio/0000-0002-6385-1609; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; De Zotti, Gianfranco/0000-0003-2868-2595; Lopez-Caniego, Marcos/0000-0003-1016-9283; de Bernardis, Paolo/0000-0001-6547-6446; Valiviita, Jussi/0000-0001-6225-3693; Toffolatti, Luigi/0000-0003-2645-7386; Mazzotta, Pasquale/0000-0002-5411-1748; Vielva, Patricio/0000-0003-0051-272X; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; White, Martin/0000-0001-9912-5070; Gruppuso, Alessandro/0000-0001-9272-5292; Zacchei, Andrea/0000-0003-0396-1192; Lilje, Per/0000-0003-4324-7794; Polenta, Gianluca/0000-0003-4067-9196; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Stolyarov, Vladislav/0000-0001-8151-828X; Masi, Silvia/0000-0001-5105-1439; Valenziano, Luca/0000-0002-1170-0104; Finelli, Fabio/0000-0002-6694-3269; Gregorio, Anna/0000-0003-4028-8785; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Hurier, Guillaume/0000-0002-1215-0706; Juvela, Mika/0000-0002-5809-4834; Hivon, Eric/0000-0003-1880-2733; Paoletti, Daniela/0000-0003-4761-6147; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Weller, Jochen/0000-0002-8282-2010; Butler, Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Ricciardi, Sara/0000-0002-3807-4043 NR 126 TC 252 Z9 251 U1 7 U2 29 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 NOV PY 2014 VL 571 AR A20 DI 10.1051/0004-6361/201321521 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600001 ER PT J AU Ade, PAR Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bemard, JP Bersanelli, M Bielewicz, P Bobin, J Bock, JJ Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Boulanger, F Bridges, M Bucher, M Burigana, C Butler, RC Calabrese, E Cardoso, JF Catalano, A Challinor, A Chamballu, A Chiang, HC Chiang, LY 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 Bemardis, 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 Dunkley, J Dupac, X Efstathiou, G Elsner, F Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Fraisse, AA Franceschi, E Gaier, TC Galeotta, S Galli, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gjerlow, E Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Gudmundsson, JE Hansen, FK Hanson, D Harrison, D Helou, G Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Homtrup, A Hovest, W Huffenberger, KM Hurier, G Jaffe, AH Jaffe, TR Jewell, J Jones, WC Juvela, M Keihanen, E Kesldtalo, R Kiiveri, K Kisner, TS Krieiss, R Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Lattanzi, M Laureijs, RJ Lawrence, CR Le Jeune, M Leach, S Leahy, JP Leonardi, R Leon-Tavares, J Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lindholm, V Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Marinucci, D Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P Meinhold, PR Melchiorri, A Mendes, L Menegoni, E Mennella, A Migliaccio, M Millea, 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 O'Dwyer, IJ Orieux, F Osborne, S Oxborrow, CA Paci, F Pagano, L Pajot, F Paladini, R Paoletti, D Partridge, B Pasian, F Patanchon, G Paykari, P Perdereaun, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Rahlin, A Rebolo, R Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ringeval, C Ristorcelli, I Rocha, G Rosset, C Roudier, G Rowan-Robinson, M Rubino-Martin, JA Rusholme, B Sandri, M Sanselme, L Santos, D Savini, G Scott, D Seiffert, MD Shellard, EPS Spencer, LD Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sureau, F 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 Valenziano, L Valiviita, J Van Tent, B Varis, J Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Wehus, IK White, M White, SDM Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bemard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bock, J. J. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bridges, M. Bucher, M. Burigana, C. Butler, R. C. Calabrese, E. Cardoso, J. -F. Catalano, A. Challinor, A. Chamballu, A. Chiang, H. C. Chiang, L. -Y 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 Bemardis, 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. Dunkley, J. Dupac, X. Efstathiou, G. Elsner, F. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Fraisse, A. A. Franceschi, E. Gaier, T. C. Galeotta, S. Galli, S. Ganga, K. Giard, M. Giardino, G. 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. Helou, G. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Homtrup, A. Hovest, W. Huffenberger, K. M. Hurier, G. Jaffe, A. H. Jaffe, T. R. Jewell, J. Jones, W. C. Juvela, M. Keihanen, E. Kesldtalo, R. Kiiveri, K. Kisner, T. S. krieiss, R. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Lattanzi, M. Laureijs, R. J. Lawrence, C. R. Le Jeune, M. Leach, S. Leahy, J. P. Leonardi, R. Leon-Tavares, J. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lindholm, V. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Marinucci, D. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Menegoni, E. Mennella, A. Migliaccio, M. Millea, 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. O'Dwyer, I. J. Orieux, F. Osborne, S. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paladini, R. Paoletti, D. Partridge, B. Pasian, F. Patanchon, G. Paykari, P. Perdereaun, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Rahlin, A. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ringeval, C. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rowan-Robinson, M. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Sanselme, L. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sureau, F. 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. Tuerler, M. Valenziano, L. Valiviita, J. Van Tent, B. Varis, J. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Wehus, I. K. White, M. White, S. D. M. Yvon, D. Zacchei, A. Zonca, A. TI Planck 2013 results. XV. CMB power spectra and likelihood SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmic background radiation; cosmological parameters; cosmology: observations; methods: data analysis ID PROBE WMAP OBSERVATIONS; SOUTH-POLE TELESCOPE; ATACAMA COSMOLOGY TELESCOPE; STAR-FORMING GALAXIES; MICROWAVE BACKGROUND ANISOTROPY; SUPERNOVA LEGACY SURVEY; LOW-RESOLUTION DATA; SUNYAEV-ZELDOVICH; EXTRAGALACTIC SOURCES; COMPONENT SEPARATION AB This paper presents the Planck 2013 likelihood, a complete statistical description of the two-point correlation function of the CMB temperature fluctuations that accounts for all known relevant uncertainties, both instrumental and astrophysical in nature. We use this likelihood to derive our best estimate of the CMB angular power spectrum from Planck over three decades in multipole moment, t, covering 2 2500. The main source of uncertainty at S 1500 is cosmic variance. Uncertainties in small-scale foreground modelling and instrumental noise dominate the error budget at higher Es. For < 50, our likelihood exploits all Planck frequency channels from 30 to 353 GHz, separating the cosmological CMB signal from diffuse Galactic foregrounds through a physically motivated Bayesian component separation technique. At 50, we employ a correlated Gaussian likelihood approximation based on a fine-grained set of angular cross-spectra derived from multiple detector combinations between the 100, 143, and 217 GHz frequency channels, marginalising over power spectrum foreground templates. We validate our likelihood through an extensive suite of consistency tests, and assess the impact of residual foreground and instrumental uncertainties on the final cosmological parameters. We find good internal agreement among the high- cross-spectra with residuals below a few fiK2 at S 1000, in agreement with estimated calibration uncertainties. We compare our results with foreground-cleaned CMB maps derived from all Planck frequencies, as well as with cross-spectra derived from the 70 GHz Planck map, and find broad agreement in terms of spectrum residuals and cosmological parameters. We further show that the best-fit ACDM cosmology is in excellent agreement with preliminary Planck EE and T E polarisation spectra. We find that the standard ACDM cosmology is well constrained by Planck from the measurements at C 1500. One specific example is the spectral index of scalar perturbations, for which we report a 5.4o- deviation from scale invariance, ns = 1. Increasing the multipole range beyond = 1500 does not increase our accuracy for the ACDM parameters, but instead allows us to study extensions beyond the standard model. We find no indication of significant departures from the ACDM framework. Finally, we report a tension between the Planck best-fit ACDM model and the low- spectrum in the form of a power deficit of 5-10% at 40, with a statistical significance of 2.5-3o-. Without a theoretically motivated model for this power deficit, we do not elaborate further on its cosmological implications, but note that this is our most puzzling finding in an otherwise remarkably consistent data set. C1 [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Le Jeune, M.; Patanchon, G.; Piat, M.; Remazeilles, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, APC, CNRS IN2P3, CEA lrfu,Observ Paris,Sorbonne Paris Cite, F-75205 Paris 13, France. [Lahteenmaki, A.; Leon-Tavares, J.; Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Kunz, M.] African Inst Math Sci, ZA-7945 Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy. 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[Chiang, L. -Y] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D.; Migliaccio, M.; Sutton, D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Ringeval, C.] Univ Louvain, Ctr Cosmol Particle Phys & Phenomenol, Inst Math & Phys, B-1348 Louvain, Belgium. [Eriksen, H. K.; Gjerlow, E.; Hansen, F. K.; Lilje, P. B.; Valiviita, J.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife 38205, Spain. [Barreiro, R. B.; Bonavera, L.; Curto, A.; Diego, J. M.; Gonzalez-Nuevo, J.; Herranz, D.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Toffolatti, L.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain. [Bartlett, J. G.; Bock, J. J.; Colombo, L. P. L.; Crill, B. P.; Dore, O.; Gaier, T. C.; Gorski, K. M.; Hanson, D.; Holmes, W. A.; Jewell, J.; Lawrence, C. R.; Mitra, S.; O'Dwyer, I. J.; Pietrobon, D.; Prezeau, G.; Rocha, G.; Roudier, G.; Seiffert, M. D.; Wade, L. A.; Wehus, I. K.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Bonaldi, A.; Davies, R. D.; Davis, R. J.; Dickinson, C.; Leahy, J. P.; Maffei, B.; Noviello, F.; Remazeilles, M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Bridges, M.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; Migliaccio, M.; Stolyarov, V.; Sutton, D.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Couchot, F.; Henrot-Versille, S.; Perdereaun, O.; Plaszczynski, S.; Tristram, M.; Tucci, M.] Univ Paris 11, CNRS IN2P3, LAL, F-91898 Orsay, France. [Catalano, A.; Coulais, A.; Lamarre, J. -M.; Roudier, G.] CNRS, LERMA, Observ Paris, F-75014 Paris, France. [Arnaud, M.; Bobin, J.; Chamballu, A.; Marshall, D. J.; Paykari, P.; Pratt, G. W.; Starck, J. -L.; Sureau, F.] Univ Paris Diderot, CEA Saclay, CNRS, IRFU Serv Astrophys CEA DSM,Lab AIM, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France. [Catalano, A.; Combet, C.; Hurier, G.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Sanselme, L.; Santos, D.] Univ Joseph Fourier Grenoble I, CNRS IN2P3, Inst Natl Polytech Grenoble, F-38026 Grenoble, France. [Van Tent, B.] Univ Paris 11, Phys Theor Lab, F-91405 Orsay, France. [Van Tent, B.] CNRS, F-91405 Orsay, France. [Kisner, T. S.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Knoche, J.; Matthai, F.; Rachen, J. P.; Reinecke, M.; Riller, T.; White, S. D. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Hanson, D.] McGill Univ, Montreal H3A 2T8, PQ, Canada. [Tuovinen, J.; Varis, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo 02044, Finland. [Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Co Kildare, Ireland. [Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Crill, B. P.] CALTECH, Observ Cosmol, Pasadena, CA 91125 USA. [Savini, G.] UCL, Opt Sci Lab, London, England. [Lesgourgues, J.] Ecole Polytech Fed Lausanne, SB ITP LPPC, CH-1015 Lausanne, Switzerland. [Baccigalupi, C.; Bielewicz, P.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Leach, S.; Paci, F.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Ade, P. A. R.; Munshi, D.; Spencer, L. D.; Sudiwala, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Moss, A.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [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.; Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Armitage-Caplan, C.; Calabrese, E.; Dunkley, J.] Univ Oxford, Subdept Astrophys, Oxford OX1 3RH, England. [Lesgourgues, J.] CERN, PH TH, Div Theory, CH-1211 Geneva 23, Switzerland. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Colombi, S.; Delouis, J. -M.; Elsner, F.; Hivon, E.; Prunet, S.; Ringeval, C.; Wandelt, B. D.] Univ Paris 06, UMR7095, F-75014 Paris, France. [Banday, A. J.; Bemard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, IRAP, UPS OMP, F-31028 Toulouse 4, France. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, E-18071 Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Bouchet, FR (reprint author), CNRS, Inst Astrophys Paris, UMR 7095, 98bis Bd Arago, F-75014 Paris, France. EM bouchet@iap.fr RI Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Lattanzi, Massimiliano/D-8120-2011; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; bonavera, laura/E-9368-2017; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Mazzotta, Pasquale/B-1225-2016; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Martinez-Gonzalez, Enrique/E-9534-2015; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; White, Martin/I-3880-2015; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Remazeilles, Mathieu/N-1793-2015; Barreiro, Rita Belen/N-5442-2014; Butler, Reginald/N-4647-2015; OI Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Lattanzi, Massimiliano/0000-0003-1059-2532; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; bonavera, laura/0000-0001-8039-3876; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Toffolatti, Luigi/0000-0003-2645-7386; Mazzotta, Pasquale/0000-0002-5411-1748; Vielva, Patricio/0000-0003-0051-272X; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; White, Martin/0000-0001-9912-5070; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; Maris, Michele/0000-0001-9442-2754; Finelli, Fabio/0000-0002-6694-3269; De Zotti, Gianfranco/0000-0003-2868-2595; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Polenta, Gianluca/0000-0003-4067-9196; Lopez-Caniego, Marcos/0000-0003-1016-9283; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Gregorio, Anna/0000-0003-4028-8785; Butler, Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Hurier, Guillaume/0000-0002-1215-0706; Juvela, Mika/0000-0002-5809-4834; Molinari, Diego/0000-0002-7799-3915; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993 FU ESA FX The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU). A description of the Planck Collaboration and a list of its members with the technical or scientific activities they have been involved into, can be found at http: //www. set ups. esa. int/index. phprproj net= planck&page=Planck_Collaboration. We acknowledge the use of the CLASS Boltzmann code (Lesgourgues 201D and the Monte Python package (Audren et al, 2013) in earlier stages of this work. The likelihood code and some of the validation work was built on the library pmclib from the CosmoPMC package (Kilhinger et al. 2011). This research used resources of the IN2P3 Computer Center (http //cc.in2p3.fr) as well as of the Planck-HFI data processing centre infrastructures hosted at the Institut d'Astrophysique de Paris (France) and financially supported by CNES. NR 124 TC 399 Z9 398 U1 19 U2 63 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 NOV PY 2014 VL 571 AR A15 DI 10.1051/0004-6361/201321573 PG 60 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600023 ER PT J AU Ade, PAR Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F 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 Bobin, J Bock, JJ Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Bridges, M Bucher, M Burigana, C Butler, RC Cardoso, JF Catalano, A Challinor, A Chamballu, A Chiang, LY Chiang, HC Christensen, PR Church, S Clements, DL Colombi, S Colombo, LPL 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 Dunkley, J Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Fergusson, J Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Hanson, D Harrison, D Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Jaffe, TR Jaffe, AH Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leahy, JP Leonardi, R Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Matarrese, S Matthai, F Mazzotta, P McEwen, JD 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 Naselsky, P Natoli, P Netterfield, CB Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S Oxborrow, CA Paci, F Pagano, L Pajot, F Paoletti, D Pasian, F Patanchon, G Peiris, HV Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Rath, C Rebolo, R Remazeilles, M Renault, C Ricciardi, S Riller, T Ringeval, C Ristorcelli, I Rocha, G Rosset, C Roudier, G Rowan-Robinson, M Rusholme, B Sandri, M Santos, D Savini, G Scott, D Seiffert, MD Shellard, EPS Spencer, LD Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sureau, F Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Tavagnacco, D Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Tuovinen, J Valenziano, L Valiviita, J Van Tent, B Varis, J Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. 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. Bobin, J. Bock, J. J. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Bridges, M. Bucher, M. Burigana, C. Butler, R. C. Cardoso, J. -F. Catalano, A. Challinor, A. Chamballu, A. Chiang, L. -Y Chiang, H. C. Christensen, P. R. Church, S. Clements, D. L. Colombi, S. Colombo, L. P. L. 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. Dunkley, J. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Fergusson, J. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Hanson, D. Harrison, D. 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. Jaffe, T. R. Jaffe, A. H. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leahy, J. P. Leonardi, R. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Matthai, F. Mazzotta, P. McEwen, J. D. 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. Naselsky, P. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Osborne, S. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paoletti, D. Pasian, F. Patanchon, G. Peiris, H. V. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Raeth, C. Rebolo, R. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ringeval, C. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rowan-Robinson, M. Rusholme, B. Sandri, M. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sureau, F. 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. Valenziano, L. Valiviita, J. Van Tent, B. Varis, J. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Yvon, D. Zacchei, A. Zonca, A. TI Planck 2013 results. XXV. Searches for cosmic strings and other topological defects SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmic background radiation; cosmological parameters; early Universe; large-scale structure of Universe; cosmology: theory; cosmology: observations ID MICROWAVE BACKGROUND FLUCTUATIONS; NON-GAUSSIANITY; HIGHER CRITICISM; VACUUM STRINGS; POWER SPECTRUM; WMAP DATA; EVOLUTION; ANISOTROPY; NETWORKS; WAVELETS AB Planck data have been used to provide stringent new constraints on cosmic strings and other defects. We describe forecasts of the CMB power spectrum induced by cosmic strings, calculating these from network models and simulations using line-of-sight Boltzmann solvers. We have studied Nambu-Goto cosmic strings, as well as field theory strings for which radiative effects are important, thus spanning the range of theoretical uncertainty in the underlying strings models. We have added the angular power spectrum from strings to that for a simple adiabatic model, with the extra fraction defined as f(10) at multipole l = 10. This parameter has been added to the standard six parameter fit using CO S M OM C with flat priors. For the Nambu-Goto string model, we have obtained a constraint on the string tension of G mu/c(2) < 1.5 x 10(-7) and f(10) < 0.015 at 95% confidence that can be improved to G mu/c(2) < 1.3 x 10(-7) and f(10) < 0.010 on inclusion of high-l CMB data. For the Abelian-Higgs field theory model we find, G mu(AH)/c2 < 3.2x10(-7) and f(10) < 0.028. The marginalised likelihoods for f(10) and in the f(10)-Omega(b)h(2) plane are also presented. We have additionally obtained comparable constraints on f(10) for models with semilocal strings and global textures. In terms of the effective defect energy scale these are somewhat weaker at G mu/c(2) < 1.1 x 10(-6). We have made complementarity searches for the specific non-Gaussian signatures of cosmic strings, calibrating with all-sky Planck resolution CMB maps generated from networks of post-recombination strings. We have validated our non-Gaussian searches using these simulated maps in a Planck-realistic context, estimating sensitivities of up to Delta G mu/c(2) approximate to 4 x 10(-7). We have obtained upper limits on the string tension at 95% confidence of G mu/c(2) < 9.0 x 10(-7) with modal bispectrum estimation and G mu/c(2) < 7.8 x 10(-7) for real space searches with Minkowski functionals. These are conservative upper bounds because only post-recombination string contributions have been included in the non-Gaussian analysis. 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, Sorbonne Paris Cite, APC, CNRS IN2P3,CEA Lrfu,Observ Paris, F-75205 Paris 13, France. [Lahteenmaki, A.; Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Kunz, M.] African Inst Math Sci, ZA-7701 Rondebosch Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, I-00044 Frascati, Italy. [Mandolesi, N.] Agenzia Spaziale Italiana, I-00198 Rome, Italy. [Ashdown, M.; Bridges, M.; Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa. [Bond, J. R.; Hanson, D.; Martin, P. G.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Banday, A. 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[Ashdown, M.; Bridges, M.; Challinor, A.; Gratton, S.; Harrison, D.; Lasenby, A.; Migliaccio, M.; Stolyarov, V.; Sutton, D.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Couchot, F.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.; Tucci, M.] Univ Paris 11, LAL, CNRS, IN2P3, F-91898 Orsay, France. [Catalano, A.; Coulais, A.; Lamarre, J. -M.; Roudier, G.] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Arnaud, M.; Bobin, J.; Chamballu, A.; Marshall, D. J.; Pratt, G. W.; Starck, J. -L.; Sureau, F.] Univ Paris Diderot, CEA Saclay, Lab AIM, IRFU Serv Astrophys CEA DSM CNRS, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, UMR 5141, Lab Traitement & Commun Informat, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France. [Catalano, A.; Macias-Perez, J. F.; Perotto, L.; Renault, C.; Santos, D.] Univ Grenoble 1, Lab Phys Subatom & Cosmol, Inst Natl Polytech Grenoble, CNRS IN2P3, F-38026 Grenoble, France. [Van Tent, B.] Univ Paris 11, Phys Theor Lab, F-91405 Orsay, France. [Van Tent, B.] CNRS, F-91405 Orsay, France. [Kisner, T. S.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Knoche, J.; Matthai, F.; Rachen, J. P.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Raeth, C.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Hanson, D.] McGill Univ, Montreal, PQ H3A 2T8, Canada. [Tuovinen, J.; Varis, J.] VTT Tech Res Ctr Finland, MilliLab, Espoo 02044, Finland. [Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Crill, B. P.] CALTECH, Pasadena, CA 91125 USA. [Savini, G.] UCL, Opt Sci Lab, London, England. [Lesgourgues, J.] Ecole Polytech Fed Lausanne, SB ITP LPPC, CH-1015 Lausanne, Switzerland. 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J.; Bielewicz, 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, Dept Fis Teor & Cosmos, Fac Ciencias, Granada 1807, Spain. [Huffenberger, K. M.] Univ Miami, Coral Gables, FL 33124 USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Moss, A (reprint author), Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. EM adam.moss@nottingham.ac.uk RI Remazeilles, Mathieu/N-1793-2015; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; bonavera, laura/E-9368-2017; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Martinez-Gonzalez, Enrique/E-9534-2015; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Barreiro, Rita Belen/N-5442-2014; Butler, Reginald/N-4647-2015; OI Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; bonavera, laura/0000-0001-8039-3876; De Zotti, Gianfranco/0000-0003-2868-2595; Lopez-Caniego, Marcos/0000-0003-1016-9283; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017 FU ESA; CNES FX The development of Planck has been supported by: ESA; CNES and CNRS /INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collabora tion. We also wish to acknowledge the use of the COSMOS supercomputer, part of the DiRAC HPC Facility funded by STFC and the UK Large Facilities Capital Fund, use of the Andromeda cluster of the University of Geneva, and resources of the National Energy Research Scientific Computing Center. NR 120 TC 150 Z9 149 U1 3 U2 22 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 NOV PY 2014 VL 571 AR A25 DI 10.1051/0004-6361/201321621 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600028 ER PT J AU Ade, PAR Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F 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 Bobin, J Bock, JJ Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Bridges, M Bucher, M Burigana, C Butler, RC Cardoso, JF Catalano, A Challinor, A Chamballu, A Chary, RR Chiang, HC Chiang, LY Christensen, PR Church, S Clements, DL Colombi, S Colombo, LPL 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 Diego, JM Dole, H Donzelli, S Dore, O Douspis, M Ducout, A Dupac, X Efstathiou, G Elsner, F Ensslin, TA Eriksen, HK Fantaye, Y Fergusson, J Finelli, F Forni, O Frailis, M Franceschi, E Frommert, M Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Hansen, M 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 Jaffe, AH Jaffe, TR Jones, WC Juvela, M Keihanen, E Keskitalo, R Kim, J Kisner, TS Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leahy, JP Leonardi, R Leroy, C Lesgourgues, J Liguori, M Lille, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Mangilli, A Marinucci, D Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P McEwen, JD 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 Osborne, S Oxborrowl, CA Paci, F Pagano, L Pajot, F Paoletti, D Pasian, F Patanchon, G Peiris, HV Perdereau, O Perotto, L Perrotta, F Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pogosyan, D Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Racine, B Rath, C Rebolo, R Reinecke, M Remazeilles, M Renault, C Renzi, A Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Rotti, A Roudier, G Rubino-Martin, JA Ruiz-Granadosioi, B Rusholme, B Sandri, M Santos, D Savini, G Scott, D Seiffert, MD Shellard, EPS Souradeep, T Spencer, LD Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sureau, F Sutter, P 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 Valenziano, L Valiviita, J Van Tent, B Varis, J Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Wehus, IK White, M Wilkinson, A Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. 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. Bobin, J. Bock, J. J. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Bridges, M. Bucher, M. Burigana, C. Butler, R. C. Cardoso, J. -F. Catalano, A. Challinor, A. Chamballu, A. Chary, R. -R. Chiang, H. C. Chiang, L. -Y Christensen, P. R. Church, S. Clements, D. L. Colombi, S. Colombo, L. P. L. 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. 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. Fergusson, J. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Frommert, M. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Hansen, M. 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. Jaffe, A. H. Jaffe, T. R. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kim, J. Kisner, T. S. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leahy, J. P. Leonardi, R. Leroy, C. Lesgourgues, J. Liguori, M. Lille, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Mangilli, A. Marinucci, D. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. McEwen, J. D. 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. Osborne, S. Oxborrowl, C. A. Paci, F. Pagano, L. Pajot, F. Paoletti, D. Pasian, F. Patanchon, G. Peiris, H. V. Perdereau, O. Perotto, L. Perrotta, F. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pogosyan, D. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Racine, B. Raeth, C. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Renzi, A. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Rotti, A. Roudier, G. Rubino-Martin, J. A. Ruiz-Granadosioi, B. Rusholme, B. Sandri, M. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Souradeep, T. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sureau, F. Sutter, P. 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. Tuerler, M. Valenziano, L. Valiviita, J. Van Tent, B. Varis, J. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Wehus, I. K. White, M. Wilkinson, A. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. XXIII. Isotropy and statistics of the CMB SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmic background radiation; cosmology: observations; cosmology: miscellaneous ID MICROWAVE-ANISOTROPY-PROBE; PRIMORDIAL NON-GAUSSIANITY; DIRECTIONAL SPHERICAL WAVELETS; HEMISPHERICAL POWER ASYMMETRY; DEPENDENT NON-GAUSSIANITIES; POINT CORRELATION-FUNCTIONS; WMAP DATA; BACKGROUND ANISOTROPY; MINKOWSKI FUNCTIONALS; COLD SPOT AB The two fundamental assumptions of the standard cosmological model - that the initial fluctuations are statistically isotropic and Gaussian - are rigorously tested using maps of the cosmic microwave background (CMB) anisotropy from the Planck satellite. The detailed results are based on studies of four independent estimates of the CMB that are compared to simulations using a fiducial Lambda CDM model and incorporating essential aspects of the Planck measurement process. Deviations from isotropy have been found and demonstrated to be robust against component separation algorithm, mask choice, and frequency dependence. Many of these anomalies were previously observed in the WMAP data, and are now confirmed at similar levels of significance (about 3 sigma). However, we find little evidence of non-Gaussianity, with the exception of a few statistical signatures that seem to be associated with specific anomalies. In particular, we find that the quadrupole-octopole alignment is also connected to a low observed variance in the CMB signal. A power asymmetry is now found to persist on scales corresponding to about l = 600 and can be described in the low-l regime by a phenomenological dipole modulation model. However, any primordial power asymmetry is strongly scale-dependent and does not extend to arbitrarily small angular scales. Finally, it is plausible that some of these features may be reflected in the angular power spectrum of the data, which shows a deficit of power on similar scales. Indeed, when the power spectra of two hemispheres defined by a preferred direction are considered separately, one shows evidence of a deficit in power, while its opposite contains oscillations between odd and even modes that may be related to the parity violation and phase correlations also detected in the data. Although these analyses represent a step forward in building an understanding of the anomalies, a satisfactory explanation based on physically motivated models is still lacking. C1 [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Piat, M.; Racine, B.; Remazeilles, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, CNRS IN2P3,CEA lrfu,APC, F-75205 Paris 13, France. 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EM martinez@ifca.unican.es RI Butler, Reginald/N-4647-2015; Barreiro, Rita Belen/N-5442-2014; Remazeilles, Mathieu/N-1793-2015; Renzi, Alessandro/K-4114-2015; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; bonavera, laura/E-9368-2017; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Cruz, Marcos/N-3429-2014; Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; White, Martin/I-3880-2015; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Herranz, Diego/K-9143-2014 OI Pierpaoli, Elena/0000-0002-7957-8993; Juvela, Mika/0000-0002-5809-4834; Molinari, Diego/0000-0002-7799-3915; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Butler, Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Renzi, Alessandro/0000-0001-9856-1970; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; bonavera, laura/0000-0001-8039-3876; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; De Zotti, Gianfranco/0000-0003-2868-2595; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; Cruz, Marcos/0000-0002-4767-530X; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; White, Martin/0000-0001-9912-5070; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; 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); MICINN (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); PRACE (EU) FX The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collabora tion. We acknowledge the use of resources from the Norewegian national super computing facilities NOTUR. The modal and KSW bispectrum estimator analysis was performed on the COSMOS supercomputer, part of the STFC DiRAC HPC Facility. We further acknowledge the computer resources and technical assistance provided by the Spanish Supercomputing Network nodes at Universidad de Cantabria and Universidad Politecnica de Madrid as well as by the Advanced Computing and e-Science team at IFCA. Some of the results in this paper have been derived using the HEALPix package. NR 150 TC 293 Z9 293 U1 10 U2 35 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 NOV PY 2014 VL 571 AR A23 DI 10.1051/0004-6361/201321534 PG 48 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600009 ER PT J AU Ade, PAR Aghanim, N Alves, MIR Armitage-CaplanI, C Amaud, M Ashdown, M Atrio-Barandela, F Aumont, J Ausse, H Baccigalupi, C Banday, AJ Barreiro, RB Barrenass, R Bartelmann, M Bartlett, JG Bartolo, N Basak, S Battaner, E Battye, R Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bertincourt, B Bethermin, M Bielewicz, P Bikmaev, I Blanchard, A Bobin, J Bock, JJ Bohringer, H Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Boulanger, F Bourdin, H Bowyer, JW Bridges, M Brown, ML Bucher, M Burenin, R Burigana, C Butler, RC Calabrese, E Cappellini, B Cardoso, JF Carr, R Carvalho, P Casale, M Castexl, G Catalano, A Challinor, A Chamballu, A Chary, RR Chen, X Chiang, HC Chiang, LY Chon, G Christensen, PR Churazov, E Church, S Clemens, M Clements, DL Colombi, S Colombo, LPL Combet, C Comis, B Couchot, E Coulais, A Crill, BP Cruz, M Curto, A Cuttaia, F Da Silva, A Dahle, H Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Dechelette, T Delabrouille, J Delouis, JM Democles, J Desert, FX Dick, J Dickinson, C Diego, JM Dolag, K Dole, H Donzelli, S Dore, O Douspis, M Ducout, A Dunkley, J Dupac, X Efstathiou, G Elsner, F Ensslin, TA Eriksen, HK Fabre, O Falgarone, E Falvella, MC Fantaye, Y FergussonI, J Filliard, C Finelli, F Flores-Cacho, I Foley, S Forni, O Fosalba, P Frailis, M Fraisse, AA Franceschi, E Freschi, M Fromenteau, S Frommert, M Gaier, TC Galeotta, S Gallegos, J Galli, S Gandolfo, B Ganga, K Gauthier, C Genova-Santos, RT Ghosh, T Giard, M Giardino, G Gilfanov, M Girard, D Giraud-Heraud, Y Gjerlow, E Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Gudmundsson, JE Haissinski, J Hamann, J Hansen, FK Hansen, M Hanson, D Harrison, DL Heavens, A Helou, G Hempel, A Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Ho, S Hobson, M Holmes, WA Hornstrup, A Hou, Z Hovest, W Huey, G Huffenberger, KM Hurier, G Ilic, S Jaffe, AH Jaffe, TR Jasches, J Jewell, J Jones, WC Juvela, M Kalberla, P Kangaslahti, P Keihanen, E Kerp, J Keskitalo, R Khamitov, I Kiiveri, K Kim, J Kisnerl, TS Kneissl, R Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lacasa, E Lagache, G Lahteenmaki, A Lamarre, JM Langer, M Lasenby, A Lattanzi, M Laureijs, RJ Lavabre, A Lawrence, CR Le Jeune, M Leach, S Leahy, JP Leonardi, R Leon-Tavares, J Leroy, C Lesgourgues, J Lewis, A Li, C Liddle, A Liguori, M Lilie, PB Linden-Vornle, M Lindholm, V Lopez-Caniego, M Lowe, S Lubin, PM Macias-Perez, JF MacTavish, CJ Maffei, B Maggio, G Maino, D Mandolesi, N Mangilli, A Marcos-Caballero, A Marinucci, D Maris, M Marleau, F Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matsumura, T Matthai, E Maurin, L Mazzotta, P McDonald, A McEwen, JD McGehee, P Mei, S Meinhold, PR Melchiorri, A Melin, JB Mendes, L Menegoni, E Mennella, A Migliaccio, M Mikkelsen, K Millea, M Miniscalco, R Mitra, S Miville-Deschenes, MA Molinari, D Moneti, A Montier, L Morgante, G Morisset, N Mortlock, D Moss, A Munshi, D Murphy, JA Naselsky, P Nati, E Natoli, P Negrello, M Nesvadba, NPH Netterfield, CB Norgaard-Nielsen, HU North, C Noviello, F Novikov, D Novikov, I O'Dwyer, IJ Orieux, F Osborne, S O'Sullivan, C Oxborrow, CA Paci, F Pagano, L Pajot, F Paladini, R Pandolfi, S Paoletti, D Partridge, B Pasian, F Patanchon, G Paykari, P Pearson, D Pearson, TJ Peel, M Peiris, HV Perdereau, O Perotto, L Perrotta, F Pettorino, V Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Platania, P Pogosyan, D Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Pullen, AR Rachen, JP Racine, B Rahlin, A Rath, C Reach, WT Rebolo, R Reinecke, M Remazeilles, M Renault, C Renzi, A Riazuelo, A Ricciardi, S Rillerl, T Ringeval, C Ristorcelli, I Robbers, G Rocha, G Roman, M Rosset, C Rossetti, M Roudier, G Rowan-Robinson, M Rubino-Martin, JA Ruiz-Granados, B Rusholme, B Salerno, E Sandri, M Sanselme, L Santos, D Savelainen, M Savini, G Schaefer, BM Schiavon, F Scott, D Seiffert, MD Serra, P Shellard, EPS Smith, K Smoot, GE Souradeep, T Spencer, LD Starck, JL Stolyarov, V Stompor, R Sudiwala, R Sunyaev, R Sureau, F Sutteer, P Sutton, D Suur-Uski, AS Sygnet, JE Tauber, JA Tavagnacco, D Taylor, D Terenzi, L Texier, D Toffolatti, L Tomasi, M Torre, JP Tristram, M Tucci, M Tuovinen, J Turler, M Tuttlebee, M Umana, G Valenziano, L Valiviita, J Van Tent, B Varisi, J Vibert, L Viel, M Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Watson, C Watson, R Wehus, IK Welikala, N Weller, J White, M White, SDM Wilkinson, A Winkel, B Xia, JQ Yvon, D Zacchei, A Zibin, JP Zonca, A AF Ade, P. A. R. Aghanim, N. Alves, M. I. R. Armitage-Caplan, C., I Amaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Ausse, H. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Barrenass, R. Bartelmann, M. Bartlett, J. G. Bartolo, N. Basak, S. Battaner, E. Battye, R. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bertincourt, B. Bethermin, M. Bielewicz, P. Bikmaev, I. Blanchard, A. Bobin, J. Bock, J. J. Boehringer, H. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Boulanger, F. Bourdin, H. Bowyer, J. W. Bridges, M. Brown, M. L. Bucher, M. Burenin, R. Burigana, C. Butler, R. C. Calabrese, E. Cappellini, B. Cardoso, J. -F. Carr, R. Carvalho, P. Casale, M. Castexl, G. Catalano, A. Challinor, A. Chamballu, A. Chary, R. -R. Chen, X. Chiang, H. C. Chiang, L. -Y Chon, G. Christensen, P. R. Churazov, E. Church, S. Clemens, M. Clements, D. L. Colombi, S. Colombo, L. P. L. Combet, C. Comis, B. Couchot, E. Coulais, A. Crill, B. P. Cruz, M. Curto, A. Cuttaia, F. Da Silva, A. Dahle, H. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Dechelette, T. Delabrouille, J. Delouis, J. -M. Democles, J. Desert, F. -X. Dick, J. Dickinson, C. Diego, J. M. Dolag, K. Dole, H. Donzelli, S. Dore, O. Douspis, M. Ducout, A. Dunkley, J. Dupac, X. Efstathiou, G. Elsner, F. Ensslin, T. A. Eriksen, H. K. Fabre, O. Falgarone, E. Falvella, M. C. Fantaye, Y. Fergusson, J., I Filliard, C. Finelli, F. Flores-Cacho, I. Foley, S. Forni, O. Fosalba, P. Frailis, M. Fraisse, A. A. Franceschi, E. Freschi, M. Fromenteau, S. Frommert, M. Gaier, T. C. Galeotta, S. Gallegos, J. Galli, S. Gandolfo, B. Ganga, K. Gauthier, C. Genova-Santos, R. T. Ghosh, T. Giard, M. Giardino, G. Gilfanov, M. Girard, D. Giraud-Heraud, Y. Gjerlow, E. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Gudmundsson, J. E. Haissinski, J. Hamann, J. Hansen, F. K. Hansen, M. Hanson, D. Harrison, D. L. Heavens, A. Helou, G. Hempel, A. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Ho, S. Hobson, M. Holmes, W. A. Hornstrup, A. Hou, Z. Hovest, W. Huey, G. Huffenberger, K. M. Hurier, G. Ilic, S. Jaffe, A. H. Jaffe, T. R. Jasches, J. Jewell, J. Jones, W. C. Juvela, M. Kalberla, P. Kangaslahti, P. Keihanen, E. Kerp, J. Keskitalo, R. Khamitov, I. Kiiveri, K. Kim, J. Kisnerl, T. S. Kneissl, R. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lacasa, E. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Langer, M. Lasenby, A. Lattanzi, M. Laureijs, R. J. Lavabre, A. Lawrence, C. R. Le Jeune, M. Leach, S. Leahy, J. P. Leonardi, R. Leon-Tavares, J. Leroy, C. Lesgourgues, J. Lewis, A. Li, C. Liddle, A. Liguori, M. Lilie, P. B. Linden-Vornle, M. Lindholm, V. Lopez-Caniego, M. Lowe, S. Lubin, P. M. Macias-Perez, J. F. MacTavish, C. J. Maffei, B. Maggio, G. Maino, D. Mandolesi, N. Mangilli, A. Marcos-Caballero, A. Marinucci, D. Maris, M. Marleau, F. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matsumura, T. Matthai, E. Maurin, L. Mazzotta, P. McDonald, A. McEwen, J. D. McGehee, P. Mei, S. Meinhold, P. R. Melchiorri, A. Melin, J. -B. Mendes, L. Menegoni, E. Mennella, A. Migliaccio, M. Mikkelsen, K. Millea, M. Miniscalco, R. Mitra, S. Miville-Deschenes, M. -A. Molinari, D. Moneti, A. Montier, L. Morgante, G. Morisset, N. Mortlock, D. Moss, A. Munshi, D. Murphy, J. A. Naselsky, P. Nati, E. Natoli, P. Negrello, M. Nesvadba, N. P. H. Netterfield, C. B. Norgaard-Nielsen, H. U. North, C. Noviello, F. Novikov, D. Novikov, I. O'Dwyer, I. J. Orieux, F. Osborne, S. O'Sullivan, C. Oxborrow, C. A. Paci, F. Pagano, L. Pajot, F. Paladini, R. Pandolfi, S. Paoletti, D. Partridge, B. Pasian, F. Patanchon, G. Paykari, P. Pearson, D. Pearson, T. J. Peel, M. Peiris, H. V. Perdereau, O. Perotto, L. Perrotta, F. Pettorino, V. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Platania, P. Pogosyan, D. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Pullen, A. R. Rachen, J. P. Racine, B. Rahlin, A. Raeth, C. Reach, W. T. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Renzi, A. Riazuelo, A. Ricciardi, S. Rillerl, T. Ringeval, C. Ristorcelli, I. Robbers, G. Rocha, G. Roman, M. Rosset, C. Rossetti, M. Roudier, G. Rowan-Robinson, M. Rubino-Martin, J. A. Ruiz-Granados, B. Rusholme, B. Salerno, E. Sandri, M. Sanselme, L. Santos, D. Savelainen, M. Savini, G. Schaefer, B. M. Schiavon, F. Scott, D. Seiffert, M. D. Serra, P. Shellard, E. P. S. Smith, K. Smoot, G. E. Souradeep, T. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sudiwala, R. Sunyaev, R. Sureau, F. Sutteer, P. Sutton, D. Suur-Uski, A-S. Sygnet, J. -E Tauber, J. A. Tavagnacco, D. Taylor, D. Terenzi, L. Texier, D. Toffolatti, L. Tomasi, M. Torre, J. -P. Tristram, M. Tucci, M. Tuovinen, J. Tuerler, M. Tuttlebee, M. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Varisi, J. Vibert, L. Viel, M. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Watson, C. Watson, R. Wehus, I. K. Welikala, N. Weller, J. White, M. White, S. D. M. Wilkinson, A. Winkel, B. Xia, J. -Q. Yvon, D. Zacchei, A. Zibin, J. P. Zonca, A. CA Planck Collaboration TI Planck 2013 results. I. Overview of products and scientific results SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology: observations; cosmic background radiation; space vehicles: instruments; instrumentation: detectors ID PROBE WMAP OBSERVATIONS; SOUTH-POLE TELESCOPE; GALAXY CLUSTER SURVEY; ATACAMA COSMOLOGY TELESCOPE; EXTRAGALACTIC POINT SOURCES; MICROWAVE BACKGROUND MAPS; HUBBLE-SPACE-TELESCOPE; IN-FLIGHT PERFORMANCE; PRE-LAUNCH STATUS; COMPONENT SEPARATION AB The European Space Agency's Planck satellite, dedicated to studying the early Universe and its subsequent evolution, was launched 14 May 2009 and has been scanning the microwave and submillimetre sky continuously since 12 August 2009. In March 2013, ESA and the Planck Collaboration released the initial cosmology products based on the first 15.5 months of Planck data, along with a set of scientific and technical papers and a web-based explanatory supplement. This paper gives an overview of the mission and its performance, the processing, analysis, and characteristics of the data, the scientific results, and the science data products and papers in the release. The science products include maps of the cosmic microwave background (CMB) and diffuse extragalactic foregrounds, a catalogue of compact Galactic and extragalactic sources, and a list of sources detected through the Sunyaev-Zeldovich effect. The likelihood code used to assess cosmological models against the Planck data and a lensing likelihood are described. Scientific results include robust support for the standard six-parameter Lambda CDM model of cosmology and improved measurements of its parameters, including a highly significant deviation from scale invariance of the primordial power spectrum. The Planck values for these parameters and others derived from them are significantly different from those previously determined. Several large-scale anomalies in the temperature distribution of the CMB, first detected by WMAP, are confirmed with higher confidence. Planck sets new limits on the number and mass of neutrinos, and has measured gravitational lensing of CMB anisotropies at greater than 25 sigma. Planck finds no evidence for non-Gaussianity in the CMB. Planck's results agree well with results from the measurements of baryon acoustic oscillations. Planck finds a lower Hubble constant than found in some more local measures. Some tension is also present between the amplitude of matter fluctuations (sigma(8)) derived from CMB data and that derived from Sunyaev-Zeldovich data. The Planck and WMAP power spectra are off set from each other by an average level of about 2% around the first acoustic peak. Analysis of Planck polarization data is not yet mature, therefore polarization results are not released, although the robust detection of E-mode polarization around CMB hot and cold spots is shown graphically. C1 [Bartlett, J. G.; Bucher, M.; Cardoso, J. -F.; Castexl, G.; Delabrouille, J.; Fromenteau, S.; Ganga, K.; Gauthier, C.; Giraud-Heraud, Y.; Le Jeune, M.; Maurin, L.; Patanchon, G.; Piat, M.; Racine, B.; Remazeilles, M.; Roman, M.; Rosset, C.; Roudier, G.; Smoot, G. E.; Stompor, R.; Welikala, N.] Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, CNRS IN2P3,CEA lrfu,APC, F-75205 Paris 13, France. 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EM jtauber@cosmos.esa.int RI Butler, Reginald/N-4647-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; bonavera, laura/E-9368-2017; SERRA, PAOLO/G-9678-2014; White, Martin/I-3880-2015; Pearson, Timothy/N-2376-2015; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Ghosh, Tuhin/E-6899-2016; Tomasi, Maurizio/I-1234-2016; Lattanzi, Massimiliano/D-8120-2011; Fosalba Vela, Pablo/I-5515-2016; Novikov, Igor/N-5098-2015; Lahteenmaki, Anne/L-5987-2013; Herranz, Diego/K-9143-2014; Toffolatti, Luigi/K-5070-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Pullen, Anthony/I-7007-2015; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Ruiz-Granados, Beatriz/K-2798-2014; Cruz, Marcos/N-3429-2014; Langer, Mathieu/C-5100-2013; Martinez-Gonzalez, Enrique/E-9534-2015; Salerno, Emanuele/A-2137-2010; Churazov, Eugene/A-7783-2013; Barreiro, Rita Belen/N-5442-2014; Remazeilles, Mathieu/N-1793-2015; Renzi, Alessandro/K-4114-2015; OI Reach, William/0000-0001-8362-4094; Hurier, Guillaume/0000-0002-1215-0706; Juvela, Mika/0000-0002-5809-4834; Watson, Robert/0000-0002-5873-0124; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; Bethermin, Matthieu/0000-0002-3915-2015; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Polenta, Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; bonavera, laura/0000-0001-8039-3876; SERRA, PAOLO/0000-0002-7609-3931; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; De Zotti, Gianfranco/0000-0003-2868-2595; Lopez-Caniego, Marcos/0000-0003-1016-9283; Masi, Silvia/0000-0001-5105-1439; White, Martin/0000-0001-9912-5070; Pearson, Timothy/0000-0001-5213-6231; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Lattanzi, Massimiliano/0000-0003-1059-2532; Herranz, Diego/0000-0003-4540-1417; Toffolatti, Luigi/0000-0003-2645-7386; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Pullen, Anthony/0000-0002-2091-8738; Vielva, Patricio/0000-0003-0051-272X; Cruz, Marcos/0000-0002-4767-530X; Langer, Mathieu/0000-0002-9088-2718; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Salerno, Emanuele/0000-0002-3433-3634; Weller, Jochen/0000-0002-8282-2010; Molinari, Diego/0000-0002-7799-3915; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Matarrese, Sabino/0000-0002-2573-1243; Viel, Matteo/0000-0002-2642-5707; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Peel, Mike/0000-0003-3412-2586; Gregorio, Anna/0000-0003-4028-8785; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Renzi, Alessandro/0000-0001-9856-1970; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104 FU CNES; CNRS/INSU-IN2P3; ASI; Danish Natural Research Council; ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MICINN (Spain); JA (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); PRADE (EU) FX Planck is too large a project to allow full acknowledge of all contributions by individuals, institutions, industries, and funding agencies. The main entities involved in the mission operations are as follows. The European Space Agency operates the satellite via its Mission Operations Centre located at ESOC (Darmstadt, Germany) and coordinates scientific operations via the Planck Science Office located at ESAC (Madrid, Spain). Two Consortia, comprising around 100 scientific institutes within Europe, the USA, and Canada, and funded by agencies from the participating countries, developed the scientific instruments LFI and HFI, and continue to operate them via instrument Operations Teams located in Trieste (Italy) and Orsay (France). The Consortia are also responsible for scientific processing of the acquired data. The Consortia are led by the Principal Investigators: J.-L. Puget in France for HFI (funded principally by CNES and CNRS/INSU-IN2P3) and N. Mandolesi in Italy for LFI (funded principally via ASI). NASA's UK Planck Project, based at JPL and involving scientists at many UK institutions, contributes significantly to the efforts of these two Consortia. A third Consortium, led by H. U. Norgaard and Nielsen and supported by the Danish Natural Research Council, contributed to the reflector programme. The author list for this paper has been selected by the Planck Science Team from the Planck Collaboration, and is composed of individuals from all of the above entities who have made multi-year contributions to the development of the mission. It does not pretend to be inclusive of all contributions to Planck. A description of the Planck Collaboration and a list of its members indicating which technical or scientific activities they have been involved in, can be found at (http://www.rssd.esa.int/index.php?project=PLANCK&page=Planck_Collaborat ion). The Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, and JA (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRADE (EU). NR 134 TC 4000 Z9 4005 U1 34 U2 111 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 NOV PY 2014 VL 571 AR A1 DI 10.1051/0004-6361/201321529 PG 48 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600007 ER PT J AU Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bock, JJ Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Bridges, M Bucher, M Burigana, C Butler, RC Cardoso, JF Catalano, A Chamballu, A Chiang, LY Cristensen, PR Church, S Olombi, SC Colombo, LPL Crill, BP Cruz, M Curto, A Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Rose, A de Zotti, G Delabrouillei, J Dick, J Dickinson, C Diego, JM Dole, H Donzeli, S Dore, O Douspis, M Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Franceschi, E Gaier, TC Galeotta, 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, D Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Jaffe, AH Jaffe, TR Jewell, J Jones, WC Juvela, M Kaneaslahti, P Keihanen, E Keskitalo, R Kuveri, K Kisner, TS Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leahy, JP Leonardi, R Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lindholm, V Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maino, D Mandolesi, N Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Mieliaccio, M Mitra, S Moneti, A Montier, L Morgante, G Mortlock, D Moss, A Munshi, D Naselsky, P Natoli, P Netterfield, CB Norgaard-Nielsen, HU Novikov, D Novikov, I O'Dwyer, IJ Osborne, S Paci, F Pagano, L Paladini, R Paoletti, D Partridge, B Pasian, F Patanchon, G Pearson, D Peel, M Perdereau, O Perotto, L Perrotta, F Pierpaoli, E Pietrobon, D Plaszczynski, S Platania, P Pointecouteau, E Polenta, G Ponthieu, N Popa, I Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Rebolo, R Reinecke, M Remazeilles, M Ricciardi, S Riller, T Rocha, G Rosset, C Rossetti, M Roudier, G Rubino-Martin, JA Rusholme, B Sandri, M Salltos, D Scott, A Seitiert, MA Shellard, EPS Spencer, LD Starck, JL Stolyarov, V Stompor, R Stueau, F Sutton, D Sum-Uski, AS Sygnet, JF Tauber, JA Tavaenacco, D Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Tuovinen, J Turler, M Umana, G Valenziano, L Vaiiviita, J Van Tent, B Varis, J Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Watson, R Wilkinson, A Yvon, D Zacchei, A Zonca, A AF Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bock, J. J. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Bridges, M. Bucher, M. Burigana, C. Butler, R. C. Cardoso, J. -F. Catalano, A. Chamballu, A. Chiang, L. -Y Cristensen, P. R. Church, S. Olombi, S. C. Colombo, L. P. L. Crill, B. P. Cruz, M. Curto, A. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rose, A. de Zotti, G. Delabrouillei, J. Dick, J. Dickinson, C. Diego, J. M. Dole, H. Donzeli, S. Dore, O. Douspis, M. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Gaier, T. C. Galeotta, 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. 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. Jaffe, A. H. Jaffe, T. R. Jewell, J. Jones, W. C. Juvela, M. Kaneaslahti, P. Keihanen, E. Keskitalo, R. Kuveri, K. Kisner, T. S. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leahy, J. P. Leonardi, R. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lindholm, V. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maino, D. Mandolesi, N. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Mieliaccio, M. Mitra, S. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Moss, A. Munshi, D. Naselsky, P. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Novikov, D. Novikov, I. O'Dwyer, I. J. Osborne, S. Paci, F. Pagano, L. Paladini, R. Paoletti, D. Partridge, B. Pasian, F. Patanchon, G. Pearson, D. Peel, M. Perdereau, O. Perotto, L. Perrotta, F. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Platania, P. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, I. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Rebolo, R. Reinecke, M. Remazeilles, M. Ricciardi, S. Riller, T. Rocha, G. Rosset, C. Rossetti, M. Roudier, G. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Salltos, D. Scott, D. Seitiert, M. A. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Stueau, F. Sutton, D. Sum-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Tavaenacco, D. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Tucci, M. Tuovinen, J. Turler, M. Umana, G. Valenziano, L. Vaiiviita, J. Van Tent, B. Varis, J. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Watson, R. Wilkinson, A. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. III. LFI systematic uncertainties SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmic background radiation; cosmology: observations; methods: data analysis ID PERFORMANCE; RADIOMETERS; MAPS; SKY AB We present the current estimate of instrumental and systematic effect uncertainties for the Planck-Low Frequency Instrument relevant to the first release of the Planck cosmological results. We give an overview of the main effects and of the tools and methods applied to assess residuals in maps and power spectra. We also present an overall budget of known systematic effect uncertainties, which are dominated by sidelobe straylight pick-up and imperfect calibration. However, even these two effects are at least two orders of magnitude weaker than the cosmic microwave background fluctuations as measured in terms of the angular temperature power spectrum. A residual signal above the noise level is present in the multipole range l < 20, most notably at 30GHz, and is probably caused by residual Galactic straylight contamination. Current analysis aims to further reduce the level of spurious signals in the data and to improve the systematic effects modelling, in particular with respect to straylight and calibration uncertainties. C1 [Bucher, M.; Cardoso, J. -F.; Delabrouillei, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Remazeilles, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, Sorbonne Paris Cite, CNRS, IN2P3,CEA Irfu,Observ Paris,APC, F-75205 Paris 13, France. [Lahteenmaki, A.; Poutanen, T.] Aalto Univ Metsahovi Radio Observ, Kylmala 02540, Finland. [Kunz, M.] African Inst Math Sci, ZA-7701 Rondebosch Cape Town, South Africa. [Natoli, P.; Polenta, G.] Aeenzia Spaziale Italiana, Sci Data Ctr, I-00133 Rome, Italy. [Mandolesi, N.] Agenzia Spaziale ilaliana, I-00198 Rome, Italy. [Ashdown, M.; Bridges, M.; Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Bond, J. R.; Hanson, D.; Martin, P. G.] Univ Toronto, CITA, 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, F-4 Toulouse 4, France. [Bock, J. J.; Dore, O.; Hildebrandt, S. R.; Prezeau, G.; Rocha, G.; Seitiert, M. A.] CALTECH, Pasadena, CA 91125 USA. [Shellard, E. P. S.] Univ Cambridge, Ctr Theoret Cosmol, DAMTP, Cambridge CB3 0WA, England. [Hernandez-Monteagudo, C.] CEFCA, Teruel 44001, Spain. [Borrill, J.; Keskitalo, R.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Rebolo, R.] CSIC, 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.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Kunz, M.; Tucci, M.] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland. [Atrio-Barandela, F.] Univ Salamanca, Fac Ciencias, Dept Fis Fundamental, E-37008 Salamanca, Spain. [Toffolatti, L.] Univ Oviedo, Dept Fis, Oviedo 33007, Spain. [Cruz, M.] Univ Cantabria, Dept Matemat Estadist & Computac, E-39005 Santander, Spain. [Netterfield, C. B.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada. [Rachen, J. P.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Keskitalo, R.] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Colombo, L. P. L.; Pierpaoli, E.] Univ So Calif, Dana & David Dornsife Coll Letter Arts & Sci, Dept Phys & Astron, Los Angeles, CA 90089 USA. [Benoit-Levy, A.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Huffenberger, K. M.] Florida State Univ, Dept Phys, Tallahassee, FL USA. [Juvela, M.; Keihanen, E.; Kuveri, K.; Kurki-Suonio, H.; Lindholm, V.; Poutanen, T.; Sum-Uski, A. -S.; Vaiiviita, J.] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland. [Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 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, Urbana, IL USA. [Liguori, M.; Matarrese, S.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Burigana, C.; Mandolesi, N.; Natoli, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Pagano, L.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Benoit, A.; Bersanelli, M.; Maino, D.; Mennella, A.; Rossetti, M.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy. [Gregorio, A.; Tavaenacco, D.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy. [Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Cristensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark. [Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain. [Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain. [Laureijs, R. J.; Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands. [Partridge, B.] Haverford Coll, Dept Astron, Haverford, PA 19041 USA. [Kuveri, K.; Kurki-Suonio, H.; Lahteenmaki, A.; Lindholm, V.; Poutanen, T.; Sum-Uski, A. -S.; Vaiiviita, J.] Univ Helsinki, Helsinki Inst Phys, FIN-00014 Helsinki, Finland. [Umana, G.] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [Benoit, A.; de Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Frailis, M.; Galeotta, S.; Gregorio, A.; Maris, M.; Pasian, F.; Tavaenacco, D.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Massardi, M.] Ist Radioastron, INAF, I-40129 Bologna, Italy. [Burigana, C.; Butler, R. C.; Cuttaia, F.; de Rose, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Paoletti, D.; Ricciardi, S.; Sandri, M.; Terenzi, L.; Valenziano, L.; Villa, F.] IASF Bologna, INAF, I-40129 Bologna, Italy. [Bersanelli, M.; Donzeli, S.; Maino, D.; Mennella, A.; Rossetti, M.; Tomasi, M.] IASF Bologna, INAF, I-40129 Milan, Italy. [Finelli, F.; Paoletti, D.] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy. [Melchiorri, A.; Pagano, L.] Univ Roma La Sapienza, Ist Nazl Fis Nucl, Sez Roma 1, I-00185 Rome, Italy. [Ponthieu, N.] Univ Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France. 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[Cardoso, J. -F.] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France. [Catalano, A.; Macias-Perez, J. F.; Perotto, L.; Salltos, D.] Univ Grenoble 1, CNRS, IN2P3, Inst Natl Polytech Grenoble,Lab Phys Subatom & Co, F-38026 Grenoble, France. [Van Tent, B.] Univ Paris 11, Phys Theor Lab, F-91405 Orsay, France. [Van Tent, B.] CNRS, F-91405 Orsay, France. [Kisner, T. S.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Ensslin, T. A.; Hernandez-Monteagudo, C.; Hovest, W.; Knoche, J.; Matthai, F.; Rachen, J. P.; Reinecke, M.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Hanson, D.] McGill Univ, McGill Phys, Montreal, PQ H3A 2T8, Canada. [Tuovinen, J.; Varis, J.] VTT Tech Res Ctr Finland, MilliLab, 02044 Espoo, Finland. [Cristensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Crill, B. P.] CALTECH, Pasadena, CA 91125 USA. [Lesgourgues, J.] Ecole Polytech Fed Lausanne, SB ITP LPPC, CH-1015 Lausanne, Switzerland. [Baccigalupi, C.; Bielewicz, P.; Danese, L.; de Zotti, G.; Dick, J.; Gonzalez-Nuevo, J.; Paci, F.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Munshi, D.; Spencer, L. D.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Moss, A.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [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.; Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Armitage-Caplan, C.] Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England. [Lesgourgues, J.] CERN, PH TH, Div Theory, CH-1211 Geneva 23, Switzerland. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Olombi, S. C.; Hivon, E.; Prunet, S.; Wandelt, B. D.] Univ Paris 06, UMR7095, F-75014 Paris, France. [Banday, A. J.; Bernard, J. -P.; Bielewicz, 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. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Mennella, A (reprint author), Univ Milan, Dipartimento Fis, Via Celoria 16, I-20133 Milan, Italy. EM aniello.mennella@fisica.unimi.it RI Butler, Reginald/N-4647-2015; Barreiro, Rita Belen/N-5442-2014; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; bonavera, laura/E-9368-2017; Remazeilles, Mathieu/N-1793-2015; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Cruz, Marcos/N-3429-2014; Martinez-Gonzalez, Enrique/E-9534-2015; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Mazzotta, Pasquale/B-1225-2016; OI Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Peel, Mike/0000-0003-3412-2586; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Colombo, Loris/0000-0003-4572-7732; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; bonavera, laura/0000-0001-8039-3876; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; De Zotti, Gianfranco/0000-0003-2868-2595; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Pierpaoli, Elena/0000-0002-7957-8993; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; Cruz, Marcos/0000-0002-4767-530X; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; Mazzotta, Pasquale/0000-0002-5411-1748; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Valiviita, Jussi/0000-0001-6225-3693; Juvela, Mika/0000-0002-5809-4834; Watson, Robert/0000-0002-5873-0124; Zacchei, Andrea/0000-0003-0396-1192; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X NR 56 TC 35 Z9 34 U1 2 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2014 VL 571 AR A3 DI 10.1051/0004-6361/201321574 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600024 ER PT J AU Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartlett, JG Benabed, K Benoit-Ley, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bock, JJ Bond, JR Borrill, J Bouchet, FR Bridges, M Burigana, C Butler, RC Cardoso, JF Catalano, A Challinor, A Chamballu, A Chiang, HC Chiang, LY Christensen, PR Clements, DL Colombo, LPL Couchot, F Crill, BP Curto, A Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Diego, JM Donzelli, S Dore, O Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Giard, M Giardino, G Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Hanson, D Harrison, DL Helou, G Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hovest, W Huffenberger, KM Jones, WC Juvela, M Keihanen, E Keskitalo, R Kisner, TS Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leonardi, R Lewis, A Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Mandolesi, N Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Mazzotta, P Meinhold, PR Melchiorri, A Mendes, L Migliaccio, M Mitra, S Moneti, A Montier, L Morgante, G Mortlock, D Moss, A Munshi, D Naselsky, P Nati, F Natoli, P Norgaard-Nielsen, HU Noviello, F Novikov, D Novikov, I Osborne, S Oxborrow, CA Pagano, L Pajot, F Paoletti, D Pasian, F Patanchon, G Perdereau, O Perrotta, F Piacentini, F Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Pratt, GW Prezeau, G Puget, JL Rachen, JP Reach, WT Reinecke, M Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Rubino-Martin, JA Rusholme, B Santos, D Savini, G Scott, D Seiffert, MD Shellard, EPS Spencer, LD Sunyaev, R Sureau, F Suur-Uski, AS Sygnet, JF Tauber, JA Tavagnacco, D Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Turler, M Valenziano, L Valiviita, J Van Tent, B Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD White, M Yvon, D Zacchei, A Zibin, JP Zonca, A AF Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Benabed, K. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bock, J. J. Bond, J. R. Borrill, J. Bouchet, F. R. Bridges, M. Burigana, C. Butler, R. C. Cardoso, J. -F. Catalano, A. Challinor, A. Chamballu, A. Chiang, H. C. Chiang, L. -Y Christensen, P. R. Clements, D. L. Colombo, L. P. L. Couchot, F. 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. Diego, J. M. Donzelli, S. Dore, O. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Hanson, D. Harrison, D. L. Helou, G. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hovest, W. Huffenberger, K. M. Jones, W. C. Juvela, M. Keihanen, E. Keskitalo, R. Kisner, T. S. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leonardi, R. Lewis, A. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Mandolesi, N. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Mazzotta, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Migliaccio, M. Mitra, S. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Moss, A. Munshi, D. Naselsky, P. Nati, F. Natoli, P. Norgaard-Nielsen, H. U. Noviello, F. Novikov, D. Novikov, I. Osborne, S. Oxborrow, C. A. Pagano, L. Pajot, F. Paoletti, D. Pasian, F. Patanchon, G. Perdereau, O. Perrotta, F. Piacentini, F. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Pratt, G. W. Prezeau, G. Puget, J. -L. Rachen, J. P. Reach, W. T. Reinecke, M. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Rubino-Martin, J. A. Rusholme, B. Santos, D. Savini, G. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Sunyaev, R. Sureau, F. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Tavagnacco, D. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Tucci, M. Tuerler, M. Valenziano, L. Valiviita, J. Van Tent, B. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. White, M. Yvon, D. Zacchei, A. Zibin, J. P. Zonca, A. CA Planck Collaboration TI Planck 2013 results. XXVII. Doppler boosting of the CMB: Eppur si muove SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology: observations; cosmic background radiation; reference systems; relativistic processes ID SKY MAPS; MICROWAVE; ABERRATION; DIPOLE; ANISOTROPY AB Our velocity relative to the rest frame of the cosmic microwave background (CMB) generates a dipole temperature anisotropy on the sky which has been well measured for more than 30 years, and has an accepted amplitude of v/c = 1 x 23(-10), or v = 369 km s(-1). In addition to this signal generated by Doppler boosting of the CMB monopole, our motion also modulates and aberrates the CMB temperature fluctuations (as well as every other source of radiation at cosmological distances). This is an order 10 3 e ff ect applied to fluctuations which are already one part in roughly 105, so it is quite small. Nevertheless, it becomes detectable with the all- sky coverage, high angular resolution, and low noise levels of the Planck satellite. Here we report a first measurement of this velocity signature using the aberration and modulation e ff ects on the CMB temperature anisotropies, finding a component in the known dipole direction, (l; b) = (264 ffi; 48 ffi), of 384 km s 1 +/- 78 km s 1 (stat :) +/- 115 km s 1 (syst :). This is a significant confirmation of the expected velocity. C1 [Bartlett, J. G.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Patanchon, G.; Rosset, C.] Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, CNRS IN2P3,CEA Irfu,APC, F-75205 Paris 13, France. [Lahteenmaki, A.] Aalto Univ, Metsahovi Radio Observ, Aalto 00076, Finland. [Lahteenmaki, A.] Dept Radio Sci & Engn, Aalto 00076, Finland. [Kunz, M.] African Inst Math Sci, ZA-7945 Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana, Sci Data Ctr, I-00133 Rome, Italy. [Mandolesi, N.] Agenzia Spaziale Italiana, I-00198 Rome, Italy. [Ashdown, M.; Bridges, M.; Curto, A.; Hobson, M.; Lasenby, A.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa. [Bond, J. R.; Hanson, D.; Martin, P. G.] Univ Toronto, CITA, University Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] CNRS, IRAP, F-31028 Toulouse 4, France. [Bock, J. J.; Helou, G.; Hildebrandt, S. R.; Prezeau, G.; Rocha, G.; Seiffert, M. D.] CALTECH, Pasadena, CA 91125 USA. [Challinor, A.; Shellard, E. P. S.] Univ Cambridge, DAMTP, Ctr Theoret Cosmol, Cambridge CB3 0WA, England. [Borrill, J.; Keskitalo, R.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Chamballu, A.; Yvon, D.] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. [Linden-Vornle, M.; Norgaard-Nielsen, H. U.; Oxborrow, C. A.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Kunz, M.; Tucci, M.] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland. [Atrio-Barandela, F.] Univ Salamanca, Fac Ciencias, Dept Fis Fundamental, E-37008 Salamanca, Spain. [Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain. [Rachen, J. P.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Keskitalo, R.] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA. [Scott, D.; Zibin, J. P.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Colombo, L. P. L.; Pierpaoli, E.] Univ So Calif, Dept Phys & Astron, Dana & David Dornsife Coll Letter Arts & Sci, Los Angeles, CA 90089 USA. [Benoit-Levy, A.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Lewis, A.] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Huffenberger, K. M.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Juvela, M.; Keihanen, E.; Kurki-Suonio, H.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland. [Chiang, H. C.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [White, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 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, Urbana, IL USA. [Liguori, M.; Matarrese, S.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Burigana, C.; Mandolesi, N.; Natoli, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Nati, F.; Pagano, L.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Bersanelli, M.; Tomasi, M.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy. [Gregorio, A.; Tavagnacco, D.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy. [Mazzotta, P.; Vittorio, N.] Univ Roma Tor Vergata, Dipartmento Fis, I-00133 Rome, Italy. [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark. [Rubino-Martin, J. A.] Univ La Laguna, Dept Astrofis, Tenerife 38206, Spain. [Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Madrid 28692, Spain. [Giardino, G.; Laureijs, R. J.; Tauber, J. A.] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands. [Kurki-Suonio, H.; Lahteenmaki, A.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Helsinki Inst Phys, FIN-00014 Helsinki, Finland. [de Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Polenta, G.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Frailis, M.; Galeotta, S.; Gregorio, A.; Maris, M.; Pasian, F.; Tavagnacco, D.; Zacchei, A.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy. [Massardi, M.] INAF Ist Radioastron, I-40129 Bologna, 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.; Ricciardi, S.; Terenzi, L.; Valenziano, L.; Villa, F.] INAF IASF Bologna, I-20133 Bologna, Italy. [Bersanelli, M.; Donzelli, S.; Tomasi, M.] INAF IASF Milano, Milan, Italy. [Finelli, F.; Paoletti, D.] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy. [Melchiorri, A.; Pagano, L.] Univ Roma La Sapienza, Sez Roma 1, Ist Nazl Fis Nucl, I-00185 Rome, Italy. [Gregorio, A.] Ist Nazl Fis Nucl, I-34127 Trieste, Italy. [Ponthieu, N.] Univ Grenoble 1, CNRS INSU, Inst Planetol & Astrophys Grenoble, UMR 5274, F-38041 Grenoble, France. [Tuerler, M.] Univ Geneva, ISDC Data Ctr Astrophys, CH-1290 Sauverny, Switzerland. [Mitra, S.] IUCAA, Pune 411007, Maharashtra, India. [Clements, D. L.; Mortlock, D.; Novikov, D.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Rusholme, B.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Aghanim, N.; Aumont, J.; Chamballu, A.; Kunz, M.; Pajot, F.; Ponthieu, N.; Puget, J. -L.] Univ Paris 11, Inst Astrophys Spatiale, CNRS, UMR 8617, F-91405 Orsay, France. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Cardoso, J. -F.; Hivon, E.; Moneti, A.; Sygnet, J. -F.; Wandelt, B. D.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Popa, L.] Inst Space Sci, Bucharest 077125, Romania. [Chiang, L. -Y] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Bridges, M.; Challinor, A.; Efstathiou, G.; Gratton, S.; Harrison, D. L.; Migliaccio, M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Eriksen, H. K.; Hansen, F. K.; Lilje, P. B.; Valiviita, J.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife 38205, Spain. [Barreiro, R. B.; Curto, A.; Diego, J. M.; Gonzalez-Nuevo, J.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Toffolatti, L.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, Santander 39065, Spain. [Bartlett, J. G.; Bock, J. J.; Colombo, L. P. L.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Lawrence, C. R.; Mitra, S.; Pietrobon, D.; Prezeau, G.; Rocha, G.; Seiffert, M. D.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Davies, R. D.; Davis, R. J.; Noviello, F.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Bridges, M.; Challinor, A.; Gratton, S.; Harrison, D. L.; Lasenby, A.; Migliaccio, M.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Couchot, F.; Perdereau, O.; Plaszczynski, S.; Tristram, M.; Tucci, M.] Univ Paris 11, CNRS, IN2P3, LAL, F-91405 Orsay, France. [Catalano, A.; Lamarre, J. -M.] CNRS, Observ Paris, LERMA, F-75014 Paris, France. [Arnaud, M.; Bobin, J.; Chamballu, A.; Marshall, D. J.; Pratt, G. W.; Sureau, F.] Univ Paris Diderot, CNRS, CEA DSM, Lab AIM,IRFU Serv Astrophys, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, Lab Traitement & Commun Informat, UMR 5141, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France. [Catalano, A.; Macias-Perez, J. F.; Santos, D.] Univ Grenoble 1, Inst Natl Polytech Grenoble, CNRS IN2P3, Lab Phys Subatom & Cosmol, F-38026 Grenoble, France. [Van Tent, B.] Univ Paris 11, Phys Theor Lab, F-91405 Orsay, France. [Van Tent, B.] CNRS, F-91405 Orsay, France. [Kisner, T. S.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Ensslin, T. A.; Hovest, W.; Knoche, J.; Rachen, J. P.; Reinecke, M.; Riller, T.; Sunyaev, R.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Hanson, D.] McGill Univ, McGill Phys, Montreal, PQ H3A 2T8, Canada. [Christensen, P. R.; Naselsky, P.; Novikov, I.] Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Crill, B. P.] CALTECH, Observat Cosmol, Pasadena, CA 91125 USA. [Savini, G.] UCL, Opt Sci Lab, London, England. [Baccigalupi, C.; Bielewicz, P.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Munshi, D.; Spencer, L. D.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Moss, A.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Sunyaev, R.] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Osborne, S.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Armitage-Caplan, C.] Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Hivon, E.; Wandelt, B. D.] Univ Paris 06, UMR7095, F-75014 Paris, France. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Scott, D (reprint author), Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V5Z 1M9, Canada. EM dscott@phas.ubc.ca RI Barreiro, Rita Belen/N-5442-2014; Butler, Reginald/N-4647-2015; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; Nati, Federico/I-4469-2016; popa, lucia/B-4718-2012; Piacentini, Francesco/E-7234-2010; Atrio-Barandela, Fernando/A-7379-2017; White, Martin/I-3880-2015; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Martinez-Gonzalez, Enrique/E-9534-2015; Gonzalez-Nuevo, Joaquin/I-3562-2014; OI Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Ricciardi, Sara/0000-0002-3807-4043; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Nati, Federico/0000-0002-8307-5088; Piacentini, Francesco/0000-0002-5444-9327; Atrio-Barandela, Fernando/0000-0002-2130-2513; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; De Zotti, Gianfranco/0000-0003-2868-2595; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; White, Martin/0000-0001-9912-5070; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Pierpaoli, Elena/0000-0002-7957-8993; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Bouchet, Francois/0000-0002-8051-2924; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Reach, William/0000-0001-8362-4094 FU ESA FX The development of Planck has been supported by: ESA; CNES and CNRS / INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at h t t p : / / w w w. s c i o p s. e s a. i n t / i n d e x. p h p ? p r o j e c t = p l a n c k & p a g e = P l a n c k _ C o l l a b o r a t i o n. Some of the results in this paper have been derived using the H E A L P i x package. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the O ffi ce of Science of the US Department of Energy under Contract No. DE-AC02-05CH11231. We acknowledge support from the Science and Technology Facilities Council [ grant number ST / I000976 / 1]. NR 66 TC 80 Z9 79 U1 3 U2 10 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2014 VL 571 AR A27 DI 10.1051/0004-6361/201321556 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600019 ER PT J AU Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bock, JJ Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Bridges, M Bucher, M Burigana, C Butler, RC Cappellini, B Cardoso, JF Catalano, A Chamballu, A Chen, X Chiang, LY Christensen, PR Church, S Colombi, S Colombo, LPL Crill, BP Cruz, M Curto, A Cattaia, 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 Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Falvella, MC Finelli, F Forni, O Frailis, M Franceschi, E Gaier, TC Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gjerlow, E Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Hanson, D Harrison, D Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Jaffe, AH Jaffe, TR Jewel, J Jones, WC Juvela, M Kangaslahti, P Keihanen, E Keskitalo, R Kiiveri, K Kisner, TS Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Lattanzi, M Laureijs, RJ Lawrence, CR Leach, S Leahy, JP Leonardi, R Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lindholm, V Lopez-Caniego, M Lubin, PM Macias-Perez, JE Maggio, G Maino, D Mandolesi, N Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Moneti, A Montier, L Morgantes, G Morisset, N Mortlock, D Moss, A Munshi, D Naseisky, P Natoli, P Netterfield, CB Norgaard-Nielsen, HU Novikov, D Novikov, I O'Dwyer, IJ Osborne, S Paci, F Pagano, L Paladini, R Paoletti, D Partridge, B Pasian, F Patanchon, G Peel, M Perdereau, O Perotto, L Perrotta, F Pierpaoli, E Pietrobon, D Plaszczynski, S Platania, P Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Reach, WT Rebolo, R Reinecke, M Remazeilles, M Ricciardi, S Riller, T Robbers, G Rocha, G Rosset, C Rossetti, M Roudier, G Rubino-Martin, JA Rusholme, B Salerno, E Sandri, M Santos, D Scott, D Seiffert, MD Shellard, EPS Spencer, LD Starck, JL Stolyarov, V Stompor, R Sureau, F 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 Varis, J Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Watson, R Wehus, IK White, SDM Wilkson, A Yvon, D Zacchei, A Zonca, A AF Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bock, J. J. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Bridges, M. Bucher, M. Burigana, C. Butler, R. C. Cappellini, B. Cardoso, J. -F. Catalano, A. Chamballu, A. Chen, X. Chiang, L. -Y Christensen, P. R. Church, S. Colombi, S. Colombo, L. P. L. Crill, B. P. Cruz, M. Curto, A. Cattaia, 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. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Falvella, M. C. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Gaier, T. C. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gjerlow, E. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Hanson, D. Harrison, D. 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. Jaffe, A. H. Jaffe, T. R. Jewel, J. Jones, W. C. Juvela, M. Kangaslahti, P. Keihanen, E. Keskitalo, R. Kiiveri, K. Kisner, T. S. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Lattanzi, M. Laureijs, R. J. Lawrence, C. R. Leach, S. Leahy, J. P. Leonardi, R. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lindholm, V. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. E. Maggio, G. Maino, D. Mandolesi, N. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Moneti, A. Montier, L. Morgantes, G. Morisset, N. Mortlock, D. Moss, A. Munshi, D. Naseisky, P. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Novikov, D. Novikov, I. O'Dwyer, I. J. Osborne, S. Paci, F. Pagano, L. Paladini, R. Paoletti, D. Partridge, B. Pasian, F. Patanchon, G. Peel, M. Perdereau, O. Perotto, L. Perrotta, F. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Platania, P. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Reach, W. T. Rebolo, R. Reinecke, M. Remazeilles, M. Ricciardi, S. Riller, T. Robbers, G. Rocha, G. Rosset, C. Rossetti, M. Roudier, G. Rubino-Martin, J. A. Rusholme, B. Salerno, E. Sandri, M. Santos, D. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sureau, F. 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. Tuerler, M. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Varis, J. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Watson, R. Wehus, I. K. White, S. D. M. Wilkson, A. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. II. Low Frequency Instrument data processing SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmic background radiation; methods: data analysis; cosmology: observations; surveys ID MAP-MAKING ALGORITHM; PRE-LAUNCH STATUS; DATA SETS; RADIOMETERS; NOISE AB We describe the data processing pipeline of the Planck Low Frequency Instrument (LFI) data processing centre (DPC) to create and characterize full-sky maps based on the first 15.5 months of operations at 30, 44, and 70 GHz. In particular, we discuss the various steps involved in reducing the data, from telemetry packets through to the production of cleaned, calibrated timelines and calibrated frequency maps. Data are continuously calibrated using the modulation induced on the mean temperature of the cosmic microwave background radiation by the proper motion of the spacecraft. Sky signals other than the dipole are removed by an iterative procedure based on simultaneous fitting of calibration parameters and sky maps. Noise properties are estimated from time-ordered data after the sky signal has been removed, using a generalized least squares map-making algorithm. A destriping code (Madam) is employed to combine radiometric data and pointing information into sky maps, minimizing the variance of correlated noise. Noise covariance matrices, required to compute statistical uncertainties on LFI and Planck products, are also produced. Main beams are estimated down to the approximate to-20 dB level using Jupiter transits, which are also used for the geometrical calibration of the focal plane. C1 [Bucher, M.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Remazeilles, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, CNRS IN2P3,CEA lrfu,APC, F-75205 Paris 13, France. [Lahteenmaki, A.; Poutanen, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Kunz, M.] African Inst Math Sci, ZA-7945 Cape Town, South Africa. [Natoli, P.; Polenta, G.] Aeenzia Spaziale Italiana, Sci Data Ctr, I-00133 Rome, Italy. [Falvella, M. C.; Mandolesi, N.] Agenzia Spaziale Ilaliana, Rome, Italy. [Ashdown, M.; Bridges, M.; Curto, A.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Bond, J. R.; Hanson, D.; Martin, P. G.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Salerno, E.] CNR, ISTI, I-56100 Pisa, Italy. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.] CNRS, IRAP, F-31028 Toulouse 4, France. [Bock, J. J.; Dore, O.; Hildebrandt, S. R.; Prezeau, G.; Rocha, G.; Seiffert, M. D.] CALTECH, Pasadena, CA 91125 USA. [Shellard, E. P. S.] Univ Cambridge, Ctr Theoret Cosmol, DAMTP, Cambridge CB3 0WA, England. 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EM zacchei@oats.inaf.it RI Barreiro, Rita Belen/N-5442-2014; Remazeilles, Mathieu/N-1793-2015; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Tomasi, Maurizio/I-1234-2016; Lattanzi, Massimiliano/D-8120-2011; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; popa, lucia/B-4718-2012; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; bonavera, laura/E-9368-2017; Martinez-Gonzalez, Enrique/E-9534-2015; Salerno, Emanuele/A-2137-2010; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Cruz, Marcos/N-3429-2014; Butler, Reginald/N-4647-2015; OI Pierpaoli, Elena/0000-0002-7957-8993; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Peel, Mike/0000-0003-3412-2586; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Tomasi, Maurizio/0000-0002-1448-6131; Lattanzi, Massimiliano/0000-0003-1059-2532; Colombo, Loris/0000-0003-4572-7732; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; bonavera, laura/0000-0001-8039-3876; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; De Zotti, Gianfranco/0000-0003-2868-2595; Reach, William/0000-0001-8362-4094; Juvela, Mika/0000-0002-5809-4834; Watson, Robert/0000-0002-5873-0124; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Salerno, Emanuele/0000-0002-3433-3634; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; Cruz, Marcos/0000-0002-4767-530X; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Butler, Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924 NR 54 TC 48 Z9 47 U1 2 U2 14 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2014 VL 571 AR A2 DI 10.1051/0004-6361/201321550 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600016 ER PT J AU Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bock, JJ Bonaldi, A Bond, JR Borrill, J Bouchet, FR Bridges, M Bucher, M Burigana, C Butler, RC Cardoso, JF Catalano, A Chamballu, A Chiang, LY Christensen, PR Church, S 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 Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Franceschi, E Gaier, TC Galeotta, S Ganga, K Giard, M Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Hanson, D Harrison, D Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Jaffe, AH Jaffe, TR Jewell, J Jones, WC Juvela, M Kangaslahti, P Keihanen, E Keskitalo, R Kiiveri, K Kisner, TS Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leahy, JP Leonardi, R Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lindholm, V Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maino, D Mandolesi, N Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Moneti, A Montier, L Morgante, G Mortlock, D Moss, A Munshi, D Naselsky, P Natoli, P Netterfield, CB Norgaard-Nielsen, HU Novikov, D Novikov, I O'Dwyer, IJ Osborne, S Paci, F Pagano, L Paoletti, D Partridge, B Pasian, F Patanchon, G Perdereau, O Perotto, L Perrotta, F Pierpaoli, E Pietrobon, D Plaszczynski, S Platania, P Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Rebolo, R Reinecke, M Remazeilles, M Ricciardi, S Riller, T Rocha, G Rosset, C Roudier, G Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Scott, D Seiffert, MD Shellard, EPS Spencer, LD Starck, JL Stolyarov, V Stompor, R Sureau, F 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 Varis, J Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Zacchei, A Zonca, A AF Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bock, J. J. Bonaldi, A. Bond, J. R. Borrill, J. Bouchet, F. R. Bridges, M. Bucher, M. Burigana, C. Butler, R. C. Cardoso, J. -F. Catalano, A. Chamballu, A. Chiang, L. -Y Christensen, P. R. Church, S. 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. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Gaier, T. C. Galeotta, S. Ganga, K. Giard, M. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Hanson, D. Harrison, D. 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. Jaffe, A. H. Jaffe, T. R. Jewell, J. Jones, W. C. Juvela, M. Kangaslahti, P. Keihanen, E. Keskitalo, R. Kiiveri, K. Kisner, T. S. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leahy, J. P. Leonardi, R. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lindholm, V. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maino, D. Mandolesi, N. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Moss, A. Munshi, D. Naselsky, P. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Novikov, D. Novikov, I. O'Dwyer, I. J. Osborne, S. Paci, F. Pagano, L. Paoletti, D. Partridge, B. Pasian, F. Patanchon, G. Perdereau, O. Perotto, L. Perrotta, F. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Platania, P. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Rebolo, R. Reinecke, M. Remazeilles, M. Ricciardi, S. Riller, T. Rocha, G. Rosset, C. Roudier, G. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sureau, F. 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. Tuerler, M. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Varis, J. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. IV. Low Frequency Instrument beams and window functions SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: data analysis; cosmic background radiation; telescopes ID PROBE WMAP OBSERVATIONS; PRE-LAUNCH STATUS; POWER SPECTRUM; MICROWAVE; MAPS; ERRORS AB This paper presents the characterization of the in-flight beams, the beam window functions, and the associated uncertainties for the Planck Low Frequency Instrument (LFI). Knowledge of the beam profiles is necessary for determining the transfer function to go from the observed to the actual sky anisotropy power spectrum. The main beam distortions affect the beam window function, complicating the reconstruction of the anisotropy power spectrum at high multipoles, whereas the sidelobes affect the low and intermediate multipoles. The in-flight assessment of the LFI main beams relies on the measurements performed during Jupiter observations. By stacking the data from multiple Jupiter transits, the main beam profiles are measured down to -20 dB at 30 and 44 GHz, and down to -25 dB at 70 GHz. The main beam solid angles are determined to better than 0.2% at each LFI frequency band. The Planck pre-launch optical model is conveniently tuned to characterize the main beams independently of any noise effects. This approach provides an optical model whose beams fully reproduce the measurements in the main beam region, but also allows a description of the beams at power levels lower than can be achieved by the Jupiter measurements themselves. The agreement between the simulated beams and the measured beams is better than 1% at each LFI frequency band. The simulated beams are used for the computation of the window functions for the effective beams. The error budget for the window functions is estimated from both main beam and sidelobe contributions, and accounts for the radiometer bandshapes. 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EM sandri@iasfbo.inaf.it RI Barreiro, Rita Belen/N-5442-2014; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; popa, lucia/B-4718-2012; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; Remazeilles, Mathieu/N-1793-2015; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Vielva, Patricio/F-6745-2014; Martinez-Gonzalez, Enrique/E-9534-2015; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Valiviita, Jussi/A-9058-2016; Butler, Reginald/N-4647-2015; OI Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Valenziano, Luca/0000-0002-1170-0104; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Finelli, Fabio/0000-0002-6694-3269; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; De Zotti, Gianfranco/0000-0003-2868-2595; Lopez-Caniego, Marcos/0000-0003-1016-9283; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Toffolatti, Luigi/0000-0003-2645-7386; Vielva, Patricio/0000-0003-0051-272X; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; Valiviita, Jussi/0000-0001-6225-3693; Pierpaoli, Elena/0000-0002-7957-8993; Juvela, Mika/0000-0002-5809-4834; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Umana, Grazia/0000-0002-6972-8388; Scott, Douglas/0000-0002-6878-9840; Frailis, Marco/0000-0002-7400-2135; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Butler, Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099 FU CNES; CNRS/INSU-IN2P3-INP; ASI; Italian Space Agency (ASI); INAF; Academy of Finland [253204, 256265, 257989]; European Community [RI-283493]; Spanish Ministerio de Ciencia e Innovacion through the Plan Nacional del Espacio y Plan Nacional de Astronomia y Astrofisica; Space Agency of the German Aerospace Center (DLR) [50OP0901]; Max Planck Society; National Energy Research Scientific Computing Center - Office of Science of the US Department of Energy [DE-AC02-05CH11231]; ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MICINN (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); PRACE (EU) FX Planck is too large a project to allow full acknowledgement of all contributions by individuals, institutions, industries, and funding agencies. The main entities involved in the mission operations are as follows. The European Space Agency (ESA) operates the satellite via its Mission Operations Centre located at ESOC (Darmstadt, Germany) and coordinates scientific operations via the Planck Science Office located at ESAC (Madrid, Spain). Two Consortia, comprising around 50 scientific institutes within Europe, the USA, and Canada, and funded by agencies from the participating countries, developed the scientific instruments LFI and HFI, and continue to operate them via Instrument Operations Teams located in Trieste (Italy) and Orsay (France). The Consortia are also responsible for scientific processing of the acquired data. The Consortia are led by the Principal Investigators: J. L. Puget in France for HFI (funded principally by CNES and CNRS/INSU-IN2P3-INP) and N. Mandolesi in Italy for LFI (funded principally via ASI). NASA US Planck Project, based at JPL and involving scientists at many US institutions, contributes significantly to the efforts of these two Consortia. The author list for this paper has been selected by the Planck Science Team, and is composed of individuals from all of the above entities who have made multi-year contributions to the development of the mission. It does not pretend to be inclusive of all contributions. The Planck-LFI project is developed by an International Consortium lead by Italy and involving Canada, Finland, Germany, Norway, Spain, Switzerland, UK, USA. The Italian contribution to Planck is supported by the Italian Space Agency (ASI) and INAF. This work was supported by the Academy of Finland grants 253204, 256265, and 257989. This work was granted access to the HPC resources of CSC made available within the Distributed European Computing Initiative by the PRACE-2IP, receiving funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement RI-283493. We thank CSC-IT Center for Science Ltd (Finland) for computational resources. We acknowledge financial support provided by the Spanish Ministerio de Ciencia e Innovacion through the Plan Nacional del Espacio y Plan Nacional de Astronomia y Astrofisica. We acknowledge the Max Planck Institute for Astrophysics Planck Analysis Centre (MPAC), funded by the Space Agency of the German Aerospace Center (DLR) under grant 50OP0901 with resources of the German Federal Ministry of Economics and Technology, and by the Max Planck Society. This work has made use of the Planck satellite simulation package (Level-S), which is assembled by the Max Planck Institute for Astrophysics Planck Analysis Centre (MPAC) Reinecke et al. (2006). We acknowledge financial support provided by the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the US Department of Energy under Contract No. DE-AC02-05CH11231. Some of the results in this paper have been derived using the HEALPix package Gorski et al. (2005). The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU).; A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collabora tion NR 59 TC 41 Z9 40 U1 3 U2 11 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2014 VL 571 AR A4 DI 10.1051/0004-6361/201321544 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600014 ER PT J AU Aghanim, N Armitage-Caplan, C Arnaud, M Ashdown, M Atrio-Barandela, F Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Battaner, E Benabed, K Benoit, A Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bock, JJ Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Bridges, M Bucher, M Burigana, C Butler, RC Cappellini, B Cardoso, JF Catalano, A Chamballu, A Chen, X Chiang, LY Christensen, PR Church, S 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 Dupac, X Efstathiou, G Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Franceschi, E Gaier, TC Galeotta, S Ganga, K Giard, M Giardino, G Giraud-Heraud, Y Gjerlow, E Gonzalez-Nuevo, J Gorski, KM Gratton, S Gregorio, A Gruppuso, A Hansen, FK Hanson, D Harrison, D Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Jaffe, AH Jaffe, TR Jewell, J Jones, WC Juvela, M Kangaslahti, P Keihanen, E Keskitalo, R Kisner, TS Knoche, J Knox, L Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Laureijs, RJ Lawrence, CR Leach, S Leahy, JP Leonard, R Lesgourgues, J Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maino, D Mandolesi, N Maris, M Marshall, DJ Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Matthai, F Mazzotta, P Meinhold, PR Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Moneti, A Montier, L Morgante, G Mortlock, D Moss, A Munshi, D Naselsky, P Natoli, P Netterfield, CB Norgaard-Nielsen, HU Novikov, D Novikov, I O'Dwyer, IJ Osborne, S Paci, F Pagano, L Paladini, R Paoletti, D Partridge, B Pasian, F Patanchon, G Pearson, D Peel, M Perdereau, O Perotto, L Perrotta, F Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Ponthieu, N Popa, L Poutanen, T Pratt, GW Prezeau, G Prunet, S Puget, JL Rachen, JP Rebolo, R Reinecke, M Remazeilles, M Ricciardi, S Riller, T Rocha, G Rosset, C Rossetti, M Roudier, G Rubino-Martin, JA Rusholme, B Sandri, M Santos, D Scott, D Seiffert, MD Shellard, EPS Spencer, LD Starck, JL Stolyarov, V Stompor, R Sureau, F 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 Varis, J Vielva, P Villa, F Vittorio, N Wade, LA Wandelt, BD Watson, R Wilkinson, A Yvon, D Zacchei, A Zonca, A AF Aghanim, N. Armitage-Caplan, C. Arnaud, M. Ashdown, M. Atrio-Barandela, F. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Battaner, E. Benabed, K. Benoit, A. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bock, J. J. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Bridges, M. Bucher, M. Burigana, C. Butler, R. C. Cappellini, B. Cardoso, J. -F. Catalano, A. Chamballu, A. Chen, X. Chiang, L. -Y Christensen, P. R. Church, S. 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. Dupac, X. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Gaier, T. C. Galeotta, S. Ganga, K. Giard, M. Giardino, G. Giraud-Heraud, Y. Gjerlow, E. Gonzalez-Nuevo, J. Gorski, K. M. Gratton, S. Gregorio, A. Gruppuso, A. Hansen, F. K. Hanson, D. Harrison, D. 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. Jaffe, A. H. Jaffe, T. R. Jewell, J. Jones, W. C. Juvela, M. Kangaslahti, P. Keihanen, E. Keskitalo, R. Kisner, T. S. Knoche, J. Knox, L. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Laureijs, R. J. Lawrence, C. R. Leach, S. Leahy, J. P. Leonard, R. Lesgourgues, J. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maino, D. Mandolesi, N. Maris, M. Marshall, D. J. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Matthai, F. Mazzotta, P. Meinhold, P. R. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Moss, A. Munshi, D. Naselsky, P. Natoli, P. Netterfield, C. B. Norgaard-Nielsen, H. U. Novikov, D. Novikov, I. O'Dwyer, I. J. Osborne, S. Paci, F. Pagano, L. Paladini, R. Paoletti, D. Partridge, B. Pasian, F. Patanchon, G. Pearson, D. Peel, M. Perdereau, O. Perotto, L. Perrotta, F. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Ponthieu, N. Popa, L. Poutanen, T. Pratt, G. W. Prezeau, G. Prunet, S. Puget, J. -L. Rachen, J. P. Rebolo, R. Reinecke, M. Remazeilles, M. Ricciardi, S. Riller, T. Rocha, G. Rosset, C. Rossetti, M. Roudier, G. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Santos, D. Scott, D. Seiffert, M. D. Shellard, E. P. S. Spencer, L. D. Starck, J. -L. Stolyarov, V. Stompor, R. Sureau, F. 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. Tuerler, M. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Varis, J. Vielva, P. Villa, F. Vittorio, N. Wade, L. A. Wandelt, B. D. Watson, R. Wilkinson, A. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck 2013 results. V. LFI calibration SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmic background radiation; instrumentation: polarimeters; methods: data analysis ID MICROWAVE-ANISOTROPY-PROBE; PRE-LAUNCH STATUS; WMAP OBSERVATIONS; SKY MAPS; GHZ AB We discuss the methods employed to photometrically calibrate the data acquired by the Low Frequency Instrument on Planck. Our calibration is based on a combination of the orbital dipole plus the solar dipole, caused respectively by the motion of the Planck spacecraft with respect to the Sun and by motion of the solar system with respect to the cosmic microwave background (CMB) rest frame. The latter provides a signal of a few mK with the same spectrum as the CMB anisotropies and is visible throughout the mission. In this data release we rely on the characterization of the solar dipole as measured by WMAP. We also present preliminary results (at 44 GHz only) on the study of the Orbital Dipole, which agree with the WMAP value of the solar system speed within our uncertainties. We compute the calibration constant for each radiometer roughly once per hour; in order to keep track of changes in the detectors' gain. Since non-idealities in the optical response of the beams proved to be important, we implemented a fast convolution algorithm which considers the full beam response in estimating the signal generated by the dipole. Moreover, in order to further reduce the impact of residual systematics due to sidelobes, we estimated time variations in the calibration constant of the 30 GHz radiometers (the ones with the largest sidelobes) using the signal of an internal reference load at 4 K instead of the CMB dipole. We have estimated the accuracy of the LFI calibration following two strategies: (1) we have run a set of simulations to assess the impact of statistical errors and systematic effects in the instrument and in the calibration procedure; and (2) we have performed a number of internal consistency checks on the data and on the brightness temperature of Jupiter. Errors in the calibration of this Planck/LFI data release are expected to be about 0.6% at 44 and 70 GHz, and 0.8% at 30 GHz. Both these preliminary results at low and high l are consistent with WMAP results within uncertainties and comparison of power spectra indicates good consistency in the absolute calibration with HFI (0.3%) and a 1.4 sigma discrepancy with WMAP (0.9%). C1 [Bucher, M.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Patanchon, G.; Remazeilles, M.; Rosset, C.; Roudier, G.; Stompor, R.] Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, APC,CNRS IN2P3,CEA lrfu, F-75205 Paris 13, France. 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EM maurizio.tomasi@unimi.it RI Butler, Reginald/N-4647-2015; Barreiro, Rita Belen/N-5442-2014; Tomasi, Maurizio/I-1234-2016; Novikov, Igor/N-5098-2015; Colombo, Loris/J-2415-2016; popa, lucia/B-4718-2012; Atrio-Barandela, Fernando/A-7379-2017; Stolyarov, Vladislav/C-5656-2017; bonavera, laura/E-9368-2017; Remazeilles, Mathieu/N-1793-2015; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Valiviita, Jussi/A-9058-2016; Mazzotta, Pasquale/B-1225-2016; Kurki-Suonio, Hannu/B-8502-2016; Yvon, Dominique/D-2280-2015; Vielva, Patricio/F-6745-2014; Martinez-Gonzalez, Enrique/E-9534-2015; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; OI Gregorio, Anna/0000-0003-4028-8785; Butler, Reginald/0000-0003-4366-5996; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379; Maris, Michele/0000-0001-9442-2754; Franceschi, Enrico/0000-0002-0585-6591; Matarrese, Sabino/0000-0002-2573-1243; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Barreiro, Rita Belen/0000-0002-6139-4272; Umana, Grazia/0000-0002-6972-8388; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Peel, Mike/0000-0003-3412-2586; Tomasi, Maurizio/0000-0002-1448-6131; Colombo, Loris/0000-0003-4572-7732; Atrio-Barandela, Fernando/0000-0002-2130-2513; Stolyarov, Vladislav/0000-0001-8151-828X; bonavera, laura/0000-0001-8039-3876; De Zotti, Gianfranco/0000-0003-2868-2595; de Bernardis, Paolo/0000-0001-6547-6446; Morgante, Gianluca/0000-0001-9234-7412; Remazeilles, Mathieu/0000-0001-9126-6266; Toffolatti, Luigi/0000-0003-2645-7386; Valiviita, Jussi/0000-0001-6225-3693; Mazzotta, Pasquale/0000-0002-5411-1748; Kurki-Suonio, Hannu/0000-0002-4618-3063; Vielva, Patricio/0000-0003-0051-272X; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; Starck, Jean-Luc/0000-0003-2177-7794; Juvela, Mika/0000-0002-5809-4834; Hivon, Eric/0000-0003-1880-2733; Paoletti, Daniela/0000-0003-4761-6147; Pierpaoli, Elena/0000-0002-7957-8993; Lilje, Per/0000-0003-4324-7794; Rubino-Martin, Jose Alberto/0000-0001-5289-3021; Masi, Silvia/0000-0001-5105-1439; Valenziano, Luca/0000-0002-1170-0104; Finelli, Fabio/0000-0002-6694-3269; Scott, Douglas/0000-0002-6878-9840; Polenta, Gianluca/0000-0003-4067-9196; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Watson, Robert/0000-0002-5873-0124; Zacchei, Andrea/0000-0003-0396-1192 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); MICINN (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); PRACE (EU) FX The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, 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); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collabora tion. NR 69 TC 47 Z9 46 U1 3 U2 11 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2014 VL 571 AR A5 DI 10.1051/0004-6361/201321527 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600006 ER PT J AU Aleksic, J Ansoldi, S Antonelli, LA Antoranz, P Babic, A Bangale, P de Almeida, UB Barrio, JA Gonzalez, JB Bednarek, W Bernardini, E Biland, A Blanch, O Bonnefoy, S Bonnoli, G Borracci, F Bretz, T Carmona, E Carosi, A Fidalgo, DC Colin, P Colombo, E Contreras, JL Cortina, J Covino, S Da Vela, P Dazzi, F De Angelis, A De Caneva, G De Lotto, B Mendez, CD Doert, M Dominguez, A Prester, DD Dorner, D Doro, M Einecke, S Eisenacher, D Elsaesser, D Farina, E Ferenc, D Fonseca, MV Font, L Frantzen, K Fruck, C Lopez, RJG Garczarczyk, M Terrats, DG Gaug, M Godinovic, N Munoz, AG Gozzini, SR Hadasch, D Hayashida, M Herrera, J Herrero, A Hildebrand, D Hose, J Hrupec, D Idec, W Kadenius, V Kellermann, H Klepser, S Kodani, K Konno, Y Krause, J Kubo, H Kushida, J La Barbera, A Lelas, D Lewandowska, N Lindfors, E Lombardi, S Lopez, M Lopez-Coto, R Lopez-Oramas, A Lorenz, E Lozano, I Makariev, M Mallot, K Maneva, G Mankuzhiyil, N Mannheim, K Maraschi, L Marcote, B Mariotti, M Martinez, M Mazin, D Menzel, U Meucci, M Miranda, JM Mirzoyan, R Moralejo, A Munar-Adrover, P Nakajima, D Niedzwiecki, A Nilsson, K Nishijima, K Noda, K Nowak, N Wilhelmi, EDO Orito, R Overkemping, A Paiano, S Palatiello, M Paneque, D Paoletti, R Paredes, JM Paredes-Fortuny, X Partini, S Persic, M Prada, F Moroni, PGP Prandini, E Preziuso, S Puljak, I Reinthal, R Rhode, W Ribo, M Rico, J Garcia, JR Rugamer, S Saggion, A Saito, T Saito, K Satalecka, K Scalzotto, V Scapin, V Schultz, C Schweizer, T Shore, SN Sillanpaa, A Sitarek, J Snidaric, I Sobczynska, D Spanier, F Stamatescu, V Stamerra, A Steinbring, T Storz, J Strzys, M Sun, S Suric, T Takalo, L Takami, H Tavecchio, F Temnikov, P Terzic, T Tescaro, D Teshima, M Thaele, J Tibolla, O Torres, DF Toyama, T Treves, A Uellenbeck, M Vogler, P Wagner, RM Zandanel, F Zanin, R AF Aleksic, J. Ansoldi, S. Antonelli, L. A. Antoranz, P. Babic, A. Bangale, P. de Almeida, U. Barres Barrio, J. A. Becerra Gonzalez, J. Bednarek, W. Bernardini, E. Biland, A. Blanch, O. Bonnefoy, S. Bonnoli, G. Borracci, F. Bretz, T. Carmona, E. Carosi, A. Carreto Fidalgo, D. Colin, P. Colombo, E. Contreras, J. L. Cortina, J. Covino, S. Da Vela, P. Dazzi, F. De Angelis, A. De Caneva, G. De Lotto, B. Delgado Mendez, C. Doert, M. Dominguez, A. Prester, D. Dominis Dorner, D. Doro, M. Einecke, S. Eisenacher, D. Elsaesser, D. Farina, E. Ferenc, D. Fonseca, M. V. Font, L. Frantzen, K. Fruck, C. Garcia Lopez, R. J. Garczarczyk, M. Garrido Terrats, D. Gaug, M. Godinovic, N. Gonzalez Munoz, A. Gozzini, S. R. Hadasch, D. Hayashida, M. Herrera, J. Herrero, A. Hildebrand, D. Hose, J. Hrupec, D. Idec, W. Kadenius, V. Kellermann, H. Klepser, S. Kodani, K. Konno, Y. Krause, J. Kubo, H. Kushida, J. La Barbera, A. Lelas, D. Lewandowska, N. Lindfors, E. Lombardi, S. Lopez, M. Lopez-Coto, R. Lopez-Oramas, A. Lorenz, E. Lozano, I. Makariev, M. Mallot, K. Maneva, G. Mankuzhiyil, N. Mannheim, K. Maraschi, L. Marcote, B. Mariotti, M. Martinez, M. Mazin, D. Menzel, U. Meucci, M. Miranda, J. M. Mirzoyan, R. Moralejo, A. Munar-Adrover, P. Nakajima, D. Niedzwiecki, A. Nilsson, K. Nishijima, K. Noda, K. Nowak, N. de Ona Wilhelmi, E. Orito, R. Overkemping, A. Paiano, S. Palatiello, M. Paneque, D. Paoletti, R. Paredes, J. M. Paredes-Fortuny, X. Partini, S. Persic, M. Prada, F. Moroni, P. G. Prada Prandini, E. Preziuso, S. Puljak, I. Reinthal, R. Rhode, W. Ribo, M. Rico, J. Garcia, J. Rodriguez Ruegamer, S. Saggion, A. Saito, T. Saito, K. Satalecka, K. Scalzotto, V. Scapin, V. Schultz, C. Schweizer, T. Shore, S. N. Sillanpaa, A. Sitarek, J. Snidaric, I. Sobczynska, D. Spanier, F. Stamatescu, V. Stamerra, A. Steinbring, T. Storz, J. Strzys, M. Sun, S. Suric, T. Takalo, L. Takami, H. Tavecchio, F. Temnikov, P. Terzic, T. Tescaro, D. Teshima, M. Thaele, J. Tibolla, O. Torres, D. F. Toyama, T. Treves, A. Uellenbeck, M. Vogler, P. Wagner, R. M. Zandanel, F. Zanin, R. TI MAGIC reveals a complex morphology within the unidentified gamma-ray source HESS J1857+026 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE acceleration of particles; gamma rays: ISM; ISM: clouds; HII regions; ISM: individual objects: HESS J1857+026; pulsars: individual: PSR J1856+0245 ID H-II REGIONS; STAR-FORMING REGIONS; GALACTIC RING SURVEY; PULSAR WIND NEBULAE; SUPERNOVA REMNANT; INNER GALAXY; ATOMIC GAS; EMISSION; CONSTRAINTS; ABSORPTION AB Aims. HESS J1857+026 is an extended TeV gamma-ray source that was discovered by H. E. S. S. as part of its Galactic plane survey. Given its broadband spectral energy distribution and its spatial coincidence with the young energetic pulsar PSR J1856+0245, the source has been put forward as a pulsar wind nebula (PWN) candidate. MAGIC has performed follow-up observations aimed at mapping the source down to energies approaching 100 GeV in order to better understand its complex morphology. Methods. HESS J1857+026 was observed by MAGIC in 2010, yielding 29 h of good quality stereoscopic data that allowed us to map the source region in two separate ranges of energy. Results. We detected very-high-energy gamma-ray emission from HESS J1857+026 with a significance of 12 sigma above 150 GeV. The differential energy spectrum between 100 GeV and 13 TeV is described well by a power law function dN/dE = N-0(E/1TeV)(-Gamma) with N-0 = (5.37 +/- 0.44(stat) +/- 1.5(sys)) X 10(-12) (TeV-1 cm(-2) s(-1)) and Gamma = 2.16 +/- 0.07(stat) +/- 0.15(sys), which bridges the gap between the GeV emission measured by Fermi-LAT and the multi-TeV emission measured by H.E.S.S.. In addition, we present a detailed analysis of the energy-dependent morphology of this region. We couple these results with archival multiwavelength data and outline evidence in favor of a two-source scenario, whereby one source is associated with a PWN, while the other could be linked with a molecular cloud complex containing an HII region and a possible gas cavity. C1 [Aleksic, J.; Blanch, O.; Cortina, J.; Gonzalez Munoz, A.; Klepser, S.; Lopez-Coto, R.; Lopez-Oramas, A.; Martinez, M.; Moralejo, A.; Rico, J.; Sitarek, J.; Stamatescu, V.] IFAE, Bellaterra 08193, Spain. [Ansoldi, S.; De Angelis, A.; De Lotto, B.; Mankuzhiyil, N.; Palatiello, M.; Persic, M.] Univ Udine, I-33100 Udine, Italy. [Ansoldi, S.; De Angelis, A.; De Lotto, B.; Mankuzhiyil, N.; Palatiello, M.; Persic, M.] INFN Trieste, I-33100 Udine, Italy. [Antonelli, L. A.; Bonnoli, G.; Carosi, A.; Covino, S.; La Barbera, A.; Lombardi, S.; Maraschi, L.; Stamerra, A.; Tavecchio, F.] INAF Natl Inst Astrophys, I-00136 Rome, Italy. [Antoranz, P.; Da Vela, P.; Meucci, M.; Miranda, J. M.; Paoletti, R.; Partini, S.; Preziuso, S.] Univ Siena, I-53100 Siena, Italy. [Antoranz, P.; Da Vela, P.; Meucci, M.; Miranda, J. M.; Paoletti, R.; Partini, S.; Preziuso, S.] INFN Pisa, I-53100 Siena, Italy. [Babic, A.; Prester, D. Dominis; Ferenc, D.; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Suric, T.; Terzic, T.] Univ Rijeka, Rudjer Boskov Inst, Croatian MAGIC Consortium, Zagreb 10000, Croatia. [Babic, A.; Prester, D. Dominis; Ferenc, D.; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Suric, T.; Terzic, T.] Univ Split, Zagreb 10000, Croatia. [Bangale, P.; de Almeida, U. Barres; Borracci, F.; Colin, P.; Dazzi, F.; Fruck, C.; Hose, J.; Kellermann, H.; Krause, J.; Lorenz, E.; Mazin, D.; Menzel, U.; Mirzoyan, R.; Noda, K.; Nowak, N.; Paneque, D.; Garcia, J. Rodriguez; Schweizer, T.; Strzys, M.; Sun, S.; Teshima, M.; Toyama, T.; Wagner, R. M.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Barrio, J. A.; Bonnefoy, S.; Carreto Fidalgo, D.; Contreras, J. L.; Fonseca, M. V.; Lopez, M.; Lozano, I.; Satalecka, K.; Scapin, V.] Univ Complutense, E-28040 Madrid, Spain. [Becerra Gonzalez, J.; Colombo, E.; Garcia Lopez, R. J.; Herrera, J.; Herrero, A.; Tescaro, D.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Bednarek, W.; Idec, W.; Niedzwiecki, A.; Sobczynska, D.] Univ Lodz, PL-90236 Lodz, Poland. [Bernardini, E.; De Caneva, G.; Garczarczyk, M.; Gozzini, S. R.; Klepser, S.; Mallot, K.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Biland, A.; Hildebrand, D.; Prandini, E.; Vogler, P.] ETH, CH-8093 Zurich, Switzerland. [Bretz, T.; Dorner, D.; Eisenacher, D.; Elsaesser, D.; Lewandowska, N.; Mannheim, K.; Ruegamer, S.; Spanier, F.; Steinbring, T.; Storz, J.; Tibolla, O.] Univ Wurzburg, D-97074 Wurzburg, Germany. [Carmona, E.; Delgado Mendez, C.] Ctr Invest Energet Medioambient & Tecnol, Madrid 28040, Spain. [Doert, M.; Einecke, S.; Frantzen, K.; Overkemping, A.; Rhode, W.; Thaele, J.; Uellenbeck, M.] Tech Univ Dortmund, D-44221 Dortmund, Germany. [Dominguez, A.; Prada, F.; Zandanel, F.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Doro, M.; Mariotti, M.; Paiano, S.; Saggion, A.; Scalzotto, V.; Schultz, C.] Univ Padua, I-35131 Padua, Italy. [Doro, M.; Mariotti, M.; Paiano, S.; Saggion, A.; Scalzotto, V.; Schultz, C.] Ist Nazl Fis Nucl, I-35131 Padua, Italy. [Farina, E.; Treves, A.] Univ Insubria, I-22100 Como, Italy. [Font, L.; Garrido Terrats, D.; Gaug, M.] Univ Autonoma Barcelona, Dept Fis, Unitat Fis Radiac, Bellaterra 08193, Spain. [Font, L.; Garrido Terrats, D.; Gaug, M.] Univ Autonoma Barcelona, CERES IEEC, Bellaterra 08193, Spain. [Hadasch, D.; de Ona Wilhelmi, E.; Torres, D. F.] CSIC, IEEC, Inst Ciencies Espai, Bellaterra 08193, Spain. [Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Nakajima, D.; Nishijima, K.; Orito, R.; Saito, T.; Saito, K.; Takami, H.] Kyoto Univ, Div Phys & Astron, Japanese MAGIC Consortium, Kyoto 6068501, Japan. [Kadenius, V.; Lindfors, E.; Nilsson, K.; Reinthal, R.; Sillanpaa, A.; Takalo, L.] Univ Turku, Tuorla Observ, Finnish MAGIC Consortium, SF-20500 Turku, Finland. [Kadenius, V.; Lindfors, E.; Nilsson, K.; Reinthal, R.; Sillanpaa, A.; Takalo, L.] Univ Oulu, Dept Phys, SF-90100 Oulu, Finland. [Makariev, M.; Maneva, G.; Temnikov, P.] Bulgarian Acad Sci, Inst Nucl Res & Nucl Energy, BU-1784 Sofia, Bulgaria. [Marcote, B.; Munar-Adrover, P.; Paredes, J. M.; Paredes-Fortuny, X.; Ribo, M.; Zanin, R.] Univ Barcelona, ICC, IEEC UB, E-08028 Barcelona, Spain. [Moroni, P. G. Prada; Shore, S. N.] Univ Pisa, I-56126 Pisa, Italy. [Moroni, P. G. Prada; Shore, S. N.] Ist Nazl Fis Nucl, I-56126 Pisa, Italy. [Becerra Gonzalez, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Becerra Gonzalez, J.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Becerra Gonzalez, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Bretz, T.] Ecole Polytech Fed Lausanne, Lausanne, Switzerland. [Dominguez, A.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Lindfors, E.; Nilsson, K.] Finnish Ctr Astron, ESO FINCA, Turku, Finland. [Prada, F.] UAM, CSIC, Inst Fis Teor, Madrid 28049, Spain. [Stamatescu, V.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. [Wagner, R. M.] Stockholm Univ, Oskar Klein Ctr Cosmoparticle Phys, S-10691 Stockholm, Sweden. [Zandanel, F.] Univ Amsterdam, GRAPPA Inst, NL-1098 XH Amsterdam, Netherlands. RP Stamatescu, V (reprint author), IFAE, Campus UAB, Bellaterra 08193, Spain. EM klepser@ifae.es; julkrau@googlemail.com; vstamatescu@ifae.es RI Barrio, Juan/L-3227-2014; Martinez Rodriguez, Manel/C-2539-2017; Cortina, Juan/C-2783-2017; GAug, Markus/L-2340-2014; Antoranz, Pedro/H-5095-2015; Fonseca Gonzalez, Maria Victoria/I-2004-2015; Delgado, Carlos/K-7587-2014; Stamatescu, Victor/C-9945-2016; Font, Lluis/L-4197-2014; Contreras Gonzalez, Jose Luis/K-7255-2014; Temnikov, Petar/L-6999-2016; Maneva, Galina/L-7120-2016; Makariev, Martin/M-2122-2016; Torres, Diego/O-9422-2016; Miranda, Jose Miguel/F-2913-2013 OI Stamerra, Antonio/0000-0002-9430-5264; Prandini, Elisa/0000-0003-4502-9053; Becerra Gonzalez, Josefa/0000-0002-6729-9022; Covino, Stefano/0000-0001-9078-5507; de Ona Wilhelmi, Emma/0000-0002-5401-0744; Tavecchio, Fabrizio/0000-0003-0256-0995; Bonnoli, Giacomo/0000-0003-2464-9077; Antonelli, Lucio Angelo/0000-0002-5037-9034; Doro, Michele/0000-0001-9104-3214; Barrio, Juan/0000-0002-0965-0259; Cortina, Juan/0000-0003-4576-0452; Dominguez, Alberto/0000-0002-3433-4610; Prada Moroni, Pier Giorgio/0000-0001-9712-9916; LA BARBERA, ANTONINO/0000-0002-5880-8913; De Lotto, Barbara/0000-0003-3624-4480; Persic, Massimo/0000-0003-1853-4900; Farina, Emanuele Paolo/0000-0002-6822-2254; GAug, Markus/0000-0001-8442-7877; Antoranz, Pedro/0000-0002-3015-3601; Fonseca Gonzalez, Maria Victoria/0000-0003-2235-0725; Delgado, Carlos/0000-0002-7014-4101; Stamatescu, Victor/0000-0001-9030-7513; Font, Lluis/0000-0003-2109-5961; Contreras Gonzalez, Jose Luis/0000-0001-7282-2394; Temnikov, Petar/0000-0002-9559-3384; Torres, Diego/0000-0002-1522-9065; Miranda, Jose Miguel/0000-0002-1472-9690 FU German BMBF and MPG; Italian INFN; Swiss National Fund SNF; Spanish MICINN; CPAN [CSD2007-00042]; MultiDark [CSD2009-00064]; Academy of Finland [127740]; DFG Cluster of Excellence "Origin and Structure of the Universe"; Croatian Science Foundation [09/176]; DFG Collaborative Research Centers [SFB823/C4, SFB876/C3]; Polish MNiSzW [745/N-HESS-MAGIC/2010/0] FX We would like to thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MICINN is gratefully acknowledged. This work was also supported by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 127740 of the Academy of Finland, by the DFG Cluster of Excellence "Origin and Structure of the Universe", by the Croatian Science Foundation Project 09/176, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. NR 47 TC 4 Z9 4 U1 1 U2 17 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 NOV PY 2014 VL 571 AR A96 DI 10.1051/0004-6361/201423517 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600036 ER PT J AU Beltran, MT Sanchez-Monge, A Cesaroni, R Kumar, MSN Galli, D Walmsley, CM Etoka, S Furuya, RS Moscadelli, L Stanke, T van der Tak, FFS Vig, S Wang, KS Zinnecker, H Elia, D Schisano, E AF Beltran, M. T. Sanchez-Monge, A. Cesaroni, R. Kumar, M. S. N. Galli, D. Walmsley, C. M. Etoka, S. Furuya, R. S. Moscadelli, L. Stanke, T. van der Tak, F. F. S. Vig, S. Wang, K. -S. Zinnecker, H. Elia, D. Schisano, E. TI Filamentary structure and Keplerian rotation in the high-mass star-forming region G35.03+0.35 imaged with ALMA SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: individual objects: G35.03+0.35; ISM: molecules; stars: formation; stars: kinematics and dynamics; HII regions ID EXTENDED GREEN OBJECTS; WIDE-FIELD CAMERA; PROTOSTELLAR OBJECTS; PHOTOMETRIC SYSTEM; IRAS 20126+4104; GALACTIC PLANE; GLIMPSE SURVEY; MOLECULAR GAS; HII-REGIONS; LINE SURVEY AB Context. Theoretical scenarios propose that high-mass stars are formed by disk-mediated accretion. Aims. To test the theoretical predictions on the formation of massive stars, we wish to make a thorough study at high-angular resolution of the structure and kinematics of the dust and gas emission toward the high-mass star-forming region G35.03+0.35, which harbors a disk candidate around a B-type (proto) star. Methods. We carried out ALMA Cycle 0 observations at 870 mu m of dust of typical high-density, molecular outflow, and cloud tracers with resolutions of < 0".5. Complementary Subaru COMICS 25 mu m observations were carried out to trace the mid-infrared emission toward this star-forming region. Results. The submillimeter continuum emission has revealed a filamentary structure fragmented into six cores, called A-F. The filament could be in quasi-equilibrium taking into account that the mass per unit length of the filament, 200-375 M-circle dot/pc, is similar to the critical mass of a thermally and turbulently supported infinite cylinder, similar to 335 M-circle dot/pc. The cores, which are on average separated by similar to 0.02 pc, have deconvolved sizes of 1300-3400 AU, temperatures of 35-240 K, H-2 densities > 10(7) cm(-3), and masses in the range 1-5 M-circle dot, and they are subcritical. Core A, which is associated with a hypercompact HII region and could be the driving source of the molecular outflow observed in the region, is the most chemically rich source in G35.03+0.35 with strong emission of typical hot core tracers such as CH3CN. Tracers of high density and excitation show a clear velocity gradient along the major axis of the core, which is consistent with a disk rotating about the axis of the associated outflow. The PV plots along the SE-NW direction of the velocity gradient show clear signatures of Keplerian rotation, although infall could also be present, and they are consistent with the pattern of an edge-on Keplerian disk rotating about a star with a mass in the range 5-13 M-circle dot. The high t(ff)/t(rot) ratio for core A suggests that the structure rotates fast and that the accreting material has time to settle into a centrifugally supported disk. Conclusions. G35.03+0.35 is one of the most convincing examples of Keplerian disks rotating about high-mass (proto) stars. This supports theoretical scenarios according to which high-mass stars, at least B-type stars, would form through disk-mediated accretion. C1 [Beltran, M. T.; Sanchez-Monge, A.; Cesaroni, R.; Galli, D.; Walmsley, C. M.; Moscadelli, L.] INAF, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Sanchez-Monge, A.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Kumar, M. S. N.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Walmsley, C. M.] DIAS, Dublin 2, Ireland. [Etoka, S.] Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Manchester M13 9PL, Lancs, England. [Etoka, S.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Furuya, R. S.] Univ Tokushima, Tokushima, Tokushima 7708502, Japan. [Stanke, T.] ESO, D-85748 Garching, Germany. [van der Tak, F. F. S.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [van der Tak, F. F. S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Vig, S.] Indian Inst Space Sci & Technol, Dept Earth & Space Sci, Thiruvananthapuram 695547, Kerala, India. [Wang, K. -S.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Wang, K. -S.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Zinnecker, H.] NASA, Ames Res Ctr, SOFIA, Ctr Sci, Moffett Field, CA 94035 USA. [Elia, D.] INAF, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy. [Schisano, E.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. RP Beltran, MT (reprint author), INAF, Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy. OI Moscadelli, Luca/0000-0002-8517-8881; Galli, Daniele/0000-0001-7706-6049; Beltran Sorolla, Maria Teresa/0000-0003-3315-5626; Elia, Davide/0000-0002-9120-5890; Cesaroni, Riccardo/0000-0002-2430-5103 FU ALMA [2011.0.00275] FX We thank Claudia Cyganowski for kindly providing the 8.4 GHz continuum emission data of this region. This paper makes use of the following ALMA data: ADS/JAO. ALMA#2011.0.00275. S. ALMA is a partnership of ESO (representing its member states), the NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. We acknowledge the Italian ARC for the computational support. R.S.F. acknowledges T. Usuda, T. Inagaki, S. S. Hayashi, and H. Shinnaga for their help with the Subaru observations and data reduction. This work is based (in part) on archival data obtained with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by an award issued by JPL/Caltech. The ATLASGAL project is a collaboration between the Max-Planck-Gesellschaft, the European Southern Observatory (ESO), and the Universidad de Chile. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research made use of data products from the Midcourse Space Experiment. Processing of the data was funded by the Ballistic Missile Defense Organization with additional support from the NASA Office of Space Science. This research also made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 78 TC 8 Z9 8 U1 1 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2014 VL 571 AR A52 DI 10.1051/0004-6361/201424031 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600051 ER PT J AU De Looze, I Fritz, J Baes, M Bendo, GJ Cortese, L Boquien, M Boselli, A Camps, P Cooray, A Cormier, D Davies, JI De Geyter, G Hughes, TM Jones, AP Karczewski, OL Lebouteiller, V Lu, NY Madden, SC Remy-Ruyer, A Spinoglio, L Smith, MWL Viaene, S Wilson, CD AF De Looze, Ilse Fritz, Jacopo Baes, Maarten Bendo, George J. Cortese, Luca Boquien, Mederic Boselli, Alessandro Camps, Peter Cooray, Asantha Cormier, Diane Davies, Jon I. De Geyter, Gert Hughes, Thomas M. Jones, Anthony P. Karczewski, Oskar L. Lebouteiller, Vianney Lu, Nanyao Madden, Suzanne C. Remy-Ruyer, Aurelie Spinoglio, Luigi Smith, Matthew W. L. Viaene, Sebastien Wilson, Christine D. TI High-resolution, 3D radiative transfer modeling I. The grand-design spiral galaxy M 51 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radiative transfer; dust, extinction; galaxies: individual: M 51; galaxies: ISM; infrared: galaxies ID HERSCHEL REFERENCE SURVEY; STAR-FORMING GALAXIES; SPECTRAL ENERGY-DISTRIBUTION; LARGE-MAGELLANIC-CLOUD; INITIAL MASS FUNCTION; DIGITAL SKY SURVEY; EDGE-ON GALAXIES; POLYCYCLIC AROMATIC-HYDROCARBONS; MULTIBAND IMAGING PHOTOMETER; SPITZER-SPACE-TELESCOPE AB Context. Dust reprocesses about half of the stellar radiation in galaxies. The thermal re-emission by dust of absorbed energy is considered to be driven merely by young stars so is often applied to tracing the star formation rate in galaxies. Recent studies have argued that the old stellar population might be responsible for a non-negligible fraction of the radiative dust heating. Aims. In this work, we aim to analyze the contribution of young (less than or similar to 100 Myr) and old (similar to 10 Gyr) stellar populations to radiative dust heating processes in the nearby grand-design spiral galaxy M 51 using radiative transfer modeling. High-resolution 3D radiative transfer (RT) models are required to describe the complex morphologies of asymmetric spiral arms and clumpy star-forming regions and to model the propagation of light through a dusty medium. Methods. In this paper, we present a new technique developed to model the radiative transfer effects in nearby face-on galaxies. We construct a high-resolution 3D radiative transfer model with the Monte-Carlo code SKIRT to account for the absorption, scattering, and non-local thermal equilibrium (NLTE) emission of dust in M51. The 3D distribution of stars is derived from the 2D morphology observed in the IRAC 3.6 mu m, GALEX FUV, H alpha, and MIPS 24 mu m wavebands, assuming an exponential vertical distribution with an appropriate scale height. The dust geometry is constrained through the far-ultraviolet (FUV) attenuation, which is derived from the observed total-infrared-to-far-ultraviolet luminosity ratio. The stellar luminosity, star formation rate, and dust mass have been scaled to reproduce the observed stellar spectral energy distribution (SED), FUV attenuation, and infrared SED. Results. The dust emission derived from RT calculations is consistent with far-infrared and submillimeter observations of M51, implying that the absorbed stellar energy is balanced by the thermal re-emission of dust. The young stars provide 63% of the energy for heating the dust responsible for the total infrared emission (8-1000 mu m), while 37% of the dust emission is governed through heating by the evolved stellar population. In individual wavebands, the contribution from young stars to the dust heating dominates at all infrared wavebands but gradually decreases towards longer infrared and submillimeter wavebands for which the old stellar population becomes a non-negligible source of heating. Upon extrapolation of the results for M51, we present prescriptions for estimating the contribution of young stars to the global dust heating based on a tight correlation between the dust heating fraction and specific star formation rate. C1 [De Looze, Ilse; Fritz, Jacopo; Baes, Maarten; Camps, Peter; De Geyter, Gert; Hughes, Thomas M.; Viaene, Sebastien] Univ Ghent, Sterrenkundig Observatorium, B-9000 Ghent, Belgium. [De Looze, Ilse; Boquien, Mederic] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Bendo, George J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, UK ALMA Reg Ctr Node, Manchester M13 9PL, Lancs, England. [Cortese, Luca] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Boselli, Alessandro] Univ Aix Marseille, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Boselli, Alessandro] CNRS, UMR 7326, F-13388 Marseille 13, France. [Cooray, Asantha] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Cooray, Asantha] CALTECH, Div Phys Astron & Math, Pasadena, CA 91125 USA. [Cormier, Diane; Smith, Matthew W. L.] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, D-69120 Heidelberg, Germany. [Davies, Jon I.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Jones, Anthony P.] CNRS, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France. [Jones, Anthony P.; Remy-Ruyer, Aurelie] Univ Paris 11, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France. [Karczewski, Oskar L.] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Lebouteiller, Vianney; Madden, Suzanne C.; Remy-Ruyer, Aurelie] Univ Paris 07, Lab AIM, CEA, IRFU,Serv Astrophys, F-91191 Gif Sur Yvette, France. [Lu, Nanyao] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. [Spinoglio, Luigi] INAF IAPS, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy. [Wilson, Christine D.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. RP De Looze, I (reprint author), Univ Ghent, Sterrenkundig Observatorium, Krijgslaan 281 S9, B-9000 Ghent, Belgium. EM Ilse.DeLooze@ugent.be RI Boquien, Mederic/J-5964-2015; OI Boquien, Mederic/0000-0003-0946-6176; Cortese, Luca/0000-0002-7422-9823 FU Belgian Science Policy Office (BELSPO) through the PRODEX project "Herschel-PACS Guaranteed Time and Open Time Programs: Science Exploitation" [C90370]; Belgian Science Policy Office (BELSPO) through the CHARM framework (Contemporary physical challenges in Heliospheric and AstRophysical Models), a phase VII Interuniversity Attraction Pole (IAP) program; Australian Research Council [130100664]; BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain) FX We thank the referee for useful comments and suggestions. We thank Richard Tuffs, Cristina Popescu, Simone Bianchi, Manolis Xilouris, and Giovanni Natale for fruitful discussions on the analysis of the dust heating fractions and the clumpiness of dust. We thank Robert C. Kennicutt Jr. for useful suggestions. We also thank Brent Groves for kindly providing us the dust masses associated with the emission spectra of the young HII regions with surrounding PDR envelopes. IDL is a postdoctoral researcher of the FWO-Vlaanderen (Belgium). M.B., J.F. and T.H. acknowledge the financial support of the Belgian Science Policy Office (BELSPO) through the PRODEX project "Herschel-PACS Guaranteed Time and Open Time Programs: Science Exploitation" (C90370). P.C. acknowledges the financial support of the Belgian Science Policy Office (BELSPO) through the CHARM framework (Contemporary physical challenges in Heliospheric and AstRophysical Models), a phase VII Interuniversity Attraction Pole (IAP) program. L.C. acknowledges support under the Australian Research Council's Discovery Projects funding scheme (project number 130100664). 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); INAFIFSI/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). NR 197 TC 17 Z9 17 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2014 VL 571 AR A69 DI 10.1051/0004-6361/201424747 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT9ZK UT WOS:000345282600096 ER PT J AU Grabbe, S Sridhar, B Mukherjee, A AF Grabbe, Shon Sridhar, Banavar Mukherjee, Avijit TI Clustering Days and Hours with Similar Airport Traffic and Weather Conditions SO JOURNAL OF AEROSPACE INFORMATION SYSTEMS LA English DT Article AB On any given day, constraints in the National Airspace System (for instance, weather) necessitate the implementation of traffic flow management initiatives, such as ground delay programs. The goal of this study is to take a preliminary step toward informing future decision making by applying data-mining techniques to identify similar days in the National Airspace System in terms of the cause and location of historically implemented ground delay programs. In the first part of this study, a modified K-means clustering algorithm was applied to all days from 2010 through 2012, resulting in the identification of 45 national-level daily clusters that represent unique combinations of historically implemented ground delay programs. The second part of this study focused on verifying the stated causes of the historical ground delay programs. Findings from this initial study indicated that it is possible to identify similar days under which the National Airspace System operates, and clustering techniques appear to be promising methods for identifying the major causes of ground delay programs. C1 [Grabbe, Shon] NASA, Ames Res Ctr, Syst Modeling & Optimizat Branch, Moffett Field, CA 94035 USA. [Sridhar, Banavar] NASA, Ames Res Ctr, Aviat Syst Program, Moffett Field, CA 94035 USA. [Mukherjee, Avijit] Univ Calif Santa Cruz, Moffett Field, CA 94035 USA. RP Grabbe, S (reprint author), NASA, Ames Res Ctr, Syst Modeling & Optimizat Branch, Mail Stop 210-15, Moffett Field, CA 94035 USA. EM shon.grabbe@nasa.gov NR 32 TC 2 Z9 2 U1 1 U2 3 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 1940-3151 EI 2327-3097 J9 J AEROSP INFORM SYST JI J. Aerosp. Inf. Syst. PD NOV PY 2014 VL 11 IS 11 BP 751 EP 763 DI 10.2514/1.I010212 PG 13 WC Engineering, Aerospace SC Engineering GA CA1KI UT WOS:000348671100001 ER PT J AU Bloem, M Bambos, N AF Bloem, Michael Bambos, Nicholas TI Air Traffic Control Area Configuration Advisories from Near-Optimal Distinct Paths SO JOURNAL OF AEROSPACE INFORMATION SYSTEMS LA English DT Article ID K SHORTEST PATHS; DISJOINT PATHS; ALGORITHM AB Area of specialization supervisors dynamically configure available air traffic control resources so that air traffic can operate safely and efficiently. It is proposed to assist supervisors with this process by presenting them with a set of near-optimal and meaningfully different configuration advisories. To find such a set of advisories, a problem is defined that is equivalent to finding optimal and other near-optimal and distinct paths in a time-expanded graph. It is shown that this problem is nondeterministic polynomial-time hard, and then four algorithms are motivated and specified. One is a benchmark that solves the problem to optimality, one is a novel heuristic based on value iteration, and a third is a novel heuristic based on the A* algorithm. The fourth algorithm solves to optimality the lowest-cost paths problem relaxation of the problem. When used to solve realistic problem instances, the lowest-cost paths algorithm rarely returned feasible solutions and the optimal algorithm required excessive computation times, but the two novel heuristics found feasible and often optimal solutions in just a few seconds. The A* -based heuristic achieved lower computation times, whereas the value iteration-based heuristic typically found more advisories and lower-cost advisories. C1 [Bloem, Michael] NASA, Ames Res Ctr, Syst Modeling & Optimizat Branch, Moffett Field, CA 94035 USA. [Bambos, Nicholas] Stanford Univ, Dept Management Sci, Stanford, CA 94305 USA. [Bambos, Nicholas] Stanford Univ, Dept Engn & Elect Engn, Stanford, CA 94305 USA. RP Bloem, M (reprint author), NASA, Ames Res Ctr, Syst Modeling & Optimizat Branch, MS 210-15, Moffett Field, CA 94035 USA. EM michael.bloem@nasa.gov; bambos@stanford.edu NR 31 TC 0 Z9 0 U1 0 U2 2 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 1940-3151 EI 2327-3097 J9 J AEROSP INFORM SYST JI J. Aerosp. Inf. Syst. PD NOV PY 2014 VL 11 IS 11 BP 764 EP 784 DI 10.2514/1.I010219 PG 21 WC Engineering, Aerospace SC Engineering GA CA1KI UT WOS:000348671100002 ER PT J AU Gao, F He, T Masek, JG Shuai, YM Schaaf, CB Wang, ZS AF Gao, Feng He, Tao Masek, Jeffrey G. Shuai, Yanmin Schaaf, Crystal B. Wang, Zhuosen TI Angular Effects and Correction for Medium Resolution Sensors to Support Crop Monitoring SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE SENSING LA English DT Article DE Advanced wide field sensor (AWiFS); bi-directional reflectance distribution function (BRDF); crop condition; directional reflectance; Landsat; time-series analysis ID REFLECTANCE DISTRIBUTION FUNCTION; BIDIRECTIONAL REFLECTANCE; NADIR REFLECTANCE; MODEL INVERSION; FOREST CANOPY; LANDSAT DATA; BRDF; SURFACE; MODIS; ALBEDO AB Remote sensing imagery at medium spatial resolutions (20-60 m) such as Landsat, the advanced wide field sensor (AWiFS) and the disaster monitoring constellation (DMC) have been broadly used in mapping crop types and monitoring crop conditions. This paper examines the influence of viewing and illumination angular effects on surface reflectance of typical surface and crop types for both narrow swath (e.g., Landsat) and wide swath (e.g., AWiFS) sensors. Three types of angular effects: 1) view angle effect; 2) day of year effect; and 3) mean local time drift effect were analyzed based on both field and satellite bi-directional reflectance distribution function (BRDF) measurements. In order to correct these angular effects, a BRDF look-up map (LUM) for major cover types was built using the cropland data layer (CDL) and the Moderate-Resolution Imaging Spectroradiometer (MODIS) BRDF products. The BRDF LUM was applied to an AWiFS image to correct view angle effects in an agricultural area in central Illinois. The resulting nadir BRDF-adjusted reflectance (NBAR) provides a consistent data source for intra-annual crop condition monitoring and inter-annual time-series analysis. C1 [Gao, Feng] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA. [He, Tao] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Masek, Jeffrey G.; Shuai, Yanmin; Wang, Zhuosen] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Shuai, Yanmin] Earth Resources Technol Inc, Silver Spring, MD USA. [Schaaf, Crystal B.] Univ Massachusetts, Sch Environm, Boston, MA 02125 USA. RP Gao, F (reprint author), ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA. EM feng.gao@ars.usda.gov; the@umd.edu; jeffrey.g.masek@nasa.gov; shuaiym@gmail.com; Crystal.Schaaf@umb.edu; zhuosen.wang@nasa.gov RI Masek, Jeffrey/D-7673-2012; He, Tao/H-5130-2012 OI He, Tao/0000-0003-2079-7988 FU NASA Land Cover Project Science Office; NASA Terrestrial Ecology program; U.S. Geological Survey (USGS) Landsat Science Team program FX This work was supported in part by the NASA Land Cover Project Science Office, in part by the NASA Terrestrial Ecology program, and in part by the U.S. Geological Survey (USGS) Landsat Science Team program. USDA and NASA are equal opportunity providers and employers. NR 29 TC 7 Z9 7 U1 1 U2 10 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1939-1404 EI 2151-1535 J9 IEEE J-STARS JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens. PD NOV PY 2014 VL 7 IS 11 SI SI BP 4480 EP 4489 DI 10.1109/JSTARS.2014.2343592 PG 10 WC Engineering, Electrical & Electronic; Geography, Physical; Remote Sensing; Imaging Science & Photographic Technology SC Engineering; Physical Geography; Remote Sensing; Imaging Science & Photographic Technology GA AY9MR UT WOS:000347875700018 ER PT J AU Heracleous, L Gonzalez, SA AF Heracleous, Loizos Gonzalez, Steven A. TI Two modest proposals for propelling NASA forward SO SPACE POLICY LA English DT Editorial Material DE NASA; Johnson Space Center; Organizational change AB The external and internal environments of NASA have been shifting, necessitating new approaches to problem solving and innovation. Based on a strategic alignment analysis, and an understanding of NASA's internal and external contexts, we have two modest proposals: First, give NASA flexibility to manage its human resources and infrastructure based on market-based, competitive, performance-oriented principles. Second, it is time for NASA to become a real network organization. One that is properly integrated both internally (across NASA centers) as well as externally with whatever organizations have superior space-related knowledge and technology, wherever they are. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Heracleous, Loizos] Univ Warwick, Warwick Business Sch, Coventry CV4 7AL, W Midlands, England. [Gonzalez, Steven A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Heracleous, L (reprint author), Univ Warwick, Warwick Business Sch, Scarman Rd, Coventry CV4 7AL, W Midlands, England. EM loizos.heracleous@wbs.ac.uk; steven.a.gonzalez@nasa.gov NR 0 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0265-9646 EI 1879-338X J9 SPACE POLICY JI Space Policy PD NOV PY 2014 VL 30 IS 4 BP 190 EP 192 DI 10.1016/j.spacepol.2014.08.008 PG 3 WC International Relations; Social Sciences, Interdisciplinary SC International Relations; Social Sciences - Other Topics GA AY7YE UT WOS:000347770900003 ER PT J AU Kimball, MO Mustafi, S AF Kimball, Mark O. Mustafi, Shuvo TI SCW 2013-Preface SO CRYOGENICS LA English DT Editorial Material C1 [Kimball, Mark O.; Mustafi, Shuvo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kimball, MO (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM mark.kimball@nasa.gov; shuvo.mustafi@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0011-2275 EI 1879-2235 J9 CRYOGENICS JI Cryogenics PD NOV-DEC PY 2014 VL 64 BP 99 EP 99 DI 10.1016/j.cryogenics.2014.09.002 PG 1 WC Thermodynamics; Physics, Applied SC Thermodynamics; Physics GA AY4XE UT WOS:000347577600014 ER PT J AU Dye, SA Johnson, WL Plachta, DW Mills, GL Buchanan, L Kopelove, AB AF Dye, S. A. Johnson, W. L. Plachta, D. W. Mills, G. L. Buchanan, L. Kopelove, A. B. TI Design, fabrication and test of Load Bearing multilayer insulation to support a broad area cooled shield SO CRYOGENICS LA English DT Article DE Integrated multilayer insulation; Load Bearing MLI; Broad area cooled shield; Active thermal control ID THERMAL PERFORMANCE AB Improvements in cryogenic propellant storage are needed to achieve reduced or Zero Boil Off of cryopropellants, critical for long duration missions. Techniques for reducing heat leak into cryotanks include using passive multi-layer insulation (MLI) and vapor cooled or actively cooled thermal shields. Large scale shields cannot be supported by tank structural supports without heat leak through the supports. Traditional MLI also cannot support shield structural loads, and separate shield support mechanisms add significant heat leak. Quest Thermal Group and Ball Aerospace, with NASA SBIR support, have developed a novel Load Bearing multi-layer insulation (LBMLI) capable of self-supporting thermal shields and providing high thermal performance. We report on the development of LBMLI, including design, modeling and analysis, structural testing via vibe and acoustic loading, calorimeter thermal testing, and Reduced Boil-Off (RBO) testing on NASA large scale cryotanks. LBMLI uses the strength of discrete polymer spacers to control interlayer spacing and support the external load of an actively cooled shield and external MLI. Structural testing at NASA Marshall was performed to beyond maximum launch profiles without failure. LBMLI coupons were thermally tested on calorimeters, with superior performance to traditional MLI on a per layer basis. Thermal and structural tests were performed with LBMLI supporting an actively cooled shield, and comparisons are made to the performance of traditional MLI and thermal shield supports. LBMLI provided a 51% reduction in heat leak per layer over a previously tested traditional MLI with tank standoffs, a 38% reduction in mass, and was advanced to TRL5. Active thermal control using LBMLI and a broad area cooled shield offers significant advantages in total system heat flux, mass and structural robustness for future Reduced Boil-Off and Zero Boil-Off cryogenic missions with durations over a few weeks. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Dye, S. A.; Kopelove, A. B.] Quest Thermal Grp, Arvada, CO 80004 USA. [Johnson, W. L.] NASA, Kennedy Space Ctr, Cryogen Test Lab, Houston, TX USA. [Plachta, D. W.] NASA, Glenn Res Ctr, Prop & Propellants Branch, Houston, TX USA. [Mills, G. L.; Buchanan, L.] Ball Aerosp & Technol Corp, Boulder, CO 80301 USA. RP Kopelove, AB (reprint author), Quest Thermal Grp, 6452 Fig St Unit A, Arvada, CO 80004 USA. EM alan.kopelove@questthermal.com FU NASA Space Technology Mission Directorate's Game Changing Development program; Cryogenic Propellant Storage & Transfer Technology Demonstration Mission [NNK12EA61C] FX The authors gratefully acknowledge the support of the NASA Space Technology Mission Directorate's Game Changing Development program and the Cryogenic Propellant Storage & Transfer Technology Demonstration Mission (contract NNK12EA61C); and the work of NASA team members at Glenn Research Center, Marshall Space Flight Center, Kennedy Space Center and Ames Research Center. NR 15 TC 2 Z9 2 U1 1 U2 8 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0011-2275 EI 1879-2235 J9 CRYOGENICS JI Cryogenics PD NOV-DEC PY 2014 VL 64 BP 135 EP 140 DI 10.1016/j.cryogenics.2014.06.001 PG 6 WC Thermodynamics; Physics, Applied SC Thermodynamics; Physics GA AY4XE UT WOS:000347577600019 ER PT J AU Paine, CG AF Paine, Christopher G. TI Comparison of mechanical cryocoolers versus stored cryogens for balloon-borne observations SO CRYOGENICS LA English DT Article DE ULD ballooning; Cryocoolers; Cryogens AB This study examines the relative mass required in the use of stored cryogens and mechanical cryocoolers, for cooling of detectors and optics in stratospheric-balloon borne observatories. Lofted mass per unit heat removed from a cryogenic instrument is calculated, as a function of temperature, for three cooling approaches: (a) the use of stored cryogens; (b) use of an acoustic-Stirling ("pulse tube") mechanical cryocooler powered by electric storage batteries; and (c) the same cryocooler with solar-electric energy collection partially or fully replacing storage batteries. For the latter case, the mission duration at which the systems masses are equal is also found. Principal conclusions are (1) stored cryogens can provide cooling for lower mass than storage-battery operated cryocoolers over most of the temperature range considered, but the difference is not large; (2) solar-conversion systems can be the lower-mass option at higher temperature, but the mission duration for equal mass increases rapidly below similar to 30 K. (C) 2014 Elsevier Ltd. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Paine, CG (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM cpaine@jpl.nasa.gov NR 2 TC 0 Z9 0 U1 1 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0011-2275 EI 1879-2235 J9 CRYOGENICS JI Cryogenics PD NOV-DEC PY 2014 VL 64 BP 153 EP 156 DI 10.1016/j.cryogenics.2014.06.002 PG 4 WC Thermodynamics; Physics, Applied SC Thermodynamics; Physics GA AY4XE UT WOS:000347577600022 ER PT J AU Deserranno, D Zagarola, M Li, X Mustafi, S AF Deserranno, D. Zagarola, M. Li, X. Mustafi, S. TI Optimization of a Brayton cryocooler for ZBO liquid hydrogen storage in space SO CRYOGENICS LA English DT Article DE Thermodynamics; Brayton cycle; Space cryogenics AB NASA is evaluating and developing technology for long-term storage of cryogenic propellant in space. A key technology is a cryogenic refrigerator which intercepts heat loads to the storage tank, resulting in a reduced- or zero-boil-off condition. Turbo-Brayton cryocoolers are particularly well suited for cryogen storage applications because the technology scales well to high capacities and low temperatures. In addition, the continuous-flow nature of the cycle allows direct cooling of the cryogen storage tank without mass and power penalties associated with a cryogenic heat transport system. To quantify the benefits and mature the cryocooler technology, Creare Inc. performed a design study and technology demonstration effort for NASA on a 20 W, 20 K cryocooler for liquid hydrogen storage. During the design study, we optimized these key components: three centrifugal compressors, a modular high-capacity plate-fin recuperator, and a single-stage turboalternator. The optimization of the compressors and turboalternator were supported by component testing. The optimized cryocooler has an overall flight mass of 88 kg and a specific power of 61 W/W. The coefficient of performance of the cryocooler is 23% of the Carnot cycle. This is significantly better performance than any 20 K space cryocooler existing or under development. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Deserranno, D.; Zagarola, M.] Creare Res & Dev Inc, Hanover, NH 03755 USA. [Li, X.; Mustafi, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Deserranno, D (reprint author), Creare Res & Dev Inc, POB 71, Hanover, NH 03755 USA. EM dxd@creare.com FU NASA Goddard Space Flight Center [NNG12LN29P] FX We gratefully acknowledge NASA Goddard Space Flight Center for their the support of this work (Contract No. NNG12LN29P). NR 20 TC 3 Z9 3 U1 2 U2 11 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0011-2275 EI 1879-2235 J9 CRYOGENICS JI Cryogenics PD NOV-DEC PY 2014 VL 64 BP 172 EP 181 DI 10.1016/j.cryogenics.2014.04.025 PG 10 WC Thermodynamics; Physics, Applied SC Thermodynamics; Physics GA AY4XE UT WOS:000347577600025 ER PT J AU Mitsuishi, I Ezoe, Y Ishikawa, K Ohashi, T Fujimoto, R Mitsuda, K Tsunematsu, S Yoshida, S Kanao, K Murakami, M DiPirro, M Shirron, P AF Mitsuishi, I. Ezoe, Y. Ishikawa, K. Ohashi, T. Fujimoto, R. Mitsuda, K. Tsunematsu, S. Yoshida, S. Kanao, K. Murakami, M. DiPirro, M. Shirron, P. CA SXS Team TI He flow rate measurements on the engineering model for the Astro-H Soft X-ray Spectrometer dewar SO CRYOGENICS LA English DT Article DE Space cryogenics; X-ray microcalorimeter; Porous plug phase separator; Superfluid film flow; Mass flow ID SUPERFLUID FILM FLOW; POROUS PLUG; SUPPRESSION; SYSTEM AB The sixth X-ray Japanese astronomy satellite, namely Astro-H, will be launched in 2015. The Soft X-ray Spectrometer onboard the Astro-H is a 6 x 6 X-ray microcalorimeter array and provides us with both a high energy resolution of <7 eV at 0.5-10 key and a 3' x 3' modest imaging capability for the first time. To cool the detector down to the operation temperature of 50 mK, five cryocoolers, a 30-L superfluid helium cryostat, and a 3-stage adiabatic demagnetization refrigerator are utilized. A very small heat load up to similar to 0.9 mW on the helium tank is allowable to realize the helium lifetime of >3 years, which consequently requires that the vapor flow rate out of the helium tank should be very small <42 mu g/s. We adopted a porous plug phase separator in combination with a film flow suppression system composed of an orifice, a heat exchanger and knife edge devices to retain the liquid helium under zero gravity and safely vent the small amount of the helium vapor. We measured helium mass flow rates from the helium tank equipped in the engineering model dewar. We tilted the dewar at an angle of 75 degrees so that one side of the porous plug located at the top of the helium tank attaches the liquid helium and the porous plug separates the liquid and vapor helium by thermomechanical effect. Helium mass flow rates were measured at helium tank temperatures of 1.3, 1.5 and 1.9 K. We confirmed that resultant mass flow rates are in good agreement within the systematic error or low compared to component test results and achieve all the requirements. The film flow suppression also worked normally. Therefore, we concluded that the SXS helium vent system satisfactorily performs integrated into the dewar. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Mitsuishi, I.; Ezoe, Y.; Ohashi, T.] Tokyo Metropolitan Univ, Dept Phys, Tokyo, Japan. [Mitsuishi, I.] Nagoya Univ, Div Particle & Astrophy Sci, Nagoya, Aichi 4648602, Japan. [Ishikawa, K.] RIKEN, Inst Phys & Chem Res, Wako, Saitama, Japan. [Fujimoto, R.] Kanazawa Univ, Fac Math & Phys, Kanazawa, Ishikawa 9201192, Japan. [Mitsuda, K.] ISAS JAXA, Dept Space Astron & Astrophys, Sagamihara, Kanagawa, Japan. [Tsunematsu, S.; Yoshida, S.; Kanao, K.] Sumitomo Heavy Ind Ltd, Tokyo, Japan. [Murakami, M.] Univ Tsukuba, Grad Sch Syst & Informat Engn, Tsukuba, Ibaraki 305, Japan. [DiPirro, M.; Shirron, P.] NASA GSFC, Cryogen & Fluid Branch, Greenbelt, MD USA. RP Mitsuishi, I (reprint author), Nagoya Univ, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648602, Japan. EM mitsuisi@u.phys.nagoya-u.ac.jp NR 12 TC 3 Z9 4 U1 0 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0011-2275 EI 1879-2235 J9 CRYOGENICS JI Cryogenics PD NOV-DEC PY 2014 VL 64 BP 189 EP 193 DI 10.1016/j.cryogenics.2014.02.013 PG 5 WC Thermodynamics; Physics, Applied SC Thermodynamics; Physics GA AY4XE UT WOS:000347577600027 ER PT J AU Canavan, ER James, BL Hatt, TP Oliver, A Sullivan, DF AF Canavan, E. R. James, B. L. Hatt, T. P. Oliver, A. Sullivan, D. F. TI The Astro-H high temperature superconductor lead assemblies SO CRYOGENICS LA English DT Article DE Space flight; High temperature superconductor; Current leads ID YBCO-COATED CONDUCTORS; YBA2CU3O7-DELTA; STRESS AB The Soft X-ray Spectrometer (SXS) instrument, one of several instruments on JAXA's Astro-H mission, will observe diffuse X-ray sources with unparalleled spectral resolution using a microcalorimeter array operating at 50 mK. The array is cooled with a multi-stage Adiabatic Demagnetization Refrigerator mounted on a 401 helium tank. The tank is at the center of a typical "shell in shell" cryostat, with the innermost shield cooled by a JT cryocooler, and successive outer shields cooled by stirling-cycle cryocoolers. To achieve a multi-year liquid helium lifetime and to avoid exceeding the limited capacity of the JT cooler, very strict requirements are placed on every source of heat leak into these surfaces from the higher temperature shields. However, each ADR stage draws a maximum of 2 A, and the Wiedemann-Franz Law precludes even an optimized set of normal-metal leads capable of such high current from achieving the required low thermal conductance. Instead, a set of lead assemblies have been developed based on narrow high temperature superconductor (HTS) tapes derived from commercially available coated conductors. Although the HTS tapes are flexible and have high tensile strength, they are extremely sensitive to damage through a number of mechanisms. A robust set of assemblies have been developed that provide mechanical support to the tapes, provide appropriate interfaces at either end, and yet still meet the challenging thermal requirements. An Engineering Model (EM) set of HTS lead assemblies have survived environmental testing, both as individual units and as part of the EM cryostat, and have performed without problem in recent operation of the EM instrument. The Flight Model (FM) HTS lead assemblies are currently nearing completion. Published by Elsevier Ltd. C1 [Canavan, E. R.; James, B. L.; Hatt, T. P.; Sullivan, D. F.] NASA, Goddard Space Flight Ctr, Cryogen & Fluids Branch, Greenbelt, MD 20771 USA. [Oliver, A.] Tai Yang Res Co, Tallahassee, FL 32304 USA. RP Canavan, ER (reprint author), NASA, Goddard Space Flight Ctr, Code 552, Greenbelt, MD 20771 USA. EM Edgar.R.Canavan@nasa.gov NR 14 TC 2 Z9 2 U1 2 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0011-2275 EI 1879-2235 J9 CRYOGENICS JI Cryogenics PD NOV-DEC PY 2014 VL 64 BP 194 EP 200 DI 10.1016/j.cryogenics.2014.06.003 PG 7 WC Thermodynamics; Physics, Applied SC Thermodynamics; Physics GA AY4XE UT WOS:000347577600028 ER PT J AU Shirron, P DiPirro, M Kimball, M Sneiderman, G Porter, FS Kilbourne, C Kelley, R Fujimoto, R Yoshida, S Takei, Y Mitsuda, K AF Shirron, P. DiPirro, M. Kimball, M. Sneiderman, G. Porter, F. S. Kilbourne, C. Kelley, R. Fujimoto, R. Yoshida, S. Takei, Y. Mitsuda, K. TI Operation of an ADR using helium exchange gas as a substitute for a failed heat switch SO CRYOGENICS LA English DT Article DE Adiabatic demagnetization; ADR; Space cryogenics; Exchange gas ID X-RAY SPECTROMETER; DESIGN AB The Soft X-ray Spectrometer (SXS) is one of four instruments on the Japanese Astro-H mission, which is currently planned for launch in late 2015. The SXS will perform imaging spectroscopy in the soft X-ray band (0.3-12 key) using a 6 x 6 pixel array of microcalorimeters cooled to 50 mK. The detectors are cooled by a 3-stage adiabatic demagnetization refrigerator (ADR) that rejects heat to either a superfluid helium tank (at 1.2 K) or to a 4.5 K Joule-Thomson (JT) cryocooler. Four gas-gap heat switches are used in the assembly to manage heat flow between the ADR stages and the heat sinks. The engineering model (EM) ADR was assembled and performance tested at NASA/GSFC in November 2011, and subsequently installed in the EM dewar at Sumitomo Heavy Industries, Japan. During the first cooldown in July 2012, a failure of the heat switch that linked the two colder stages of the ADR to the helium tank was observed. Operation of the ADR requires some mechanism for thermally linking the salt pills to the heat sink, and then thermally isolating them. With the failed heat switch unable to perform this function, an alternate plan was devised which used carefully controlled amounts of exchange gas in the dewar's guard vacuum to facilitate heat exchange. The process was successfully demonstrated in November 2012, allowing the ADR to cool the detectors to 50 mK for hold times in excess of 10 h. This paper describes the exchange-gas-assisted recycling process, and the strategies used to avoid helium contamination of the detectors at low temperature. Published by Elsevier Ltd. C1 [Shirron, P.; DiPirro, M.; Kimball, M.; Sneiderman, G.; Porter, F. S.; Kilbourne, C.; Kelley, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fujimoto, R.] Kanazawa Univ, Inst Sci & Engn, Kanazawa, Ishikawa 9201192, Japan. [Yoshida, S.] Sumitomo Heavy Ind, Niihama, Ehime 7920001, Japan. [Takei, Y.; Mitsuda, K.] Japan Aerosp Explorat Agcy JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan. RP DiPirro, M (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM peter.shirron@nasa.gov RI Porter, Frederick/D-3501-2012 OI Porter, Frederick/0000-0002-6374-1119 NR 10 TC 1 Z9 1 U1 0 U2 2 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0011-2275 EI 1879-2235 J9 CRYOGENICS JI Cryogenics PD NOV-DEC PY 2014 VL 64 BP 207 EP 212 DI 10.1016/j.cryogenics.2014.04.011 PG 6 WC Thermodynamics; Physics, Applied SC Thermodynamics; Physics GA AY4XE UT WOS:000347577600030 ER PT J AU Tuttle, J Canavan, E DiPirro, M Li, XY Franck, R Renbarger, M Copp, T Hahn, M AF Tuttle, Jim Canavan, Ed DiPirro, Mike Li, Xiaoyi Franck, Randy Renbarger, Mike Copp, Tracy Hahn, Matt TI The area-density-dependence of Ball IR Black's low-temperature emissivity SO CRYOGENICS LA English DT Article DE BIRB; Emissivity; JWST AB Ball Infrared Black (TM), (BIRB) produced by Ball Aerospace and Technologies Corp, is a proprietary surface coating used in space-flight applications. It has a high total hemispheric emissivity at cryogenic temperatures, making it valuable for radiative cooling of components with very low operating temperatures. BATC is capable of controlling the mass per unit area of their BIRB coating, which impacts its effective thickness. In a previous publication we presented the results of total hemispheric emissivity measurements on a relatively high area-density coating of BIRB at temperatures between 300 and 20 K. These measurements were made in a small cryostat using a new technique. We have recently performed similar measurements on two lower area-density BIRB samples. The emissivity values for all samples were at least 0.95 between 30 and 300 K. Published by Elsevier Ltd. C1 [Tuttle, Jim; Canavan, Ed; DiPirro, Mike; Li, Xiaoyi] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Franck, Randy; Renbarger, Mike; Copp, Tracy; Hahn, Matt] Ball Aerosp & Technol Corp, Boulder, CO USA. RP Tuttle, J (reprint author), NASA GSFC, Code 552, Greenbelt, MD 20771 USA. EM James.g.tuttle@nasa.gov FU NASA's James Webb Space Telescope program FX This work was supported by NASA's James Webb Space Telescope program. NR 3 TC 1 Z9 1 U1 0 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0011-2275 EI 1879-2235 J9 CRYOGENICS JI Cryogenics PD NOV-DEC PY 2014 VL 64 BP 240 EP 243 DI 10.1016/j.cryogenics.2014.04.024 PG 4 WC Thermodynamics; Physics, Applied SC Thermodynamics; Physics GA AY4XE UT WOS:000347577600035 ER PT J AU Hartwig, JW Darr, SR McQuillen, JB Rame, E Chato, DJ AF Hartwig, J. W. Darr, S. R. McQuillen, J. B. Rame, E. Chato, D. J. TI A steady state pressure drop model for screen channel liquid acquisition devices SO CRYOGENICS LA English DT Article DE Liquid acquisition devices; Liquid hydrogen; Cryogenic fluid management; Porous screen; Thermodynamic vent heat exchanger; Fuel depot ID BUBBLE POINT TESTS; HYDROGEN AB This paper presents the derivation of a simplified one dimensional (1D) steady state pressure drop model for flow through a porous liquid acquisition device (LAD) inside a cryogenic propellant tank. Experimental data is also presented from cryogenic LAD tests in liquid hydrogen (LH2) and liquid oxygen (LOX) to compare against the simplified model and to validate the model at cryogenic temperatures. The purpose of the experiments was to identify the various pressure drop contributions in the analytical model which govern LAD channel behavior during dynamic, steady state outflow. LH2 pipe flow of LAD screen samples measured the second order flow-through-screen (FfS) pressure drop, horizontal LOX LAD outflow tests determined the relative magnitude of the third order frictional and dynamic losses within the channel, while LH2 inverted vertical outflow tests determined the magnitude of the first order hydrostatic pressure loss and validity of the full ID model. When compared to room temperature predictions, the FTS pressure drop is shown to be temperature dependent, with a significant increase in flow resistance at LH2 temperatures. Model predictions of frictional and dynamic losses down the channel compare qualitatively with LOX LADs data. Meanwhile, the 1D model predicted breakdown points track the trends in the LH2 inverted outflow experimental results, with discrepancies being due to a non-uniform injection velocity across the LAD screen not accounted for in the model. Published by Elsevier Ltd. C1 [Hartwig, J. W.; Chato, D. J.] Glenn Res Ctr, Prop & Propellants Branch, Cleveland, OH USA. [Darr, S. R.] Univ Florida, Gainesville, FL 32611 USA. [McQuillen, J. B.] Glenn Res Ctr, Fluid Phys & Transport Branch, Cleveland, OH USA. [Rame, E.] Glenn Res Ctr, Natl Ctr Micrograv Res, Cleveland, OH USA. RP Hartwig, JW (reprint author), NASA Glenn Res Ctr, M-S 301-3, Cleveland, OH 44135 USA. EM Jason.W.Hartwig@nasa.gov RI Chato, David/B-2698-2013 OI Chato, David/0000-0003-2990-0646 FU Cryogenic Propellant Storage and Transfer (CPST) Project under the Space Technology Mission Directorate's (STMD) Technology Demonstration Program at NASA FX This work was funded by the Cryogenic Propellant Storage and Transfer (CPST) Project under the Space Technology Mission Directorate's (STMD) Technology Demonstration Program at NASA. The authors wish to extend sincere gratitude to the support staff at the Small Multipurpose Research Facility (SMiRF) at NASA Glenn. NR 22 TC 6 Z9 6 U1 1 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0011-2275 EI 1879-2235 J9 CRYOGENICS JI Cryogenics PD NOV-DEC PY 2014 VL 64 BP 260 EP 271 DI 10.1016/j.cryogenics.2014.03.005 PG 12 WC Thermodynamics; Physics, Applied SC Thermodynamics; Physics GA AY4XE UT WOS:000347577600039 ER PT J AU DeLee, CH Barfknecht, P Breon, S Boyle, R DiPirro, M Francis, J Huynh, J Li, X McGuire, J Mustafi, S Tuttle, J Wegel, D AF DeLee, C. H. Barfknecht, P. Breon, S. Boyle, R. DiPirro, M. Francis, J. Huynh, J. Li, X. McGuire, J. Mustafi, S. Tuttle, J. Wegel, D. TI Techniques for on-orbit cryogenic servicing SO CRYOGENICS LA English DT Article DE Satellite servicing; Cryogenic fluid transfer; Cryogen freezing; Solid cryogen; Robotic refueling mission; On-orbit resupply; No vent fill; Autogenous pressurization; Spacecraft servicing mission concepts AB NASA (National Aeronautics and Space Administration) has a renewed interest in on-orbit cryogen storage and transfer to support its mission to explore near-earth objects such as asteroids and comets. The Cryogenic Propellant Storage and Transfer Technology Demonstration Mission (CPST-TDM), managed by the NASA Glenn Research Center (CRC) and scheduled for launch in 2018, will demonstrate numerous key technologies applicable to a cryopropellant fuel depot. As an adjunct to the CPST-TDM work, experiments at NASA Goddard Space Flight Center (GSFC) will support the development of techniques to manage and transfer cryogens on-orbit and expand these techniques as they may be applicable to servicing science missions using solid cryogens such as the Wide-field Infrared Survey Explorer (WISE). The results of several ground experiments are described, including autogenous pressurization used for transfer of liquid nitrogen and argon, characterization of the transfer and solidification of argon, and development of robotic tools for cryogen transfer. Published by Elsevier Ltd. C1 [DeLee, C. H.; Barfknecht, P.; Boyle, R.; DiPirro, M.; Francis, J.; Huynh, J.; Li, X.; Mustafi, S.; Tuttle, J.; Wegel, D.] Goddard Space Flight Ctr, Cryogen & Fluids Branch, Greenbelt, MD USA. [Breon, S.] Goddard Space Flight Ctr, Mech Syst Div, Greenbelt, MD USA. [McGuire, J.] Goddard Space Flight Ctr, Satellite Servicing Capabil Off, Greenbelt, MD USA. RP DeLee, CH (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM hudson.delee@nasa.gov FU Satellite Servicing Capabilities Office (SSCO) at the NASA Goddard Space Flight Center FX This work was supported by the Satellite Servicing Capabilities Office (SSCO) at the NASA Goddard Space Flight Center. NR 10 TC 0 Z9 0 U1 1 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0011-2275 EI 1879-2235 J9 CRYOGENICS JI Cryogenics PD NOV-DEC PY 2014 VL 64 BP 289 EP 294 DI 10.1016/j.cryogenics.2014.02.016 PG 6 WC Thermodynamics; Physics, Applied SC Thermodynamics; Physics GA AY4XE UT WOS:000347577600042 ER PT J AU Hartwig, JW Chato, DJ McQuillen, JB Vera, J Kudlac, MT Quinn, FD AF Hartwig, J. W. Chato, D. J. McQuillen, J. B. Vera, J. Kudlac, M. T. Quinn, F. D. TI Screen channel liquid acquisition device outflow tests in liquid hydrogen SO CRYOGENICS LA English DT Article DE Liquid acquisition devices; Liquid hydrogen; Cryogenic fluid management; Subcooled liquid; Thermodynamic vent heat exchanger; Fuel depot ID BUBBLE POINT TESTS AB This paper presents experimental design and test results of the recently concluded 1-g inverted vertical outflow testing of two 325 x 2300 full scale liquid acquisition device (LAD) channels in liquid hydrogen (LH2). One of the channels had a perforated plate and internal cooling from a thermodynamic vent system (TVS) to enhance performance. The LADs were mounted in a tank to simulate 1-g outflow over a wide range of LH2 temperatures (20.3-24.2 K), pressures (100-350 kPa), and flow rates (0.010-0.055 kg/s). Results indicate that the breakdown point is dominated by liquid temperature, with a second order dependence on mass flow rate through the LAD. The best performance is always achieved in the coldest liquid states for both channels, consistent with bubble point theory. Higher flow rates cause the standard channel to break down relatively earlier than the TVS cooled channel. Both the internal TVS heat exchanger and subcooling the liquid in the propellant tank are shown to significantly improve LAD performance. Published by Elsevier Ltd. C1 [Hartwig, J. W.; Chato, D. J.] Glenn Res Ctr, Prop & Propellants Branch, Cleveland, OH USA. [McQuillen, J. B.] Glenn Res Ctr, Fluid Phys & Transport Branch, Cleveland, OH USA. [Vera, J.; Kudlac, M. T.; Quinn, F. D.] Glenn Res Ctr, Fluids Syst & Engn Branch, Cleveland, OH USA. RP Hartwig, JW (reprint author), NASA Glenn Res Ctr, M-S 301-3, Cleveland, OH 44135 USA. EM Jason.W.Hartwig@nasa.gov RI Chato, David/B-2698-2013 OI Chato, David/0000-0003-2990-0646 FU Cryogenic Propellant Storage and Transfer (CPST) Project under the Office of the Chief Technologist (OCT) at NASA FX This work was funded by the Cryogenic Propellant Storage and Transfer (CPST) Project under the Office of the Chief Technologist (OCT) at NASA. The authors wish to extend sincere gratitude to the support staff at the Small Multipurpose Research Facility (SMiRF) at NASA Glenn. NR 29 TC 7 Z9 7 U1 1 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0011-2275 EI 1879-2235 J9 CRYOGENICS JI Cryogenics PD NOV-DEC PY 2014 VL 64 BP 295 EP 306 DI 10.1016/j.cryogenics.2014.02.011 PG 12 WC Thermodynamics; Physics, Applied SC Thermodynamics; Physics GA AY4XE UT WOS:000347577600043 ER PT J AU Hegde, U Gotti, D Hicks, M AF Hegde, U. Gotti, D. Hicks, M. TI The transition to turbulence of buoyant near-critical water jets SO JOURNAL OF SUPERCRITICAL FLUIDS LA English DT Article DE Transition; Turbulence; Jets; Supercritical ID SUPERCRITICAL FLUIDS; CRITICAL-POINT; FLOWS; INSTABILITY AB Observations of near-critical water jets are reported in the injection Reynolds number range of approximately 300-3000 to characterize their transition to turbulence. Three types of cases are described: (i) subcritical jet injected into subcritical water, (ii) supercritical jet injected into supercritical water, and (iii) supercritical jet injected into subcritical water. In each case, the working pressure was kept above the critical value to eliminate two-phase effects. For cases (i) and (ii), the transition behavior follows well known characteristics with transition to turbulence initially occurring near the tip of the jet with the transition location moving upstream nearer to the nozzle exit with an increase in injection Reynolds number. However, the transition behavior for case (iii) is quite different with significant buoyant effects leading to turbulent behavior at lower Reynolds numbers. Consideration of the pseudocritical region with strongly varying fluid properties, which is established in the mixing region between the jet and the cell fluid, yields an effective Froude number that is useful to elucidate this difference. The effective Froude number incorporates the Prandtl number of the mixing region to account for the large disparity between viscous and thermal length scales. (C) 2014 Elsevier B.V. All rights reserved. C1 [Hegde, U.; Gotti, D.] Natl Ctr Space Explorat Res, Cleveland, OH USA. [Hicks, M.] NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA. RP Hegde, U (reprint author), NASA, John H Glenn Res Ctr, MS 110-3, Cleveland, OH 44135 USA. EM uday.g.hegde@nasa.gov; daniel.j.gotti@nasa.gov; michael.c.hicks@nasa.gov FU NASA [NNC08BA08B] FX U. Hegde and D. Gotti were supported under NASA Contract NNC08BA08B. The assistance of J. Owens and W. Yanis of the National Center for Space Exploration in the conduct of the experiments is gratefully acknowledged. NR 22 TC 3 Z9 3 U1 1 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0896-8446 EI 1872-8162 J9 J SUPERCRIT FLUID JI J. Supercrit. Fluids PD NOV PY 2014 VL 95 BP 195 EP 203 DI 10.1016/j.supflu.2014.08.005 PG 9 WC Chemistry, Physical; Engineering, Chemical SC Chemistry; Engineering GA AY1NY UT WOS:000347360800023 ER PT J AU Nast, TC Frank, DJ Feller, J AF Nast, T. C. Frank, D. J. Feller, J. TI Multilayer insulation considerations for large propellant tanks SO CRYOGENICS LA English DT Article DE Cryogenic insulation; Hydrogen tank insulation AB Multilayer insulation (MLI) systems for cryogenic instrument Dewars have demonstrated very high thermal performance in ground and orbit. Ground tests of insulation systems on propellant storage size tanks have shown performance and repeatability issues. This paper presents a summary of studies for National Aeronautics and Space Administration (NASA) focused on MU I systems on the larger Tank-age. The sensitivity of boil off to MLI thermal conductivity is presented. The effect of compressions, assembly joints and MLI parameters are presented. A novel large tank simulator approach for MLI testing is presented along with recommendations for maturation of the MLI technology. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Nast, T. C.; Frank, D. J.] Lockheed Martin Adv Technol Ctr, Palo Alto, CA USA. [Feller, J.] NASA, Ames Res Ctr, Mountain View, CA USA. RP Frank, DJ (reprint author), Lockheed Martin Adv Technol Ctr, Palo Alto, CA USA. EM dave.frank@lmco.com NR 23 TC 3 Z9 3 U1 1 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0011-2275 EI 1879-2235 J9 CRYOGENICS JI Cryogenics PD NOV-DEC PY 2014 VL 64 BP 105 EP 111 DI 10.1016/j.cryogenics.2014.02.014 PG 7 WC Thermodynamics; Physics, Applied SC Thermodynamics; Physics GA AY4XE UT WOS:000347577600016 ER PT J AU Han, WQ Vialard, J McPhaden, MJ Lee, T Masumoto, Y Feng, M De Ruijter, WPM AF Han, Weiqing Vialard, Jerome McPhaden, Michael J. Lee, Tong Masumoto, Yukio Feng, Ming De Ruijter, Will P. M. TI INDIAN OCEAN DECADAL VARIABILITY A Review SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID SEA-SURFACE TEMPERATURE; ASIAN-AUSTRALIAN MONSOON; NORTH-ATLANTIC OSCILLATION; WESTERN TROPICAL PACIFIC; HEAT-CONTENT VARIABILITY; CLIMATE SYSTEM MODEL; INDO-PACIFIC; TIME SCALES; LEVEL-RISE; MULTIDECADAL VARIABILITY C1 [Han, Weiqing] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA. [Vialard, Jerome] Univ Paris 06, Lab Ocanographie Exprimentat & Approches Numeriqu, IRD, CNRS,MNHN, Paris, France. [McPhaden, Michael J.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. [Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Masumoto, Yukio] Japan Agcy Marine Earth Sci & Technol, Climate Variat Predictabil & Applicabil Res Progr, Yokohama, Kanagawa, Japan. [Feng, Ming] Ctr Environm & Life Sci, CSIRO Marine & Atmospher Res, Floreat, WA, Australia. [De Ruijter, Will P. M.] Univ Utrecht, Inst Marine & Atmospher Res, Utrecht, Netherlands. RP Han, WQ (reprint author), Univ Colorado, Dept Atmospher & Ocean Sci, UCB 311, Boulder, CO 80309 USA. EM weiqing.han@colorado.edu RI Vialard, Jerome/C-2809-2008; McPhaden, Michael/D-9799-2016; de Ruijter, Wilhelmus/I-2541-2016; Feng, Ming/F-5411-2010 OI Vialard, Jerome/0000-0001-6876-3766; Feng, Ming/0000-0002-2855-7092 FU NSF CAREER Award [OCE 0847605]; NOAA; CSIRO Wealth from Oceans Flagship; Australian Climate Change Science Program FX We thank the member of the CLIVAR/GOOS Indian Ocean Panel for their help and support for writing this review. We also would like to express our appreciation of Dr. Yuanlong Li for processing the D20 and OSCAR surface current data and of Dr. John Antonov for providing the upper-ocean heat content data. We thank Drs. Paul Durack, Benjamin Hamlington, M. Lengaigne, A. G. Nidheesh, Tomoki Tozuka, and Laurie Trenary for providing high-resolution original figures. Dr. Shang-Ping Xie, Dr. Gerald Meehl, and an anonymous reviewer provided valuable constructive reviews of an earlier version of this manuscript. W. Han is supported by NSF CAREER Award OCE 0847605. M. J. McPhaden is supported by NOAA. Ming Feng is supported by CSIRO Wealth from Oceans Flagship and the Australian Climate Change Science Program. The research described in this paper was in part carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). NR 207 TC 23 Z9 24 U1 3 U2 35 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD NOV PY 2014 VL 95 IS 11 BP 1679 EP 1703 DI 10.1175/BAMS-D-13-00028.1 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AX9LU UT WOS:000347225100003 ER PT J AU Liu, YCM Huang, J Wang, C Klecker, B Galvin, AB Simunac, KDC Popecki, MA Kistler, L Farrugia, C Lee, MA Kucharek, H Opitz, A Luhmann, JG Jian, L AF Liu, Y. C-M. Huang, J. Wang, C. Klecker, B. Galvin, A. B. Simunac, K. D. C. Popecki, M. A. Kistler, L. Farrugia, C. Lee, M. A. Kucharek, H. Opitz, A. Luhmann, J. G. Jian, Lan TI A statistical analysis of heliospheric plasma sheets, heliospheric current sheets, and sector boundaries observed in situ by STEREO SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE heliospheric plasma sheet; heliospheric current sheet; sectory boundary; interchange reconnection; flux rope; slow solar wind ID SOLAR-WIND; CORONAL STREAMERS; RECONNECTION; ORIGIN; BLOBS AB The heliocentric orbits of STEREO A and B with a separation in longitude increasing by about 45 degrees per year provide the unique opportunity to study the evolution of the heliospheric plasma sheet (HPS) on a time scale of up to 2days and to investigate the relative locations of HPSs and heliospheric current sheets (HCSs). Previous work usually determined the HCS locations based only on the interplanetary magnetic field. A recent study showed that a HCS can be taken as a global structure only when it matches with a sector boundary (SB). Using magnetic field and suprathermal electron data, it was also shown that the relative location of HCS and SB can be classified into five different types of configurations. However, only for two out of these five configurations, the HCS and SB are located at the same position and only these will therefore be used for our study of the HCS/HPS relative location. We find that out of 37 SBs in our data set, there are 10 suitable HPS/HCS event pairs. We find that an HPS can either straddle or border the related HCS. Comparing the corresponding HPS observations between STEREO A and B, we find that the relative HCS/HPS locations are mostly similar. In addition, the time difference of the HPSs observations between STEREO A and B match well with the predicted time delay for the solar wind coming out of a similar region of the Sun. We therefore conclude that HPSs are stationary structures originating at the Sun. C1 [Liu, Y. C-M.; Huang, J.; Wang, C.] Chinese Acad Sci, Ctr Space Sci & Appl Res, State Key Lab Space Weather, Beijing, Peoples R China. [Huang, J.] Univ Chinese Acad Sci, Coll Earth Sci, Beijing, Peoples R China. [Klecker, B.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Galvin, A. B.; Simunac, K. D. C.; Popecki, M. A.; Kistler, L.; Farrugia, C.; Lee, M. A.; Kucharek, H.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Opitz, A.] CNRS, UMR 5187, Toulouse, France. [Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Jian, Lan] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Jian, Lan] NASA, Goddard Space Flight Ctr, Heliophy Sci Div, Greenbelt, MD 20771 USA. RP Liu, YCM (reprint author), Chinese Acad Sci, Ctr Space Sci & Appl Res, State Key Lab Space Weather, Beijing, Peoples R China. EM liuyong@spaceweather.ac.cn RI HUANG, Jia/L-2507-2013; Jian, Lan/B-4053-2010 OI Jian, Lan/0000-0002-6849-5527 FU Chinese Academy of Science [Y32135A47S]; Chinese National Science Foundation [411774149]; Specialized Research Fund for State Key laboratory of China; NASA [NAS5-00132, NNX10AQ29G, NNX13AP39G] FX This work is supported by the Chinese Academy of Science "Hundred Talented Program" of contract Y32135A47S, the Chinese National Science Foundation of contract 411774149, and the Specialized Research Fund for State Key laboratory of China. The work at UNH is supported by NASA under contract NAS5-00132, grants NNX10AQ29G and NNX13AP39G. The solar wind and IMF data are provided by the STEREO Science Center (stereo-ssc.nascom.nasa.gov). The authors are also grateful for Y. D. Liu at the Center for Space Science and Applied Research in China for helpful discussions. NR 35 TC 6 Z9 7 U1 1 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD NOV PY 2014 VL 119 IS 11 BP 8721 EP 8732 DI 10.1002/2014JA019956 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AX2RO UT WOS:000346792100001 ER PT J AU Omidi, N Russell, CT Jian, LK Isenberg, P Wei, HY AF Omidi, N. Russell, C. T. Jian, L. K. Isenberg, P. Wei, H. Y. TI Generation and propagation of ion cyclotron waves in nonuniform magnetic field: Application to the corona and solar wind SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article DE ion cyclotron waves; solar wind; corona ID MINOR IONS; ELECTROMAGNETIC-WAVES; KINETIC DISSIPATION; INVERSE CORRELATION; 1 AU; ACCELERATION; TURBULENCE; HELICITY; INSTABILITY; VELOCITY AB With the objective to understand the generation, propagation, and nonlinear evolution of ion cyclotron waves (ICWs) in the corona and solar wind, we use electromagnetic hybrid (kinetic ions and fluid electrons) simulations with a nonuniform magnetic field. ICWs are generated by the temperature anisotropy of O5+ ions as minority species in a proton-electron plasma with uniform density. A number of magnetic field models are used including radial and spiral with field strength decreasing linearly or with the square of the radial distance. O5+ ions with perpendicular temperature larger than parallel are initially placed in the high-magnetic field regions. These ions are found to expand outward along the magnetic field. Associated with this expansion, ion cyclotron waves propagating along the magnetic field are also seen to expand outward. These waves are generated at frequencies below the local gyrofrequency of O5+ ions propagating parallel and antiparallel to the magnetic field. Through analysis of the simulation results we demonstrate that wave generation and absorption take place at all radial distances. Comparing the simulation results to observations of ICWs in the solar wind shows some of the observed wave characteristics may be explained by the mechanism discussed in this paper. C1 [Omidi, N.] Solana Sci Inc, Solana Beach, CA USA. [Russell, C. T.; Wei, H. Y.] Univ Calif Los Angeles, IGPP, Los Angeles, CA USA. [Jian, L. K.] NASA GSFC, Greenbelt, MD USA. [Jian, L. K.] Univ Maryland, Dept Astron, College Pk, MD USA. [Isenberg, P.] Univ New Hampshire, Inst Study Earth, Oceans & Space, Durham, NH USA. RP Omidi, N (reprint author), Solana Sci Inc, Solana Beach, CA 92075 USA. EM omidi@solanasci.com RI Jian, Lan/B-4053-2010 OI Jian, Lan/0000-0002-6849-5527 FU NASA [NNX12AB29G, NNX13AI65G, NNX13AF97G] FX Work for this project was supported by NASA grants NNX12AB29G, NNX13AI65G, and NNX13AF97G. Request for simulation data used in this study may be made to N. Omidi at omidi@solanasci.com. NR 52 TC 2 Z9 2 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD NOV PY 2014 VL 119 IS 11 BP 8750 EP 8763 DI 10.1002/2014JA020315 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AX2RO UT WOS:000346792100003 ER PT J AU Livneh, B Deems, JS Schneider, D Barsugli, JJ Molotch, NP AF Livneh, Ben Deems, Jeff S. Schneider, Dominik Barsugli, Joseph J. Molotch, Noah P. TI Filling in the gaps: Inferring spatially distributed precipitation from gauge observations over complex terrain SO WATER RESOURCES RESEARCH LA English DT Article ID CONTERMINOUS UNITED-STATES; SNOW WATER EQUIVALENT; HYDROLOGICALLY BASED DATASET; LAND-SURFACE FLUXES; MOUNTAINOUS TERRAIN; OROGRAPHIC PRECIPITATION; INCORPORATING ELEVATION; OBSERVATION NETWORK; VEGETATION MODEL; SIERRA-NEVADA AB In recent decades, computational hydrology has trended toward higher-resolution distributed models of the land surface. The accuracy of these models is limited, by uncertainty in distributed precipitation forcings. In this research, different precipitation distribution schemes were compared through inter-station transfer experiments, as well as within a distributed hydrologic model applied at <= 150 m resolution over four study catchments in complex terrain. Distributed precipitation estimates were derived using multiplicative spatial scaling (MSS) and map-based precipitation (MBP) techniques including both climatological and time-varying spatial information from a range of native spatial resolutions (500 m-4 km). The primary interest was to evaluate a novel application of satellite-based snow water equivalent (SWE) reconstruction (RSWE) as a surrogate for cold season precipitation against a common source of spatial precipitation information: the Parameter-elevation Regressions on Independent Slopes Model (PRISM). An elevation-based orographic precipitation gradient and simple inverse-distance interpolation were also included as a baseline. For the case of RSWE, MSS was very sensitive to differences between observed SWE and reconstructed SWE, producing positive biases in the catchment water balance. Over 12 year simulations, daily streamflow correlations from the uncalibrated model were highest for RSWE when adjusted for accumulation-season sublimation, and for monthly PRISM, both achieving R=0.8, where the former performed better during anomalous years for both MSS and MBP. Annual water balance ratios were much more sensitive to the choice of distribution scheme, with large overestimates,>30%, for RSWE products using the MSS techniques versus MBP (<15%). Overall, PRISM performed best using MSS, while RSWE performed best using MBP. C1 [Livneh, Ben; Deems, Jeff S.; Barsugli, Joseph J.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Livneh, Ben; Deems, Jeff S.] Univ Colorado, Western Water Assessment, Boulder, CO 80309 USA. [Deems, Jeff S.] Univ Colorado, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA. [Schneider, Dominik; Molotch, Noah P.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA. [Schneider, Dominik; Molotch, Noah P.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. [Molotch, Noah P.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Livneh, B (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. EM ben.livneh@colorado.edu RI Livneh, Ben/I-2939-2015; Barsugli, Joseph/K-3541-2015; Molotch, Noah/C-8576-2009; Schneider, Dominik/O-7396-2016; Deems, Jeffrey/E-6484-2016; OI Barsugli, Joseph/0000-0002-3078-6396; Schneider, Dominik/0000-0002-5846-5033; Deems, Jeffrey/0000-0002-3265-8670; LIVNEH, BEN/0000-0001-5445-2473 FU NOAA Climate Program Office through the Western Water Assessment RISA at CIRES, University of Colorado-Boulder FX We would like to acknowledge Leanne Lestak for her GIS assistance. This research was funded by the NOAA Climate Program Office through the Western Water Assessment RISA at CIRES, University of Colorado-Boulder. The data used to produce the results of this paper can be obtained by contacting the corresponding author directly (ben.livneh@colorado.edu). NR 73 TC 9 Z9 9 U1 0 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD NOV PY 2014 VL 50 IS 11 BP 8589 EP 8610 DI 10.1002/2014WR015442 PG 22 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA AX0PQ UT WOS:000346654600013 ER PT J AU Wang, SG Liang, X AF Wang, Shugong Liang, Xu TI A parameter estimation framework for Multiscale Kalman Smoother algorithm in precipitation data fusion SO WATER RESOURCES RESEARCH LA English DT Article ID SCALE-RECURSIVE ESTIMATION; SURFACE SOIL-MOISTURE; DATA ASSIMILATION; EM ALGORITHM; RAINFALL; PRODUCTS; MODELS; SYSTEM; NEXRAD; FILTER AB A new effective parameter estimation approach is presented for the Multiscale Kalman Smoother (MKS) algorithm. As demonstrated, it shows promising potentials in deriving better data products involving sources from different spatial scales and precisions. The proposed approach employs a multiobjective parameter estimation framework, which includes three multiobjective estimation schemes (MO schemes), rather than using the conventional maximum likelihood scheme (ML scheme), to estimate the MKS parameters. Unlike the ML scheme, the MO schemes are not built on strict statistical assumptions related to prediction errors and observation errors, rather, they directly associate the fused data of multiple scales with multiple objective functions. In the MO schemes, objective functions are defined to facilitate consistency among the fused data at multiple scales and the input data at their original scales as well in terms of spatial patterns and magnitudes. Merits of the new approach are evaluated through a Monte Carlo experiment and a series of comparison analyses using synthetic precipitation data that contain noises which follow either the multiplicative error model or the additive error model. Our results show that the MKS fused precipitation performs better using the MO framework. Improvements are particularly significant for the fused precipitation associated with fine spatial resolutions. This is due mainly to the adoption of more criteria and constraints in the MO framework. The weakness of the original ML scheme, arising from its blindly putting more weights into the data associated with finer resolutions, is circumvented in the proposed new MO framework. C1 [Wang, Shugong] Sci Applicat Int Corp, Mclean, VA USA. [Wang, Shugong] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Liang, Xu] Univ Pittsburgh, Dept Civil & Environm Engn, Pittsburgh, PA 15260 USA. RP Liang, X (reprint author), Univ Pittsburgh, Dept Civil & Environm Engn, Pittsburgh, PA 15260 USA. EM xuliang@pitt.edu FU NASA [NNA07CN83A, NNX12AQ25G]; U.S. Department of Transportation [OASRTRS-14-H-PIT] FX The authors are thankful to the Associate Editor and the reviewers for their valuable comments and suggestions. We thank Jeen-Shang Lin for the valuable discussions. We also thank Server Levent Yilmaz for his help in providing computing assistance of using the TeraGrid resources of the Center for Simulation and Modeling at the University of Pittsburgh. This work was partially supported by the NASA grants NNA07CN83A and NNX12AQ25G and by the U.S. Department of Transportation grant OASRTRS-14-H-PIT to the University of Pittsburgh. NR 38 TC 0 Z9 0 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD NOV PY 2014 VL 50 IS 11 BP 8675 EP 8693 DI 10.1002/2013WR014942 PG 19 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA AX0PQ UT WOS:000346654600017 ER PT J AU Perrot, D Molotch, NP Williams, MW Jepsen, SM Sickman, JO AF Perrot, Danielle Molotch, Noah P. Williams, Mark W. Jepsen, Steven M. Sickman, James O. TI Relationships between stream nitrate concentration and spatially distributed snowmelt in high-elevation catchments of the western US SO WATER RESOURCES RESEARCH LA English DT Article ID COLORADO FRONT RANGE; ATMOSPHERIC NITROGEN DEPOSITION; GREEN LAKES VALLEY; ROCKY-MOUNTAINS; SIERRA-NEVADA; UNITED-STATES; WATER EQUIVALENT; CLIMATE-CHANGE; SEASONAL SNOW; COVERED AREA AB This study compares stream nitrate (NO3-) concentrations to spatially distributed snowmelt in two alpine catchments, the Green Lakes Valley, Colorado (GLV4) and Tokopah Basin, California (TOK). A snow water equivalent reconstruction model and Landsat 5 and 7 snow cover data were used to estimate daily snowmelt at 30 m spatial resolution in order to derive indices of new snowmelt areas (NSAs). Estimates of NSA were then used to explain the NO3- flushing behavior for each basin over a 12 year period (19962007). To identify the optimal method for defining NSAs and elucidate mechanisms underlying catchment NO3- flushing, we conducted a series of regression analyses using multiple thresholds of snowmelt based on temporal and volumetric metrics. NSA indices defined by volume of snowmelt (e.g., snowmelt <= 30 cm) rather than snowmelt duration (e.g., snowmelt <= 9 days) were the best predictors of stream NO3- concentrations. The NSA indices were better correlated with stream NO3- concentration in TOK (average R-2 = 0.68) versus GLV4 (average R-2 = 0.44). Positive relationships between NSA and stream NO3- concentration were observed in TOK with peak stream NO3- concentration occurring on the rising limb of snowmelt. Positive and negative relationships between NSA and stream NO3- concentration were found in GLV4 with peak stream NO3- concentration occurring as NSA expands. Consistent with previous works, the contrasting NO3- flushing behavior suggests that streamflow in TOK was primarily influenced by overland flow and shallow subsurface flow, whereas GLV4 appeared to be more strongly influenced by deeper subsurface flow paths. C1 [Perrot, Danielle; Molotch, Noah P.; Williams, Mark W.] Univ Colorado, Inst Arctic & Alpine Res, Dept Geog, Boulder, CO 80309 USA. [Molotch, Noah P.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Jepsen, Steven M.] Univ Calif, Sierra Nevada Res Inst, Merced, CA USA. [Sickman, James O.] Univ Calif Riverside, Dept Environm Sci, Riverside, CA 92521 USA. RP Molotch, NP (reprint author), Univ Colorado, Inst Arctic & Alpine Res, Dept Geog, Boulder, CO 80309 USA. EM noah.molotch@colorado.edu RI Molotch, Noah/C-8576-2009 FU NSF [EAR1032295, EAR1032308]; NSF's Boulder Creek Critical Zone Observatory FX This project was funded by NSF Hydrological Sciences grants EAR1032295 and EAR1032308, the NSF-funded Niwot Ridge Long-Term Ecological Research project, and NSF's Boulder Creek Critical Zone Observatory. Many thanks to Suzanne Anderson, Nel Caine, Galen McLauren, Michael Gleason, and Leah Meromy. Data can be obtained from http://niwot.colorado.edu/ and http://ccb.ucr.edu/emeraldlake/. NR 53 TC 3 Z9 3 U1 2 U2 24 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0043-1397 EI 1944-7973 J9 WATER RESOUR RES JI Water Resour. Res. PD NOV PY 2014 VL 50 IS 11 BP 8694 EP 8713 DI 10.1002/2013WR015243 PG 20 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA AX0PQ UT WOS:000346654600018 ER PT J AU Uckun, S Mackey, R Do, M Zhou, R Huang, E Shah, JJ AF Uckun, Serdar Mackey, Ryan Do, Minh Zhou, Rong Huang, Eric Shah, Jami J. TI Measures of product design adaptability for changing requirements SO AI EDAM-ARTIFICIAL INTELLIGENCE FOR ENGINEERING DESIGN ANALYSIS AND MANUFACTURING LA English DT Article DE Adaptability; Changeability; Reliability; Robustness; Survivability ID FLEXIBILITY; CUSTOMIZATION; ARCHITECTURE AB Adaptability can have many different definitions: reliability, robustness, survivability, and changeability (adaptability to requirements change). In this research, we focused entirely on the last type. We discuss two alternative approaches to requirements change adaptability. One is the valuation approach that is based on utility and cost of design changes in response to modified requirements. The valuation approach is theoretically sound because it is based on utility and decision theory, but it may be difficult to use in the real world. The second approach is based on examining product architecture characteristics that facilitate changes that include modularity, hierarchy, interfaces, performance sensitivity, and design margins. This approach is heuristic in nature but more practical to use. If calibrated, it could serve as a surrogate for real adaptability. These measures were incorporated in a software tool for exploring alternative configurations of fractionated space satellite systems. C1 [Uckun, Serdar] Telact, Palo Alto, CA USA. [Mackey, Ryan] CALTECH, Jet Prop Lab, NASA, Pasadena, CA USA. [Do, Minh] NASA Ames, Moffett Field, CA USA. [Zhou, Rong; Huang, Eric] PARC, Palo Alto, CA USA. [Shah, Jami J.] Arizona State Univ, Dept Mech & Aeronaut Engn, Design Automat Lab, Tempe, AZ 85287 USA. RP Shah, JJ (reprint author), Arizona State Univ, Dept Mech & Aeronaut Engn, Design Automat Lab, Tempe, AZ 85287 USA. EM jami.shah@asu.edu FU DARPA's F6 program FX This study was supported by DARPA's F6 program. The views expressed are those of the authors and do not reflect the official policy or position of the Department of Defense or the US government. This paper is based on work done jointly by PARC, NASA Jet Propulsion Laboratory, Mission Control Technologies, and Arizona State University. The Jet Propulsion Laboratory, California Institute of Technology, portion was carried out under a contract with the National Aeronautics and Space Administration. NR 37 TC 1 Z9 1 U1 1 U2 8 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0890-0604 EI 1469-1760 J9 AI EDAM JI AI EDAM-Artif. Intell. Eng. Des. Anal. Manuf. PD NOV PY 2014 VL 28 IS 4 SI SI BP 353 EP 368 DI 10.1017/S0890060414000523 PG 16 WC Computer Science, Artificial Intelligence; Computer Science, Interdisciplinary Applications; Engineering, Multidisciplinary; Engineering, Manufacturing SC Computer Science; Engineering GA AW5RN UT WOS:000346331800005 ER PT J AU Zhu, L Jacob, DJ Mickley, LJ Marais, EA Cohan, DS Yoshida, Y Duncan, BN Abad, GG Chance, KV AF Zhu, Lei Jacob, Daniel J. Mickley, Loretta J. Marais, Eloise A. Cohan, Daniel S. Yoshida, Yasuko Duncan, Bryan N. Abad, Gonzalo Gonzalez Chance, Kelly V. TI Anthropogenic emissions of highly reactive volatile organic compounds in eastern Texas inferred from oversampling of satellite (OMI) measurements of HCHO columns SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE HCHO; ozone monitoring instrument; anthropogenic; highly reactive VOC; oversampling ID OZONE MONITORING INSTRUMENT; ISOPRENE EMISSIONS; NORTH-AMERICA; TROPOSPHERIC DEGRADATION; FORMALDEHYDE COLUMNS; TRANSPORT MODEL; AIR-QUALITY; HOUSTON; INDUSTRIAL; SO2 AB Satellite observations of formaldehyde (HCHO) columns provide top-down constraints on emissions of highly reactive volatile organic compounds (HRVOCs). This approach has been used previously in the US to estimate isoprene emissions from vegetation, but application to anthropogenic emissions has been stymied by lack of a discernable HCHO signal. Here we show that temporal oversampling of HCHO data from the Ozone Monitoring Instrument (OMI) for 2005-2008 enables detection of urban and industrial plumes in eastern Texas including Houston, Port Arthur, and Dallas/Fort Worth. By spatially integrating the HCHO enhancement in the Houston plume observed by OMI we estimate an anthropogenic HCHO source of 250 +/- 140 kmol h(-1). This implies that anthropogenic HRVOC emissions in Houston are 4.8 +/- 2.7 times higher than reported by the US Environmental Protection Agency inventory, and is consistent with field studies identifying large ethene and propene emissions from petrochemical industrial sources. C1 [Zhu, Lei; Jacob, Daniel J.; Mickley, Loretta J.; Marais, Eloise A.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Cohan, Daniel S.] Rice Univ, Houston, TX USA. [Yoshida, Yasuko] Sci Syst & Applicat Inc, Lanham, MD USA. [Yoshida, Yasuko; Duncan, Bryan N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Abad, Gonzalo Gonzalez; Chance, Kelly V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhu, L (reprint author), Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. EM leizhu@fas.harvard.edu RI Cohan, Daniel/E-6595-2010; Duncan, Bryan/A-5962-2011; OI Cohan, Daniel/0000-0003-0415-7980; Chance, Kelly/0000-0002-7339-7577; Marais, Eloise/0000-0001-5477-8051; Gonzalez Abad, Gonzalo/0000-0002-8090-6480 FU NASA Aura Science Team; Air Quality Applied Sciences Team FX This work was supported by the NASA Aura Science Team and Air Quality Applied Sciences Team. The authors thank Barry Lefer and James Flynn at the University of Houston and Xiong Liu at the Harvard-Smithsonian Center for Astrophysics for their help. We thank two anonymous reviewers who provided thorough and thoughtful comments. NR 53 TC 15 Z9 15 U1 9 U2 48 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-9326 J9 ENVIRON RES LETT JI Environ. Res. Lett. PD NOV PY 2014 VL 9 IS 11 AR 114004 DI 10.1088/1748-9326/9/11/114004 PG 7 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AW9JS UT WOS:000346573900010 ER PT J AU Keppel-Aleks, G Wolf, AS Mu, MQ Doney, SC Morton, DC Kasibhatla, PS Miller, JB Dlugokencky, EJ Randerson, JT AF Keppel-Aleks, Gretchen Wolf, Aaron S. Mu, Mingquan Doney, Scott C. Morton, Douglas C. Kasibhatla, Prasad S. Miller, John B. Dlugokencky, Edward J. Randerson, James T. TI Separating the influence of temperature, drought, and fire on interannual variability in atmospheric CO2 SO GLOBAL BIOGEOCHEMICAL CYCLES LA English DT Article DE carbon cycle; climate variability; drought; fire; terrestrial ecosystems; atmospheric CO2 ID CARBON-DIOXIDE VARIABILITY; SEA-SURFACE TEMPERATURE; SOUTHERN-OSCILLATION; TROPICAL TEMPERATURE; CLIMATE-CHANGE; EL-NINO; SENSITIVITY; CYCLE; FLUXES; MODEL AB The response of the carbon cycle in prognostic Earth system models (ESMs) contributes significant uncertainty to projections of global climate change. Quantifying contributions of known drivers of interannual variability in the growth rate of atmospheric carbon dioxide (CO2) is important for improving the representation of terrestrial ecosystem processes in these ESMs. Several recent studies have identified the temperature dependence of tropical net ecosystem exchange (NEE) as a primary driver of this variability by analyzing a single, globally averaged time series of CO2 anomalies. Here we examined how the temporal evolution of CO2 in different latitude bands may be used to separate contributions from temperature stress, drought stress, and fire emissions to CO2 variability. We developed atmospheric CO2 patterns from each of these mechanisms during 1997-2011 using an atmospheric transport model. NEE responses to temperature, NEE responses to drought, and fire emissions all contributed significantly to CO2 variability in each latitude band, suggesting that no single mechanism was the dominant driver. We found that the sum of drought and fire contributions to CO2 variability exceeded direct NEE responses to temperature in both the Northern and Southern Hemispheres. Additional sensitivity tests revealed that these contributions are masked by temporal and spatial smoothing of CO2 observations. Accounting for fires, the sensitivity of tropical NEE to temperature stress decreased by 25% to 2.90.4 Pg C yr(-1)K(-1). These results underscore the need for accurate attribution of the drivers of CO2 variability prior to using contemporary observations to constrain long-term ESM responses. C1 [Keppel-Aleks, Gretchen] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Wolf, Aaron S.] Univ Michigan, Dept Earth & Environm Sci, Ann Arbor, MI 48109 USA. [Mu, Mingquan; Randerson, James T.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA USA. [Doney, Scott C.] Woods Hole Oceanog Inst, Dept Marine Chem & Geochem, Woods Hole, MA 02543 USA. [Morton, Douglas C.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Kasibhatla, Prasad S.] Duke Univ, Nicholas Sch Environm, Durham, NC USA. [Miller, John B.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. [Miller, John B.; Dlugokencky, Edward J.] NOAA, Earth Syst Res Lab, Global Monitoring Div, Boulder, CO USA. RP Keppel-Aleks, G (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. EM gkeppela@umich.edu RI Doney, Scott/F-9247-2010; Morton, Douglas/D-5044-2012 OI Doney, Scott/0000-0002-3683-2437; FU Department of Energy Office of Science Biological and Environmental Research Division; National Science Foundation Decadal and Regional Climate Prediction using Earth System Models (EaSM) program [NSF AGS 1048890, AGS 1048827]; NASA Carbon Cycle Science [NASA NNX11AF96G]; NOAA; NOAA's Climate Program Office's Atmospheric Chemistry, Carbon Cycle, and Climate (AC4) program FX This work was supported by the Department of Energy Office of Science Biological and Environmental Research Division, the National Science Foundation Decadal and Regional Climate Prediction using Earth System Models (EaSM) program (NSF AGS 1048890 and AGS 1048827), and NASA Carbon Cycle Science (NASA NNX11AF96G). G.K.A. acknowledges a NOAA Climate and Global Change postdoctoral fellowship. J.B.M. and E.J.D. thank NOAA's Climate Program Office's Atmospheric Chemistry, Carbon Cycle, and Climate (AC4) program for support, including that for collection and analysis of CO2 observations used in this study. CO2 observations were downloaded from ftp://aftp.cmdl.noaa.gov/data/trace_gases/co2/flask/surface/. NCEP Reanalysis data were provided by the NOAA/OAR/ESRL PSD, Boulder, Colorado, USA, from their Web site at http://www.esrl.noaa.gov/psd/. CRU temperature data were retrieved from http://www.cru.uea.ac.uk/cru/data/temperature/#datdow. GPCP data were from precip.gsfc.nasa.gov, and GFED data were from http://www.globalfiredata.org/Data/index.html. NR 58 TC 8 Z9 8 U1 3 U2 32 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0886-6236 EI 1944-9224 J9 GLOBAL BIOGEOCHEM CY JI Glob. Biogeochem. Cycle PD NOV PY 2014 VL 28 IS 11 BP 1295 EP 1310 DI 10.1002/2014GB004890 PG 16 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA AW9RE UT WOS:000346594100009 ER PT J AU Iturbe, X Ebrahim, A Benkrid, K Hong, C Arslan, T Perez, J Keymeulen, D Santambrogio, MD AF Iturbe, Xabier Ebrahim, Ali Benkrid, Khaled Hong, Chuan Arslan, Tughrul Perez, Jon Keymeulen, Didier Santambrogio, Marco D. TI R3TOS-BASED AUTONOMOUS FAULT-TOLERANT SYSTEMS SO IEEE MICRO LA English DT Article ID FPGAS; RECONFIGURATION AB This article describes the contributions of the reliable reconfigurable real-time operating system (r3tos) for building an autonomous fault-tolerant system using currently available xilinx partially reconfigurable field-programmable gate arrays. The authors present an r3tos-based inverter controller of a real-world railway traction system that is proven to recover from most of the errors provoked to it without requiring any human intervention. C1 [Iturbe, Xabier; Ebrahim, Ali; Benkrid, Khaled; Hong, Chuan; Arslan, Tughrul] Univ Edinburgh, Edinburgh EH8 9YL, Midlothian, Scotland. [Perez, Jon] IK4 Ikerlan, Dept Elect, Bilbao, Spain. [Keymeulen, Didier] Jet Prop Lab, Pasadena, CA USA. Politecn Milan, Milan, Italy. [Ebrahim, Ali; Arslan, Tughrul] Univ Edinburgh, Syst Level Integrat Res Grp, Edinburgh EH8 9YL, Midlothian, Scotland. [Arslan, Tughrul] Univ Edinburgh, Sch Engn, Edinburgh EH8 9YL, Midlothian, Scotland. RP Iturbe, X (reprint author), 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Xabier.Iturbe@jpl.nasa.gov NR 15 TC 1 Z9 1 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 0272-1732 EI 1937-4143 J9 IEEE MICRO JI IEEE Micro PD NOV-DEC PY 2014 VL 34 IS 6 BP 19 EP 29 PG 11 WC Computer Science, Hardware & Architecture; Computer Science, Software Engineering SC Computer Science GA AX0HQ UT WOS:000346634000004 ER PT J AU Wilson, WC Atkinson, GM AF Wilson, William C. Atkinson, Gary M. TI Passive Wireless Sensor Applications for NASA's Extreme Aeronautical Environments SO IEEE SENSORS JOURNAL LA English DT Article DE Wireless sensor networks; harsh environments; passive sensors ID TEMPERATURE; AIRCRAFT; DEVICES; SPACE AB NASA aeronautical programs require rigorous ground and flight testing. Many of the testing environments can be extremely harsh. These environments include cryogenic temperatures and high temperatures (>1500 degrees C). Temperature, pressure, vibration, ionizing radiation, and chemical exposure may all be a part of the harsh environment found in testing. This paper presents a survey of research opportunities for universities and industry to develop new wireless sensors that address anticipated structural health monitoring and testing needs for aeronautical vehicles. Potential applications of passive wireless sensors for ground testing and high-altitude aircraft operations are presented. Some of the challenges and issues of the technology are also presented. C1 [Wilson, William C.] NASA, Nondestruct Evaluat Branch, Langley Res Ctr, Hampton, VA 23681 USA. [Atkinson, Gary M.] Virginia Commonwealth Univ, Dept Elect & Comp Engn, Richmond, VA 23284 USA. RP Wilson, WC (reprint author), NASA, Nondestruct Evaluat Branch, Langley Res Ctr, Hampton, VA 23681 USA. EM william.c.wilson@nasa.gov; gmatkins@vcu.edu FU NASA Vehicle Safety Systems Technologies Project; Aviation Safety Program through the Aeronautics Research Mission Directorate FX This work was supported in part by the NASA Vehicle Safety Systems Technologies Project and in part by the Aviation Safety Program through the Aeronautics Research Mission Directorate. The associate editor coordinating the review of this paper and approving it for publication was Prof. Ali Abedi. NR 55 TC 9 Z9 9 U1 3 U2 20 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1530-437X EI 1558-1748 J9 IEEE SENS J JI IEEE Sens. J. PD NOV PY 2014 VL 14 IS 11 BP 3745 EP 3753 DI 10.1109/JSEN.2014.2322959 PG 9 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Physics, Applied SC Engineering; Instruments & Instrumentation; Physics GA AX5KC UT WOS:000346963700002 ER PT J AU Malocha, DC Fisher, B Youngquist, R Weeks, A Gallagher, M AF Malocha, Donald C. Fisher, Brian Youngquist, Robert Weeks, Arthur Gallagher, Mark TI Surface Acoustic Wave Pulsed-Correlator Transceiver for Aerospace Applications SO IEEE SENSORS JOURNAL LA English DT Article DE Aerospace; correlator; matched filter; orthogonal; sensor; signal to noise ratio; surface acoustic wave; transceiver; wireless ID SAW RFID TAGS; SENSORS; DEVICE AB This paper will present current efforts on wireless passive surface acoustic wave (SAW) sensor transceiver development for aerospace applications. Our group's SAW sensor work has been sponsored by NASA for the past ten years in efforts to develop wireless sensing for ground base and space exploration in extreme environments. The devices are radiation hard and work from cryogenic to several hundred degrees centigrade with standard device processing. The focus of this paper will be on a synchronous, pulsed correlator transceiver for interrogation of SAW delay-line sensors. The 915-MHz system has a bandwidth of 15 MHz and uses a pulsed noise-generated signal of 1-mu s duration. The design principles, system analysis, and receiver measurements are given. The prediction of signal-to-noise ratio versus range is shown for given system parameters. The system development leading to the first testing of SAW liquid level sensors at NASA KSC will be discussed. C1 [Malocha, Donald C.; Fisher, Brian; Weeks, Arthur; Gallagher, Mark] Univ Cent Florida, Dept Elect & Comp Engn, Orlando, FL 32816 USA. [Youngquist, Robert] NASA, Cocoa Beach, FL 32899 USA. RP Malocha, DC (reprint author), Univ Cent Florida, Dept Elect & Comp Engn, Orlando, FL 32816 USA. EM donald.malocha@ucf.edu; brian.fisher@knights.ucf.edu; robert.c.youngquist@nasa.gov; arthur.weeks@ucf.edu; mgallagher@knights.ucf.edu FU state of Florida Space organizations; Florida Space Institute; Florida Space Grant Consortium; Florida I-4 High Technology Corridor; NASA Graduate Student Research Program (GSRP) FX This work was supported by grants and contracts by the state of Florida Space organizations, Florida Space Institute, Florida Space Grant Consortium and Florida I-4 High Technology Corridor, and the NASA Graduate Student Research Program (GSRP), which have not only provided directed research support, but have aided many graduate students through scholarships and grants. The associate editor coordinating the review of this paper and approving it for publication was Prof. Ali Abedi. NR 21 TC 1 Z9 1 U1 0 U2 13 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1530-437X EI 1558-1748 J9 IEEE SENS J JI IEEE Sens. J. PD NOV PY 2014 VL 14 IS 11 BP 3775 EP 3781 DI 10.1109/JSEN.2014.2329179 PG 7 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Physics, Applied SC Engineering; Instruments & Instrumentation; Physics GA AX5KC UT WOS:000346963700006 ER PT J AU Simon, MN Carter, LM Campbell, BA Phillips, RJ Mattei, S AF Simon, Molly N. Carter, Lynn M. Campbell, Bruce A. Phillips, Roger J. Mattei, Stefania TI Studies of lava flows in the Tharsis region of Mars using SHARAD SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; radar observations; volcanism; dielectric properties ID RADAR AB The Tharsis region of Mars is covered in volcanic flows that can stretch for tens to hundreds of kilometers. Radar measurements of the dielectric properties of these flows can provide information regarding their composition and density. SHARAD (shallow radar), a sounding radar on the Mars Reconnaissance Orbiter, detects basal interfaces beneath flows in some areas of Tharsis northwest and west of Ascraeus Mons, with additional detections south of Pavonis Mons. Comparisons with 12.6 cm ground-based radar images suggest that SHARAD detects basal interfaces primarily in dust or regolith-mantled regions. We use SHARAD data to estimate the real relative permittivity of the flows by comparing the measured time delay of returns from the subsurface with altimetry measurements of the flow heights relative to the surrounding plains. In cases where the subsurface interface is visible at different depths, spanning tens of meters, it is also possible to measure the loss tangent (tan ) of the material. The permittivity values calculated range from 7.6 to 11.6, with an average of 9.6, while the mean loss tangent values range from 7.8 x 10(-3) to 2.9 x 10(-2) with an average of 1.0 x 10(-2). These permittivity and loss tangent estimates for the flows northwest of Ascraeus Mons, west of Ascraeus Mons, and south of Pavonis Mons are consistent with the lab-measured values for dense, low-titanium basalt. C1 [Simon, Molly N.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Carter, Lynn M.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. [Campbell, Bruce A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Phillips, Roger J.] SW Res Inst, Planetary Sci Directorate, Boulder, CO USA. [Mattei, Stefania] CORiSTA, Naples, Italy. RP Simon, MN (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. EM msimon@lpl.arizona.edu RI Carter, Lynn/D-2937-2012 FU NASA Undergraduate Student Research Program; NASA MRO project FX Funding for this project was provided by the NASA Undergraduate Student Research Program and by the NASA MRO project. SHARAD was contributed by the Italian Space Agency; we thank Principle Investigator Roberto Seu and the SHARAD operations team for their efforts in acquiring this data. The SHARAD data were processed at the Smithsonian Institution and Southwest Research Institute in Boulder, CO. They are also available through the NASA Planetary Data System. NR 24 TC 0 Z9 0 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD NOV PY 2014 VL 119 IS 11 BP 2291 EP 2299 DI 10.1002/2014JE004666 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AW5XU UT WOS:000346345100001 ER PT J AU Hanley, J Dalton, JB Chevrier, VF Jamieson, CS Barrows, RS AF Hanley, Jennifer Dalton, J. Brad, III Chevrier, Vincent F. Jamieson, Corey S. Barrows, R. Scott TI Reflectance spectra of hydrated chlorine salts: The effect of temperature with implications for Europa SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Europa; perchlorates; salts; chlorides; spectra ID INFRARED MAPPING SPECTROMETER; SUBSURFACE OCEAN; MU-M; SURFACE MATERIAL; ICE; MINERALS; GALILEO; WATER; STABILITY; SPECTROSCOPY AB Hydrated chlorine salts are expected to exist on a variety of planetary bodies, including inner planets such as Mars and outer planet satellites such as Europa. However, detection by remote sensing has been limited due to a lack of comparison data in spectral libraries. In addition, at low temperatures spectral features of many H2O-bearing species deviate from their room temperature behavior. Thus, we acquired spectra of NaCl, NaClO(4)nH(2)O, MgCl(2)nH(2)O, Mg(ClO4)(2)6H(2)O, and Mg(ClO3)(2)6H(2)O from 0.35 to 2.5 mu m at both 298 and 80K to observe the effects of temperature on diagnostic spectral features. In the near-infrared, the strongest spectral features often arise from water molecules. Increasing hydration states increases the depth and width of water bands. Interestingly, at low temperature these bands become narrower with sharper, better defined minima, allowing individual bands to be more easily resolved. We also measured frozen eutectic solutions of NaCl, MgCl2, and KCl. We show that while care must be taken to acquire laboratory spectra of all hydrated phases at the relevant conditions (e.g., temperature and pressure) for the planetary body being studied, chlorine salts do possess distinct spectral features that should allow for their detection by remote sensing. C1 [Hanley, Jennifer] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA. [Dalton, J. Brad, III] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Chevrier, Vincent F.] Univ Arkansas, Arkansas Ctr Space & Planetary Sci, Fayetteville, AR 72701 USA. [Jamieson, Corey S.] SETI Inst, Mountain View, CA USA. [Barrows, R. Scott] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. RP Hanley, J (reprint author), SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA. EM jhanley@boulder.swri.edu FU Strategic University Research Partnership Program; National Aeronautics and Space Administration FX Spectra are available online in the supporting information. This research was partially carried out at the Jet Propulsion Laboratory/California Institute of Technology and was sponsored by the Strategic University Research Partnership Program and the National Aeronautics and Space Administration. The authors would like to thank Thomas B. McCord and Roger Clark for their valuable comments and suggestions to improve the quality of the paper. NR 45 TC 12 Z9 12 U1 4 U2 22 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD NOV PY 2014 VL 119 IS 11 BP 2370 EP 2377 DI 10.1002/2013JE004565 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AW5XU UT WOS:000346345100006 ER PT J AU Freed, AM Johnson, BC Blair, DM Melosh, HJ Neumann, GA Phillips, RJ Solomon, SC Wieczorek, MA Zuber, MT AF Freed, Andrew M. Johnson, Brandon C. Blair, David M. Melosh, H. J. Neumann, Gregory A. Phillips, Roger J. Solomon, Sean C. Wieczorek, Mark A. Zuber, Maria T. TI The formation of lunar mascon basins from impact to contemporary form SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE lunar; mascons; gravity; basins; impact ID ORIGIN; MOON; DEFORMATION; SIMULATIONS; GRAIL; CRUST AB Positive free-air gravity anomalies associated with large lunar impact basins represent a superisostatic mass concentration or mascon. High-resolution lunar gravity data from the Gravity Recovery and Interior Laboratory spacecraft reveal that these mascons are part of a bulls-eye pattern in which the central positive anomaly is surrounded by an annulus of negative anomalies, which in turn is surrounded by an outer annulus of positive anomalies. To understand the origin of this gravity pattern, we modeled numerically the entire evolution of basin formation from impact to contemporary form. With a hydrocode, we simulated impact excavation and collapse and show that during the major basin-forming era, the preimpact crust and mantle were sufficiently weak to enable a crustal cap to flow back over and cover the mantle exposed by the impact within hours. With hydrocode results as initial conditions, we simulated subsequent cooling and viscoelastic relaxation of topography using a finite element model, focusing on the mare-free Freundlich-Sharonov and mare-infilled Humorum basins. By constraining these models with measured free-air and Bouguer gravity anomalies as well as surface topography, we show that lunar basins evolve by isostatic adjustment from an initially subisostatic state following the collapse stage. The key to the development of a superisostatic inner basin center is its mechanical coupling to the outer basin that rises in response to subisostatic stresses, enabling the inner basin to rise above isostatic equilibrium. Our calculations relate basin size to impactor diameter and velocity, and they constrain the preimpact lunar thermal structure, crustal thickness, viscoelastic rheology, and, for the Humorum basin, the thickness of its postimpact mare fill. C1 [Freed, Andrew M.; Blair, David M.; Melosh, H. J.] Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA. [Johnson, Brandon C.; Melosh, H. J.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Johnson, Brandon C.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. [Neumann, Gregory A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Phillips, Roger J.] SW Res Inst, Planetary Sci Directorate, Boulder, CO USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA. [Wieczorek, Mark A.] Univ Paris Diderot, Inst Phys Globe Paris, Sorbonne Paris Cite, Paris 13, France. RP Freed, AM (reprint author), Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA. EM freed@purdue.edu RI Wieczorek, Mark/G-6427-2010; Neumann, Gregory/I-5591-2013; OI Wieczorek, Mark/0000-0001-7007-4222; Neumann, Gregory/0000-0003-0644-9944; Johnson, Brandon/0000-0002-4267-093X FU NASA Discovery Program; NASA Science Mission Directorate FX We gratefully acknowledge the developers of iSALE (www.isale-code.de/projects/iSALE), including Gareth Collins, Kai Wunnemann, Dirk Elbeshausen, and Boris Ivanov. We thank Boris Ivanov, an anonymous reviewer, Gareth Collins, and another Associate Editor for their constructive comments on an earlier draft. The GRAIL mission is supported by the NASA Discovery Program and is performed under contract to the Massachusetts Institute of Technology and the Jet Propulsion Laboratory. The Lunar Reconnaissance Orbiter LOLA investigation is supported by the NASA Science Mission Directorate under contract to the NASA Goddard Space Flight Center and Massachusetts Institute of Technology. Data from the GRAIL and LOLA missions have been archived in the Geosciences Node of the NASA Planetary Data System. NR 35 TC 11 Z9 11 U1 2 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD NOV PY 2014 VL 119 IS 11 BP 2378 EP 2397 DI 10.1002/2014JE004657 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AW5XU UT WOS:000346345100007 ER PT J AU Leveille, RJ Bridges, J Wiens, RC Mangold, N Cousin, A Lanza, N Forni, O Ollila, A Grotzinger, J Clegg, S Siebach, K Berger, G Clark, B Fabre, C Anderson, R Gasnault, O Blaney, D Deflores, L Leshin, L Maurice, S Newsom, H AF Leveille, Richard J. Bridges, John Wiens, Roger C. Mangold, Nicolas Cousin, Agnes Lanza, Nina Forni, Olivier Ollila, Ann Grotzinger, John Clegg, Samuel Siebach, Kirsten Berger, Gilles Clark, Ben Fabre, Cecile Anderson, Ryan Gasnault, Olivier Blaney, Diana Deflores, Lauren Leshin, Laurie Maurice, Sylvestre Newsom, Horton TI Chemistry of fracture-filling raised ridges in Yellowknife Bay, Gale Crater: Window into past aqueous activity and habitability on Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mars; diagenesis; mudstone; smectite; magnesium; LIBS ID INDUCED BREAKDOWN SPECTROSCOPY; DEPTH-PROFILE ANALYSIS; CLAY MINERAL FORMATION; CEMENT STRATIGRAPHY; MERIDIANI-PLANUM; SNC METEORITE; SAPONITE; CHEMCAM; INSTRUMENT; HISTORY AB The ChemCam instrument package on the Curiosity rover was used to characterize distinctive raised ridges in the Sheepbed mudstone, Yellowknife Bay formation, Gale Crater. The multilayered, fracture-filling ridges are more resistant to erosion than the Sheepbed mudstone rock in which they occur. The bulk average composition of the raised ridges is enriched in MgO by 1.2-1.7 times (average of 8.3-11.4 wt %; single-shot maximum of 17.0 wt %) over that of the mudstone. Al2O3 is anticorrelated with MgO, while Li is somewhat enriched where MgO is highest. Some ridges show a variation in composition with different layers on a submillimeter scale. In particular, the McGrath target shows similar high-MgO resistant outer layers and a low-MgO, less resistant inner layer. This is consistent with the interpretation that the raised ridges are isopachous fracture-filling cements with a stratigraphy that likely reveals changes in fluid composition or depositional conditions over time. Overall, the average composition of the raised ridges is close to that of a Mg- and Fe-rich smectite, or saponite, which may also be the main clay mineral constituent of the host mudstone. These analyses provide evidence of diagenesis and aqueous activity in the early postdepositional history of the Yellowknife Bay formation, consistent with a low salinity to brackish fluid at near-neutral or slightly alkaline pH. The fluids that circulated through the fractures likely interacted with the Sheepbed mudstone and (or) other stratigraphically adjacent rock units of basaltic composition and leached Mg from them preferentially. C1 [Leveille, Richard J.] Canadian Space Agcy, St Hubert, PQ, Canada. [Leveille, Richard J.] McGill Univ, Dept Nat Resource Sci, Montreal, PQ, Canada. [Bridges, John] Univ Leicester, Dept Phys & Astron, Space Res Ctr, Leicester LE1 7RH, Leics, England. [Wiens, Roger C.; Cousin, Agnes; Lanza, Nina; Clegg, Samuel] Los Alamos Natl Lab, Los Alamos, NM USA. [Mangold, Nicolas] Univ Nantes, Lab Planetol & Geodynam Nantes, Nantes, France. [Forni, Olivier; Berger, Gilles; Gasnault, Olivier; Maurice, Sylvestre] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Forni, Olivier; Berger, Gilles; Gasnault, Olivier; Maurice, Sylvestre] CNRS, IRAP, Toulouse, France. [Ollila, Ann; Newsom, Horton] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. [Grotzinger, John; Siebach, Kirsten] CALTECH, Lab Planetol & Geodynam Nantes, Pasadena, CA 91125 USA. [Clark, Ben] Space Sci Inst, Boulder, CO USA. [Fabre, Cecile] Univ Lorraine, GeoRessources UMR CNRS, Nancy, France. [Anderson, Ryan] US Geol Survey, Flagstaff, AZ 86001 USA. [Blaney, Diana; Deflores, Lauren] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Leshin, Laurie] Rensselaer Polytech Inst, Troy, NY USA. RP Leveille, RJ (reprint author), Canadian Space Agcy, St Hubert, PQ, Canada. EM rich.leveille@gmail.com RI BERGER, Gilles/F-7118-2016; OI Gasnault, Olivier/0000-0002-6979-9012; Siebach, Kirsten/0000-0002-6628-6297; Clegg, Sam/0000-0002-0338-0948 FU NASA's Mars Program Office; Canadian Space Agency; Centre National d'Etudes Spatiales (CNES) FX The MSL mission is funded by NASA's Mars Program Office. R.J.L. received financial support from the Canadian Space Agency. The French contribution to ChemCam on MSL is supported by the Centre National d'Etudes Spatiales (CNES). We acknowledge the whole MSL team and JPL, in particular, for developing and leading this successful mission. We also thank the reviewers for their excellent comments, which greatly helped to improve the manuscript. The data reported in this paper are archived at the Planetary Data System, accessible at http://pds-geosciences.wustl.edu/missions/msl/index.htm. NR 72 TC 21 Z9 21 U1 2 U2 24 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD NOV PY 2014 VL 119 IS 11 BP 2398 EP 2415 DI 10.1002/2014JE004620 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AW5XU UT WOS:000346345100008 ER PT J AU Vega, MA Chandrasekar, V Carswell, J Beauchamp, RM Schwaller, MR Nguyen, C AF Vega, Manuel A. Chandrasekar, V. Carswell, James Beauchamp, Robert M. Schwaller, Mathew R. Cuong Nguyen TI Salient features of the dual-frequency, dual-polarized, Doppler radar for remote sensing of precipitation SO RADIO SCIENCE LA English DT Article DE radar; GPM; ground validation; dual-frequency; remote sensing ID CSU-CHILL RADAR; WEATHER RADARS; ANTENNA; PATTERN AB The global precipitation measurement (GPM) mission is an international satellite mission to obtain accurate observations of precipitation on a global scale every 3 h. Its (GPM) core satellite was launched on 27 February 2014 with two science instruments: the microwave imager and the dual-frequency precipitation radar. Ground validation is an integral part of the GPM mission where instruments are deployed to complement and correlate with spacecraft instruments. The dual-frequency, dual-polarization, Doppler radar (D3R) is a critical ground validation instrument that was developed for the GPM program. This paper describes the salient features of the D3R in the context of the GPM ground validation mission. The engineering and architectural overview of the radar is described, and observations from successful GPM ground validation field experiments are presented. C1 [Vega, Manuel A.; Schwaller, Mathew R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. [Vega, Manuel A.; Chandrasekar, V.; Beauchamp, Robert M.; Cuong Nguyen] Colorado State Univ, Dept Elect & Comp Engn, Ft Collins, CO 80523 USA. [Carswell, James] Remote Sensing Solut, Barnstable, MA USA. RP Vega, MA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. EM Manuel.Vega@nasa.gov RI Measurement, Global/C-4698-2015 FU NASA GPM program FX This research is supported by the NASA GPM program. The authors are grateful for the early support of Arthur Hou for this project. The authors acknowledge the scientific and operations support from the GPM leadership including Ramesh Kakar, Walt Petersen, and Gail Skofronick Jackson. The radar was developed, assembled, and tested originally at the CSU-CHILL facility; we thank the generous support of the CHILL staff for their assistance. In addition, we would like to thank Nitin Bharadwaj for his contributions to the early development and waveform design, Kumar Vijay Mishra for his early work on the digital receiver, and Ken Hersey for his contributions to antenna pattern characterization and laser tracker coalignment of the antennas. We would like to acknowledge the participation of David Wolff and Walt Petersen in the field programs for all the logistical support. We would also like to acknowledge the help of many others not mentioned here during antenna pattern measurements, integration and testing, field deployments, etc. Finally, we would like to thank the reviewers for their valuable comments and suggestions. The data used for the figures in this work will be made available by contacting the first author. NR 25 TC 9 Z9 9 U1 3 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0048-6604 EI 1944-799X J9 RADIO SCI JI Radio Sci. PD NOV PY 2014 VL 49 IS 11 BP 1087 EP 1105 DI 10.1002/2014RS005529 PG 19 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA AW9QP UT WOS:000346592500008 ER PT J AU Yue, XN Schreiner, WS Pedatella, N Anthes, RA Mannucci, AJ Straus, PR Liu, JY AF Yue, Xinan Schreiner, William S. Pedatella, Nicholas Anthes, Richard A. Mannucci, Anthony J. Straus, Paul R. Liu, Jann-Yenq TI Space Weather Observations by GNSS Radio Occultation: From FORMOSAT-3/COSMIC to FORMOSAT-7/COSMIC-2 SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE radio occultation; ionosphere; GNSS ID MISSION AB The joint Taiwan-United States FORMOSAT-3/COSMIC (Constellation Observing System for Meteorology, Ionosphere, and Climate) mission, hereafter called COSMIC, is the first satellite constellation dedicated to remotely sense Earth's atmosphere and ionosphere using a technique called Global Positioning System (GPS) radio occultation (RO). The occultations yield abundant information about neutral atmospheric temperature and moisture as well as space weather estimates of slant total electron content, electron density profiles, and an amplitude scintillation index, S4. With the success of COSMIC, the United States and Taiwan are moving forward with a follow-on RO mission named FORMOSAT-7/COSMIC-2 (COSMIC-2), which will ultimately place 12 satellites in orbit with two launches in 2016 and 2019. COSMIC-2 satellites will carry an advanced Global Navigation Satellite System (GNSS) RO receiver that will track both GPS and Russian Global Navigation Satellite System signals, with capability for eventually tracking other GNSS signals from the Chinese BeiDou and European Galileo system, as well as secondary space weather payloads to measure low-latitude plasma drifts and scintillation at multiple frequencies. COSMIC-2 will provide 4-6 times (10-15X in the low latitudes) the number of atmospheric and ionospheric observations that were tracked with COSMIC and will also improve the quality of the observations. In this article we focus on COSMIC/COSMIC-2 measurements of key ionospheric parameters. C1 [Yue, Xinan; Pedatella, Nicholas] UCAR COSM Program Off, Boulder, CO 80307 USA. [Schreiner, William S.] UCAR CDAAC, Boulder, CO USA. [Anthes, Richard A.] UCAR, Boulder, CO USA. [Mannucci, Anthony J.] NASA, JPL, Ionospher & Atmospher Remote Sensing Grp, Washington, DC USA. [Straus, Paul R.] Aerosp Corp, COSM 2, White Plains, NY USA. [Liu, Jann-Yenq] NSPO, Hsinchu, Taiwan. [Liu, Jann-Yenq] Natl Cent Univ Taiwan, Zhongli, Taiwan. RP Yue, XN (reprint author), UCAR COSM Program Off, Boulder, CO 80307 USA. EM xinanyue@ucar.edu RI Pedatella, Nicholas/Q-2242-2015; Liu, Jann-Yenq/Q-1668-2015 OI Pedatella, Nicholas/0000-0002-8878-5126; FU National Science Foundation [AGS-1033112] FX This material is based upon work supported by the National Science Foundation under the Cooperative Agreement AGS-1033112. The authors would like to acknowledge the National Science Foundation, Taiwan's NSPO, NOAA, NASA, and USAF for their support on FORMOSAT-3/COSMIC and continuing support on FORMOSAT-7/COSMIC-2. Portions of this research were carried out at JPL, California Institute of Technology, under a contract with NASA. Data from COSMIC, and many other missions, are processed, archived, and made freely available to the community by UCAR CDAAC (http://cdaac-www.cosmic.ucar.edu/cdaac/). NR 17 TC 19 Z9 19 U1 1 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD NOV PY 2014 VL 12 IS 11 BP 616 EP 621 DI 10.1002/2014SW001133 PG 6 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AW5YJ UT WOS:000346346500002 ER PT J AU Schwadron, NA Blake, JB Case, AW Joyce, CJ Kasper, J Mazur, J Petro, N Quinn, M Porter, JA Smith, CW Smith, S Spence, HE Townsend, LW Turner, R Wilson, JK Zeitlin, C AF Schwadron, N. A. Blake, J. B. Case, A. W. Joyce, C. J. Kasper, J. Mazur, J. Petro, N. Quinn, M. Porter, J. A. Smith, C. W. Smith, S. Spence, H. E. Townsend, L. W. Turner, R. Wilson, J. K. Zeitlin, C. TI Does the worsening galactic cosmic radiation environment observed by CRaTER preclude future manned deep space exploration? SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE radiation; solar wind; solar evolution ID INTERPLANETARY MAGNETIC-FIELD; ADVANCED COMPOSITION EXPLORER; CORONAL ELECTRON-TEMPERATURE; PROTRACTED SOLAR MINIMUM; RAY MODULATION; FLUX; TRANSPORT; WIND; HELIOSPHERE; MODEL AB The Sun and its solar wind are currently exhibiting extremely low densities and magnetic field strengths, representing states that have never been observed during the space age. The highly abnormal solar activity between cycles 23 and 24 has caused the longest solar minimum in over 80 years and continues into the unusually small solar maximum of cycle 24. As a result of the remarkably weak solar activity, we have also observed the highest fluxes of galactic cosmic rays in the space age and relatively small solar energetic particle events. We use observations from the Cosmic Ray Telescope for the Effects of Radiation (CRaTER) on the Lunar Reconnaissance Orbiter to examine the implications of these highly unusual solar conditions for human space exploration. We show that while these conditions are not a show stopper for long-duration missions (e.g., to the Moon, an asteroid, or Mars), galactic cosmic ray radiation remains a significant and worsening factor that limits mission durations. While solar energetic particle events in cycle 24 present some hazard, the accumulated doses for astronauts behind 10 g/cm(2) shielding are well below current dose limits. Galactic cosmic radiation presents a more significant challenge: the time to 3% risk of exposure-induced death (REID) in interplanetary space was less than 400 days for a 30 year old male and less than 300 days for a 30 year old female in the last cycle 23-24 minimum. The time to 3% REID is estimated to be approximate to 20% lower in the coming cycle 24-25 minimum. If the heliospheric magnetic field continues to weaken over time, as is likely, then allowable mission durations will decrease correspondingly. Thus, we estimate exposures in extreme solar minimum conditions and the corresponding effects on allowable durations. C1 [Schwadron, N. A.; Joyce, C. J.; Quinn, M.; Smith, C. W.; Smith, S.; Spence, H. E.; Wilson, J. K.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Blake, J. B.; Mazur, J.] Aerosp Corp, El Segundo, CA 90245 USA. [Case, A. W.; Kasper, J.] Harvard Smithsonian Ctr Astrophys, Div High Energy Astrophys, Cambridge, MA 02138 USA. [Kasper, J.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Petro, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Porter, J. A.; Townsend, L. W.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA. [Turner, R.] Analyt Serv Inc, Arlington, VA USA. [Zeitlin, C.] Univ New Hampshire, SW Res Inst, Durham, NH 03824 USA. RP Schwadron, NA (reprint author), Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. EM n.schwadron@unh.edu RI Kasper, Justin/D-1152-2010; Petro, Noah/F-5340-2013 OI Kasper, Justin/0000-0002-7077-930X; FU LRO program [NNG11PA03C]; EMMREM [NNX07AC14G]; C-SWEPA (NASA) [NNX07AC14G]; Sun-2-Ice (NSF) [AGS1135432]; DoSEN (NASA) [NNX13AC89G]; DREAM (NASA) [NNX10AB17A]; DREAM2 (NASA) [NNX14AG13A] FX We thank all those who made CRaTER possible. CRaTER is primarily funded by the LRO program (contract NNG11PA03C). This work was also funded by EMMREM (grant NNX07AC14G), C-SWEPA (NASA grant NNX07AC14G), Sun-2-Ice (NSF grant AGS1135432) projects, and DoSEN (NASA grant NNX13AC89G), DREAM (NASA grant NNX10AB17A), and DREAM2 (NASA grant NNX14AG13A). CRaTER data are available at http://crater-web.sr.unh.edu. NR 61 TC 9 Z9 9 U1 4 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD NOV PY 2014 VL 12 IS 11 BP 622 EP 632 DI 10.1002/2014SW001084 PG 11 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AW5YJ UT WOS:000346346500003 ER PT J AU Rizzi, SA Aumann, AR Lopes, LV Burley, CL AF Rizzi, Stephen A. Aumann, Aric R. Lopes, Leonard V. Burley, Casey L. TI Auralization of Hybrid Wing-Body Aircraft Flyover Noise from System Noise Predictions SO JOURNAL OF AIRCRAFT LA English DT Article; Proceedings Paper CT 51st AIAA Aerospace Sciences Meeting and Exhibit Including the New Horizons Forum and Aerospace Exposition CY JAN 06-11, 2013 CL Grapevine, TX SP AIAA AB System noise assessments of a state-of-the-art reference aircraft (similar to a Boeing 777-200ER with GE90-like turbofan engines) and several hybrid wing-body aircraft configurations were recently performed using NASA engine and aircraft system analysis tools. The hybrid wing-body aircraft were sized to an equivalent mission as the reference aircraft and assessments were performed using measurements of airframe shielding from a series of propulsion airframe aeroacoustic experiments. The focus of this work is to auralize flyover noise from the reference aircraft and the best hybrid wing-body configuration using source noise predictions and shielding data based largely on the earlier assessments. Here, auralization refers to the process by which numerical predictions are converted into audible pressure time histories. It entails synthesis of the source noise and propagation of that noise to a receiver on the ground. For each aircraft, three flyover conditions are auralized. These correspond to approach, sideline, and cutback operating states, but flown in straight and level flight trajectories. The auralizations are performed using synthesis and simulation tools developed at NASA. Audio and visual presentations are provided to allow the reader to experience the flyover from the perspective of a listener in the simulated environment. C1 [Rizzi, Stephen A.; Lopes, Leonard V.; Burley, Casey L.] NASA, Langley Res Ctr, Aeroacoust Branch, Hampton, VA 23681 USA. [Aumann, Aric R.] Analyt Serv & Mat Inc, Struct Acoust Branch, Hampton, VA 23666 USA. RP Rizzi, SA (reprint author), NASA, Langley Res Ctr, Aeroacoust Branch, MS 463, Hampton, VA 23681 USA. NR 35 TC 2 Z9 2 U1 3 U2 7 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0021-8669 EI 1533-3868 J9 J AIRCRAFT JI J. Aircr. PD NOV-DEC PY 2014 VL 51 IS 6 BP 1914 EP 1926 DI 10.2514/1.C032572 PG 13 WC Engineering, Aerospace SC Engineering GA AW0KJ UT WOS:000345980800020 ER PT J AU Dunning, PD Stanford, BK Kim, HA Jutte, CV AF Dunning, Peter D. Stanford, Bret K. Kim, H. Alicia Jutte, Christine V. TI Aeroelastic tailoring of a plate wing with functionally graded materials SO JOURNAL OF FLUIDS AND STRUCTURES LA English DT Article DE Functionally graded materials; Aeroelastic tailoring; Plate wing; Doublet Lattice Method; Flutter; Genetic algorithm ID STABILITY; DIVERGENCE; FLUTTER; PANELS AB A functionally graded material (FGM) provides a spatial blend of material properties throughout a structure. This paper studies the efficacy of FGM for the aeroelastic tailoring of a metallic cantilever plate-like wing, wherein a genetic algorithm provides Pareto trade-off curves between static and dynamic aeroelastic metrics. A key comparison is between the effectiveness of material grading, geometric grading (i.e. plate thickness variations), and using both simultaneously. The introduction of material grading does, in some cases, improve the aeroelastic performance. This improvement, and the physical mechanism upon which it is based, depends on numerous factors: the two sets of metallic material parameters used for grading; the sweep of the plate; the aspect ratio of the plate; and whether the material is graded continuously or discretely. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Dunning, Peter D.] Natl Inst Aerosp, Hampton, VA 23666 USA. [Stanford, Bret K.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Kim, H. Alicia] Univ Bath, Bath BA2 7AY, Avon, England. [Jutte, Christine V.] Craig Technol Inc, Cape Canaveral, FL 32920 USA. RP Dunning, PD (reprint author), Natl Inst Aerosp, Hampton, VA 23666 USA. EM p.d.dunning@bath.ac.uk; bret.k.stanford@nasa.gov; h.a.kim@bath.ac.uk; christine.vjutte@nasa.gov OI Kim, Hyunsun Alicia/0000-0002-5629-2466; Dunning, Peter/0000-0002-7645-7598 FU National Aeronautics and Space Administration's Fundamental Aeronautics Program FX This work is funded by the Fixed Wing project under the National Aeronautics and Space Administration's Fundamental Aeronautics Program. The authors would also like to thank Dr. Maxwell Blair for providing his DLM code. NR 22 TC 6 Z9 6 U1 0 U2 8 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0889-9746 J9 J FLUID STRUCT JI J. Fluids Struct. PD NOV PY 2014 VL 51 BP 292 EP 312 DI 10.1016/j.jfluidstructs.2014.09.008 PG 21 WC Engineering, Mechanical; Mechanics SC Engineering; Mechanics GA AW3UM UT WOS:000346211500020 ER PT J AU Sigler, MF Stabeno, PJ Eisner, LB Napp, JM Mueter, FJ AF Sigler, Michael F. Stabeno, Phyllis J. Eisner, Lisa B. Napp, Jeffrey M. Mueter, Franz J. TI Spring and fall phytoplankton blooms in a productive subarctic ecosystem, the eastern Bering Sea, during 1995-2011 SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY LA English DT Article DE Phytoplankton bloom; Spring; Fall; Bering Sea; Climate; Zooplankton ID OSCILLATING CONTROL HYPOTHESIS; CLIMATE-CHANGE; MIDDLE SHELF; ICE ALGAE; NORTHERN; VARIABILITY; IMPACTS; SEDIMENTATION; REANALYSIS; DYNAMICS AB The timing and magnitude of phytoplankton blooms in subarctic ecosystems often strongly influence the amount of energy that is transferred through subsequent trophic pathways. In the eastern Bering Sea, spring bloom timing has been linked to ice retreat timing and production of zooplankton and fish. A large part of the eastern Bering Sea shelf (similar to 500 km wide) is ice-covered during winter and spring. Four oceanographic moorings have been deployed along the 70-m depth contour of the eastern Bering Sea shelf with the southern location occupied annually since 1995, the two northern locations since 2004 and the remaining location since 2001. Chlorophyll a fluorescence data from the four moorings provide 37 realizations of a spring bloom and 33 realizations of a fall bloom. We found that in the eastern Bering Sea: if ice was present after mid-March, spring bloom timing was related to ice retreat timing (p < 0.001, df=1, 24); if ice was absent or retreated before mid-March, a spring bloom usually occurred in May or early June (average day 148, SE=3.5, n=11). A fall bloom also commonly occurred, usually in late September (average day 274, SE=4.2, n=33), and its timing was not significantly related to the timing of storms (p=0.88, df= 1, 27) or fall water column overturn (p = 0.49, df=1, 27). The magnitudes of the spring and fall blooms were correlated (p=0.011, df=28). The interval between the spring and fall blooms varied between four to six months depending on year and location. We present a hypothesis to explain how the large crustacean zooplankton taxa Calanus spp. likely respond to variation in the interval between blooms (spring to fall and fall to spring). Published by Elsevier Ltd. C1 [Sigler, Michael F.] NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK 99801 USA. [Stabeno, Phyllis J.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. [Eisner, Lisa B.; Napp, Jeffrey M.] NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Seattle, WA 98115 USA. [Mueter, Franz J.] Univ Alaska Fairbanks, Juneau Ctr Fisheries & Oceans, Juneau, AK 99801 USA. RP Sigler, MF (reprint author), NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 17109 Pt Lena Loop Rd, Juneau, AK 99801 USA. EM mike.sigler@noaa.gov; phyllis.stabeno@noaa.gov; lisa.eisner@noaa.gov; jeff.napp@noaa.gov; fmueter@alaska.edu FU North Pacific Research Board and NOAA's North Pacific Climate Regimes and Ecosystem Productivity (NPCREP); Fisheries Oceanography Coordinated Investigations programs FX We thank D. Kachel for data analysis, S. Salo for providing the ice data and W. Floering and C. Dewitt for deploying and recovering the moorings. We thank the officers and crews of the NOAA ships Miller Freeman and Oscar Dyson for their invaluable assistance in deploying and recovering the moorings. We thank Zach Brown, Rolf Gradinger, Mike Lomas and one anonymous reviewer whose comments improved our manuscript. The research was generously supported by the North Pacific Research Board and NOAA's North Pacific Climate Regimes and Ecosystem Productivity (NPCREP) and Fisheries Oceanography Coordinated Investigations programs. This is BEST-BSIERP publication no. 122 and NPRB publication no. 459. This is contribution FOCI-B807 to the Ecosystems 82 Fisheries Oceanography Coordinated Investigations and 3953 to the Pacific Marine Environmental Laboratory. The findings and conclusions in this paper are those of the authors and do not necessarily represent the views of NOAA's National Marine Fisheries Service or Oceans and Atmospheric Research. NR 53 TC 30 Z9 30 U1 3 U2 24 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0645 EI 1879-0100 J9 DEEP-SEA RES PT II JI Deep-Sea Res. Part II-Top. Stud. Oceanogr. PD NOV PY 2014 VL 109 SI SI BP 71 EP 83 DI 10.1016/j.dsr2.2013.12.007 PG 13 WC Oceanography SC Oceanography GA AU7UZ UT WOS:000345807900007 ER PT J AU De Forest, L Duffy-Anderson, JT Heintz, RA Matarese, AC Siddon, EC Smart, TI Spies, IB AF De Forest, Lisa Duffy-Anderson, J. T. Heintz, R. A. Matarese, A. C. Siddon, E. C. Smart, T. I. Spies, I. B. TI Taxonomy of the early life stages of arrowtooth flounder (Atheresthes stomias) and Kamchatka flounder (A-evermanni) in the eastern Bering Sea, with notes on distribution and condition SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY LA English DT Article DE Arrowtooth flounder; Kamchatka flounder; Atheresthes; Bering Sea ID POLLOCK THERAGRA-CHALCOGRAMMA; IDENTIFICATION; ZOOPLANKTON; COI AB Arrowtooth flounder (Atheresthes stomias) and Kamchatka flounder (A. evermanni) are closely related flatfish species that co-occur in the eastern Bering Sea. As adults, arrowtooth flounder can be distinguished from Kamchatka flounder; however, larvae and early juveniles can only be indentified to the genus level due to morphological similarities. This has precluded studies of ecology for the early life stages of both species in the eastern Bering Sea. In this study, we developed a generic technique to identify the larvae and early juveniles of the two species using mtDNA cytochrome oxidase subunit I (COI). Genetically identified specimens were then examined to determine a visual identification method based on pigment patterns and morphology. Specimens 6.0-12.0 mm SL and >= 18.0 mm SL can be identified to the species level, but species identification of individuals 12.1-17.9 mm SL by visual means alone remains elusive. The distribution of larvae (< 25.0 mm SL) of both arrowtooth flounder and Kamchatka flounder is similar in the eastern Bering Sea; however, juvenile (>= 25.0 mm SL) Kamchatka flounder occur closer to the shelf break and in deeper water than juvenile arrowtooth flounder. Condition was determined for larvae and juveniles of each species by analyzing lipid content (%) and energy density (KJ/g dry mass). Kamchatka flounder larvae on average had higher lipid content than arrowtooth flounder larvae, but were also larger on average than arrowtooth flounder larvae in the summer. When corrected for length, both species had similar lipid content in the larval and juvenile stages. Published by Elsevier Ltd. C1 [De Forest, Lisa; Duffy-Anderson, J. T.; Matarese, A. C.; Smart, T. I.; Spies, I. B.] NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Seattle, WA 98115 USA. [Heintz, R. A.; Siddon, E. C.] NOAA, Alaska Fisheries Sci Ctr, Auke Bay Labs, Natl Marine Fisheries Serv, Juneau, AK 99801 USA. RP De Forest, L (reprint author), NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Seattle, WA 98115 USA. EM Lisa.DeForest@noaa.gov NR 26 TC 1 Z9 1 U1 1 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0645 EI 1879-0100 J9 DEEP-SEA RES PT II JI Deep-Sea Res. Part II-Top. Stud. Oceanogr. PD NOV PY 2014 VL 109 SI SI BP 181 EP 189 DI 10.1016/j.dsr2.2014.05.005 PG 9 WC Oceanography SC Oceanography GA AU7UZ UT WOS:000345807900016 ER PT J AU Bingham, FM Busecke, J Gordon, AL Giulivi, CF Li, ZJ AF Bingham, Frederick M. Busecke, Julius Gordon, Arnold L. Giulivi, Claudia F. Li, Zhijin TI The North Atlantic subtropical surface salinity maximum as observed by Aquarius SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE ocean salinity; Aquarius ID TROPICAL PACIFIC-OCEAN; LAYER SALINITY; EKMAN TRANSPORT; CIRCULATION; MODEL; FLOW; CURRENTS; WATER AB Aquarius satellite-derived sea surface salinity (SSS) data from August 2011 through September 2013 reveals significant seasonal migration and freshening of the subtropical surface salinity maximum (SSS-max) area in the North Atlantic, in good agreement with in situ observations, including those obtained as part of the SPURS (Salinity Processes in the Upper Ocean Regional Study) field experiment in 2012-2013. The SSS-max fluctuated in surface areaas defined by the 37.4 surface isohalineduring the course of the Aquarius time series by about 67%. The SSS-max has a surprisingly large amount of non-seasonal variability, including a general decrease in salinity throughout the eastern subtropical North Atlantic between 2011-2012 and 2012-2013 of about 0.1-0.2. The documented seasonal variability is weakest in the maximum salinity area and increases toward the north and south, respectively. This is consistent with the important role played by Ekman transport and regional excess of evaporation over precipitation in the formation of the SSS-max. Key Points North Atlantic surface salinity maximum documented from August 2011 to September 2013 Aquarius satellite sea surface salinity data are used Feature shows long-term fluctuations and documents seasonal variability C1 [Bingham, Frederick M.] Univ N Carolina, Ctr Marine Sci, Wilmington, NC 28403 USA. [Busecke, Julius; Gordon, Arnold L.; Giulivi, Claudia F.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Li, Zhijin] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Bingham, FM (reprint author), Univ N Carolina, Ctr Marine Sci, Wilmington, NC 28403 USA. EM binghamf@uncw.edu RI Gordon, Arnold/H-1049-2011 OI Gordon, Arnold/0000-0001-6480-6095 FU NASA [NNX09AU70G, NNX11AE83G, NNX09AU68G] FX Support was provided by NASA under grants NNX09AU70G and NNX11AE83G to UNCW and NNX09AU68G to Lamont-Doherty Earth Observatory. Three anonymous reviewers read this manuscript carefully and provided constructive comments. The SPURS central mooring observations were supported by NASA grant NNX11AE84G. Figure 7 data were provided by J. D'Addezio. Lamont-Doherty Earth Observatory contribution 7838. The gridded sea surface salinity (SOOP) data set was made freely available by the French Sea Surface Salinity Observation Service. Data were obtained from the following sources: Aquarius data (PO. DAAC data archive), http://podaac.jpl.nasa.gov; SOOP data, http://www. legos. obs-mip.fr/observations/sss/; JAMSTEC MOAA GPV, http://www.jamstec.go.jp/ARGO/argo_web/MapQ/Mapdataset_e. html; SPURS Central mooring data, http://uop.whoi.edu/projects/ SPURS/ spurs. html; ERAI data, https://climatedataguide.ucar.edu/climate-data/era-interim; Mixed-layer depth climatology, http://www.ifremer. NR 40 TC 5 Z9 5 U1 1 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD NOV PY 2014 VL 119 IS 11 BP 7741 EP 7755 DI 10.1002/2014JC009825 PG 15 WC Oceanography SC Oceanography GA AW2FG UT WOS:000346102900021 ER PT J AU Yin, XB Boutin, J Reverdin, G Lee, T Arnault, S Martin, N AF Yin, Xiaobin Boutin, Jacqueline Reverdin, Gilles Lee, Tong Arnault, Sabine Martin, Nicolas TI SMOS Sea Surface Salinity signals of tropical instability waves SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article DE SMOS; Sea Surface Salinity; tropical instability waves ID PACIFIC-OCEAN; EQUATORIAL PACIFIC; ATLANTIC-OCEAN; NUMERICAL-MODEL; HEAT-BUDGET; TEMPERATURE; IMPACT; VARIABILITY; ENERGETICS AB Sea Surface Salinity (SSS) measurements from the Soil Moisture and Ocean Salinity (SMOS) mission provide an unprecedented opportunity to observe the salinity structure of tropical instability waves (TIWs) from space, especially during the intense 2010 La Nina condition. In the eastern equatorial Pacific Ocean, SMOS SSS signals correlate well and have similar amplitude to 1 m salinity from the Tropical Atmosphere Ocean (TAO) array at six locations with strong TIW signals. At these locations, the linear negative relationships between SMOS SSS and OSTIA SST signals vary from -0.20 degrees C-1 to -0.25 degrees C-1, which are comparable to the ones obtained from TAO. From June to December 2010, the largest TIW signals and meridional gradients of both SSS and SST appear around 2 degrees N west of 100 degrees W. They shift southward and cross the equator at 90 degrees W. In addition to the large negative correlation band around 2 degrees N, a band of negative correlations between SSS and SST signals also exists around 8 degrees N west of 110 degrees W for the 33 day signals. The peak amplitude of the 33 day SMOS SSS signals west of 135 degrees W is reduced by >40% with respect to values east of 135 degrees W, while the reduction for SST is much lower (<20%). The amplitudes and longitudinal extents of TIW signals and the dominant westward propagation speed of 17 day TIWs (as detected by SMOS and Aquarius) at the equator decrease from 2010 to 2013 associated with the transition from a strong La Nina to non-La Nina conditions. C1 [Yin, Xiaobin] ARGANS, Plymouth, Devon, England. [Yin, Xiaobin; Boutin, Jacqueline; Reverdin, Gilles; Arnault, Sabine; Martin, Nicolas] Univ Paris 06, CNRS, Sorbonne Univ, IRD,MNHN,LOCEAN Lab, Paris, France. [Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Yin, XB (reprint author), ARGANS, Plymouth, Devon, England. EM xylod@locean-ipsl.upmc.fr RI Boutin, Jacqueline/M-2253-2016 FU European Space Agency (ESA) FX We thank two anonymous reviewers for their constructive comments. This work was funded by the European Space Agency (ESA) Support to Science element project entitled SMOS1Surface Ocean and Synergy and by the CNES/TOSCA/SMOSGLOSCAL project. Daily SSS from LOCEAN is available upon request submitted to J. Boutin and the CATDS CEC-IFREMER SSS is obtained from the Ocean Salinity Expertise Center (CECOS) of the CNES-IFREMER Centre Aval de Traitemenent des Donnees SMOS (http://www.catds.fr/Products/Available-products-from-CEC-OS/Ifremer-Dat aset-V02). The authors would like to acknowledge the Met office for providing OSTIA SST (http://ghrsst-pp.metoffice.com/pages/latest_analysis/ostia.html), the National Climatic Data Center ( NCDC) for providing Reynolds SST (http://www.ncdc.noaa.gov/sst), and the TAO Project Office/Pacific Marine Environmental Laboratory for providing TAO SSS and SST (http://www.pmel.noaa.gov/tao). The Aquarius Combined Active Passive ( CAP) algorithm level 3 Sea Surface Salinity was obtained from the Physical Oceanography Distributed Active Archive Center (PO.DAAC) at the NASA Jet Propulsion Laboratory, Pasadena, CA (http://podaac.jpl.nasa.gov/dataset/AQUARIUS_L3_SSS_CAP_7DAY_V2). The authors would like to acknowledge the OSCAR Project Office for providing current data (http://www.oscar.noaa.gov). NR 44 TC 7 Z9 8 U1 1 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD NOV PY 2014 VL 119 IS 11 BP 7811 EP 7826 DI 10.1002/2014JC009960 PG 16 WC Oceanography SC Oceanography GA AW2FG UT WOS:000346102900025 ER PT J AU Panda, J Mosher, RN Porter, BJ AF Panda, J. Mosher, R. N. Porter, B. J. TI Noise Source Identification During Rocket Engine Test Firings and a Rocket Launch SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article AB A 70 microphone, 10x10ft, microphone phased array was built for use in the harsh environment of rocket launches. The array was set up at NASA Wallops launch pad 0A during a static-test firing of Orbital Sciences' Antares engines and again during the first launch of the Antares vehicle. It was placed 400ft away from the pad and was hoisted on a scissor lift 40ft above ground. The data sets provided unprecedented insight into rocket noise sources. The duct exit was found to be the primary source during the static-test firing; the large amount of water injected beneath the nozzle exit and inside the plume duct quenched all other sources. The maps of the noise sources during launch were found to be time dependent. As the engines came to full power and became louder, the primary source switched from the duct inlet to the duct exit. Further elevation of the vehicle caused spilling of the hot plume, resulting in a distributed noise map covering most of the pad. As the entire plume emerged from the duct, and the on-deck water system came to full power, the plume itself became the loudest noise source. These maps of the noise sources provide vital insight for optimization of sound suppression systems for future Antares launches. C1 [Panda, J.] NASA, Ames Res Ctr, Expt Aerophys Branch, Moffett Field, CA 94035 USA. [Mosher, R. N.] NASA, Langley Res Ctr, Mech Syst Branch, Hampton, VA 23681 USA. [Porter, B. J.] Aerosp Comp Inc, Expt Aerophys Branch, Moffett Field, CA 94035 USA. RP Panda, J (reprint author), NASA, Ames Res Ctr, Expt Aerophys Branch, Moffett Field, CA 94035 USA. FU NASA Marshall Space Flight Center; NASA Ames Research Center; NASA ASP innovative measurements program FX The authors would like to thank Roberto Garcia of NASA Marshall Space Flight Center and Nans Kunz of NASA Ames Research Center for partially funding this work. Additional support was provided by the NASA ASP innovative measurements program. Jeff Reddish and Mark Cording of the Wallops Flight Facility, Kevin Meehan of NASA Johnson Space Center, and Kurt Eberly and Tony Gaio of the Orbital Sciences Corporation were instrumental in coordinating this multi-agency effort. We benefited greatly from the engineering advice that Mark Cording provided. We would also like to thank Ted Garbeff for performing the modeling work for optimizing the microphone locations, Laura Kushner for photogrammetric verification of these locations, and Greg Zilliac for allowing us to setup the array during the hybrid rocket tests. Finally, the credit for the high-speed camera photos of Fig. 11 goes to the NASA imagery group at Kennedy Space Center. NR 8 TC 2 Z9 2 U1 0 U2 11 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD NOV-DEC PY 2014 VL 51 IS 6 BP 1761 EP 1772 DI 10.2514/1.A32863 PG 12 WC Engineering, Aerospace SC Engineering GA AU8QP UT WOS:000345861500001 ER PT J AU Oh, DY Snyder, JS Goebel, DM Hofer, RR Randolph, TM AF Oh, David Y. Snyder, John Steven Goebel, Dan M. Hofer, Richard R. Randolph, Thomas M. TI Solar Electric Propulsion for Discovery-Class Missions SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID ION ENGINE; MODEL AB This paper offers a user-centric consolidation and comparison of the full range of government and commercial solar electric propulsion options available in the near term for primary propulsion on deep-space science missions of the class commonly proposed to NASA's Discovery program. Unlike previous papers, this work does not emphasize feasibility from a mission-analysis perspective. Rather, it emphasizes requirements uniquely imposed by competitively reviewed cost-capped mission proposals, for which system-level flight heritage and cost credibility can trump sheer performance and mission capture. It describes criteria that mission architects and review boards can use to select and evaluate electric propulsion systems, provides descriptions of viable government and commercial electric propulsion system options, describes the modifications needed to adapt commercial electric propulsion systems to deep space, and discusses appropriate methods for costing commercial-based electric propulsion systems. It concludes that the solar electric propulsion systems best suited for Discovery missions have a solid system flight heritage that can meet the requirements for deep space with minimal modifications. Commercially developed electric propulsion systems offer significant heritage potential and, in many cases, the required changes for deep-space application introduce comparatively low technical and cost risk. C1 [Oh, David Y.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Snyder, John Steven; Hofer, Richard R.] CALTECH, Jet Prop Lab, Elect Prop Grp, Pasadena, CA 91109 USA. [Goebel, Dan M.] CALTECH, Jet Prop Lab, Prop Thermal & Mat Engn Sect, Pasadena, CA 91109 USA. [Randolph, Thomas M.] CALTECH, Jet Prop Lab, Syst Engn Grp, Pasadena, CA 91109 USA. RP Oh, DY (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM david.y.oh@jpl.nasa.gov FU NASA FX The work described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. The authors would particularly like to thank and recognize the contributions made to this paper by Damon Landau, Chris Stell, Paul Stella, Greg Cardell, Kelli McCoy, Kim Reh, Ron Reeve, Satish Khanna, and Brent Sherwood. References herein to any specific commercial product, process or service by trade name, trademark, manufacturer, or otherwise does not constitute or imply its endorsement by the United States Government or the Jet Propulsion Laboratory, California Institute of Technology. NR 76 TC 5 Z9 5 U1 1 U2 4 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD NOV-DEC PY 2014 VL 51 IS 6 BP 1822 EP 1835 DI 10.2514/1.A32889 PG 14 WC Engineering, Aerospace SC Engineering GA AU8QP UT WOS:000345861500006 ER PT J AU Jesick, M Ocampo, C AF Jesick, Mark Ocampo, Cesar TI Automated Design of Optimal Finite Thrust Orbit Insertion with Ballistic Flyby Constraints SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID FREE-RETURN; SPACE TRAJECTORIES; TRANSFERS; OPTIMIZATION; MANEUVER AB An automated method is developed to generate a minimum-fuel, finite thrust orbit insertion sequence while simultaneously generating a flyby trajectory of the same body that satisfies pre- and postflyby conditions in a general force field with ephemeris-level dynamics. The initial estimate requires no user input, and an impulsive solution is automatically converted to an optimal finite thrust transfer. As part of the initial estimate, a new method of generating ephemeris-level single flyby free returns is presented. A hybrid method is implemented for the optimal control solution whereby the costates are added to the vector of free parameters and the cost function is minimized directly. Analytic gradients are derived to decrease computation time and aid convergence of the optimization algorithm. The method is successfully applied in the Earth-moon system with application to human spaceflight and in the Saturn-Titan system with application to robotic spaceflight. C1 [Jesick, Mark] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA. [Ocampo, Cesar] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, WR Woolrich Labs, Austin, TX 78712 USA. RP Jesick, M (reprint author), CALTECH, Jet Prop Lab, Inner Planet Nav Grp, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. EM jesick@jpl.nasa.gov; cesar.ocampo@utexas.edu FU NASA's Graduate Student Researchers Program fellowship through Johnson Space Center FX This research was conducted at the University of Texas at Austin and was partially supported by NASA's Graduate Student Researchers Program fellowship through Johnson Space Center. NR 27 TC 1 Z9 1 U1 1 U2 3 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0022-4650 EI 1533-6794 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD NOV-DEC PY 2014 VL 51 IS 6 BP 1872 EP 1884 DI 10.2514/1.A32886 PG 13 WC Engineering, Aerospace SC Engineering GA AU8QP UT WOS:000345861500010 ER PT J AU Mehta, U Bowles, J Pandya, S Melton, J Huynh, L Kless, J Hawke, V AF Mehta, U. Bowles, J. Pandya, S. Melton, J. Huynh, L. Kless, J. Hawke, V. TI Conceptual stage separation from widebody subsonic carrier aircraft for space access SO AERONAUTICAL JOURNAL LA English DT Article AB Stage separation is a critical technical issue for developing two-stage-to-orbit (TSTO) launch systems with widebody carrier aircraft that use air-breathing propulsion and launch vehicle stages that use rocket propulsion. During conceptual design phases, this issue can be addressed with a combination of engineering methods, computational fluid dynamics simulations, and trajectory analysis of the mated system and the launch vehicle after staging. The outcome of such analyses helps to establish the credibility of the proposed TSTO system and formulate a ground-based test programme for the preliminary design phase. This approach is demonstrated with an assessment of stage separation from the shuttle carrier aircraft. Flight conditions are determined for safe mated flight, safe stage separation, and for the launch vehicle as it commences ascending flight. Accurate assessment of aerodynamic forces and moments is critical during staging to account for interference effects from the proximities of the two large vehicles. Interference aerodynamics have a modest impact on the separation conditions and separated flight trajectories, but have a significant impact on the interaction forces. C1 [Mehta, U.; Bowles, J.; Pandya, S.; Melton, J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huynh, L.; Kless, J.; Hawke, V.] Sci & Technol Corp, Moffett Field, CA USA. RP Mehta, U (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM unmeel.b.mehta@nasa.gov NR 26 TC 1 Z9 1 U1 1 U2 6 PU ROYAL AERONAUTICAL SOC PI LONDON PA 4 HAMILTON PL, LONDON W1J 7BQ, ENGLAND SN 0001-9240 J9 AERONAUT J JI Aeronaut. J. PD NOV PY 2014 VL 118 IS 1209 BP 1279 EP 1309 PG 31 WC Engineering, Aerospace SC Engineering GA AU3ES UT WOS:000345496000003 ER PT J AU Aliu, E Aune, T Barnacka, A Beilicke, M Benbow, W Berger, K Biteau, J Buckley, JH Bugaev, V Byrum, K Cardenzana, JV Cerruti, M Chen, X Ciupik, L Connaughton, V Cui, W Dickinson, HJ Eisch, JD Errando, M Falcone, A Federici, S Feng, Q Finley, JP Fleischhack, H Fortin, P Fortson, L Furniss, A Galante, N Gillanders, GH Griffin, S Griffiths, ST Grube, J Gyuk, G Hakansson, N Hanna, D Holder, J Hughes, G Humensky, TB Johnson, CA Kaaret, P Kar, P Kertzman, M Khassen, Y Kieda, D Krawczynski, H Krennrich, F Lang, MJ Madhavan, AS Maier, G McArthur, S McCann, A Meagher, K Millis, J Moriarty, P Mukherjee, R Nieto, D de Bhroithe, AO Ong, RA Otte, AN Park, N Pohl, M Popkow, A Prokoph, H Pueschel, E Quinn, J Ragan, K Rajotte, J Reyes, LC Reynolds, PT Richards, GT Roache, E Sembroski, GH Shahinyan, K Smith, AW Staszak, D Telezhinsky, I Tucci, JV Tyler, J Varlotta, A Vassiliev, VV Vincent, S Wakely, SP Weiner, OM Weinstein, A Welsing, R Wilhelm, A Williams, DA Zitzer, B McEnery, JE Perkins, JS Veres, P Zhu, S AF Aliu, E. Aune, T. Barnacka, A. Beilicke, M. Benbow, W. Berger, K. Biteau, J. Buckley, J. H. Bugaev, V. Byrum, K. Cardenzana, J. V. Cerruti, M. Chen, X. Ciupik, L. Connaughton, V. Cui, W. Dickinson, H. J. Eisch, J. D. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fleischhack, H. Fortin, P. Fortson, L. Furniss, A. Galante, N. Gillanders, G. H. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Hakansson, N. Hanna, D. Holder, J. Hughes, G. Humensky, T. B. Johnson, C. A. Kaaret, P. Kar, P. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Lang, M. J. Madhavan, A. S. Maier, G. McArthur, S. McCann, A. Meagher, K. Millis, J. Moriarty, P. Mukherjee, R. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Park, N. Pohl, M. Popkow, A. Prokoph, H. Pueschel, E. Quinn, J. Ragan, K. Rajotte, J. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Sembroski, G. H. Shahinyan, K. Smith, A. W. Staszak, D. Telezhinsky, I. Tucci, J. V. Tyler, J. Varlotta, A. Vassiliev, V. V. Vincent, S. Wakely, S. P. Weiner, O. M. Weinstein, A. Welsing, R. Wilhelm, A. Williams, D. A. Zitzer, B. McEnery, J. E. Perkins, J. S. Veres, P. Zhu, S. TI CONSTRAINTS ON VERY HIGH ENERGY EMISSION FROM GRB 130427A SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma-ray burst: individual (GRB 130427A) ID GAMMA-RAY BURSTS; COMPONENT; AFTERGLOWS; SWIFT; TELESCOPE; SPECTRA; MISSION; LIMITS; TEV AB Prompt emission from the very fluent and nearby (z = 0.34) gamma-ray burst GRB130427A was detected by several orbiting telescopes and by ground-based, wide-field-of-view optical transient monitors. Apart from the intensity and proximity of this GRB, it is exceptional due to the extremely long-lived high-energy (100 MeV to 100 GeV) gamma-ray emission, which was detected by the Large Area Telescope on the Fermi Gamma-Ray Space Telescope for similar to 70 ks after the initial burst. The persistent, hard-spectrum, high-energy emission suggests that the highest-energy gamma rays may have been produced via synchrotron self-Compton processes though there is also evidence that the high-energy emission may instead be an extension of the synchrotron spectrum. VERITAS, a ground-based imaging atmospheric Cherenkov telescope array, began follow-up observations of GRB130427A similar to 71 ks (similar to 20 hr) after the onset of the burst. The GRB was not detected with VERITAS; however, the high elevation of the observations, coupled with the low redshift of the GRB, make VERITAS a very sensitive probe of the emission from GRB130427A for E > 100 GeV. The non-detection and consequent upper limit derived place constraints on the synchrotron self-Compton model of high-energy gamma-ray emission from this burst. C1 [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Aune, T.; Ong, R. A.; Popkow, A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Barnacka, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Cerruti, M.; Fortin, P.; Galante, N.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Berger, K.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Berger, K.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Biteau, J.; Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Biteau, J.; Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Byrum, K.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cardenzana, J. V.; Dickinson, H. J.; Eisch, J. D.; Krennrich, F.; Madhavan, A. S.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Chen, X.; Federici, S.; Hakansson, N.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Chen, X.; Federici, S.; Fleischhack, H.; Hughes, G.; Maier, G.; de Bhroithe, A. O'Faolain; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Vincent, S.; Welsing, R.; Wilhelm, A.] DESY, D-15738 Zeuthen, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connaughton, V.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Tucci, J. V.; Varlotta, A.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA. [Falcone, A.; Veres, P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Fortson, L.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Gillanders, G. H.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Griffin, S.; Hanna, D.; Ragan, K.; Rajotte, J.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Humensky, T. B.; Nieto, D.; Weiner, O. M.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kar, P.; Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Khassen, Y.; Pueschel, E.; Quinn, J.] Natl Univ Ireland Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [McArthur, S.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Bishopstown, Cork, Ireland. [McEnery, J. E.; Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [McEnery, J. E.; Zhu, S.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.; Zhu, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Veres, P.] George Washington Univ, Dept Phys, Washington, DC 20052 USA. [Veres, P.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Veres, P.] Penn State Univ, Ctr Particle & Gravitat Astrophys, University Pk, PA 16802 USA. RP Aliu, E (reprint author), Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. EM aune@astro.ucla.edu; veres@email.gwu.edu; sjzhu@umd.edu RI Khassen, Yerbol/I-3806-2015; Nieto, Daniel/J-7250-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Nieto, Daniel/0000-0003-3343-0755; Cui, Wei/0000-0002-6324-5772; Barnacka, Anna/0000-0001-5655-4158; Lang, Mark/0000-0003-4641-4201 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U.K; NASA [NNX12AE30G] FX VERITAS is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748) and by STFC in the U.K. Additional support for observations of GRBs comes from NASA grant NNX12AE30G. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. NR 39 TC 8 Z9 8 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 1 PY 2014 VL 795 IS 1 AR L3 DI 10.1088/2041-8205/795/1/L3 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU2NO UT WOS:000345455500003 ER PT J AU Burlaga, LF Ness, NF AF Burlaga, L. F. Ness, N. F. TI INTERSTELLAR MAGNETIC FIELDS OBSERVED BY VOYAGER 1 BEYOND THE HELIOPAUSE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: magnetic fields ID SOLAR ROTATION; HELIOSHEATH; PLASMA; FLUCTUATIONS; HELIOSPHERE; REGION; SHOCK; WIND; AU AB Voyager 1 (V1) was beyond the heliopause between 2013.00 and 2014.41, where it was making in situ observations of the interstellar magnetic field (ISMF). The average azimuthal angle and elevation angle of the magnetic field B were = 292 degrees.5 +/- 1 degrees.4 and = 22.degrees 1 +/- 1 degrees.2, respectively. The angles lambda and delta varied linearly at (1 degrees.4 +/- 0 degrees.1) yr(-1) and (-1 degrees.1 +/- 0 degrees.1) yr(-1), respectively, suggesting that V1 was measuring the draped ISMF around the heliopause. The distributions of hourly averages of lambda and delta were Gaussian distributions, with most probable values 292 degrees.5 and 22 degrees.1, and standard deviations (SDs) 1 degrees.3 and 1 degrees.1, respectively. The small SD indicates little or no turbulence transverse to B. An abrupt decrease in B from 0.50 nT on 2013/129.9 to 0.46 nT on 2013/130.6 was observed, possibly associated with a weak reverse shock or magnetoacoustic pressure wave following a burst of electron plasma oscillations. Between 2013/130.6 and 2013/365.3, < B > = 0.464 +/- 0.009 nT , = 292 degrees.6 +/- 0 degrees.8, and = 22 degrees.1 +/- 1 degrees.1. The corresponding distribution of hourly averages of B was Gaussian with the most probable value 0.464 nT and sigma = 0.009 nT. Since the uncertainty s corresponds to the instrument and digitization noise, these observations provided an upper limit to the turbulence in the ISMF. The distributions of the hourly increments of B were Gaussian distributions with sigma = 0.05 nT, 0 degrees.4, and 0 degrees.4, respectively, indicating that the V1 did not detect evidence of "intermittent bursts" of interstellar turbulence. C1 [Burlaga, L. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ness, N. F.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. RP Burlaga, LF (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM lburlagahsp@verizon.net; nfnudel@yahoo.com FU NASA [NNX12AC63G, NNG14PN24P] FX T. McClanahan and S. Kramer provided support in the processing of the data. D. Berdichevsky computed correction tables for the three sensors on each of the two magnetometers. N. F. Ness was supported by NASA grant NNX12AC63G to the Catholic University of America. L. F. Burlaga was supported by NASA Contract NNG14PN24P. NR 21 TC 18 Z9 18 U1 1 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 1 PY 2014 VL 795 IS 1 AR L19 DI 10.1088/2041-8205/795/1/L19 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU2NO UT WOS:000345455500019 ER PT J AU Misra, AK Meadows, VS AF Misra, Amit K. Meadows, Victoria S. TI DISCRIMINATING BETWEEN CLOUDY, HAZY, AND CLEAR SKY EXOPLANETS USING REFRACTION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planets and satellites: atmospheres ID EXTRASOLAR PLANET ATMOSPHERE; TRANSMISSION SPECTROSCOPY; SPACE-TELESCOPE; SUPER-EARTHS; TRANSIT; PRESSURE; SPECTRUM; FEATURES; ECLIPSE; STARS AB We propose a method to distinguish between cloudy, hazy, and clear sky (free of clouds and hazes) exoplanet atmospheres that could be applicable to upcoming large aperture space-and ground-based telescopes such as the James Webb Space Telescope (JWST) and the European Extremely Large Telescope (E-ELT). These facilities will be powerful tools for characterizing transiting exoplanets, but only after a considerable amount of telescope time is devoted to a single planet. A technique that could provide a relatively rapid means of identifying haze-free targets (which may be more valuable targets for characterization) could potentially increase the science return for these telescopes. Our proposed method utilizes broadband observations of refracted light in the out-of-transit spectrum. Light refracted through an exoplanet atmosphere can lead to an increase of flux prior to ingress and subsequent to egress. Because this light is transmitted at pressures greater than those for typical cloud and haze layers, the detection of refracted light could indicate a cloud-or haze-free atmosphere. A detection of refracted light could be accomplished in < 10 hr for Jovian exoplanets with JWST and < 5 hr for super-Earths/mini-Neptunes with E-ELT. We find that this technique is most effective for planets with equilibrium temperatures between 200 and 500 K, which may include potentially habitable planets. A detection of refracted light for a potentially habitable planet would strongly suggest the planet was free of a global cloud or haze layer, and therefore a promising candidate for follow-up observations. C1 [Misra, Amit K.; Meadows, Victoria S.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Misra, Amit K.; Meadows, Victoria S.] Univ Washington, Astrobiol Program, Seattle, WA 98195 USA. [Misra, Amit K.; Meadows, Victoria S.] NASA, Astrobiol Inst, Virtual Planetary Lab, Seattle, WA 98195 USA. RP Misra, AK (reprint author), Univ Washington, Dept Astron, Seattle, WA 98195 USA. FU NASA Astrobiology Institute under Cooperative Agreement solicitation [NNH05ZDA001C] FX This work was performed by the NASA Astrobiology Institute's Virtual Planetary Laboratory, supported by the NASA Astrobiology Institute under Cooperative Agreement solicitation NNH05ZDA001C. NR 24 TC 3 Z9 3 U1 1 U2 5 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 NOV 1 PY 2014 VL 795 IS 1 AR L14 DI 10.1088/2041-8205/795/1/L14 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU2NO UT WOS:000345455500014 ER PT J AU Tiwari, SK Alexander, CE Winebarger, AR Moore, RL AF Tiwari, Sanjiv K. Alexander, Caroline E. Winebarger, Amy R. Moore, Ronald L. TI TRIGGER MECHANISM OF SOLAR SUBFLARES IN A BRAIDED CORONAL MAGNETIC STRUCTURE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: corona; Sun: flares; Sun: magnetic fields; Sun: photosphere; Sun: transition region ID ACTIVE-REGION; EVOLVING FIELDS; HEATING PROBLEM; NEUTRAL SHEETS; ALFVENIC WAVES; HI-C; ENERGY; EMISSION; WIND; FLUX AB Fine-scale braiding of coronal magnetic loops by continuous footpoint motions may power coronal heating via nanoflares, which are spontaneous fine-scale bursts of internal reconnection. An initial nanoflare may trigger an avalanche of reconnection of the braids, making a microflare or larger subflare. In contrast to this internal triggering of subflares, we observe external triggering of subflares in a braided coronal magnetic field observed by the High-resolution Coronal Imager (Hi-C). We track the development of these subflares using 12 s cadence images acquired by SDO/AIA in 1600, 193, 94 angstrom, and registered magnetograms of SDO/HMI, over four hours centered on the Hi-C observing time. These data show numerous recurring small-scale brightenings in transition-region emission happening on polarity inversion lines where flux cancellation is occurring. We present in detail an example of an apparent burst of reconnection of two loops in the transition region under the braided coronal field which is appropriate for releasing a short reconnected loop downward and a longer reconnected loop upward. The short loop presumably submerges into the photosphere, participating in observed flux cancellation. A subflare in the overlying braided magnetic field is apparently triggered by the disturbance of the braided field by the reconnection-released upward loop. At least 10 subflares observed in this braided structure appear to be triggered this way. How common this external trigger mechanism for coronal subflares is in other active regions, and how important it is for coronal heating in general, remain to be seen. C1 [Tiwari, Sanjiv K.; Alexander, Caroline E.; Winebarger, Amy R.; Moore, Ronald L.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Tiwari, SK (reprint author), NASA, George C Marshall Space Flight Ctr, Mail Code ZP 13, Huntsville, AL 35812 USA. EM sanjiv.k.tiwari@nasa.gov OI Tiwari, Sanjiv/0000-0001-7817-2978 FU NASA Postdoctoral Program at the NASA/MSFC; LWS TRT Program of the Heliophysics Division of NASA's SMD FX We thank the referee for constructive comments. The AIA and HMI data are courtesy of NASA/SDO and the AIA and HMI science teams. MSFC/NASA led the Hi-C mission and partners include the SAO in Cambridge, MA; LMSAL in Palo Alto, CA; the UCLan in Lancashire, England; and the LPIRAS in Moscow. S. K. T. and C. E. A. are supported by appointments to the NASA Postdoctoral Program at the NASA/MSFC, administered by ORAU through a contract with NASA. A. R. W. and R. L. M. are supported by funding from the LWS TRT Program of the Heliophysics Division of NASA's SMD. NR 35 TC 4 Z9 4 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 1 PY 2014 VL 795 IS 1 AR L24 DI 10.1088/2041-8205/795/1/L24 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU2NO UT WOS:000345455500024 ER PT J AU Brown, H Bollens, SM Brown, GS AF Brown, Harmon Bollens, Stephen M. Brown, Gretchen S. TI VERTICAL DISTRIBUTION AND DIEL MIGRATION OF CRANGON SEPTEMSPINOSA SAY, 1818 (DECAPODA, CARIDEA) ON GEORGES BANK, NORTHWEST ATLANTIC SO CRUSTACEANA LA English DT Article ID FLOUNDER PSEUDOPLEURONECTES-AMERICANUS; SAND SHRIMP; ULTRAVIOLET-RADIATION; PLANKTONIC COPEPOD; NEW-BRUNSWICK; LIFE-HISTORY; BROWN SHRIMP; ZOOPLANKTON; PREDATION; TEMPERATURE AB We sampled for vertical distribution and possible diel vertical migration (DVM) of Crangon septemspinosa Say, 1818 on and around Georges Bank, Northwest Atlantic, between 1995 and 1999. Both juveniles and adults were found to undergo DVM, being distributed within the lower water column (and perhaps on or in the bottom) during the day, and distributed throughout the water column at night, with higher abundances seen in all depth strata at night. Differences in vertical distribution were also found based on location and chlorophyll concentration for juveniles, but no effects were seen of season, salinity, temperature, lunar periodicity, year, or copepod prey for either juveniles or adults. Variation in vertical distribution and DVM were only moderately well explained (50% of the total variance) by the above factors, suggesting that some other factor(s) not measured by us (e.g., predation) were potentially also controlling the vertical distribution and diel migration of C. septemspinosa on Georges Bank. C1 [Brown, Harmon] NOAA, Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, Galveston Lab, Galveston, TX 77551 USA. [Bollens, Stephen M.] Washington State Univ, Sch Environm, Vancouver, WA 98686 USA. [Brown, Gretchen S.] MPH Inc, Houston, TX 77074 USA. RP Brown, H (reprint author), NOAA, Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, Galveston Lab, 4700 Ave U, Galveston, TX 77551 USA. EM harmon.brown@noaa.gov FU NSF [OCE96-17209]; NOAA by the U.S. GLOBEC Northwest Atlantic/Georges Bank Program [NA66GP0356]; National Science Foundation; National Oceanic and Atmospheric Administration FX We would like to thank Darren Gewant, Heidi Franklin and Mari Butler for their assistance with sample analysis. A great deal of thanks goes to the scientists and crews of the R/V "Albatross IV", R/V "Endeavor", and R/V "Oceanus" for their hard work and long hours in collecting samples on the broad-scale cruises. This work was supported by NSF award No. OCE96-17209 and NOAA award No. NA66GP0356 to S.M.B. provided by the U.S. GLOBEC Northwest Atlantic/Georges Bank Program, a joint program of the National Science Foundation and the National Oceanic and Atmospheric Administration. This is contribution number 749 of the U.S. GLOBEC Northwest Atlantic/Georges Bank Program. NR 47 TC 2 Z9 2 U1 0 U2 7 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0011-216X EI 1568-5403 J9 CRUSTACEANA JI Crustaceana PD NOV PY 2014 VL 87 IS 13 BP 1486 EP 1499 DI 10.1163/15685403-00003372 PG 14 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AU3EC UT WOS:000345494400002 ER PT J AU Mousis, O Hueso, R Beaulieu, JP Bouley, S Carry, B Colas, F Klotz, A Pellier, C Petit, JM Rousselot, P Ali-Dib, M Beisker, W Birlan, M Buil, C Delsanti, A Frappa, E Hammel, HB Levasseur-Regourd, AC Orton, GS Sanchez-Lavega, A Santerne, A Tanga, P Vaubaillon, J Zanda, B Baratoux, D Bohm, T Boudon, V Bouquet, A Buzzi, L Dauvergne, JL Decock, A Delcroix, M Drossart, P Esseiva, N Fischer, G Fletcher, LN Foglia, S Gomez-Forrellad, JM Guarro-Flo, J Herald, D Jehin, E Kugel, F Lebreton, JP Lecacheux, J Leroy, A Maquet, L Masi, G Maury, A Meyer, F Perez-Hoyos, S Rajpurohit, AS Rinner, C Rogers, JH Roques, F Schmude, RW Sicardy, B Tregon, B Vanhuysse, M Wesley, A Widemann, T AF Mousis, O. Hueso, R. Beaulieu, J. -P. Bouley, S. Carry, B. Colas, F. Klotz, A. Pellier, C. Petit, J. -M. Rousselot, P. Ali-Dib, M. Beisker, W. Birlan, M. Buil, C. Delsanti, A. Frappa, E. Hammel, H. B. Levasseur-Regourd, A. C. Orton, G. S. Sanchez-Lavega, A. Santerne, A. Tanga, P. Vaubaillon, J. Zanda, B. Baratoux, D. Boehm, T. Boudon, V. Bouquet, A. Buzzi, L. Dauvergne, J. -L. Decock, A. Delcroix, M. Drossart, P. Esseiva, N. Fischer, G. Fletcher, L. N. Foglia, S. Gomez-Forrellad, J. M. Guarro-Flo, J. Herald, D. Jehin, E. Kugel, F. Lebreton, J. -P. Lecacheux, J. Leroy, A. Maquet, L. Masi, G. Maury, A. Meyer, F. Perez-Hoyos, S. Rajpurohit, A. S. Rinner, C. Rogers, J. H. Roques, F. Schmude, R. W., Jr. Sicardy, B. Tregon, B. Vanhuysse, M. Wesley, A. Widemann, T. TI Instrumental methods for professional and amateur collaborations in planetary astronomy SO EXPERIMENTAL ASTRONOMY LA English DT Review DE Planetary astronomy; Professional-amateur collaborations; Imaging; Photometry; Spectroscopy ID NEAR-EARTH ASTEROIDS; TRANSIT TIMING VARIATIONS; SOUTH EQUATORIAL BELT; GROUND-BASED OBSERVATIONS; LEONID IMPACT FLASHES; SPACE-TELESCOPE FGS; GREAT RED SPOT; LIGHTCURVE INVERSION; STELLAR OCCULTATIONS; OPTIMIZATION METHODS AB Amateur contributions to professional publications have increased exponentially over the last decades in the field of planetary astronomy. Here we review the different domains of the field in which collaborations between professional and amateur astronomers are effective and regularly lead to scientific publications. We discuss the instruments, detectors, software and methodologies typically used by amateur astronomers to collect the scientific data in the different domains of interest. Amateur contributions to the monitoring of planets and interplanetary matter, characterization of asteroids and comets, as well as the determination of the physical properties of Kuiper Belt Objects and exoplanets are discussed. C1 [Mousis, O.; Petit, J. -M.; Rousselot, P.; Ali-Dib, M.; Meyer, F.; Rajpurohit, A. S.] Univ Franche Comte, Inst UTINAM, CNRS INSU, UMR 6213,Observ Sci Univers Besancon, F-25030 Besancon, France. [Hueso, R.; Sanchez-Lavega, A.; Perez-Hoyos, S.] Univ Pais Vasco UPV EHU, Escuela Tecn Super Ingn, Dept Fis Aplicada 1, Bilbao 48013, Spain. [Hueso, R.; Sanchez-Lavega, A.; Perez-Hoyos, S.] Unidad Asociada Grp Ciencias Planetarias UPV EHU, Bilbao, Spain. [Beaulieu, J. -P.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR7095, F-75014 Paris, France. [Bouley, S.] Univ Paris 11, UMR8148, Lab GEOPS, F-91405 Orsay, France. [Bouley, S.; Colas, F.; Birlan, M.; Vaubaillon, J.] Observ Paris, IMCCE, UMR8048, F-75014 Paris, France. [Carry, B.] ESA, European Space Astron Ctr, Madrid 28691, Spain. [Klotz, A.; Boehm, T.; Bouquet, A.] Univ Toulouse UPS OMP, IRAP, Toulouse, France. [Pellier, C.; Delcroix, M.] Commiss Planetary Observat, French Astron Soc SAF, F-75016 Paris, France. [Beisker, W.] IOTA ES, D-30459 Hannover, Germany. [Buil, C.] Observ Castanet, F-31320 Castanet Tolosan, France. [Buil, C.; Leroy, A.; Tregon, B.] Assoc T60, F-31400 Toulouse, France. [Delsanti, A.] Aix Marseille Univ, CNRS, Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France. [Delsanti, A.] Observ Paris, LESIA, F-92195 Meudon, France. [Frappa, E.] Euraster, F-42000 St Etienne, France. [Hammel, H. B.] AURA, Washington, DC 20005 USA. [Levasseur-Regourd, A. C.] Univ Paris 06, Univ Sorbonne, LATMOS CNRS, F-75005 Paris, France. [Orton, G. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Santerne, A.] Univ Porto, CAUP Ctr Astrofis, P-4150762 Oporto, Portugal. [Tanga, P.] Univ Nice Sophia Antipolis, CNRS, Observ Cote dAzur, Lab Lagrange,UMR 7293, F-06304 Nice 4, France. [Zanda, B.] MNHN, Lab Mineral & Cosmochim Museum, F-75005 Paris, France. [Baratoux, D.] Univ Toulouse, Geosci Environm Toulouse, UMR 5563, F-31400 Toulouse, France. [Boudon, V.] UMR 6303 CNRS Univ Bourgogne, Lab Interdisciplinaire Carnot Bourgogne, F-21078 Dijon, France. [Buzzi, L.] Osservatorio Astron Schiaparelli, I-21110 Varese, Italy. [Dauvergne, J. -L.] AFA Ciel & Espace, F-75014 Paris, France. [Dauvergne, J. -L.] Assoc T60, F-31400 Toulouse, France. [Decock, A.; Jehin, E.] Univ Liege, Inst Astrophys Geophys & Oceanog, B-4000 Liege, Belgium. [Drossart, P.; Lecacheux, J.; Maquet, L.; Roques, F.; Sicardy, B.; Widemann, T.] Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris, F-92195 Meudon, France. [Esseiva, N.] Assoc AstroQueyras, F-05350 St Veran, France. [Fischer, G.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria. [Fletcher, L. N.] Univ Oxford, Clarendon Lab, Dept Phys, Oxford OX1 3PU, England. [Foglia, S.] Astron Res Inst, Ashmore, IL 61912 USA. [Gomez-Forrellad, J. M.] Fundacio Privada Observ Esteve Duran, Seva 08553, Spain. [Guarro-Flo, J.] ARAS, Seva, Spain. [Herald, D.] IOTA, Murrumbateman, NSW, Australia. [Kugel, F.] Observ Chante Perdrix, F-04150 Dauban, Banon, France. [Lebreton, J. -P.] CNRS Univ Orleans, LPC2E, F-45071 Orleans 2, France. [Leroy, A.] LUranoscope Ile France, Gretz Armainvilliers, France. [Masi, G.] Virtual Telescope Project, I-03023 Ceccano, FR, Italy. [Maury, A.] San Pedro de Atacama Celestial Explorat, San Pedro De Atacama, Chile. [Rinner, C.] Observ Oukaimeden, Oukaimeden 40273, Morocco. [Rogers, J. H.] JUPOS Team, London W1J ODU, England. [Rogers, J. H.] British Astron Assoc, London W1J ODU, England. [Schmude, R. W., Jr.] Gordon State Coll, Barnesville, GA 30204 USA. [Tregon, B.] Lab Ondes & Mat Aquitaine CNRS Univ Bordeaux 1, UMR5798, F-33405 Talence, France. [Vanhuysse, M.] OverSky, F-33127 St Jean Dillac, France. [Wesley, A.] Canberra Astron Soc, Astron Soc Australia, Murrumbateman, NSW, Australia. RP Mousis, O (reprint author), Univ Franche Comte, Inst UTINAM, CNRS INSU, UMR 6213,Observ Sci Univers Besancon, F-25030 Besancon, France. EM olivier.mousis@obs-besancon.fr RI Fletcher, Leigh/D-6093-2011; Zanda, Brigitte/D-6787-2015; Perez-Hoyos, Santiago/L-7543-2014; BIRLAN, Mirel/B-5283-2011; OI Hueso, Ricardo/0000-0003-0169-123X; Fletcher, Leigh/0000-0001-5834-9588; Zanda, Brigitte/0000-0002-4210-7151; Perez-Hoyos, Santiago/0000-0002-2587-4682; Sanchez-Lavega, Agustin/0000-0001-7355-1522; Frappa, Eric/0000-0001-5327-7781; Santerne, Alexandre/0000-0002-3586-1316; Tanga, Paolo/0000-0002-2718-997X FU CNES; Spanish MICIIN [AYA2009-10701, AYA2012-36666]; FEDER; Grupos Gobierno Vasco [IT-464-07, UPV/EHU UFI11/55]; European Research Council/European Community under the FP7 through Starting Grant [239953]; Partenariat Hubert Curien/French-Moroccon volubis program [PHC 24675QJ]; Austrian Science Fund FWF [P24325-N16]; NASA; Royal Society Research Fellowship at the University of Oxford FX O.M. acknowledges support from CNES. RH, ASL and SPH were supported by the Spanish MICIIN project AYA2009-10701 and AYA2012-36666 with FEDER support, Grupos Gobierno Vasco IT-464-07 and UPV/EHU UFI11/55. A. S. acknowledges the support by the European Research Council/European Community under the FP7 through Starting Grant agreement number 239953. D. B. and S. B are supported by the Partenariat Hubert Curien/French-Moroccon volubis program PHC 24675QJ. G. F. was supported by the Austrian Science Fund FWF, project P24325-N16. G.O. was supported by awards from NASA to JPL/Caltech. LNF was supported by a Royal Society Research Fellowship at the University of Oxford. NR 212 TC 13 Z9 13 U1 0 U2 15 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0922-6435 EI 1572-9508 J9 EXP ASTRON JI Exp. Astron. PD NOV PY 2014 VL 38 IS 1-2 BP 91 EP 191 DI 10.1007/s10686-014-9379-0 PG 101 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU1MR UT WOS:000345385300007 ER PT J AU Rauer, H Catala, C Aerts, C Appourchaux, T Benz, W Brandeker, A Christensen-Dalsgaard, J Deleuil, M Gizon, L Goupil, MJ Gudel, M Janot-Pacheco, E Mas-Hesse, M Pagano, I Piotto, G Pollacco, D Santos, NC Smith, A Suarez, JC Szabo, R Udry, S Adibekyan, V Alibert, Y Almenara, JM Maro-Seoane, PA Ammler-von Eiff, M Asplund, M Antonello, E Barnes, S Baudin, F Belkacem, K Bergemann, M Bihain, G Birch, AC Bonfils, X Boisse, I Bonomo, AS Borsa, F Brandao, IM Brocato, E Brun, S Burleigh, M Burston, R Cabrera, J Cassisi, S Chaplin, W Charpinet, S Chiappini, C Church, RP Csizmadia, S Cunha, M Damasso, M Davies, MB Deeg, HJ Diaz, RF Dreizler, S Dreyer, C Eggenberger, P Ehrenreich, D Eigmuller, P Erikson, A Farmer, R Feltzing, S Fialho, FD Figueira, P Forveille, T Fridlund, M Garcia, RA Giommi, P Giuffrida, G Godolt, M da Silva, JG Granzer, T Grenfell, JL Grotsch-Noels, A Gunther, E Haswell, CA Hatzes, AP Hebrard, G Hekker, S Helled, R Heng, K Jenkins, JM Johansen, A Khodachenko, ML Kislyakova, KG Kley, W Kolb, U Krivova, N Kupka, F Lammer, H Lanza, AF Lebreton, Y Magrin, D Marcos-Arenal, P Marrese, PM Marques, JP Martins, J Mathis, S Mathur, S Messina, S Miglio, A Montalban, J Montalto, M Monteiro, MJPFG Moradi, H Moravveji, E Mordasini, C Morel, T Mortier, A Nascimbeni, V Nelson, RP Nielsen, MB Noack, L Norton, AJ Ofir, A Oshagh, M Ouazzani, RM Papics, P Parro, VC Petit, P Plez, B Poretti, E Quirrenbach, A Ragazzoni, R Raimondo, G Rainer, M Reese, DR Redmer, R Reffert, S Rojas-Ayala, B Roxburgh, IW Salmon, S Santerne, A Schneider, J Schou, J Schuh, S Schunker, H Silva-Valio, A Silvotti, R Skillen, I Snellen, I Sohl, F Sousa, SG Sozzetti, A Stello, D Strassmeier, KG Svanda, M Szabo, GM Tkachenko, A Valencia, D Van Grootel, V Vauclair, SD Ventura, P Wagner, FW Walton, NA Weingrill, J Werner, SC Wheatley, PJ Zwintz, K AF Rauer, H. Catala, C. Aerts, C. Appourchaux, T. Benz, W. Brandeker, A. Christensen-Dalsgaard, J. Deleuil, M. Gizon, L. Goupil, M. -J. Guedel, M. Janot-Pacheco, E. Mas-Hesse, M. Pagano, I. Piotto, G. Pollacco, D. Santos, N. C. Smith, A. Suarez, J. -C. Szabo, R. Udry, S. Adibekyan, V. Alibert, Y. Almenara, J. -M. Maro-Seoane, P. A. Ammler-von Eiff, M. Asplund, M. Antonello, E. Barnes, S. Baudin, F. Belkacem, K. Bergemann, M. Bihain, G. Birch, A. C. Bonfils, X. Boisse, I. Bonomo, A. S. Borsa, F. Brandao, I. M. Brocato, E. Brun, S. Burleigh, M. Burston, R. Cabrera, J. Cassisi, S. Chaplin, W. Charpinet, S. Chiappini, C. Church, R. P. Csizmadia, Sz. Cunha, M. Damasso, M. Davies, M. B. Deeg, H. J. Diaz, R. F. Dreizler, S. Dreyer, C. Eggenberger, P. Ehrenreich, D. Eigmueller, P. Erikson, A. Farmer, R. Feltzing, S. de Oliveira Fialho, F. Figueira, P. Forveille, T. Fridlund, M. Garcia, R. A. Giommi, P. Giuffrida, G. Godolt, M. Gomes da Silva, J. Granzer, T. Grenfell, J. L. Grotsch-Noels, A. Guenther, E. Haswell, C. A. Hatzes, A. P. Hebrard, G. Hekker, S. Helled, R. Heng, K. Jenkins, J. M. Johansen, A. Khodachenko, M. L. Kislyakova, K. G. Kley, W. Kolb, U. Krivova, N. Kupka, F. Lammer, H. Lanza, A. F. Lebreton, Y. Magrin, D. Marcos-Arenal, P. Marrese, P. M. Marques, J. P. Martins, J. Mathis, S. Mathur, S. Messina, S. Miglio, A. Montalban, J. Montalto, M. Monteiro, M. J. P. F. G. Moradi, H. Moravveji, E. Mordasini, C. Morel, T. Mortier, A. Nascimbeni, V. Nelson, R. P. Nielsen, M. B. Noack, L. Norton, A. J. Ofir, A. Oshagh, M. Ouazzani, R. -M. Papics, P. Parro, V. C. Petit, P. Plez, B. Poretti, E. Quirrenbach, A. Ragazzoni, R. Raimondo, G. Rainer, M. Reese, D. R. Redmer, R. Reffert, S. Rojas-Ayala, B. Roxburgh, I. W. Salmon, S. Santerne, A. Schneider, J. Schou, J. Schuh, S. Schunker, H. Silva-Valio, A. Silvotti, R. Skillen, I. Snellen, I. Sohl, F. Sousa, S. G. Sozzetti, A. Stello, D. Strassmeier, K. G. Svanda, M. Szabo, Gy. M. Tkachenko, A. Valencia, D. Van Grootel, V. Vauclair, S. D. Ventura, P. Wagner, F. W. Walton, N. A. Weingrill, J. Werner, S. C. Wheatley, P. J. Zwintz, K. TI The PLATO 2.0 mission SO EXPERIMENTAL ASTRONOMY LA English DT Article DE Exoplanets; Asteroseismology; Transit survey; Stellar science; Exoplanetary science ID GIANT PLANET FORMATION; SOLAR-TYPE STARS; ANGULAR-MOMENTUM TRANSPORT; MAIN-SEQUENCE STARS; DELTA-SCUTI STARS; SUN-LIKE STAR; TRANSITING EXTRASOLAR PLANETS; MASS-RADIUS RELATIONSHIPS; ENERGETIC NEUTRAL ATOMS; SPIN-ORBIT MISALIGNMENT AB PLATO 2.0 has recently been selected for ESA's M3 launch opportunity (2022/24). Providing accurate key planet parameters (radius, mass, density and age) in statistical numbers, it addresses fundamental questions such as: How do planetary systems form and evolve? Are there other systems with planets like ours, including potentially habitable planets? The PLATO 2.0 instrument consists of 34 small aperture telescopes (32 with 25 s readout cadence and 2 with 2.5 s cadence) providing a wide field-of-view (2232 deg(2)) and a large photometric magnitude range (4-16 mag). It focuses on bright (4-11 mag) stars in wide fields to detect and characterize planets down to Earth-size by photometric transits, whose masses can then be determined by ground-based radial-velocity follow-up measurements. Asteroseismology will be performed for these bright stars to obtain highly accurate stellar parameters, including masses and ages. The combination of bright targets and asteroseismology results in high accuracy for the bulk planet parameters: 2 %, 4-10 % and 10 % for planet radii, masses and ages, respectively. The planned baseline observing strategy includes two long pointings (2-3 years) to detect and bulk characterize planets reaching into the habitable zone (HZ) of solar-like stars and an additional step-and-stare phase to cover in total about 50 % of the sky. PLATO 2.0 will observe up to 1,000,000 stars and detect and characterize hundreds of small planets, and thousands of planets in the Neptune to gas giant regime out to the HZ. It will therefore provide the first large-scale catalogue of bulk characterized planets with accurate radii, masses, mean densities and ages. This catalogue will include terrestrial planets at intermediate orbital distances, where surface temperatures are moderate. Coverage of this parameter range with statistical numbers of bulk characterized planets is unique to PLATO 2.0. The PLATO 2.0 catalogue allows us to e. g.: - complete our knowledge of planet diversity for low-mass objects, - correlate the planet mean density-orbital distance distribution with predictions from planet formation theories,- constrain the influence of planet migration and scattering on the architecture of multiple systems, and - specify how planet and system parameters change with host star characteristics, such as type, metallicity and age. The catalogue will allow us to study planets and planetary systems at different evolutionary phases. It will further provide a census for small, low-mass planets. This will serve to identify objects which retained their primordial hydrogen atmosphere and in general the typical characteristics of planets in such a low-mass, low-density range. Planets detected by PLATO 2.0 will orbit bright stars and many of them will be targets for future atmosphere spectroscopy exploring their atmospheres. Furthermore, the mission has the potential to detect exomoons, planetary rings, binary and Trojan planets. The planetary science possible with PLATO 2.0 is complemented by its impact on stellar and galactic science via asteroseismology as well as light curves of all kinds of variable stars, together with observations of stellar clusters of different ages. This will allow us to improve stellar models and study stellar activity. A large number of well-known ages from red giant stars will probe the structure and evolution of our Galaxy. Asteroseismic ages of bright stars for different phases of stellar evolution allow calibrating stellar age-rotation relationships. Together with the results of ESA's Gaia mission, the results of PLATO 2.0 will provide a huge legacy to planetary, stellar and galactic science. C1 [Rauer, H.; Cabrera, J.; Csizmadia, Sz.; Dreyer, C.; Eigmueller, P.; Erikson, A.; Fridlund, M.; Godolt, M.; Grenfell, J. L.; Sohl, F.; Wagner, F. W.] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany. [Rauer, H.; Dreyer, C.] Berlin Univ Technol, Dept Astron & Astrophys, D-10623 Berlin, Germany. [Catala, C.; Goupil, M. -J.; Belkacem, K.; Lebreton, Y.; Ouazzani, R. -M.; Schneider, J.] Univ Paris 05, UPMC, CNRS, LESIA,Observ Paris,PSL Res Univ, F-92195 Meudon, France. [Aerts, C.; Marcos-Arenal, P.; Moravveji, E.; Papics, P.; Tkachenko, A.; Zwintz, K.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Leuven, Belgium. [Appourchaux, T.; Baudin, F.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Benz, W.; Alibert, Y.; Heng, K.] Univ Bern, Inst Phys, Ctr Space & Habitabil, CH-3012 Bern, Switzerland. [Brandeker, A.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden. [Christensen-Dalsgaard, J.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Deleuil, M.; Almenara, J. -M.] Lab Astrophys Marseille, F-13388 Marseille 13, France. [Gizon, L.; Ammler-von Eiff, M.; Birch, A. C.; Burston, R.; Hekker, S.; Krivova, N.; Schou, J.; Schuh, S.; Schunker, H.] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany. [Guedel, M.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Janot-Pacheco, E.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-09500900 Sao Paulo, Brazil. [Mas-Hesse, M.] Ctr Astrobiol CSIC INTA, Madrid, Spain. [Pagano, I.; Lanza, A. F.; Messina, S.] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [Piotto, G.; Damasso, M.; Nascimbeni, V.] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, I-35122 Padua, Italy. [Pollacco, D.; Wheatley, P. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Santos, N. C.; Adibekyan, V.; Boisse, I.; Brandao, I. M.; Cunha, M.; Figueira, P.; Gomes da Silva, J.; Martins, J.; Montalto, M.; Monteiro, M. J. P. F. G.; Mortier, A.; Oshagh, M.; Rojas-Ayala, B.; Santerne, A.; Sousa, S. G.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Smith, A.] UCL, Mullard Space Sci Lab, London, England. [Suarez, J. -C.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Szabo, R.; Szabo, Gy. M.] Hungarian Acad Sci, Konkoly Observ, H-1121 Budapest, Hungary. [Udry, S.; Diaz, R. F.; Eggenberger, P.; Ehrenreich, D.] Observ Geneva, CH-1290 Sauverny, Switzerland. [Maro-Seoane, P. A.] Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-14476 Golm, Germany. [Guenther, E.; Hatzes, A. P.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Antonello, E.; Borsa, F.; Poretti, E.; Rainer, M.] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. [Gizon, L.; Dreizler, S.; Marques, J. P.; Nielsen, M. B.; Ofir, A.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Barnes, S.; Bihain, G.; Chiappini, C.; Granzer, T.; Strassmeier, K. G.; Weingrill, J.] Leibniz Inst Astrophys, D-14482 Potsdam, Germany. [Bergemann, M.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. [Bonomo, A. S.; Damasso, M.; Silvotti, R.; Sozzetti, A.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy. [Brocato, E.; Giuffrida, G.; Marrese, P. M.; Ventura, P.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy. [Brun, S.; Garcia, R. A.; Mathis, S.] CEA Saclay, CEA, DSM IRFU Serv Astrophys, F-91191 Gif Sur Yvette, France. [Burleigh, M.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Noack, L.] Royal Observ Belgium, B-1180 Brussels, Belgium. [Cassisi, S.; Raimondo, G.] Osservatorio Astron Teramo, INAF, I-64100 Teramo, Italy. [Chaplin, W.; Miglio, A.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Charpinet, S.; Vauclair, S. D.] Univ Toulouse, UPS OMP, IRAP, F-31400 Toulouse, France. [Church, R. P.; Davies, M. B.; Feltzing, S.; Johansen, A.] Lund Observ, S-22100 Lund, Sweden. [Deeg, H. J.] Inst Astrofis Canarias, Tenerife, Spain. [de Oliveira Fialho, F.] Univ Sao Paulo, Polytech Sch, Lab Automat & Control, Sao Paulo, Brazil. [Farmer, R.; Haswell, C. A.; Kolb, U.; Norton, A. J.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Bonfils, X.; Forveille, T.] Observ Grenoble, Inst Planetol & Astrophys Grenoble, F-38041 Grenoble 9, France. [Giommi, P.; Giuffrida, G.; Marrese, P. M.] ASI Sci Data Ctr, I-00133 Rome, Italy. [Asplund, M.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Grotsch-Noels, A.; Montalban, J.; Morel, T.; Reese, D. R.; Salmon, S.; Van Grootel, V.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Hebrard, G.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Hekker, S.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Helled, R.] Tel Aviv Univ, Dept Geophys Atmospher & Planetary Sci, IL-69978 Tel Aviv, Israel. [Jenkins, J. M.] NASA, Ames Res Ctr, SETI Inst, Mountain View, CA USA. [Khodachenko, M. L.; Kislyakova, K. G.; Lammer, H.] Austrian Acad Sci, A-8042 Graz, Austria. [Kley, W.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Kupka, F.] Univ Vienna, Fak Math, A-1090 Vienna, Austria. [Magrin, D.; Ragazzoni, R.] Astron Observ Padova, INAF, I-35122 Padua, Italy. [Mathur, S.] Space Sci Inst, Boulder, CO 80301 USA. [Moradi, H.] Monash Univ, Sch Math Sci, Monash Ctr Astrophys, Clayton, Vic 3800, Australia. [Mordasini, C.] Max Planck Inst Astron, Planet & Star Format Dept, D-69117 Heidelberg, Germany. [Parro, V. C.] Inst Maua Tecnol, Sao Paulo, Brazil. [Petit, P.] Observ Midi Pyrenees, F-31400 Toulouse, France. [Plez, B.] Univ Montpellier 2, CNRS, Lab Univers & Particules Montpellier, F-34095 Montpellier 5, France. [Brandeker, A.; Quirrenbach, A.; Reffert, S.] Heidelberg Univ, ZAH, D-69117 Heidelberg, Germany. [Redmer, R.] Univ Rostock, Inst Phys, D-18051 Rostock, Germany. [Nelson, R. P.; Roxburgh, I. W.] Queen Mary Univ London, Sch Phys & Astron, Astron Unit, London E1 4NS, England. [Silva-Valio, A.] Univ Prebiteriana Mackenzie, CRAAM, Sao Paulo, Brazil. [Skillen, I.] Isaac Newton Grp Telescopes, Astron Grp, Santa Cruz De La Palma 38700, Spain. [Snellen, I.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Svanda, M.] Charles Univ Prague, Fac Math & Phys, Astron Inst, CR-18000 Prague 8, Czech Republic. [Szabo, Gy. M.] ELTE Gothard Astrophys Observ, H-9704 Szombathely, Hungary. [Valencia, D.] MIT, Atmosphere & Planetary Sci Dept, Cambridge, MA 02139 USA. [Walton, N. A.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Werner, S. C.] Univ Oslo, Ctr Earth Evolut & Dynam, N-0316 Oslo, Norway. [Stello, D.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. RP Rauer, H (reprint author), German Aerosp Ctr, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany. EM heike.rauer@dlr.de RI Adibekyan, Vardan/I-5026-2013; Brandao, Isa/M-5172-2013; Valio, Adriana/I-2531-2012; Marcos-Arenal, Pablo/O-4719-2016; Nielsen, Marina/F-5625-2012; Sousa, Sergio/I-7466-2013; Plez, Bertrand/G-6697-2011; Fialho, Fabio/D-6661-2012; Monteiro, Mario J.P.F.G./B-4715-2008; Werner, Stephanie/A-6438-2012; Svanda, Michal/A-6576-2008; Pagano, Isabella/I-6934-2015; Suarez, Juan Carlos/C-1015-2009; Guedel, Manuel/C-8486-2015; Figueira, Pedro/J-4916-2013; Rojas-Ayala, Barbara/G-4382-2015; Parro, Vanderlei/B-1988-2013; Kley, Wilhelm/A-4921-2012; OI Adibekyan, Vardan/0000-0002-0601-6199; Oshagh, Mahmoudreza/0000-0002-0715-8789; Brandao, Isa/0000-0002-1153-0942; Silvotti, Roberto/0000-0002-1295-8174; giommi, paolo/0000-0002-2265-5003; Messina, Sergio/0000-0002-2851-2468; Sozzetti, Alessandro/0000-0002-7504-365X; Ragazzoni, Roberto/0000-0002-7697-5555; Magrin, Demetrio/0000-0003-0312-313X; Eigmuller, Philipp/0000-0003-4096-0594; Valio, Adriana/0000-0002-1671-8370; Marcos-Arenal, Pablo/0000-0003-1549-9396; Ventura, Paolo/0000-0002-5026-6400; Weingrill, Jorg/0000-0002-0848-413X; Cassisi, Santi/0000-0001-5870-3735; Brocato, Enzo/0000-0001-7988-8177; Cunha, Margarida/0000-0001-8237-7343; Noack, Lena/0000-0001-8817-1653; Sousa, Sergio/0000-0001-9047-2965; Plez, Bertrand/0000-0002-0398-4434; Monteiro, Mario J.P.F.G./0000-0003-0513-8116; Werner, Stephanie/0000-0001-5704-0909; Svanda, Michal/0000-0002-6345-1007; Pagano, Isabella/0000-0001-9573-4928; Suarez, Juan Carlos/0000-0003-3649-8384; Guedel, Manuel/0000-0001-9818-0588; Figueira, Pedro/0000-0001-8504-283X; Rojas-Ayala, Barbara/0000-0002-0149-1302; Parro, Vanderlei/0000-0002-8232-0125; Ehrenreich, David/0000-0001-9704-5405; Garcia, Rafael/0000-0002-8854-3776; Charpinet, Stephane/0000-0002-6018-6180; Mortier, Annelies/0000-0001-7254-4363; Piotto, Giampaolo/0000-0002-9937-6387; Wheatley, Peter/0000-0003-1452-2240; Diaz, Rodrigo/0000-0001-9289-5160; Petit, Pascal/0000-0001-7624-9222; Zwintz, Konstanze/0000-0001-9229-8315; Santerne, Alexandre/0000-0002-3586-1316; Poretti, Ennio/0000-0003-1200-0473; Lanza, Antonino Francesco/0000-0001-5928-7251; Farmer, Robert/0000-0003-3441-7624; Szabo, Robert/0000-0002-3258-1909; Bonfils, Xavier/0000-0001-9003-8894 FU DLR (Deutsches Zentrum fur Luft- und Raumfahrt) [50 OW 0204]; European Research Council/European Community under the FP7 programme through ERC [320360]; Fundacao para a Ciencia e Tecnologia (Portugal) [SFRH/BPD/87857/2012]; Danish National Research Foundation [DNRF106]; ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) - European Research Council [267864]; Deutsche Forschungsgemeinschaft [SFB 963]; Helmholtz Gemeinschaft (HGF) through the HGF research alliance "Planetary Evolution and Life"; Netherlands Organisation for Scientific Research (NOW); Stellar Ages project - European Research Council [338251]; FWF NFN [S116, S116 604-N16, S116 606-N16, S116607-N16]; FWF [P25229-N27]; Spanish MINECO [AYA2012-39362-C02-01]; Interuniversity Attraction Poles Programme; Belgian Science Policy Office through the Planet Topers alliance; University of Liege; Leverhulme Foundation [EM-2012-035/4]; European Research Council/European Community under the FP7 through Starting Grant [239953]; Hungarian OTKA [K104607, K83790]; HUMAN [MB08C 81013]; City of Szombathely [S-11-1027]; Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences; Janos Bolyai Research Scholarship; KTIA URKUT [10-1-2011-0019]; European Community [269194, 312844] FX M. Ammler-von Eiff acknowledges support by DLR (Deutsches Zentrum fur Luft- und Raumfahrt) under the project 50 OW 0204. M. Bergemann acknowledges the support by the European Research Council/European Community under the FP7 programme through ERC Grant number 320360. I. Boisse acknowledges the support from the Fundacao para a Ciencia e Tecnologia (Portugal) through the grant SFRH/BPD/87857/2012. For J. Christensen-Dalsgard, funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (Grant agreement no.: 267864). L. Gizon acknowledges support from Deutsche Forschungsgemeinschaft SFB 963 "Astrophysical Flow Instabilities and Turbulence" (Project A18). M. Godolt and J. L. Grenfell have been partly supported by the Helmholtz Gemeinschaft (HGF) through the HGF research alliance "Planetary Evolution and Life". S. Hekker acknowledges financial support from the Netherlands Organisation for Scientific Research (NOW) and the Stellar Ages project funded by the European Research Council (Grant agreement number 338251). K. G. Kislyakova, N. V. Erkaev, M. L. Khodachenko, H. Lammer, M. Gudel acknowledge support by the FWF NFN project S116 "Pathways to Habitability: From Disks to Active Stars, Planets and Life", and subprojects, S116 604-N16 "Radiation & Wind Evolution from T Tauri Phase to ZAMS and Beyond", S116 606-N16 "Magnetospheric Electrodynamics of Exoplanets", S116607-N16 "Particle/Radiative Interactions with Upper Atmospheres of Planetary Bodies Under Extreme Stellar Conditions". F. Kupka is grateful for support through FWF project P25229-N27. M. Mas-Hesse was supported by Spanish MINECO under grant AYA2012-39362-C02-01. L. Noack has been funded by the Interuniversity Attraction Poles Programme initiated by the Belgian Science Policy Office through the Planet Topers alliance. D. R. Reese is supported through a post-doctoral fellowship from the "Subside federal pour la recherche 2012", University of Liege. I. W. Roxburgh gratefully acknowledges support from the Leverhulme Foundation under grant EM-2012-035/4. A. Santerne and N. C. Santos acknowledge the support by the European Research Council/European Community under the FP7 through Starting Grant agreement number 239953. S. G. Sousa acknowledges the support by the European Research Council/European Community under the FP7 through Starting Grant agreement number 239953. Gy. M. Szabo acknowledges the Hungarian OTKA Grants K104607, the HUMAN MB08C 81013 grant, by the City of Szombathely under agreement No. S-11-1027 and the Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences. R. Szabo was supported by the Janos Bolyai Research Scholarship, Hungarian OTKA grant K83790, KTIA URKUT 10-1-2011-0019 grant Lendulet-2009 Young Researchers' Program and the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreements no. 269194 (IRSES/ASK) and no. 312844 (SPACEINN). NR 395 TC 173 Z9 175 U1 11 U2 52 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0922-6435 EI 1572-9508 J9 EXP ASTRON JI Exp. Astron. PD NOV PY 2014 VL 38 IS 1-2 BP 249 EP 330 DI 10.1007/s10686-014-9383-4 PG 82 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU1MR UT WOS:000345385300010 ER PT J AU Kline, PA Flagg, TA AF Kline, Paul A. Flagg, Thomas A. TI Putting the Red Back in Redfish Lake, 20 Years of Progress Toward Saving the Pacific Northwest's Most Endangered Salmon Population SO FISHERIES LA English DT Article ID RIVER SOCKEYE-SALMON; SNAKE-RIVER; ONCORHYNCHUS-NERKA; CAPTIVE BROODSTOCKS; OLIGOTROPHIC LAKE; NURSERY LAKES; MANAGEMENT; GROWTH; IDAHO; CONSERVATION AB In November 1991, the U.S. National Marine Fisheries Service listed Snake River Sockeye Salmon (Oncorhynchus nerka) as endangered under the U.S. Endangered Species Act (ESA). The last known remnants of the Snake River stock return to Redfish Lake in the Sawtooth Valley in central Idaho. In the ensuing two decades since the ESA listing, many actions have been taken to conserve the population, including the initiation of a hatchery-based gene rescue program. The chief aim of this article is to describe the development and implementation of hatchery-based gene rescue activities, review present-day release strategies and associated adult returns, and describe a new effort underway to expand program production to more effectively address recolonization and local adaptation objectives. In addition, we describe achievable population triggers to allow the transition from a hatchery-based effort to a habitat-based effort that should allow natural population recovery to proceed. RESUMENEn noviembre de 1991, el Servicio Nacional de Pesquerias Marinas de los Estados Unidos de Norteamerica, ingreso al salmon (Oncorhynchus nerka) en el Acta de Especies Amenazadas de los Estados Unidos (AEA) bajo la categoria de amenazado. Los ultimos remanentes conocidos del stock del Rio Snake, regresaron al Lago Redfish, Valle Sawtooth, en la porcion central de Idaho. Dos decadas despues de haber ingresado esta especie al acta, se han llevado a cabo varias acciones tendientes a conservar a la poblacion, entre las que se incluye el inicio de un programa de rescate genetico. El objetivo del presente trabajo es describir el desarrollo e implementacion de actividades de rescate genetico basado en cultivos, revisar las estrategias actuales de liberacion y posterior retorno de adultos y describir la nueva iniciativa de expandir el programa de produccion para abordar de forma mas efectiva la recolonizacion y los objetivos de adaptacion local. Adicionalmente, se describe como se usaran detonantes poblacionales que permitan una transicion entre esfuerzos basados en cultivos y esfuerzos basados en habitats con el fin de facilitar la recuperacion de las poblaciones. C1 [Kline, Paul A.] Idaho Dept Fish & Game, Boise, ID 83707 USA. [Flagg, Thomas A.] NOAA, Manchester Res Stn, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Manchester, WA 98353 USA. RP Kline, PA (reprint author), Idaho Dept Fish & Game, POB 25, Boise, ID 83707 USA. EM paul.kline@idfg.idaho.gov FU Bonneville Power Administration through the Northwest Power and Conservation Council's Fish and Wildlife Program FX Work was primarily funded by the Bonneville Power Administration and coordinated through the Northwest Power and Conservation Council's Fish and Wildlife Program. NR 66 TC 4 Z9 4 U1 6 U2 29 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0363-2415 EI 1548-8446 J9 FISHERIES JI Fisheries PD NOV PY 2014 VL 39 IS 11 BP 488 EP 500 DI 10.1080/03632415.2014.966087 PG 13 WC Fisheries SC Fisheries GA AU2MI UT WOS:000345452000004 ER PT J AU Trushenski, J Blankenship, L Bowker, J Flagg, T Hesse, J Leber, K Lorenzen, K MacKinlay, D Maynard, D Moffitt, C Mudrak, V Scribner, K Stuewe, S Sweka, J Whelan, G Young-Dubovsky, C AF Trushenski, Jesse Blankenship, Lee Bowker, Jim Flagg, Tom Hesse, Jay Leber, Ken Lorenzen, Kai MacKinlay, Don Maynard, Des Moffitt, Christine Mudrak, Vince Scribner, Kim Stuewe, Scott Sweka, John Whelan, Gary Young-Dubovsky, Connie TI AFS Completes Assessment, Issues New Guidance Regarding Hatchery Operation and the Use of Hatchery-Origin Fish SO FISHERIES LA English DT Editorial Material C1 [Trushenski, Jesse] So Illinois Univ, Ctr Fisheries Aquaculture & Aquat Sci, Carbondale, IL 62901 USA. [Blankenship, Lee] Northwest Marine Technol Inc, Tumwater, WA 98501 USA. [Bowker, Jim] US Fish & Wildlife Serv, Bozeman, MT 59715 USA. [Flagg, Tom; Maynard, Des] Natl Marine Fisheries Serv, Manchester, WA 98353 USA. [Hesse, Jay] Nez Perce Tribe Dept Fisheries Resources Manageme, Lapwai, ID 83540 USA. [Leber, Ken] Mote Marine Lab, Sarasota, FL 34236 USA. [Lorenzen, Kai] Univ Florida, Gainesville, FL 32653 USA. [MacKinlay, Don] Fisheries & Oceans Canada, Ottawa, ON K1A 0E6, Canada. [Moffitt, Christine] Univ Idaho, US Geol Survey, Moscow, ID 83844 USA. [Mudrak, Vince] US Fish & Wildlife Serv, Warm Springs, GA 31830 USA. [Scribner, Kim] Michigan State Univ, Dept Zool, E Lansing, MI 48824 USA. [Stuewe, Scott] HDR, Springfield, IL 62703 USA. [Sweka, John] US Fish & Wildlife Serv, Lamar, PA 16841 USA. [Whelan, Gary] Michigan Dept Nat Resources, Lansing, MI 48909 USA. [Young-Dubovsky, Connie] US Fish & Wildlife Serv, Denver, CO 80225 USA. RP Trushenski, J (reprint author), So Illinois Univ, Ctr Fisheries Aquaculture & Aquat Sci, Life Sci 2 Room 251, Carbondale, IL 62901 USA. EM saluski@siu.edu NR 4 TC 1 Z9 1 U1 1 U2 5 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0363-2415 EI 1548-8446 J9 FISHERIES JI Fisheries PD NOV PY 2014 VL 39 IS 11 BP 543 EP 547 DI 10.1080/03632415.2014.964395 PG 5 WC Fisheries SC Fisheries GA AU2MI UT WOS:000345452000014 ER PT J AU Laurel, BJ Danley, C Haines, S AF Laurel, Benjamin J. Danley, Courtney Haines, Scott TI The effects of temperature on growth, development and settlement of northern rock sole larvae (Lepidopsetta polyxystra) SO FISHERIES OCEANOGRAPHY LA English DT Article DE climate change; dispersal; inner front; larval transport; metamorphosis; settlement dynamics ID FLOUNDER PSEUDOPLEURONECTES-AMERICANUS; SOUTHEASTERN BERING-SEA; LIFE-HISTORY TRAITS; PACIFIC COD LARVAE; REEF FISH; SUMMER FLOUNDER; METAMORPHOSIS; SIZE; SURVIVAL; FLATFISH AB Northern rock sole (Lepidopsetta polyxystra) is a commercially important fish in the North Pacific and a focal species in understanding larval transport to nursery grounds in the Bering Sea. However, the temperature-dependent vital rates and settlement dynamics for this species have not been described in detail. We reared northern rock sole larvae in the laboratory to measure growth, condition, development and settlement parameters across four temperatures (2, 4, 7 and 10 degrees C). Both length and mass-measured growth rates increased with temperature and were best described by non-linear regression. Residuals of the length-mass relationships were positively related to temperature, indicating larval condition also increased with temperature. Larval development and settlement were largely size dependent, resulting in reduced larval stage duration and earlier settlement at higher temperatures owing to more rapid growth at elevated temperatures. However, larvae at colder temperatures were less developed at a given size, but more likely to settle at smaller sizes than larvae reared in warmer conditions. These temperature-response parameters can be used to refine current and future transport models for northern rock sole larvae under changing environmental conditions in the North Pacific. C1 [Laurel, Benjamin J.; Haines, Scott] NOAA, Fisheries Behav Ecol Program, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv,Hatfield Marine Sci Ct, Newport, OR 97365 USA. [Danley, Courtney] Oregon State Univ, Hatfield Marine Sci Ctr, CIMRS, Newport, OR 97365 USA. RP Laurel, BJ (reprint author), NOAA, Fisheries Behav Ecol Program, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv,Hatfield Marine Sci Ct, Newport, OR 97365 USA. EM ben.laurel@noaa.gov FU NOAA-AFSC's Habitat and Ecological Processes Research (HEPR) Program FX This project was supported in part with funding from the NOAA-AFSC's Habitat and Ecological Processes Research (HEPR) Program. We thank Ian Bradbury, Tom Hurst and Cliff Ryer for providing feedback on earlier drafts of this manuscript. Mara Spencer and Paul Iseri collected and shipped broodstock from Kodiak, AK. Boat charters were kindly provided by Tim Tripp aboard the F/V Miss O. Whitney Clerf provided assistance in the maintenance and strip-spawning of broodstock in the laboratory and Matt Hawkyard assisted with rotifer production, feeding and larviculture. NR 45 TC 4 Z9 4 U1 1 U2 25 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1054-6006 EI 1365-2419 J9 FISH OCEANOGR JI Fish Oceanogr. PD NOV PY 2014 VL 23 IS 6 BP 495 EP 505 DI 10.1111/fog.12084 PG 11 WC Fisheries; Oceanography SC Fisheries; Oceanography GA AU4TC UT WOS:000345603300004 ER PT J AU Pearce, NJG Westgate, JA Gatti, E Pattan, JN Parthiban, G Achyuthan, H AF Pearce, Nicholas J. G. Westgate, John A. Gatti, Emma Pattan, Jinnappa N. Parthiban, Gopal Achyuthan, Hema TI Individual glass shard trace element analyses confirm that all known Toba tephra reported from India is from the c. 75-ka Youngest Toba eruption SO JOURNAL OF QUATERNARY SCIENCE LA English DT Article DE glass shards; India; Oldest Toba Tuff; tephra; Toba; trace elements; Youngest Toba Tuff ID ULTRA-DISTAL TEPHRA; PRECISION AR-40/AR-39 AGE; MULTIPLE INTERPRETIVE ERRORS; MIDDLE SON VALLEY; PENINSULAR INDIA; NORTHERN SUMATRA; TUFF; INDONESIA; SEDIMENTS; SUPERERUPTION AB Uncertainty over the identity and age of Toba tephras across peninsular India persists, with radiometric age dates contradicting earlier compositional data, which have been used to identify this important stratigraphic marker as the Youngest Toba Tuff (YTT). To address this issue, new single glass shard analyses have been performed for samples from Morgaon and Bori (north-western India), which have recently been dated at c. 800 ka. These, and indeed all Toba tephra samples thus far analysed from India, show the presence of four populations of glass shards (defined by their Ba/Y ratio), which uniquely identifies them as products of the c. 75-ka Youngest Toba eruption. Confirmation that the YTT fingerprint is characteristic comes from new analyses of Oldest Toba Tuff (OTT) glass shards from five sites in the Indian Ocean. These are compositionally identical to Layer D from the ODP site 758 sediment core (c. 800 ka), and belong to a single, low-Ba population, clearly different from YTT. These analyses show that there is essentially no reworked OTT material in the YTT eruption, and indicate unequivocally that all known Toba tephra occurrences in India belong to the c. 75-ka Youngest Toba eruption. C1 [Pearce, Nicholas J. G.] Aberystwyth Univ, Dept Geog & Earth Sci, Aberystwyth SY23 3DB, Dyfed, Wales. [Westgate, John A.] Univ Toronto, Dept Earth Sci, Toronto, ON, Canada. [Gatti, Emma] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Pattan, Jinnappa N.; Parthiban, Gopal] CSIR Natl Inst Oceanog, Panaji, Goa, India. [Achyuthan, Hema] Anna Univ, Dept Geol, Chennai 600025, Tamil Nadu, India. RP Pearce, NJG (reprint author), Aberystwyth Univ, Dept Geog & Earth Sci, Aberystwyth SY23 3DB, Dyfed, Wales. EM nick.pearce@aber.ac.uk RI Pearce, Nicholas/B-5295-2009; OI Pearce, Nicholas/0000-0003-3157-9564 FU Natural Sciences and Engineering Research Council of Canada FX We thank Dr Shyam Prasad from NIO, Goa, who provided the coarse fraction of some of the OTT samples. J.A.W. gratefully acknowledges the support of the Natural Sciences and Engineering Research Council of Canada. We thank the four anonymous referees for their positive and rapid reviews. NR 50 TC 2 Z9 3 U1 29 U2 39 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0267-8179 EI 1099-1417 J9 J QUATERNARY SCI JI J. Quat. Sci. PD NOV PY 2014 VL 29 IS 8 BP 729 EP 734 DI 10.1002/jqs.2741 PG 6 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA AU0WS UT WOS:000345343500001 ER PT J AU Thibodeau, PS Roesler, CS Drapeau, SL Matondkar, SGP Goes, JI Werdell, PJ AF Thibodeau, Patricia S. Roesler, Collin S. Drapeau, Susan L. Matondkar, S. G. Prabhu Goes, Joaquim I. Werdell, P. Jeremy TI Locating Noctiluca miliaris in the Arabian Sea: An optical proxy approach SO LIMNOLOGY AND OCEANOGRAPHY LA English DT Article ID GULF-OF-MEXICO; PHYTOPLANKTON POPULATIONS; ABSORPTION-COEFFICIENTS; SOUTHWEST MONSOON; SPRING INTERMONSOON; PIGMENT ANALYSIS; KARENIA-BREVIS; SCINTILLANS; FLUORESCENCE; DINOFLAGELLATE AB Coincident with shifting monsoon weather patterns over India, the phytoplankter Noctiluca miliaris has recently been observed to be dominating phytoplankton blooms in the northeastern Arabian Sea during the winter monsoons. Identifying the exact environmental and/or ecological conditions that favor this species has been hampered by the lack of concurrent environmental and biological observations on time and space scales relevant to ecologic and physiologic processes. We present a bio-optical proxy for N. miliaris measured on highly resolved depth scales coincident with hydrographic observations with the goal to identify conducive hydrographic conditions for the bloom. The proxy is derived from multichannel excitation chlorophyll a fluorescence and is validated with microscopy, pigment composition, and spectral absorption. Phytoplankton populations dominated by either diatoms or other dinoflagellates were additionally discerned. N. miliaris populations in full bloom were identified offshore in low-nutrient and low-N : P ratio surface waters within a narrow temperature and salinity range. These populations transitioned to high-biomass diatom-dominated coastal upwelling populations. A week later, the N. miliaris blooms were observed in declining phase, transitioning to very-low-biomass populations of non-N. miliaris dinoflagellates. There were no clear hydrographic conditions uniquely associated with the N. miliaris populations, although N. miliaris was not found in the upwelling or extremely oligotrophic waters. Taxonomic transitions were not discernible in the spatial structure of the bloom as identified by the ocean color Chl imagery, indicating that in situ observations may be necessary to resolve community structure, particularly for populations below the surface. C1 [Thibodeau, Patricia S.; Roesler, Collin S.; Drapeau, Susan L.] Bowdoin Coll, Brunswick, ME 04011 USA. [Matondkar, S. G. Prabhu] Natl Inst Oceanog, Panaji, Goa, India. [Goes, Joaquim I.] Columbia Univ, Palisades, NY USA. [Werdell, P. Jeremy] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Roesler, CS (reprint author), Bowdoin Coll, Brunswick, ME 04011 USA. EM croesler@bowdoin.edu FU National Aeronautics and Space Administration Ocean Biology and Biogeochemistry Program; Bowdoin College Grua and O'Connell award FX Funding provided by National Aeronautics and Space Administration Ocean Biology and Biogeochemistry Program. Bowdoin College Grua and O'Connell award provided funds for travel to present this research at the 2013 Association for the Sciences of Limnology and Oceanography Conference. Special thanks to the captain and crew of the R/V Sagar Sampada for their dedicated efforts. P. Thibodeau wishes to thank her undergraduate honors thesis committee members, Rachel Beane and Michele LaVigne, for comments on earlier versions of the manuscript. Two anonymous reviewers provided helpful comments, for which we are very grateful. NR 52 TC 1 Z9 1 U1 3 U2 9 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-3590 EI 1939-5590 J9 LIMNOL OCEANOGR JI Limnol. Oceanogr. PD NOV PY 2014 VL 59 IS 6 BP 2042 EP 2056 DI 10.4319/lo.2014.59.6.2042 PG 15 WC Limnology; Oceanography SC Marine & Freshwater Biology; Oceanography GA AU2QK UT WOS:000345462700018 ER PT J AU Portnoy, DS Hollenbeck, CM Belcher, CN Driggers, WB Frazier, BS Gelsleichter, J Grubbsk, RD Gold, JR AF Portnoy, D. S. Hollenbeck, C. M. Belcher, C. N. Driggers, W. B., III Frazier, B. S. Gelsleichter, J. Grubbsk, R. D. Gold, J. R. TI Contemporary population structure and post-glacial genetic demography in a migratory marine species, the blacknose shark, Carcharhinus acronotus SO MOLECULAR ECOLOGY LA English DT Review DE conservation genetics; elasmobranchs; glacial refugia; secondary contact ID GULF-OF-MEXICO; LAST GLACIAL MAXIMUM; APPROXIMATE BAYESIAN COMPUTATION; LAURENTIDE ICE-SHEET; NORTH-ATLANTIC OCEAN; WESTERN ATLANTIC; BLACKTIP SHARK; GLOBAL PHYLOGEOGRAPHY; MICROSATELLITE DATA; COASTAL WATERS AB Patterns of population structure and historical genetic demography of blacknose sharks in the western North Atlantic Ocean were assessed using variation in nuclear-encoded microsatellites and sequences of mitochondrial (mt)DNA. Significant heterogeneity and/or inferred barriers to gene flow, based on microsatellites and/or mtDNA, revealed the occurrence of five genetic populations localized to five geographic regions: the southeastern U.S Atlantic coast, the eastern Gulf of Mexico, the western Gulf of Mexico, Bay of Campeche in the southern Gulf of Mexico and the Bahamas. Pairwise estimates of genetic divergence between sharks in the Bahamas and those in all other localities were more than an order of magnitude higher than between pairwise comparisons involving the other localities. Demographic modelling indicated that sharks in all five regions diverged after the last glacial maximum and, except for the Bahamas, experienced post-glacial, population expansion. The patterns of genetic variation also suggest that the southern Gulf of Mexico may have served as a glacial refuge and source for the expansion. Results of the study demonstrate that barriers to gene flow and historical genetic demography contributed to contemporary patterns of population structure in a coastal migratory species living in an otherwise continuous marine habitat. The results also indicate that for many marine species, failure to properly characterize barriers in terms of levels of contemporary gene flow could in part be due to inferences based solely on equilibrium assumptions. This could lead to erroneous conclusions regarding levels of connectivity in species of conservation concern. C1 [Portnoy, D. S.; Hollenbeck, C. M.; Gold, J. R.] Texas A&M Univ, Harte Res Inst, Dept Life Sci, Marine Genom Lab, Corpus Christi, TX 78412 USA. [Belcher, C. N.] Georgia Dept Nat Resources, Brunswick, GA 31520 USA. [Driggers, W. B., III] Mississippi Labs, Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Pascagoula, MS 39568 USA. [Frazier, B. S.] South Carolina Dept Nat Resources, Charleston, SC 29412 USA. [Gelsleichter, J.] Univ N Florida, Jacksonville, FL 32224 USA. [Grubbsk, R. D.] Florida State Univ, Coastal & Marine Lab, St Teresa, FL 32358 USA. RP Portnoy, DS (reprint author), Texas A&M Univ, Harte Res Inst, Dept Life Sci, Marine Genom Lab, 6300 Ocean Dr, Corpus Christi, TX 78412 USA. EM david.portnoy@tamucc.edu FU National Marine Fisheries Service under SALTONSTALL-KENNEDY [NA10NMF4270218]; National Marine Fisheries Service [NA12NMF4540080] FX We thank A. Piercy (Florida Museum of Natural History, University of North Florida), R. Ford (University of North Florida), N. Hammerschlag (University of Miami), Captain G. Rapp, D. Bethea (NOAA Fisheries Panama City Laboratory), M. Drymon (Dauphin Island Sea Lab), P. J. Diaz (National Autonomous University of Mexico), K. Hannan, C. Jones and L. Jones (NMFS, Mississippi Laboratories), A. Shaw (SCDNR), D. McDowell (GADNR), G. Skomal (Massachusetts Marine Fisheries), B. Franks (Florida Southern University), C. Peterson and J. Imhoff (Florida State University), T. Guttridge (Bimini Biological Field Station) and E. Brooks (Cape Eleuthera Institute) for providing tissue samples. We also thank M. Renshaw and M. Giresi for assistance in the laboratory, and M. Hansen and four anonymous reviewers for constructive comments on drafts of this manuscript. Work was supported by the National Marine Fisheries Service under SALTONSTALL-KENNEDY GRANT NO. NA10NMF4270218 and Cooperative Research Program Grant No. NA12NMF4540080. This is contribution 720 of the South Carolina Marine Resources Center and Number 99 in the series 'Genetic Studies in Marine Fishes.' NR 120 TC 10 Z9 10 U1 10 U2 92 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 EI 1365-294X J9 MOL ECOL JI Mol. Ecol. PD NOV PY 2014 VL 23 IS 22 BP 5480 EP 5495 DI 10.1111/mec.12954 PG 16 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA AU4HW UT WOS:000345572300007 PM 25294029 ER PT J AU Montanaro, M Gerace, A Lunsford, A Reuter, D AF Montanaro, Matthew Gerace, Aaron Lunsford, Allen Reuter, Dennis TI Stray Light Artifacts in Imagery from the Landsat 8 Thermal Infrared Sensor SO REMOTE SENSING LA English DT Article DE Landsat; TIRS; stray light; ghosting; banding AB The Thermal Infrared Sensor (TIRS) has been collecting imagery of the Earth since its launch aboard Landsat 8 in early 2013. In many respects, TIRS has been exceeding its performance requirements on orbit, particularly in terms of noise and stability. However, several artifacts have been observed in the TIRS data which include banding and absolute calibration discrepancies that violate requirements in some scenes. Banding is undesired structure that appears within and between the focal plane array assemblies. In addition, in situ measurements have shown an error in the TIRS absolute radiometric calibration that appears to vary with season and location within the image. The source of these artifacts has been determined to be out-of-field radiance that scatters onto the detectors thereby adding a non-uniform signal across the field-of-view. The magnitude of this extra signal can be approximately 8% or higher (band 11) and is generally twice as large in band 11 as it is in band 10. A series of lunar scans were obtained to gather information on the source of this out-of-field radiance. Analyses of these scans have produced a preliminary map of stray light, or ghost, source locations in the TIRS out-of-field area. This dataset has been used to produce a synthetic TIRS scene that closely reproduces the banding effects seen in actual TIRS imagery. Now that the cause of the banding has been determined, a stray light optics model is in development that will pin-point the cause of the stray light source. Several methods are also being explored to correct for the banding and the absolute calibration error in TIRS imagery. C1 [Montanaro, Matthew] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA. [Gerace, Aaron] Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. [Lunsford, Allen] Catholic Univ Amer, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reuter, Dennis] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Montanaro, M (reprint author), NASA, Goddard Space Flight Ctr, Sigma Space Corp, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM matthew.montanaro@nasa.gov; gerace@cis.rit.edu; allen.w.lunsford@nasa.gov; dennis.c.reuter@nasa.gov FU NASA [NNG09HP18C, NNX09AQ57A] FX The authors would like to acknowledge the Landsat 8 Mission Operations Center team for the planning and execution of the lunar acquisition maneuvers and acknowledge Simon Hook and his team at NASA/JPL for providing the radiance measurements for the Lake Tahoe buoys. The work presented here was funded under NASA contract NNG09HP18C and NASA cooperative agreement NNX09AQ57A. NR 15 TC 24 Z9 25 U1 1 U2 15 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD NOV PY 2014 VL 6 IS 11 BP 10435 EP 10456 DI 10.3390/rs61110435 PG 22 WC Remote Sensing SC Remote Sensing GA AU3RG UT WOS:000345530700009 ER PT J AU Gerace, A Schott, J Gartley, M Montanaro, M AF Gerace, Aaron Schott, John Gartley, Michael Montanaro, Matthew TI An Analysis of the Side Slither On-Orbit Calibration Technique Using the DIRSIG Model SO REMOTE SENSING LA English DT Article DE side slither; 90 degree yaw; Landsat 8; OLI; TIRS; DIRSIG; calibration AB Pushbroom-style imaging systems exhibit several advantages over line scanners when used on space-borne platforms as they typically achieve higher signal-to-noise and reduce the need for moving parts. Pushbroom sensors contain thousands of detectors, each having a unique radiometric response, which will inevitably lead to streaking and banding in the raw data. To take full advantage of the potential exhibited by pushbroom sensors, a relative radiometric correction must be performed to eliminate pixel-to-pixel non-uniformities in the raw data. Side slither is an on-orbit calibration technique where a 90-degree yaw maneuver is performed over an invariant site to flatten the data. While this technique has been utilized with moderate success for the QuickBird satellite [1] and the RapidEye constellation [2], further analysis is required to enable its implementation for the Landsat 8 sensors, which have a 15-degree field-of-view and a 0.5% pixel-to-pixel uniformity requirement. This work uses the DIRSIG model to analyze the side slither maneuver as applicable to the Landsat sensor. A description of favorable sites, how to adjust the maneuver to compensate for the curvature of "linear" arrays, how to efficiently process the data, and an analysis to assess the quality of the side slither data, are presented. C1 [Gerace, Aaron; Schott, John; Gartley, Michael] Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14624 USA. [Montanaro, Matthew] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA. RP Gerace, A (reprint author), Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14624 USA. EM gerace@cis.rit.edu; schott@cis.rit.edu; gartley@cis.rit.edu; matthew.montanaro@nasa.gov FU NASA [NNX09AQ57A] FX The work presented here was funded under NASA cooperative agreement NNX09AQ57A. NR 21 TC 1 Z9 1 U1 2 U2 2 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD NOV PY 2014 VL 6 IS 11 BP 10523 EP 10545 DI 10.3390/rs61110523 PG 23 WC Remote Sensing SC Remote Sensing GA AU3RG UT WOS:000345530700013 ER PT J AU Liu, G Heron, SF Eakin, CM Muller-Karger, FE Vega-Rodriguez, M Guild, LS De La Cour, JL Geiger, EF Skirving, WJ Burgess, TFR Strong, AE Harris, A Maturi, E Ignatov, A Sapper, J Li, JK Lynds, S AF Liu, Gang Heron, Scott F. Eakin, C. Mark Muller-Karger, Frank E. Vega-Rodriguez, Maria Guild, Liane S. De La Cour, Jacqueline L. Geiger, Erick F. Skirving, William J. Burgess, Timothy F. R. Strong, Alan E. Harris, Andy Maturi, Eileen Ignatov, Alexander Sapper, John Li, Jianke Lynds, Susan TI Reef-Scale Thermal Stress Monitoring of Coral Ecosystems: New 5-km Global Products from NOAA Coral Reef Watch SO REMOTE SENSING LA English DT Article DE bleaching; thermal stress; satellite; remote sensing; sea surface temperature (SST); monitoring; climatology; hotspots; degree heating week; bleaching alert area ID SEA-SURFACE TEMPERATURE; CLIMATE-CHANGE; BLEACHING EVENTS; MORTALITY; ISLANDS AB The U.S. National Oceanic and Atmospheric Administration (NOAA) Coral Reef Watch (CRW) program has developed a daily global 5-km product suite based on satellite observations to monitor thermal stress on coral reefs. These products fulfill requests from coral reef managers and researchers for higher resolution products by taking advantage of new satellites, sensors and algorithms. Improvements of the 5-km products over CRW's heritage global 50-km products are derived from: (1) the higher resolution and greater data density of NOAA's next-generation operational daily global 5-km geo-polar blended sea surface temperature (SST) analysis; and (2) implementation of a new SST climatology derived from the Pathfinder SST climate data record. The new products increase near-shore coverage and now allow direct monitoring of 95% of coral reefs and significantly reduce data gaps caused by cloud cover. The 5-km product suite includes SST Anomaly, Coral Bleaching HotSpots, Degree Heating Weeks and Bleaching Alert Area, matching existing CRW products. When compared with the 50-km products and in situ bleaching observations for 2013-2014, the 5-km products identified known thermal stress events and matched bleaching observations. These near reef-scale products significantly advance the ability of coral reef researchers and managers to monitor coral thermal stress in near-real-time. C1 [Liu, Gang; Heron, Scott F.; Eakin, C. Mark; De La Cour, Jacqueline L.; Geiger, Erick F.; Skirving, William J.; Burgess, Timothy F. R.; Strong, Alan E.] US Natl Ocean & Atmospher Adm, Coral Reef Watch, College Pk, MD 20740 USA. [Liu, Gang; Heron, Scott F.; De La Cour, Jacqueline L.; Geiger, Erick F.; Skirving, William J.; Strong, Alan E.] Global Sci & Technol Inc, Greenbelt, MD 20770 USA. [Liu, Gang; Heron, Scott F.; Eakin, C. Mark; De La Cour, Jacqueline L.; Geiger, Erick F.; Skirving, William J.; Strong, Alan E.; Harris, Andy; Maturi, Eileen; Ignatov, Alexander] US Natl Ocean & Atmospher Adm, NESDIS STAR, College Pk, MD 20740 USA. [Heron, Scott F.] James Cook Univ, Dept Phys, Coll Sci Technol & Engn, Marine Geophys Lab, Townsville, Qld 4811, Australia. [Muller-Karger, Frank E.; Vega-Rodriguez, Maria] Univ S Florida, Inst Marine Remote Sensing, Coll Marine Sci, St Petersburg, FL 33701 USA. [Guild, Liane S.] US Natl Aeronaut & Space Adm, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA. [Harris, Andy] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. [Sapper, John] US Natl Ocean & Atmospher Adm, NESDIS OSPO, College Pk, MD 20740 USA. [Li, Jianke] DigitalGlobe Inc, Herndon, VA 20171 USA. [Lynds, Susan] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA. RP Liu, G (reprint author), US Natl Ocean & Atmospher Adm, Coral Reef Watch, College Pk, MD 20740 USA. EM Gang.Liu@noaa.gov; Scott.Heron@noaa.gov; Mark.Eakin@noaa.gov; carib@usf.edu; mariavegarod@mail.usf.edu; Liane.S.Guild@nasa.gov; Jacqueline.Shapo@noaa.gov; Erick.Geiger@noaa.gov; William.Skirving@noaa.gov; timburgess@mac.com; Alan.E.Strong@noaa.gov; Andy.Harris@noaa.gov; Eileen.Maturi@noaa.gov; Alex.Ignatov@noaa.gov; John.Sapper@noaa.gov; Jianke.Li@gmail.com; Susan.Lynds@colorado.edu RI De La Cour, Jacqueline/E-7920-2011; Skirving, William/E-7927-2011; Maturi, Eileen/F-5611-2010; Strong, Alan/E-7924-2011; Liu, Gang/E-7921-2011; Heron, Scott/E-7928-2011; Ignatov, Alexander/F-5594-2010; Eakin, C. Mark/F-5585-2010 OI Skirving, William/0000-0003-0167-6427; Liu, Gang/0000-0001-8369-6805; Ignatov, Alexander/0000-0002-7463-5944; FU NASA Applied Sciences Biodiversity and Ecological Forecasting program [NNX09AV24G]; NOAA Coral Reef Conservation Program FX Development of the next-generation 5-km product suite has been accomplished through a collaboration of NOAA Coral Reef Watch, the University of South Florida, NASA-Ames and the Cooperative Institute for Research in Environmental Science, with funding support from the NASA Applied Sciences Biodiversity and Ecological Forecasting program Grant NNX09AV24G and the NOAA Coral Reef Conservation Program. The CRW team at NOAA/NESDIS that develops and generates these monitoring products comprises scientists from the Center for Satellite Applications and Research (STAR) and the Office of Satellite and Product Operations (OSPO). The contents in this manuscript are solely the opinions of the authors and do not constitute a statement of policy, decision or position on behalf of NOAA or the U.S. Government. NR 64 TC 12 Z9 12 U1 5 U2 28 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD NOV PY 2014 VL 6 IS 11 BP 11579 EP 11606 DI 10.3390/rs61111579 PG 28 WC Remote Sensing SC Remote Sensing GA AU3RG UT WOS:000345530700059 ER PT J AU Barsi, JA Schott, JR Hook, SJ Raqueno, NG Markham, BL Radocinski, RG AF Barsi, Julia A. Schott, John R. Hook, Simon J. Raqueno, Nina G. Markham, Brian L. Radocinski, Robert G. TI Landsat-8 Thermal Infrared Sensor (TIRS) Vicarious Radiometric Calibration SO REMOTE SENSING LA English DT Article DE Landsat-8; TIRS; thermal infrared sensor; thermal imaging; radiometric calibration ID IN-FLIGHT VALIDATION; LAKE TAHOE; SITE; METHODOLOGY; IMAGER; CA/NV; USA AB Launched in February 2013, the Landsat-8 carries on-board the Thermal Infrared Sensor (TIRS), a two-band thermal pushbroom imager, to maintain the thermal imaging capability of the Landsat program. The TIRS bands are centered at roughly 10.9 and 12 mu m (Bands 10 and 11 respectively). They have 100 m spatial resolution and image coincidently with the Operational Land Imager (OLI), also on-board Landsat-8. The TIRS instrument has an internal calibration system consisting of a variable temperature blackbody and a special viewport with which it can see deep space; a two point calibration can be performed twice an orbit. Immediately after launch, a rigorous vicarious calibration program was started to validate the absolute calibration of the system. The two vicarious calibration teams, NASA/Jet Propulsion Laboratory (JPL) and the Rochester Institute of Technology (RIT), both make use of buoys deployed on large water bodies as the primary monitoring technique. RIT took advantage of cross-calibration opportunity soon after launch when Landsat-8 and Landsat-7 were imaging the same targets within a few minutes of each other to perform a validation of the absolute calibration. Terra MODIS is also being used for regular monitoring of the TIRS absolute calibration. The buoy initial results showed a large error in both bands, 0.29 and 0.51 W/m(2).sr.mu m or -2.1 K and -4.4 K at 300 K in Band 10 and 11 respectively, where TIRS data was too hot. A calibration update was recommended for both bands to correct for a bias error and was implemented on 3 February 2014 in the USGS/EROS processing system, but the residual variability is still larger than desired for both bands (0.12 and 0.2 W/m(2).sr.mu m or 0.87 and 1.67 K at 300 K). Additional work has uncovered the source of the calibration error: out-of-field stray light. While analysis continues to characterize the stray light contribution, the vicarious calibration work proceeds. The additional data have not changed the statistical assessment but indicate that the correction (particularly in band 11) is probably only valid for a subset of data. While the stray light effect is small enough in Band 10 to make the data useful across a wide array of applications, the effect in Band 11 is larger and the vicarious results suggest that Band 11 data should not be used where absolute calibration is required. C1 [Barsi, Julia A.] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. [Schott, John R.; Raqueno, Nina G.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA. [Hook, Simon J.; Radocinski, Robert G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Markham, Brian L.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. RP Barsi, JA (reprint author), NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Code 618, Greenbelt, MD 20771 USA. EM julia.barsi@nasa.gov; schott@cis.rit.edu; hook@jpl.nasa.gov; nina@cis.rit.edu; Brian.L.Markham@nasa.gov; Robert.G.Radocinski@jpl.nasa.gov RI Hook, Simon/D-5920-2016 OI Hook, Simon/0000-0002-0953-6165 FU NASA [NNG09HP18C, NNX11AG70G] FX Science Systems and Applications work was performed under NASA contract NNG09HP18C. The Rochester Institute of Technology work was performed under NASA contract NNX11AG70G. NR 19 TC 30 Z9 34 U1 2 U2 18 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD NOV PY 2014 VL 6 IS 11 BP 11607 EP 11626 DI 10.3390/rs61111607 PG 20 WC Remote Sensing SC Remote Sensing GA AU3RG UT WOS:000345530700060 ER PT J AU Xu, HF Shen, ZS Konishi, H AF Xu, Huifang Shen, Zhizhang Konishi, Hiromi TI Si-magnetite nano-precipitates in silician magnetite from banded iron formation: Z-contrast imaging and ab initio study SO AMERICAN MINERALOGIST LA English DT Article DE Si-magnetite; silician magnetite; banded iron formation; Z-contrast imaging; DFT ID DIFFRACTION; GAMMA-FE2O3; GENERATION; MICROSCOPY; STABILITY; EVOLUTION; DEPOSIT; OXIDES; FLUIDS; MINE AB Si-bearing magnetite or silician magnetite is common in low- and high-temperature rocks. However, details about possible Fe-silicate or Si-Fe-oxide discrete phases/nano-precipitates were not available due to the limitations of conventional high-resolution TEM. Combining Z-contrast imaging and ab initio calculation using density functional theory (DFT) method, we have derived both composition and crystals structure of the discrete nano-precipitates within host magnetite. The nano-precipitates of Si-magnetite with composition of [square Fe-0.5](VI)[Fe3+](SiO4)-Si-VI-O-IV or gamma-Fe1.5SiO4 occur in silician magnetite from a banded iron formation from Western Australia. In the Si-magnetite precipitates, Si replaces Fe3+ in tetrahedral sites of the magnetite structure and vacancies are introduced in the octahedral Fe2+ sites. The Si-magnetite precipitates distribute along {111} of the host magnetite. Widths of the precipitates are even multiples of d(111) of magnetite, such as 2d(111), 4d(111), and 6d(111). Ordering of the vacancies in the Si-magnetite will result in symmetry of P4(3)32, which is a subgroup of Fd (3) over barm for magnetite. Stacking of Si-magnetite and magnetite (111) layers along the [111] direction also occur in magnetite. The nano-precipitates result from exsolution of Si-magnetite from the host silician magnetite at low temperature. The occurrence of the thin nano-precipitates within the magnetite host results from the minimization of interfacial energy between the precipitate and the host magnetite. Relatively high concentrations of aqueous silica and Fe-silicate complex species in pore fluid might enhance the incorporation of Si into the silician magnetite during crystallization of the magnetite. C1 [Xu, Huifang; Shen, Zhizhang; Konishi, Hiromi] Univ Wisconsin, Dept Geosci, NASA Astrobiol Inst, Madison, WI 53706 USA. [Xu, Huifang; Shen, Zhizhang; Konishi, Hiromi] Univ Wisconsin, Mat Sci Program, Madison, WI 53706 USA. RP Xu, HF (reprint author), Univ Wisconsin, Dept Geosci, NASA Astrobiol Inst, 1215 W Dayton St, Madison, WI 53706 USA. EM hfxu@geology.wisc.edu FU NASA Astrobiology Institute [N07-5489]; Major Research Instrumentation (MRI) Program of NSF [DMR-0619368] FX This work is supported by NASA Astrobiology Institute (N07-5489). Authors thank Alex Kivit for helping in STEM analyses, and two anonymous reviewers for helpful comments and suggestions. Authors also thank Major Research Instrumentation (MRI) Program of NSF (DMR-0619368) for funding the aberration-corretced STEM. NR 28 TC 2 Z9 2 U1 0 U2 9 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD NOV-DEC PY 2014 VL 99 IS 11-12 BP 2196 EP 2202 DI 10.2138/am-2014-4964 PG 7 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA AT6OH UT WOS:000345058200007 ER PT J AU Treiman, AH Morris, RV Agresti, DG Graff, TG Achilles, CN Rampe, EB Bristow, TF Ming, DW Blake, DF Vaniman, DT Bish, DL Chipera, SJ Morrison, SM Downs, RT AF Treiman, Allan H. Morris, Richard V. Agresti, David G. Graff, Trevor G. Achilles, Cherie N. Rampe, Elizabeth B. Bristow, Thomas F. Ming, Douglas W. Blake, David F. Vaniman, David T. Bish, David L. Chipera, Steve J. Morrison, Shaunna M. Downs, Robert T. TI Ferrian saponite from the Santa Monica Mountains (California, USA, Earth): Characterization as an analog for clay minerals on Mars with application to Yellowknife Bay in Gale Crater SO AMERICAN MINERALOGIST LA English DT Article DE Saponite; smectite; X-ray diffraction; MSL; Mars; Griffith Park ID IRON CONTENT SAPONITE; AQUEOUS ALTERATION; GARFIELD NONTRONITE; FERROUS SAPONITE; ACID TREATMENT; MOSSBAUER DATA; RICH SAPONITE; RED-SEA; REDUCTION; SMECTITES AB Ferrian saponite from the eastern Santa Monica Mountain, near Griffith Park (Los Angeles, California), was investigated as a mineralogical analog to smectites discovered on Mars by the CheMin X-ray diffraction instrument onboard the Mars Science Laboratory (MSL) rover. The martian clay minerals occur in sediment of basaltic composition and have 02l diffraction bands peaking at 4.59 angstrom, consistent with tri-octahedral smectites. The Griffith saponite occurs in basalts as pseudomorphs after olivine and mesostasis glass and as fillings of vesicles and cracks and has 02l diffraction bands at that same position. We obtained chemical compositions (by electron microprobe), X-ray diffraction patterns with a lab version of the CheMin instrument, Mossbauer spectra, and visible and near-IR reflectance (VNIR) spectra on several samples from that locality. The Griffith saponite is magnesian, Mg/(Mg+Sigma Fe) = 65-70%, lacks tetrahedral Fe3+ and octahedral Al3+, and has Fe3+/Sigma Fe from 64 to 93%. Its chemical composition is consistent with a fully tri-octahedral smectite, but the abundance of Fe3+ gives a nominal excess charge of +1 to +2 per formula unit. The excess charge is likely compensated by substitution of O2- for OH-, causing distortion of octahedral sites as inferred from Mossbauer spectra. We hypothesize that the Griffith saponite was initially deposited with all its iron as Fe2+ and was oxidized later. X-ray diffraction shows a sharp 001 peak at 15 angstrom, 00l peaks, and a 02l diffraction band at the same position (4.59 angstrom) and shape as those of the martian samples, indicating that the martian saponite is not fully oxidized. VNIR spectra of the Griffith saponite show distinct absorptions at 1.40, 1.90, 2.30-2.32, and 2.40 mu m, arising from H2O and hydroxyl groups in various settings. The position of the similar to 2.31 mu m spectral feature varies systematically with the redox state of the octahedrally coordinated Fe. This correlation may permit surface oxidation state to be inferred (in some cases) from VNIR spectra of Mars obtained from orbit, and, in any case, ferrian saponite is a viable assignment for spectral detections in the range 2.30-2.32 mu m. C1 [Treiman, Allan H.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Morris, Richard V.; Rampe, Elizabeth B.; Ming, Douglas W.] NASA, Johnson Space Ctr, ARES Directorate, Houston, TX 77058 USA. [Agresti, David G.] Univ Alabama Birmingham, Dept Phys, Birmingham, AL 35294 USA. [Graff, Trevor G.] Jacobs Engn, Houston, TX 77058 USA. [Achilles, Cherie N.] ESCG UTC Aerosp Syst, Houston, TX 77058 USA. [Achilles, Cherie N.; Bish, David L.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA. [Bristow, Thomas F.; Blake, David F.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. [Vaniman, David T.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Chipera, Steve J.] Chesapeake Energy Corp, Oklahoma City, OK 73118 USA. [Morrison, Shaunna M.; Downs, Robert T.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. RP Treiman, AH (reprint author), Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA. EM Treiman@lpi.usra.edu FU NASA grants through the Mars Science Laboratory Mission FX We are grateful to George Harlow and the American Museum of Natural History (New York) for a sample of the Griffith saponite. Our study was assisted by D.K. Ross (EMP analyses) of Jacobs Engineering, at the Johnson Space Center. We are grateful to the ARES Division, Johnson Space Center for access to the SX-100 microprobe under a cooperative agreement with the LPI. Reviews by M.D. Dyar and J. Bridges were constructive and helpful. This work was supported by NASA grants through the Mars Science Laboratory Mission. LPI Contribution no. 1784. NR 86 TC 16 Z9 16 U1 5 U2 33 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD NOV-DEC PY 2014 VL 99 IS 11-12 BP 2234 EP 2250 DI 10.2138/am-2014-4763 PG 17 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA AT6OH UT WOS:000345058200011 ER PT J AU Righter, K Keller, LP Rahman, Z Christoffersen, R AF Righter, Kevin Keller, Lindsay P. Rahman, Zia Christoffersen, Roy TI Redox-driven exsolution of iron-titanium oxides in magnetite in Miller Range (MIL) 03346 nakhlite: Evidence for post crystallization oxidation in the nakhlite cumulate pile? SO AMERICAN MINERALOGIST LA English DT Article DE Fe-Ti oxide; nakhlite; Mars; oxygen fugacity ID NORTHWEST AFRICA 998; FE-TI OXIDES; MARTIAN METEORITE; OXYGEN FUGACITY; LHERZOLITIC SHERGOTTITES; PETROLOGY; MARS; BASALT; HISTORY; MANTLE AB The Miller Range (MIL) 03346 nakhlite contains similar to 20% mesostasis, which contains skeletal titanomagnetite. The titanomagnetite contains trellis-type {111} lamellae of ilmenite similar to those found in terrestrial titanomagnetites that have experienced subsolidus redox reactions during cooling of their host rocks. We have characterized the MIL 03346 titanomagnetite-ilmenite intergrowths by a combination of focused ion beam (FIB), energy-dispersive spectroscopy (EDX), and high-resolution transmission electron microscopy (TEM). The resulting structural and chemical analyses have been combined with temperature and f(O2) data from previous studies of MIL 03346, as well as previous work on two-oxide thermobarometry of nakhlites. Our calculations show that as MIL 03346 and other nakhlites cooled below 800 degrees C, they recorded increasingly reducing conditions, such that the lowest temperatures calculated correspond to A, conditions as low as 4 log f(O2) units below the FMQ buffer. However, the MIL 03346 lamellae must have formed by oxidation and thus record a very late stage low-temperature (<350 degrees C) oxidation event. When considered together with previous studies of MIL 03346 and nakhlites in general, the overall cooling history could be explained by early oxidation followed by intermediate stage reduction caused by S-2 loss by degassing, followed by late loss of Cl by degassing. C1 [Righter, Kevin] NASA, JSC, Mailcode KT, Houston, TX 77058 USA. [Keller, Lindsay P.] NASA, JSC, Mailcode KR, Houston, TX 77058 USA. [Rahman, Zia; Christoffersen, Roy] ESCG Jacobs, Houston, TX USA. RP Righter, K (reprint author), NASA, JSC, Mailcode KT, 2101 NASA Pkwy, Houston, TX 77058 USA. EM kevin.righter-1@nasa.gov FU RTOP from the Mars Fundamental Research program at NASA FX This research was supported by an RTOP to K.R. from the Mars Fundamental Research program at NASA. We thank the Meteorite Working Group for allowing the use of the thin section (,106) in this study. We also thank Associate Editor S. Simon for his comments and reviewers J. Karner and C. Herd for their reviews, all of which helped clarify the presentation of this information. NR 42 TC 3 Z9 3 U1 2 U2 9 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD NOV-DEC PY 2014 VL 99 IS 11-12 BP 2313 EP 2319 DI 10.2138/am-2014-4926 PG 7 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA AT6OH UT WOS:000345058200018 ER PT J AU Hickman, JE Scholes, RJ Rosenstock, TS Garcia-Pando, CP Nyamangara, J AF Hickman, Jonathan E. Scholes, Robert J. Rosenstock, Todd S. Garcia-Pando, C. Perez Nyamangara, Justice TI Assessing non-CO2 climate-forcing emissions and mitigation in sub-Saharan Africa SO CURRENT OPINION IN ENVIRONMENTAL SUSTAINABILITY LA English DT Article ID CARBON SEQUESTRATION; CONSERVATION AGRICULTURE; AGRONOMIC ASSESSMENT; GREEN REVOLUTION; N2O EMISSIONS; GAS EMISSIONS; FIRE REGIMES; LAND-USE; DUST; METHANE AB There are few direct measurements of anthropogenic climate-forcing emissions in Africa, making it difficult to accurately assess current emissions and to anticipate changes in future emissions. Emissions databases suggest that sub-Saharan Africa (SSA), home to less than 15% of the world's population, is responsible for 11% of anthropogenic methane (CH4) and 18% of anthropogenic nitrous oxide (N2O) emissions globally, though this includes substantial emissions from biomass burning that would occur in the absence of contemporary anthropogenic activity, and which may be over-estimated. SSA is also an important source of precursors to the greenhouse gas tropospheric ozone, and of mineral dust, which has a range of impacts on climate. Eliminating food insecurity and poverty is likely to take priority over greenhouse gas mitigation in the region, so innovations in mitigation must focus on ways to reduce emissions as an ancillary benefit of improving livelihoods. C1 [Hickman, Jonathan E.] Columbia Univ, Earth Inst, Agr & Food Secur Ctr, Palisades, NY 10964 USA. [Scholes, Robert J.] CSIR, Pretoria, South Africa. [Rosenstock, Todd S.] World Agroforestry Ctr, Nairobi, Kenya. [Garcia-Pando, C. Perez] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Garcia-Pando, C. Perez] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. [Nyamangara, Justice] Int Crops Res Inst Semi Arid Trop, Matopos Res Stn, Bulawayo, Zimbabwe. RP Hickman, JE (reprint author), Columbia Univ, Earth Inst, Agr & Food Secur Ctr, Palisades, NY 10964 USA. EM jeh2179@columbia.edu OI Perez Garcia-Pando, Carlos/0000-0002-4456-0697 FU Earth SystemModeling Program of the Department of Energy [DE-SC0006713] FX Carlos Perez Garcia-Pando acknowledges the NASA Modeling, Analysis and Prediction Program and the Earth SystemModeling Program of the Department of Energy, Project DE-SC0006713. NR 66 TC 4 Z9 4 U1 1 U2 20 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1877-3435 EI 1877-3443 J9 CURR OPIN ENV SUST JI Curr. Opin. Environ. Sustain. PD NOV PY 2014 VL 9-10 SI SI BP 65 EP 72 DI 10.1016/j.cosust.2014.07.010 PG 8 WC GREEN & SUSTAINABLE SCIENCE & TECHNOLOGY; Environmental Sciences SC Science & Technology - Other Topics; Environmental Sciences & Ecology GA AT9EJ UT WOS:000345230500008 ER PT J AU Siddique-E-Akbor, AHM Hossain, F Sikder, S Shum, CK Tseng, S Yi, YC Turk, FJ Limaye, A AF Siddique-E-Akbor, A. H. M. Hossain, Faisal Sikder, Safat Shum, C. K. Tseng, Steven Yi, Yuchan Turk, F. J. Limaye, Ashutosh TI Satellite Precipitation Data-Driven Hydrological Modeling for Water Resources Management in the Ganges, Brahmaputra, and Meghna Basins SO EARTH INTERACTIONS LA English DT Article DE Precipitation; Hydrologic models; Land surface model; Model evaluation/performance ID INTERNATIONAL RIVER-BASINS; PREDICTABILITY; PRODUCTS; CAPACITY; NETWORK; MISSION; SYSTEMS; IMAGERY; FLUXES; FLOOD AB The Ganges-Brahmaputra-Meghna (GBM) river basins exhibit extremes in surface water availability at seasonal to annual time scales. However, because of a lack of basinwide hydrological data from in situ platforms, whether they are real time or historical, water management has been quite challenging for the 630 million inhabitants. Under such circumstances, a large-scale and spatially distributed hydrological model, forced with more widely available satellite meteorological data, can be useful for generating high resolution basinwide hydrological state variable data [streamflow, runoff, and evapotranspiration (ET)] and for decision making on water management. The Variable Infiltration Capacity (VIC) hydrological model was therefore set up for the entire GBM basin at spatial scales ranging from 12.5 to 25 km to generate daily fluxes of surface water availability (runoff and streamflow). Results indicate that, with the selection of representative gridcell size and application of correction factors to evapotranspiration calculation, it is possible to significantly improve streamflow simulation and overcome some of the insufficient sampling and data quality issues in the ungauged basins. Assessment of skill of satellite precipitation forcing datasets revealed that the Tropical Rainfall Measuring Mission (TRMM) Multisatellite Precipitation Analysis (TMPA) product of 3B42RT fared comparatively better than the Climate Prediction Center (CPC) morphing technique (CMORPH) product for simulation of streamflow. The general conclusion that emerges from this study is that spatially distributed hydrologic modeling for water management is feasible for the GBM basins under the scenario of inadequate in situ data availability. Satellite precipitation forcing datasets provide the necessary skill for water balance studies at interannual and interseasonal scales. However, further improvement in skill may be required if these datasets are to be used for flood management at daily to weekly time scales and within a data assimilation framework. C1 [Siddique-E-Akbor, A. H. M.] Tennessee Technol Univ, Cookeville, TN 38505 USA. [Hossain, Faisal; Sikder, Safat] Univ Washington, Seattle, WA 98195 USA. [Shum, C. K.; Tseng, Steven; Yi, Yuchan] Ohio State Univ, Columbus, OH 43210 USA. [Turk, F. J.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA USA. [Limaye, Ashutosh] NASA, Marshall Space Flight Ctr, Redstone Arsenal, AL USA. RP Hossain, F (reprint author), Univ Washington, Dept Civil & Environm Engn, Seattle, WA 98195 USA. EM fhossain@uw.edu FU NASA SERVIR program [NNX12AM85AG]; Ivanhoe Foundation; NASA's SERVIR Program; OSU's Climate, Water and Carbon Program; Chinese Academy of Sciences/SAFEA International Partnership Program for Creative Research Teams [KZZD-EW-TZ-05]; International Center for Integrated Mountain Development (ICIMOD) in Nepal FX Support for this study was provided by the NASA SERVIR program (NNX12AM85AG). Partial support from the Ivanhoe Foundation (to Safat Sikder) is acknowledged. The Ohio State University (OSU) component of the research was partially supported by grants from NASA's SERVIR Program; by OSU's Climate, Water and Carbon Program; and by the Chinese Academy of Sciences/SAFEA International Partnership Program for Creative Research Teams (KZZD-EW-TZ-05). We gratefully acknowledge the tremendous support from the staff of NASA's SERVIR program and the International Center for Integrated Mountain Development (ICIMOD) in Nepal. NR 46 TC 12 Z9 12 U1 5 U2 36 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1087-3562 J9 EARTH INTERACT JI Earth Interact. PD NOV PY 2014 VL 18 AR 17 DI 10.1175/EI-D-14-0017.1 PG 25 WC Geosciences, Multidisciplinary SC Geology GA AT7NK UT WOS:000345124300001 ER PT J AU Pederson, N Dyer, JM McEwan, RW Hessl, AE Mock, CJ Orwig, DA Rieder, HE Cook, BI AF Pederson, Neil Dyer, James M. McEwan, Ryan W. Hessl, Amy E. Mock, Cary J. Orwig, David A. Rieder, Harald E. Cook, Benjamin I. TI The legacy of episodic climatic events in shaping temperate, broadleaf forests SO ECOLOGICAL MONOGRAPHS LA English DT Article DE closed-canopy forests; deciduous forests; disturbance; drought; frost; gap dynamics; historical documents; mesoscale dynamics; tree-ring analysis ID EASTERN NORTH-AMERICA; HEMLOCK-HARDWOOD FORESTS; WESTERN UNITED-STATES; OLD-GROWTH FORESTS; GREAT-LAKES REGION; TREE MORTALITY; FIRE HISTORY; NEW-ENGLAND; DISTURBANCE HISTORY; NATURAL DISTURBANCE AB In humid, broadleaf-dominated forests where gap dynamics and partial canopy mortality appears to dominate the disturbance regime at local scales, paleoecological evidence shows alteration at regional-scales associated with climatic change. Yet, little evidence of these broad-scale events exists in extant forests. To evaluate the potential for the occurrence of large-scale disturbance, we used 76 tree-ring collections spanning approximate to 840000 km(2) and 5327 tree recruitment dates spanning approximate to 1.4 million km(2) across the humid eastern United States. Rotated principal component analysis indicated a common growth pattern of a simultaneous reduction in competition in 22 populations across 61000 km(2). Growth-release analysis of these populations reveals an intense and coherent canopy disturbance from 1775 to 1780, peaking in 1776. The resulting time series of canopy disturbance is so poorly described by a Gaussian distribution that it can be described as heavy tailed, with most of the years from 1775 to 1780 comprising the heavy-tail portion of the distribution. Historical documents provide no evidence that hurricanes or ice storms triggered the 1775-1780 event. Instead, we identify a significant relationship between prior drought and years with elevated rates of disturbance with an intense drought occurring from 1772 to 1775. We further find that years with high rates of canopy disturbance have a propensity to create larger canopy gaps indicating repeated opportunities for rapid change in species composition beyond the landscape scale. Evidence of elevated, regional-scale disturbance reveals how rare events can potentially alter system trajectory: a substantial portion of old-growth forests examined here originated or were substantially altered more than two centuries ago following events lasting just a few years. Our recruitment data, comprised of at least 21 species and several shade-intolerant species, document a pulse of tree recruitment at the subcontinental scale during the late-1600s suggesting that this event was severe enough to open large canopy gaps. These disturbances and their climatic drivers support the hypothesis that punctuated, episodic, climatic events impart a legacy in broadleaf-dominated forests centuries after their occurrence. Given projections of future drought, these results also reveal the potential for abrupt, meso- to large-scale forest change in broadleaf-dominated forests over future decades. C1 [Pederson, Neil] Columbia Univ, Lamont Doherty Geol Observ, Tree Ring Lab, Palisades, NY 10964 USA. [Pederson, Neil] Columbia Univ, Palisades, NY 10964 USA. [Dyer, James M.] Ohio Univ, Dept Geog, Athens, OH 45701 USA. [McEwan, Ryan W.] Univ Dayton, Dept Biol, Dayton, OH 45469 USA. [Hessl, Amy E.] Univ Virginia, Dept Geol & Geog, Morgantown, WV 26506 USA. [Mock, Cary J.] Univ S Carolina, Dept Geog, Columbia, SC 29208 USA. [Orwig, David A.] Harvard Univ, Harvard Forest, Petersham, MA 01366 USA. [Rieder, Harald E.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Rieder, Harald E.] Columbia Univ, Dept Appl Phys & Appl Math, Palisades, NY 10964 USA. [Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Pederson, N (reprint author), Harvard Univ, Harvard Forest, Petersham, MA 01366 USA. EM adk@ldeo.columbia.edu RI Cook, Benjamin/H-2265-2012; OI Rieder, Harald/0000-0003-2705-0801 FU U.S. Department of Energy's Global Change Education Program; Kentucky State Nature Preserve Commission's Small Grant Program; Kentucky Academy of Sciences; Eastern Kentucky University's University Research Committee; Kentucky Natural History Society; Harvard Forest Long-Term Ecological Research Program [DEB-12-37491]; Harvard University; Ohio University FX Many thanks to funding agencies that contributed to the collection of some of the data used here including the U.S. Department of Energy's Global Change Education Program, the Kentucky State Nature Preserve Commission's Small Grant Program, Kentucky Academy of Sciences, Eastern Kentucky University's University Research Committee, and the Kentucky Natural History Society. Thank you to the multiple state, federal, and private organizations for permitting the coring of trees on their properties. Thanks to those who graciously provided or assisted with the collection of tree recruitment data, including C. Baisan, B. Black, A. D'Amato, L. Frelich, T. Knight, S. McClung, E. Moore, A. Savage, M. Stambaugh, and G. Wiles. Thanks to J. Kaplan and the ARVE Group for deriving a land-use map for use here covering eastern North America from 1450 to 1700. Much thanks to those who provided feedback, additional analysis, or quality control of some data that improved the manuscript, including C. Allen, S. Frank, A. C. Gonzalez, C. Leland, D. Martin-Benito, K. Ross, N. Ross, J. Testani, J. M. Varner, and two anonymous reviewers. Additional funding was provided by the Harvard Forest Long-Term Ecological Research Program (DEB-12-37491), Harvard University, and Ohio University. Lamont Contribution 7761. NR 192 TC 32 Z9 32 U1 10 U2 63 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9615 EI 1557-7015 J9 ECOL MONOGR JI Ecol. Monogr. PD NOV PY 2014 VL 84 IS 4 BP 599 EP 620 DI 10.1890/13-1025.1 PG 22 WC Ecology SC Environmental Sciences & Ecology GA AT4PU UT WOS:000344923500004 ER PT J AU Dutton, PH Jensen, MP Frey, A LaCasella, E Balazs, GH Zarate, P Chassin-Noria, O Sarti-Martinez, AL Velez, E AF Dutton, Peter H. Jensen, Michael P. Frey, Amy LaCasella, Erin Balazs, George H. Zarate, Patricia Chassin-Noria, Omar Laura Sarti-Martinez, Adriana Velez, Elizabeth TI Population structure and phylogeography reveal pathways of colonization by a migratory marine reptile (Chelonia mydas) in the central and eastern Pacific SO ECOLOGY AND EVOLUTION LA English DT Article DE Chelonia mydas; genetic stock structure; marine turtles; mtDNA; phylogeography ID TURTLES DERMOCHELYS-CORIACEA; GALAPAGOS GREEN TURTLES; MITOCHONDRIAL-DNA; STOCK STRUCTURE; GENE FLOW; GLOBAL PHYLOGEOGRAPHY; NESTING POPULATIONS; TROPICAL PACIFIC; SEA-TURTLES; CONNECTIVITY AB Climate, behavior, ecology, and oceanography shape patterns of biodiversity in marine faunas in the absence of obvious geographic barriers. Marine turtles are an example of highly migratory creatures with deep evolutionary lineages and complex life histories that span both terrestrial and marine environments. Previous studies have focused on the deep isolation of evolutionary lineages (>3 mya) through vicariance; however, little attention has been given to the pathways of colonization of the eastern Pacific and the processes that have shaped diversity within the most recent evolutionary time. We sequenced 770 bp of the mtDNA control region to examine the stock structure and phylogeography of 545 green turtles from eight different rookeries in the central and eastern Pacific. We found significant differentiation between the geographically separated nesting populations and identified five distinct stocks (F-ST=0.08-0.44, P<0.005). Central and eastern Pacific Chelonia mydas form a monophyletic group containing 3 subclades, with Hawaii more closely related to the eastern Pacific than western Pacific populations. The split between sampled central/eastern and western Pacific haplotypes was estimated at around 0.34 mya, suggesting that the Pacific region west of Hawaii has been a more formidable barrier to gene flow in C. mydas than the East Pacific Barrier. Our results suggest that the eastern Pacific was colonized from the western Pacific via the Central North Pacific and that the Revillagigedos Islands provided a stepping-stone for radiation of green turtles from the Hawaiian Archipelago to the eastern Pacific. Our results fit with a broader paradigm that has been described for marine biodiversity, where oceanic islands, such as Hawaii and Revillagigedo, rather than being peripheral evolutionary graveyards, serve as sources and recipients of diversity and provide a mechanism for further radiation. C1 [Dutton, Peter H.; Jensen, Michael P.; Frey, Amy; LaCasella, Erin] NOAA, Marine Mammal & Turtle Div, Southwest Fisheries Sci Ctr, Natl Marine Fisheries Serv, La Jolla, CA 92037 USA. [Balazs, George H.] NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96818 USA. [Zarate, Patricia] Univ Florida, Archie Carr Ctr Sea Turtle Res, Gainesville, FL 32611 USA. [Zarate, Patricia] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Chassin-Noria, Omar] Ctr Multidisciplinario Estudios Biotecnol UMSNH, Fac Biol, Morelia 58030, Michoacan, Mexico. [Laura Sarti-Martinez, Adriana] CONANP, Direcc Especies Prioritarias Conservac, Mexico City 14210, DF, Mexico. [Velez, Elizabeth] Kelonian Conservat Soc, Heredia, Costa Rica. RP Dutton, PH (reprint author), NOAA, Marine Mammal & Turtle Div, Southwest Fisheries Sci Ctr, Natl Marine Fisheries Serv, 8901 La Jolla Shores Dr, La Jolla, CA 92037 USA. EM peter.dutton@noaa.gov NR 80 TC 6 Z9 6 U1 6 U2 56 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD NOV PY 2014 VL 4 IS 22 BP 4317 EP 4331 DI 10.1002/ece3.1269 PG 15 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA AU0MD UT WOS:000345316200011 PM 25540693 ER PT J AU Wolkovich, EM Cook, BI McLauchlan, KK Davies, TJ AF Wolkovich, E. M. Cook, B. I. McLauchlan, K. K. Davies, T. J. TI Temporal ecology in the Anthropocene SO ECOLOGY LETTERS LA English DT Article DE Autocorrelation; climate change; ecological forecasting; events; non-stationarity; scaling; spatial ecology; temporal ecology ID CLIMATE-CHANGE; POPULATION-DYNAMICS; SPECIES INTERACTIONS; REGIME SHIFTS; GLACIER BAY; PHENOLOGY; VARIABILITY; GRASSLAND; PATTERNS; DROUGHT AB Two fundamental axes - space and time - shape ecological systems. Over the last 30 years spatial ecology has developed as an integrative, multidisciplinary science that has improved our understanding of the ecological consequences of habitat fragmentation and loss. We argue that accelerating climate change - the effective manipulation of time by humans - has generated a current need to build an equivalent framework for temporal ecology. Climate change has at once pressed ecologists to understand and predict ecological dynamics in non-stationary environments, while also challenged fundamental assumptions of many concepts, models and approaches. However, similarities between space and time, especially related issues of scaling, provide an outline for improving ecological models and forecasting of temporal dynamics, while the unique attributes of time, particularly its emphasis on events and its singular direction, highlight where new approaches are needed. We emphasise how a renewed, interdisciplinary focus on time would coalesce related concepts, help develop new theories and methods and guide further data collection. The next challenge will be to unite predictive frameworks from spatial and temporal ecology to build robust forecasts of when and where environmental change will pose the largest threats to species and ecosystems, as well as identifying the best opportunities for conservation. C1 [Wolkovich, E. M.] Arnold Arboretum, Boston, MA 02130 USA. [Wolkovich, E. M.] Univ British Columbia, Biodivers Res Ctr, Vancouver, BC V5Z 1M9, Canada. [Cook, B. I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Cook, B. I.] Lamont Doherty Earth Observ, Palisades, NY USA. [McLauchlan, K. K.] Kansas State Univ, Dept Geog, Manhattan, KS 66506 USA. [McLauchlan, K. K.] Univ Oxford Merton Coll, Oxford OX1 4JD, England. [Davies, T. J.] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Davies, T. J.] Univ Johannesburg, African Ctr DNA Barcoding, Johannesburg, South Africa. RP Wolkovich, EM (reprint author), Arnold Arboretum, Boston, MA 02130 USA. EM lizzie@oeb.harvard.edu RI Cook, Benjamin/H-2265-2012 FU NSERC CREATE training program in biodiversity research FX We thank D. Bolger, J. Losos, M. O'Connor, N. Pederson and D. Schluter for comments and conversations, and M. Donohue and S. Brewer for conversations, that improved this manuscript. Comments from editor Franck Courchamp and two anonymous reviewers also greatly improved this manuscript. EMW was supported in part by the NSERC CREATE training program in biodiversity research. NR 80 TC 28 Z9 28 U1 13 U2 90 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1461-023X EI 1461-0248 J9 ECOL LETT JI Ecol. Lett. PD NOV PY 2014 VL 17 IS 11 BP 1365 EP 1379 DI 10.1111/ele.12353 PG 15 WC Ecology SC Environmental Sciences & Ecology GA AT8YX UT WOS:000345215900003 PM 25199649 ER PT J AU Graham, HV Patzkowsky, ME Wing, SL Parker, GG Fogel, ML Freeman, KH AF Graham, Heather V. Patzkowsky, Mark E. Wing, Scott L. Parker, Geoffrey G. Fogel, Marilyn L. Freeman, Katherine H. TI Isotopic characteristics of canopies in simulated leaf assemblages SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID TROPICAL RAIN-FOREST; SOIL ORGANIC-CARBON; DECIDUOUS FOREST; CHEMICAL-COMPOSITION; C-13/C-12 RATIOS; VERTICAL PROFILE; STABLE-ISOTOPES; AMAZON BASIN; 50-HA PLOTS; SEED SIZE AB The geologic history of closed-canopy forests is of great interest to paleoecologists and paleoclimatologists alike. Closed canopies have pronounced effects on local, continental and global rainfall and temperature patterns. Although evidence for canopy closure is difficult to reconstruct from the fossil record, the characteristic isotope gradients of the "canopy effect" could be preserved in leaves and proxy biomarkers. To assess this, we employed new carbon isotopic data for leaves collected in diverse light environments within a deciduous, temperate forest (Maryland, USA) and for leaves from a perennially closed canopy, moist tropical forest (Bosque Protector San Lorenzo, Panama). In the tropical forest, leaf carbon isotope values range 10 parts per thousand, with higher delta C-13(leaf) values occurring both in upper reaches of the canopy, and with higher light exposure and lower humidity. Leaf fractionation (Delta(leaf)) varied negatively with height and light and positively with humidity. Vertical C-13 enrichment in leaves largely reflects changes in Delta(leaf), and does not trend with delta C-13 of CO2 within the canopy. At the site in Maryland, leaves express a more modest delta C-13 range (similar to 6 parts per thousand), with a clear trend that follows both light and leaf height. Using a model we simulate leaf assemblage isotope patterns from canopy data binned by elevation. The re-sampling (bootstrap) model determined both the mean and range of carbon isotope values for simulated leaf assemblages ranging in size from 10 to over 1000 leaves. For the tropical forest data, the canopy's isotope range is captured with 50 or more randomly sampled leaves. Thus, with a sufficient number of fossil leaves it is possible to distinguish isotopic gradients in an ancient closed canopy forest from those in an open forest. For very large leaf assemblages, mean isotopic values approximate the delta C-13 of carbon contributed by leaves to soil and are similar to observed delta C-13(litter) values at forested sites within Panama, including the site where leaves were sampled. The model predicts a persistent similar to 1 parts per thousand difference in delta C-13(litter) for the two sites which is consistent with higher water availability in the tropical forests. This work provides a new framework for linking contemporary ecological observations to the geochemical record using flux-weighted isotope data and lends insights to the effect of forest architecture on organic and isotopic records of ancient terrestrial ecosystems. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Graham, Heather V.; Patzkowsky, Mark E.; Freeman, Katherine H.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Wing, Scott L.] Smithsonian Inst, Dept Paleobiol, NHB121, Washington, DC 20013 USA. [Parker, Geoffrey G.] Smithsonian Environm Res Ctr, Forest Ecol Lab, Edgewater, MD 21037 USA. [Fogel, Marilyn L.] Univ Calif Merced, Dept Life & Environm Sci, Merced, CA 95343 USA. RP Graham, HV (reprint author), NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Greenbelt, MD 20771 USA. EM heather.v.graham@nasa.gov RI Freeman, Katherine/H-5140-2011; OI Freeman, Katherine/0000-0002-3350-7671; Wing, Scott/0000-0002-2954-8905; Parker, Geoffrey/0000-0001-7055-6491 NR 111 TC 14 Z9 14 U1 2 U2 21 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD NOV 1 PY 2014 VL 144 BP 82 EP 95 DI 10.1016/j.gca.2014.08.032 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AT4XM UT WOS:000344945600006 ER PT J AU Joswiak, DJ Nakashima, D Brownlee, DE Matrajt, G Ushikubo, T Kita, NT Messenger, S Ito, M AF Joswiak, D. J. Nakashima, D. Brownlee, D. E. Matrajt, G. Ushikubo, T. Kita, N. T. Messenger, S. Ito, M. TI Terminal particle from Stardust track 130: Probable Al-rich chondrule fragment from comet Wild 2 SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID UNEQUILIBRATED ORDINARY CHONDRITES; INTERPLANETARY DUST PARTICLES; MICROCHONDRULE-BEARING CLAST; OXYGEN-ISOTOPE SYSTEMATICS; CH CARBONACEOUS CHONDRITES; EARLY SOLAR-SYSTEM; FERROMAGNESIAN CHONDRULES; AL-26-MG-26 SYSTEMATICS; ION MICROPROBE; FEO-RICH AB A 4 x 6 mu m terminal particle from Stardust track 130, named Bidi, is composed of a refractory assemblage of Fo(97) olivine, Al- and Ti-bearing clinopyroxene and anorthite feldspar (An(97)). Mineralogically, Bidi resembles a number of components found in primitive chondritic meteorites including Al-rich chondrules, plagioclase-bearing type I ferromagnesian chondrules and amoeboid olivine aggregates (AOAs). Measured widths of augite/pigeonite lamellae in the clinopyroxene indicate fast cooling rates suggesting that Bidi is more likely to be a chondrule fragment than an AOA. Bulk element concentrations, including an Al2O3 content of 10.2 wt%, further suggests that Bidi is more akin to Al-rich rather than ferromagnesian chondrules. This is supported by high anorthite content of the plagioclase feldspar, overall bulk composition and petrogenetic analysis using a cosmochemical Al2O3-Ca2SiO4-Mg2SiO4 phase diagram. Measured minor element abundances of individual minerals in Bidi generally support an Al-rich chondrule origin but are not definitive between any of the object types. Oxygen isotope ratios obtained from olivine (+minor high-Ca pyroxene) fall between the TF and CCAM lines and overlap similar minerals from chondrules in primitive chondrites but are generally distinct from pristine AOA minerals. Oxygen isotope ratios are similar to some minerals from both Al-rich and type I ferromagnesian chondrules in unequilibrated carbonaceous, enstatite and ordinary chondrites. Although no single piece of evidence uniquely identifies Bidi as a particular object type, the preponderance of data, including mineral assemblage, bulk composition, mineral chemistry, inferred cooling rates and oxygen isotope ratios, suggest that Bidi is more closely matched to Al-rich chondrules than AOAs or plagioclase-bearing type I ferromagnesian chondrules and likely originated in a chondrule-forming region in the inner solar system. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Joswiak, D. J.; Brownlee, D. E.; Matrajt, G.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Nakashima, D.; Ushikubo, T.; Kita, N. T.] Tohoku Univ, Grad Sch Sci, Div Earth & Planetary Mat Sci, Lab Early Solar Syst Evolut, Sendai, Miyagi 9808578, Japan. [Messenger, S.] ARES, Johnson Space Ctr, Robert M Walker Lab Space Sci, Houston, TX 77058 USA. [Ito, M.] JAMSTEC, Kochi Inst Core Sample Res, Nankoku Ku, Kochi 7838502, Japan. RP Joswiak, DJ (reprint author), Univ Washington, Dept Astron, Seattle, WA 98195 USA. EM joswiak@astro.washington.edu RI Kita, Noriko/H-8035-2016 OI Kita, Noriko/0000-0002-0204-0765 FU NASA [NNX10AI89GS01, NNX09AC30G]; NSF-EAR [0319230, 0516725, 0744079, 1053466] FX We wish to thank the Discovery and Cosmochemistry programs at NASA for support of the Stardust mission, funding of instrumentation and sample procurement. Special thanks to Hanson Fong of the Materials Science and Engineering Department, University of Washington, for FESEM assistance with obtaining backscatter images. We thank Trevor Ireland and two additional reviewers for constructive comments which improved the manuscript. This work was supported by NASA Grants NNX10AI89GS01 and NNX09AC30G. The WiscSIMS lab is partially funded by NSF-EAR (0319230, 0516725, 0744079, 1053466). NR 105 TC 4 Z9 4 U1 1 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD NOV 1 PY 2014 VL 144 BP 277 EP 298 DI 10.1016/j.gca.2014.08.017 PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AT4XM UT WOS:000344945600017 ER PT J AU Joy, KH Nemchin, A Grange, M Lapen, TJ Peslier, AH Ross, DK Zolensky, ME Kring, DA AF Joy, K. H. Nemchin, A. Grange, M. Lapen, T. J. Peslier, A. H. Ross, D. K. Zolensky, M. E. Kring, D. A. TI Petrography, geochronology and source terrain characteristics of lunar meteorites Dhofar 925, 961 and Sayh al Uhaymir 449 SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID POLE-AITKEN BASIN; MARE-BASALT METEORITE; IMPACT-MELT BRECCIAS; U-PB; BOMBARDMENT HISTORY; ELECTRON-MICROPROBE; REGOLITH BRECCIAS; APOLLO 14; ICP-MS; CRUST AB Dhofar (Dho) 925, 961 and Sayh al Uhaymir (SaU) 449 are brecciated lunar meteorites consisting of mineral fragments and clasts from a range of precursor lithologies including magnesian anorthositic gabbronorite granulites; crystalline impact melt breccias; clast-bearing glassy impact melt breccias; lithic (fragmental) breccias; mare basalts; and evolved (silica-rich) rocks. On the similarity of clast type and mineral chemistry the samples are likely grouped, and were part of the same parent meteorite. Phosphate Pb-Pb ages in impact melt breccias and matrix grains demonstrate that Dho 961 records geological events spanning similar to 500 Ma between 4.35 and 3.89 Ga. These Pb-Pb ages are similar to the ages of 'ancient' intrusive magmatic samples and impact basin melt products collected on the lunar nearside by the Apollo missions. However, the samples' bulk rock composition is chemically distinct from these types of samples, and it has been suggested that they may have originated from the farside South Pole-Aitken impact basin (i.e., Jolliff et al., 2008). We test this hypothesis, and conclude that although it is possible that the samples may be from the South Pole-Aitken basin, there are other regions on the Moon that may have also sourced these complex breccias. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Joy, K. H.; Kring, D. A.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Joy, K. H.; Zolensky, M. E.; Kring, D. A.] NASA, Lunar Sci Inst, Washington, DC USA. [Nemchin, A.; Grange, M.] Curtin Univ Technol, Perth, WA 6845, Australia. [Nemchin, A.] Swedish Museum Nat Hist, S-10405 Stockholm, Sweden. [Lapen, T. J.] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77004 USA. [Peslier, A. H.; Ross, D. K.] JETS, Jacobs Technol, Houston, TX 77058 USA. [Peslier, A. H.; Ross, D. K.; Zolensky, M. E.] NASA, Johnson Space Ctr, Astromat Res & Explorat Sci, Houston, TX 77058 USA. RP Joy, KH (reprint author), Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA. EM katherine.joy@manchester.ac.uk OI Joy, Katherine/0000-0003-4992-8750; Grange, Marion/0000-0001-6405-8795 FU NASA Lunar Science Institute [NNA09DB33A]; Leverhulme Trust, UK [2011-569] FX This research was funded by NASA Lunar Science Institute contract NNA09DB33A, David A. Kring PI. KHJ acknowledges funding from the Leverhulme Trust, UK (grant 2011-569). We thank David Mann for sample preparation. We acknowledge the resources of Dr. Randy Korotev's Lunar Meteorite List, and NASA's Apollo and Lunar Meteorite sample compendium. We thank Drs. Axel Wittmann, Tomoko Arai and Romain Tartese for thoughtful reviews, and Dr. Marc Norman for his AE handling and suggestions which greatly improved this paper. This is LPI contribution number 1805. NR 132 TC 3 Z9 4 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD NOV 1 PY 2014 VL 144 BP 299 EP 325 DI 10.1016/j.gca.2014.08.013 PG 27 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AT4XM UT WOS:000344945600018 ER PT J AU Pernet-Fisher, JF Howarth, GH Liu, Y Chen, Y Taylor, LA AF Pernet-Fisher, J. F. Howarth, G. H. Liu, Y. Chen, Y. Taylor, L. A. TI Estimating the lunar mantle water budget from phosphates: Complications associated with silicate-liquid-immiscibility SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID VOLATILE ABUNDANCES; MELT INCLUSIONS; APATITE; MOON; MAGMAS; HYDROGEN; BASALTS; ROCKS; DIFFERENTIATION; WHITLOCKITE AB The discovery of water within the lunar mantle has broad implications for the formation of the Earth-Moon system, differentiation of the Moon, and the magmatic evolution of lunar basalts, as well as the highland rocks. Recently, there has been considerable interest in using combined water abundances and H-isotope systematics of lunar apatites from mare basalts to quantify the origin and extent of water within the Moon's mantle. However, the petrologic and geochemical conditions that govern apatite crystallization are not well-constrained, especially for high-FeO basaltic melts that crystallize at fO(2) values below the iron-wustite buffer. Apatites are typically located within the late-stage interstitial regions. In this contribution, we present detailed textural descriptions of late-stage inter-cumulus, residual-liquid pockets (i.e., mesostasis pockets), in order to understand the petrogenesis of lunar apatite. Results from five mare basalts demonstrate that the majority of the residual liquids in mesostasis regions have undergone silicate-liquid immiscibility (SLI) splitting into Si-K-rich (felsic) and Fe-rich (Fe-basaltic) conjugate liquids. We demonstrate the complexity of these residual liquids by documenting a wide range of water contents for apatites in several mesostasis pockets within a single mare basalt, a complexity common to many basalts. These data illustrate that individual apatite-hosting mesostasis pockets behave as independent sub-systems, even within a single rock. Furthermore, we present water concentrations for another phosphate phase, merrillite, indicating additional uncertainties during considerations of water partitioning into apatite. Fractional crystallization trends have been used in order to assess the conditions under which magmas are likely to undergo SLI. Predicted liquid lines of descent indicate that it is the late-stage residual liquids of lunar basalts with relatively low-Mg# (e. g., similar to 50) may not intersect the two-liquid field depending upon the fractionation trends in the late-stage mesostasis pockets. For samples that undergo SLI, the apatite/melt-partition coefficients required for back-calculating water abundances of the parental melts are compromised by the generation of two populations of apatites-merrillites from conjugate immiscible liquids. This process highlights an important complexity inherent to all water back-calculations that use apatite, as this requires an additional set of partition coefficients. We emphasize that the complex petrologic nature and common development of SLI of apatite-bearing, late-stage mesostasis pockets have not been considered in published apatite-volatile data. These factors, in additional to other considerations, illustrate why water back-calculations to model the primary melts from such data must be viewed with caution. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Pernet-Fisher, J. F.; Howarth, G. H.; Liu, Y.; Taylor, L. A.] Univ Tennessee, Planetary Geosci Inst, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Liu, Y.; Chen, Y.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Pernet-Fisher, JF (reprint author), Univ Tennessee, Planetary Geosci Inst, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. EM jpf@utk.edu OI Chen, Yang/0000-0003-4729-3499 FU NASA [NNX11AG58G]; Planetary Geosciences Institute at UT; JPL; NASA FX This paper has received considerable input and encouragement from many of our planetary colleagues, for which we are collectively grateful. In particular, we wish to thank Romain Tartese, Malcolm Rutherford, and one anonymous reviewer for their helpful comments and suggestions. We also wish to thank Allan Patchen, who provided assistance with the EMP analyses, and Yunbin Guan for his guidance of SIMS analysis. This work was supported by NASA Cosmochemistry Grant to L. A. T. (NNX11AG58G) and funds from the Planetary Geosciences Institute at UT. Y.L. and Y.C. are supported by funds at JPL, which is managed by California Institute of Technology under a contract with NASA. Finally we are grateful to Marc Norman for the editorial handing of this paper. NR 75 TC 8 Z9 8 U1 2 U2 19 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD NOV 1 PY 2014 VL 144 BP 326 EP 341 DI 10.1016/j.gca.2014.09.004 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AT4XM UT WOS:000344945600019 ER PT J AU Leal-Sevillano, CA Cooper, KB Decrossas, E Dengler, RJ Ruiz-Cruz, JA Montejo-Garai, JR Chattopadhyay, G Rebollar, JM AF Leal-Sevillano, Carlos A. Cooper, Ken B. Decrossas, Emmanuel Dengler, Robert J. Ruiz-Cruz, Jorge A. Montejo-Garai, Jose R. Chattopadhyay, Goutam Rebollar, Jesus M. TI Compact Duplexing for a 680-GHz Radar Using a Waveguide Orthomode Transducer SO IEEE TRANSACTIONS ON MICROWAVE THEORY AND TECHNIQUES LA English DT Article DE Duplexer; orthomode transducer; terahertz radar ID ORTHO-MODE TRANSDUCERS; IMAGING RADAR; BAND; GHZ AB A compact 680-GHz waveguide orthomode transducer (OMT) and circular horn combination has been designed, tested, and characterized in a radar transceiver's duplexer. The duplexing capability is implemented by a hybrid waveguide quasi optical solution, combining a linear polarization OMT and an external grating polarizer. Isolation between the OMT's orthogonal ports' flanges was measured with a vector network analyzer to exceed 33 dB over a >10% bandwidth between 630 and 710 GHz. Calibrated Y-factor measurements using a mixer attached to the OMT ports reveal losses through the transmit and receive paths that sum to an average of 4.7 dB of two-way loss over 660-690 GHz. This is consistent with radar sensitivity measurements comparing the new OMT/horn with a quasi-optical wire grid beam splitter. Moreover, the radar performance assessment validates the OMT as a suitable compact substitute of the wire grid for the JPL's short-range 680-GHz imaging radar. C1 [Leal-Sevillano, Carlos A.; Montejo-Garai, Jose R.; Rebollar, Jesus M.] Univ Politecn Madrid, Dept Electromagnetismo & Teoria Circuitos, ETSI Telecomunicac, E-28040 Madrid, Spain. [Cooper, Ken B.; Decrossas, Emmanuel; Dengler, Robert J.; Chattopadhyay, Goutam] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ruiz-Cruz, Jorge A.] Univ Autonoma Madrid, Escuela Politecn Super, E-28049 Madrid, Spain. RP Leal-Sevillano, CA (reprint author), Univ Politecn Madrid, Dept Electromagnetismo & Teoria Circuitos, ETSI Telecomunicac, E-28040 Madrid, Spain. EM caleal@etc.upm.es; ken.b.cooper@jpl.nasa.gov RI Ruiz-Cruz, Jorge/C-8159-2014 OI Ruiz-Cruz, Jorge/0000-0003-3909-8263 FU National Aeronautics and Space Administration, Spanish government program [TEC2013-47106-C3-1/2-R]; CONSOLIDER [CSD2008-00068]; Universidad Politecnica de Madrid FX This work was supported in part by the National Aeronautics and Space Administration, Spanish government program under Grant TEC2013-47106-C3-1/2-R, the CONSOLIDER under Grant CSD2008-00068, and a Ph.D. grant from Universidad Politecnica de Madrid. NR 20 TC 2 Z9 2 U1 1 U2 13 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9480 EI 1557-9670 J9 IEEE T MICROW THEORY JI IEEE Trans. Microw. Theory Tech. PD NOV PY 2014 VL 62 IS 11 SI SI BP 2833 EP 2842 DI 10.1109/TMTT.2014.2359636 PG 10 WC Engineering, Electrical & Electronic SC Engineering GA AT5NY UT WOS:000344990700034 ER PT J AU Schlecht, E Siles, JV Lee, C Lin, R Thomas, B Chattopadhyay, G Mehdi, I AF Schlecht, Erich Siles, Jose V. Lee, Choonsup Lin, Robert Thomas, Bertrand Chattopadhyay, Goutam Mehdi, Imran TI Schottky Diode Based 1.2 THz Receivers Operating at Room-Temperature and Below for Planetary Atmospheric Sounding SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Article DE Schottky diode mixer; room temperature heterodyne receiver; subharmonic mixer; local oscillator; varactor; frequency multiplier; broadband terahertz (THz) receiver ID MIXER; BAND; NOISE; OPTIMIZATION; MULTIPLIERS; DESIGN AB In this paper, we report on the design, fabrication and test of two designs for all-solid-state planar Schottky diode based receivers working in the 1.2 THz range. At room temperature, a double side-band (DSB) mixer noise temperature of 2800 K and a conversion loss of 10.5 dB have been measured at 1134 GHz. When the mixers are cooled down to 120 K, they exhibit DSB noise temperatures as low as about 2000 K and conversion loss of 12 dB. The compact local oscillator source (LO) is based on a x2x3 chain and sufficiently pumps the sub-harmonic mixer with 1.5-2.5 mW of power. The receivers provide around 15% RF bandwidth and are well suited for planetary missions to investigate methane and other key lines. C1 [Schlecht, Erich; Siles, Jose V.; Lee, Choonsup; Lin, Robert; Chattopadhyay, Goutam; Mehdi, Imran] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Thomas, Bertrand] Radiometer Phys GmbH, D-53340 Meckenheim, Germany. RP Schlecht, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Erich.Schlecht@jpl.nasa.gov FU JPL Strategic Research and Technology Development Program (RTD); NASA Planetary Instrument Definition and Development Program FX The authors are grateful for the fabrication of the waveguide blocks by Arizona State University and by the JPL Space Instruments Shop, in particular P. Bruneau. The research described herein was carried out at the Jet Propulsion Laboratory, California Institute of Technology, USA, under contract with the National Aeronautics and Space Administration. Funding from the JPL Strategic Research and Technology Development Program (RTD) and the NASA Planetary Instrument Definition and Development Program is gratefully acknowledged. NR 38 TC 8 Z9 8 U1 5 U2 17 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD NOV PY 2014 VL 4 IS 6 BP 661 EP 669 DI 10.1109/TTHZ.2014.2361621 PG 9 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA AT5MY UT WOS:000344988200005 ER PT J AU Bandi, T Affolderbach, C Stefanucci, C Merli, F Skrivervik, AK Mileti, G AF Bandi, Thejesh Affolderbach, Christoph Stefanucci, Camillo Merli, Francesco Skrivervik, Anja K. Mileti, Gaetano TI Compact High-Performance Continuous-Wave Double-Resonance Rubidium Standard With 1.4 x 10(-13) tau(-1/2) Stability SO IEEE TRANSACTIONS ON ULTRASONICS FERROELECTRICS AND FREQUENCY CONTROL LA English DT Article ID FREQUENCY STANDARDS; VAPOR; SHIFTS; NOISE AB We present our studies on a compact high-performance continuous wave (CW) double-resonance (DR) rubidium frequency standard in view of future portable applications. Our clock exhibits a short-term stability of 1.4 x 10(-13) tau(-1/2), consistent with the short-term noise budget for an optimized DR signal. The metrological studies on the medium- to long-term stability of our Rb standard with measured stabilities are presented. The dependence of microwave power shift on light intensity, and the possibility to suppress the microwave power shift is demonstrated. The instabilities arising from the vapor cell geometric effect are evaluated, and are found to act on two different time scales (fast and slow stem effects). The resulting medium-to long-term stability limit is around 5.5 x 10(-14). Further required improvements, particularly focusing on medium-to long-term clock performance, are discussed. C1 [Bandi, Thejesh; Affolderbach, Christoph; Mileti, Gaetano] Univ Neuchatel, Inst Phys, LTF, CH-2000 Neuchatel, Switzerland. [Stefanucci, Camillo; Merli, Francesco; Skrivervik, Anja K.] Ecole Polytech Fed Lausanne, Lab Electromagnet & Acoust LEMA, CH-1015 Lausanne, Switzerland. RP Bandi, T (reprint author), CALTECH, Jet Prop Lab, Quantum Sci & Technol Grp, Pasadena, CA 91125 USA. EM thejesh.bandi@unine.ch; gaetano.mileti@unine.ch FU SNSF [140712]; European Space Agency (ESA) FX This work was supported by the SNSF (grant no. 140712) and the European Space Agency (ESA). NR 29 TC 10 Z9 10 U1 1 U2 12 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0885-3010 EI 1525-8955 J9 IEEE T ULTRASON FERR JI IEEE Trans. Ultrason. Ferroelectr. Freq. Control PD NOV PY 2014 VL 61 IS 11 BP 1769 EP 1778 DI 10.1109/TUFFC.2013.005955 PG 10 WC Acoustics; Engineering, Electrical & Electronic SC Acoustics; Engineering GA AT6ZN UT WOS:000345085700001 PM 25389156 ER PT J AU Gabriel, PM Yeh, PS Tsay, SC AF Gabriel, Philip M. Yeh, Penshu Tsay, Si-Chee TI Effects of Tunable Data Compression on Geophysical Products Retrieved from Surface Radar Observations with Applications to Spaceborne Meteorological Radars SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID CLOUDS; RAIN AB This paper presents results and analyses of applying an international space data compression standard to weather radar measurements that can easily span eight orders of magnitude and typically require a large storage capacity as well as significant bandwidth for transmission. By varying the degree of the data compression, the nonlinear response of models that relates measured radar reflectivity and/or Doppler spectra to the moments and properties of the particle size distribution characterizing clouds and precipitation was analyzed. Preliminary results for the meteorologically important phenomena of clouds and light rain indicate that for a +/- 0.5-dB calibration uncertainty, typical for the ground-based pulsed-Doppler 94-GHz (or 3.2mm, W band) weather radar used as a proxy for spaceborne radar in this study, a lossless compression ratio of only 1.2 is achievable. However, further analyses of the nonlinear response of various models of rainfall rate, liquid water content, and median volume diameter show that a lossy data compression ratio exceeding 15 is realizable. The exploratory analyses presented are relevant to future satellite missions, where the transmission bandwidth is premium and storage requirements of vast volumes of data are potentially problematic. C1 [Gabriel, Philip M.] Colorado State Univ, Ft Collins, CO 80523 USA. [Yeh, Penshu; Tsay, Si-Chee] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gabriel, PM (reprint author), Colorado State Univ, Dept Atmospher Sci, 200 West Lake St,1371 Campus Delivery, Ft Collins, CO 80523 USA. EM gabriel@atmos.colostate.edu FU NASA GSFC Earth Sciences Division FX The authors thank the continuous support of SMARTLabs deployments, as part of NASA Radiation Sciences Program managed by Dr. Hal B. Maring. We also thank the Mission Planning and Technology Development and the Earth Observing System Project Science Office, managed by Drs. Lisa W. Callahan and Steven E. Platnick, respectively, at the NASA GSFC Earth Sciences Division for providing partial funds for analyzing radar data. We are grateful for the insightful conversations on radar statistics with Dr. James B. Mead, president of ProSensing Inc., and to Dr. Cuong M. Nguyen at Colorado State University for the MATLAB code used to perform insightful statistical experiments. Finally, we extend our appreciation to the anonymous reviewers, whose suggestions and comments helped us clarify the presentation and content of this paper. NR 19 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 NOV PY 2014 VL 31 IS 11 BP 2431 EP 2441 DI 10.1175/JTECH-D-13-00257.1 PG 11 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA AT5UR UT WOS:000345008300004 ER PT J AU Verkhoglyadova, OP Leroy, SS Ao, CO AF Verkhoglyadova, Olga P. Leroy, Stephen S. Ao, Chi O. TI Estimation of Winds from GPS Radio Occultations SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID BAYESIAN INTERPOLATION; TROPICAL BELT; ASSIMILATION; IMPACT; STRATOSPHERE; ATMOSPHERE; MISSION; SYSTEM; CHAMP; WIDTH AB GPS radio occultations (RO) offer the possibility to map winds in the upper troposphere and lower stratosphere (UTLS) region because geopotential height is the independent coordinate of retrieval. Most other sounders do not offer this possibility because their independent coordinate of retrieval is pressure. To estimate the precision with which GPS radio occultation data can map winds, dry pressure profiles are simulated from the Interim European Centre for Medium-Range Weather Forecasts Re-Analysis (ERA-Interim) at the actual locations of the Challenging Minisatellite Payload (CHAMP) and the Constellation Observing System for Meteorology, Ionosphere and Climate (COSMIC) soundings for the year 2007. Monthly wind maps were created by using Bayesian interpolation on subsampled ERA-Interim data in 3-5-day bins and subsequent averaging over a month. Mapping winds in this approach requires that 1) geostrophy approximates winds; 2) dry pressure approximates pressure in the UTLS; and 3) geopotential height can be mapped accurately given sparse, nonuniform distributions of data. This study found that, under these conditions, it is possible to map monthly winds near the tropopause with an accuracy of 5.6ms(-1) with CHAMP alone and 4.5ms(-1) with COSMIC alone. The dominant contributors to uncertainty are undersampling of the atmosphere and ageostrophy, particularly at the leading and trailing edges of the subtropical jet. The former is reduced with increased density of GPS RO soundings. The latter cannot be reduced even after iteration for balanced winds. Nevertheless, it is still possible to capture the general wind pattern and to determine the position of the subtropical jet despite the uncertainty in its magnitude. COSMIC radio occultation measurements from 2006 through 2011 were used to estimate monthly geostrophic winds maps in UTLS. The resultant wind dataset is posted online. C1 [Verkhoglyadova, Olga P.; Ao, Chi O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Leroy, Stephen S.] Harvard Univ, Harvard Sch Engn & Appl Sci, Cambridge, MA 02138 USA. RP Verkhoglyadova, OP (reprint author), CALTECH, Jet Prop Lab, M-S 138-310,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM olga.verkhoglyadova@jpl.nasa.gov OI Verkhoglyadova, Olga/0000-0002-9295-9539 FU NASA [NNX10AK55G] FX The authors thank the reviewers for their useful comments. Portions of this work were done at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. S. Leroy acknowledges support from NASA Grant NNX10AK55G to Harvard University. Government sponsorship acknowledged. NR 28 TC 6 Z9 6 U1 1 U2 6 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 NOV PY 2014 VL 31 IS 11 BP 2451 EP 2461 DI 10.1175/JTECH-D-14-00061.1 PG 11 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA AT5UR UT WOS:000345008300006 ER PT J AU Yorks, JE McGill, MJ Scott, VS Wake, SW Kupchock, A Hlavka, DL Hart, WD Selmer, PA AF Yorks, John E. McGill, Matthew J. Scott, V. Stanley Wake, Shane W. Kupchock, Andrew Hlavka, Dennis L. Hart, William D. Selmer, Patrick A. TI The Airborne Cloud-Aerosol Transport System: Overview and Description of the Instrument and Retrieval Algorithms SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID SPECTRAL-RESOLUTION LIDAR; INCOHERENT DOPPLER LIDAR; BACKSCATTER COEFFICIENTS; OPTICAL RADAR; EXTINCTION; SCATTERING; PROFILES; WINDS; TROPOSPHERE; INVERSION AB The Airborne Cloud-Aerosol Transport System (ACATS) is a Doppler wind lidar system that has recently been developed for atmospheric science capabilities at the NASA Goddard Space Flight Center (GSFC). ACATS is also a high-spectral-resolution lidar (HSRL), uniquely capable of directly resolving backscatter and extinction properties of a particle from a high-altitude aircraft. Thus, ACATS simultaneously measures optical properties and motion of cloud and aerosol layers. ACATS has flown on the NASA ER-2 during test flights over California in June 2012 and science flights during the Wallops Airborne Vegetation Experiment (WAVE) in September 2012. This paper provides an overview of the ACATS method and instrument design, describes the ACATS HSRL retrieval algorithms for cloud and aerosol properties, and demonstrates the data products that will be derived from the ACATS data using initial results from the WAVE project. The HSRL retrieval algorithms developed for ACATS have direct application to future spaceborne missions, such as the Cloud-Aerosol Transport System (CATS) to be installed on the International Space Station (ISS). Furthermore, the direct extinction and particle wind velocity retrieved from the ACATS data can be used for science applications such as dust or smoke transport and convective outflow in anvil cirrus clouds. C1 [Yorks, John E.; Kupchock, Andrew; Hlavka, Dennis L.; Hart, William D.; Selmer, Patrick A.] Sci Syst & Applicat Inc, Lanham, MD USA. [Yorks, John E.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [McGill, Matthew J.; Scott, V. Stanley; Wake, Shane W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Yorks, JE (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 612, Greenbelt, MD 20771 USA. EM john.e.yorks@nasa.gov OI Hlavka, Dennis/0000-0002-2976-7243 FU NASA's Earth Science Technology Office (ESTO) Advanced Component Technology (ACT) program; NASA's Airborne Instrument Technology Transfer (AITT) FX NASA's Earth Science Technology Office (ESTO) Advanced Component Technology (ACT) program funded the development of the ACATS receiver subsystem. NASA's Airborne Instrument Technology Transfer (AITT) program funded ACATS instrument integration and ER-2 test flights. A special thanks to all the engineers at Sigma Space Corporation who were involved in building ACATS. We also thank Russ Dickerson for the valuable discussions. NR 49 TC 5 Z9 5 U1 3 U2 15 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 NOV PY 2014 VL 31 IS 11 BP 2482 EP 2497 DI 10.1175/JTECH-D-14-00044.1 PG 16 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA AT5UR UT WOS:000345008300008 ER PT J AU Craig, L Moharreri, A Rogers, DC Anderson, B Dhaniyala, S AF Craig, Lucas Moharreri, Arash Rogers, David C. Anderson, Bruce Dhaniyala, Suresh TI Aircraft-Based Aerosol Sampling in Clouds: Performance Characterization of Flow-Restriction Aerosol Inlets SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID BREAKUP; DEFORMATION AB Interaction of liquid cloud droplets and ice particles with aircraft aerosol inlets can result in the generation of a large number of secondary particles and contaminate aerosol measurements. Recent studies have shown that a sampler designed with a perpendicular subsampling tube located within a flow-through conduit (i.e., a flow-restriction inlet) was best suited for in-cloud sampling. Analysis of field data obtained from different flow-restriction inlets shows that their critical cloud droplet breakup diameters are strongly dependent on design details and operating conditions. Using computational fluid dynamics (CFD) simulations, in-cloud sampling performance of a selected inlet can be predicted reasonably accurately for known operating conditions. To understand the relation between inlet design parameters and its sampling performance, however, CFD calculations are impractical. Here, using a simple, representative one-dimensional velocity profile and a validated empirical droplet breakup criteria, a parametric study is conducted to understand the relationship between different inlet design features and operating conditions on its critical breakup diameters. The results of this study suggest that an optimal inlet for in-cloud aerosol sampling should have a combination of a restriction nozzle at the aft end of the flow-through conduit to minimize wall-impaction shatter artifacts and a blunt leading edge to minimize shatter artifact generation from the aerodynamic breakup of cloud droplets. Inlets for in-cloud aerosol sampling from aircraft will, therefore, differ significantly in design from those used for clear-air aerosol sampling. C1 [Craig, Lucas; Moharreri, Arash] Clarkson Univ, Dept Mech & Aeronaut Engn Dept, Potsdam, NY 13699 USA. [Rogers, David C.] NCAR, Res Aviat Facil, Earth Observing Lab, Broomfield, CO USA. [Anderson, Bruce] NASA Langley Res Ctr, Chem & Dynam Branch, Langley, VA USA. [Dhaniyala, Suresh] Clarkson Univ, Mech & Aeronaut Engn Dept, Potsdam, NY 13699 USA. RP Dhaniyala, S (reprint author), Clarkson Univ, Mech & Aeronaut Engn Dept, 8 Clarkson Ave, Potsdam, NY 13699 USA. EM sdhaniya@clarkson.edu FU NSF [AGS-1044989, AGS-1121915]; NASA's Graduate Student Research Fellowship (GSRP) [NNX09AJ08H] FX The authors acknowledge funding support from NSF (Grants AGS-1044989 and AGS-1121915) and NASA's Graduate Student Research Fellowship (GSRP; Cooperative Agreement NNX09AJ08H). We also thank NCAR's RAF and NASA for flight time. NR 13 TC 2 Z9 2 U1 1 U2 9 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 NOV PY 2014 VL 31 IS 11 BP 2512 EP 2521 DI 10.1175/JTECH-D-14-00022.1 PG 10 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA AT5UR UT WOS:000345008300010 ER PT J AU Nemeth, NN AF Nemeth, Noel N. TI Unit-sphere multiaxial stochastic-strength model applied to a composite material SO JOURNAL OF COMPOSITE MATERIALS LA English DT Article DE Batdorf; failure modes; Weibull; brittle; polymer matrix composite; graphite; anisotropy; failure probability; multiaxial; strength; unit cell ID PROBABILISTIC-STATISTICAL APPROACH; CERAMIC-MATRIX COMPOSITES; NUCLEAR-GRADE GRAPHITE; MECHANICAL-BEHAVIOR; SIC/SIC COMPOSITES; FIBER COMPOSITES; FRACTURE; FAILURE; STRESS; SIZE AB The Batdorf "unit-sphere" methodology has been extended to predict the multiaxial stochastic strength response of anisotropic (specifically transversely isotropic) brittle materials, including polymer matrix composites, by considering (1) nonrandom orientation of intrinsic flaws and (2) critical strength or fracture toughness changing with flaw orientation relative to the material microstructure. The equations developed to characterize these properties are general and can model tightly defined or more diffuse material anisotropy textures describing flaw populations. In this paper, results from finite element analysis of a fiber-reinforced matrix unit cell were used with the unit-sphere model to predict the biaxial strength response of a unidirectional polymer matrix composite previously reported from the World-Wide Failure Exercise. Findings regarding stress-state interactions, thermal residual stresses, and failure modes are also provided. The unit-sphere methodology is an attempt to provide an improved mechanistic basis to the problem of predicting strength response of an anisotropic and composite material under multiaxial loading as compared to polynomial interaction equation formulations. The methodology includes consideration of strength scatter to predict material probability of failure, shear sensitivity of flaws, and accounting for multiple failure modes regarding overall failure response. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Nemeth, NN (reprint author), NASA, Glenn Res Ctr, 21000 Brookpark Rd,Mail Stop 49-7, Cleveland, OH 44135 USA. EM noel.n.nemeth@nasa.gov FU NASA Fundamental Aeronautics Program, Supersonics Project FX This work was funded by the NASA Fundamental Aeronautics Program, Supersonics Project. NR 50 TC 2 Z9 2 U1 2 U2 7 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0021-9983 EI 1530-793X J9 J COMPOS MATER JI J. Compos Mater. PD NOV PY 2014 VL 48 IS 27 BP 3395 EP 3424 DI 10.1177/0021998313509865 PG 30 WC Materials Science, Composites SC Materials Science GA AU0TF UT WOS:000345336700007 ER PT J AU Mobley, ML McCulley, RL Burke, IC Peterson, G Schimel, DS Cole, CV Elliott, ET Westfall, DG AF Mobley, Megan L. McCulley, Rebecca L. Burke, Ingrid C. Peterson, Gary Schimel, David S. Cole, C. Vernon Elliott, Edward T. Westfall, Dwayne G. TI Grazing and No-Till Cropping Impacts on Nitrogen Retention in Dryland Agroecosystems SO JOURNAL OF ENVIRONMENTAL QUALITY LA English DT Article ID SOIL ORGANIC-MATTER; SHORTGRASS STEPPE; RIVER-BASIN; GRASSLAND; CARBON; N-15; MINERALIZATION; CULTIVATION; ECOSYSTEMS; MANAGEMENT AB As the world's population increases, marginal lands such as drylands are likely to become more important for food production. One proven strategy for improving crop production in drylands involves shifting from conventional tillage to no-till to increase water use efficiency, especially when this shift is coupled with more intensive crop rotations. Practices such as no-till that reduce soil disturbance and increase crop residues may promote C and N storage in soil organic matter, thus promoting N retention and reducing N losses. By sampling soils 15 yr after a N-15 tracer addition, this study compared long-term soil N retention across several agricultural management strategies in current and converted shortgrass steppe ecosystems: grazed and ungrazed native grassland, occasionally mowed planted perennial grassland, and three cropping intensities of no-till dryland cropping. We also examined effects of the environmental variables site location and topography on N retention. Overall, the long-term soil N retention of > 18% in these managed semiarid ecosystems was high compared with published values for other cropped or grassland ecosystems. Cropping practices strongly influenced long-term N retention, with planted perennial grass systems retaining > 90% of N-15 in soil compared with 30% for croplands. Grazing management, topography, and site location had smaller effects on long-term N retention. Estimated 15-yr N losses were low for intact and cropped systems. This work suggests that semiarid perennial grass ecosystems are highly N retentive and that increased intensity of semiarid land management can increase the amount of protein harvested without increasing N losses. C1 [Mobley, Megan L.; Burke, Ingrid C.] Univ Wyoming, Haub Sch Environm & Nat Resources, Dept Bot, Dept Ecosyst Sci & Management, Laramie, WY 82071 USA. [Mobley, Megan L.; Burke, Ingrid C.] Univ Wyoming, Program Ecol, Laramie, WY 82071 USA. [McCulley, Rebecca L.] Univ Kentucky, Dept Plant & Soil Sci, Lexington, KY 40546 USA. [Peterson, Gary; Westfall, Dwayne G.] Colorado State Univ, Dept Soil & Crop Sci, Ft Collins, CO 80523 USA. [Schimel, David S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cole, C. Vernon; Elliott, Edward T.] Colorado State Univ, Nat Resource Ecol Lab, Ft Collins, CO 80523 USA. [Cole, C. Vernon] ARS, USDA, Ft Collins, CO 80521 USA. RP Mobley, ML (reprint author), Univ Wyoming, Haub Sch Environm & Nat Resources, Dept Bot, Dept Ecosyst Sci & Management, Laramie, WY 82071 USA. EM meg.mobley@alumni.duke.edu RI Burke, Ingrid/A-1420-2009 OI Burke, Ingrid/0000-0003-4717-6399 FU National Science Foundation [BSR-8605190]; Colorado State University Experiment Station; National Science Foundation Shortgrass Steppe LongTerm Ecological Research Project [BSR-8612105, DEB-0217631]; California Institute of Technology, Government FX This paper is based on two long-term research projects supported by many grants and institutions. 'the initial experiments on no till cropping systems and 15N labeling were funded by the National Science Foundation (BSR-8605190 and the Colorado State University Experiment Station. The long-term 15N study on the shortgrass steppe was funded by the National Science Foundation Shortgrass Steppe LongTerm Ecological Research Project (BSR-8612105, DEB-0217631). 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. Copyright 2013 California Institute of Technology, Government sponsorship acknowledged. All projects represented close collaborations with the USDA Agricultural Research Service. A multitude of field technicians from Colorado State University assisted with field and lab work. NR 48 TC 0 Z9 0 U1 1 U2 24 PU AMER SOC AGRONOMY PI MADISON PA 677 S SEGOE RD, MADISON, WI 53711 USA SN 0047-2425 EI 1537-2537 J9 J ENVIRON QUAL JI J. Environ. Qual. PD NOV-DEC PY 2014 VL 43 IS 6 BP 1963 EP 1971 DI 10.2134/jeq2013.12.0530 PG 9 WC Environmental Sciences SC Environmental Sciences & Ecology GA AT7DD UT WOS:000345096000015 PM 25602213 ER PT J AU Zhang, J Fryauf, DM Norris, KJ Wei, M Leon, JJD Kobayashi, NP AF Zhang, Junce Fryauf, David M. Norris, Kate J. Wei, Min Leon, Juan J. Diaz Kobayashi, Nobuhiko P. TI Raman spectroscopy of indium phosphide nanowire networks coated with gold clusters SO JOURNAL OF MATERIALS SCIENCE-MATERIALS IN ELECTRONICS LA English DT Article ID SCATTERING; NANOPARTICLES; SHAPE AB Enhanced Raman signal of the longitudinal optical phonon mode in indium phosphide nanowire networks with gold coating of up to 5 nm thickness was observed experimentally to further study the phonon spectrum of nanowire networks. Indium phosphide nanowire networks coated with different nominal thicknesses of gold were prepared and optically studied. Scanning electron microscopy, photoluminescence spectroscopy and Raman spectroscopy were used to study the dependence of surface morphology and phonon modes of the nanowire networks on the nominal thickness of the gold coating. The Raman peak of longitudinal optical phonon mode for as grown sample was negligible, while the peak intensity for 1 and 5 nm gold coated sample reached to 1,379 and 792 a.u. respectively. Electromagnetic enhancement and extinction coefficient are discussed to qualitatively assess the role of the gold coating on indium phosphide nanowire networks. C1 [Zhang, Junce; Fryauf, David M.; Norris, Kate J.; Leon, Juan J. Diaz; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. [Zhang, Junce; Fryauf, David M.; Norris, Kate J.; Leon, Juan J. Diaz; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, NASA, Ames Res Ctr, Adv Studies Labs, Moffett Field, CA 94035 USA. [Wei, Min] Univ Elect Sci & Technol China, Sch Microelect & Solid Elect, Chengdu 610054, Peoples R China. RP Zhang, J (reprint author), Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. EM juncezhang@gmail.com RI Kobayashi, Nobuhiko/E-3834-2012 FU NASA SBIR [NNX11CE14P]; National Science Foundation Graduate Research Fellowship [DGE-0809125]; Semiconductor Research Corporation CSR fund FX This work was partially supported by NASA SBIR NNX11CE14P. This work is also partially supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-0809125 and Semiconductor Research Corporation CSR fund (Dr. Victor Zhirnov). We would like to thank Quantum Systems Laboratory at Hewlett-Packard Laboratories (Palo Alto, California) and the MACS facility (Moffett Field, California) at the Advanced Studies Laboratories, a strategic partnership between the University of California Santa Cruz and NASA Ames Research Center, for their continuous support on analytical equipment. NR 17 TC 2 Z9 2 U1 0 U2 10 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 2014 VL 25 IS 11 BP 4867 EP 4871 DI 10.1007/s10854-014-2245-z PG 5 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Engineering; Materials Science; Physics GA AT3BD UT WOS:000344808800024 ER PT J AU Arbuckle, JG Hobbs, J Loy, A Morton, LW Prokopy, LS Tyndall, J AF Arbuckle, J. G., Jr. Hobbs, J. Loy, A. Morton, L. W. Prokopy, L. S. Tyndall, J. TI Understanding Corn Belt farmer perspectives on climate change to inform engagement strategies for adaptation and mitigation SO JOURNAL OF SOIL AND WATER CONSERVATION LA English DT Article DE adaptation; agriculture; climate change; communication; extension; latent class analysis ID UNITED-STATES; PERCEPTIONS; AGRICULTURE; SCIENCE; POLICY; VULNERABILITY; WILLINGNESS; CHALLENGES; EXPERIENCE; INTERFACE AB Development of extension and outreach that effectively engage farmers in climate change adaptation and/or mitigation activities can be informed by an improved understanding of farmers' perspectives on climate change and related impacts. This research employed latent class analysis (LCA) to analyze data from a survey of 4,778 farmers from 11 US Corn Belt states. The research focused on two related research questions: (1) to what degree do farmers differ on key measures of beliefs about climate change, experience with extreme weather, perceived risks to agriculture, efficacy, and level of support for public and private adaptive and mitigative action; and (2) are there potential areas of common ground among farmers? Results indicate that farmers have highly heterogeneous perspectives, and six distinct classes of farmers are identified. We label these as the following: the concerned (14%), the uneasy (25%), the uncertain (25%), the unconcerned (13%), the confident (18%), and the detached (5%). These groups of farmers differ primarily in terms of beliefs about climate change, the degree to which they had experienced extreme weather, and risk perceptions. Despite substantial differences on these variables, areas of similarity were discerned on variables measuring farmers' (1) confidence that they will be able to deal with increases in weather variability and (2) support for public and private efforts to help farmers adapt to increased weather variability. These results can inform segmented approaches to outreach that target subpopulations of farmers as well as broader engagement strategies that would reach wider populations. Further, findings suggest that strategies with specific reference to climate change might be most effective in engaging the subpopulations of farmers who believe that climate change is occurring and a threat, but that use of less charged terms such as weather variability would likely be more effective with a broader range of farmers. Outreach efforts that (1) appeal to farmers' problem solving capacity and (2) employ terms such as "weather variability" instead of more charged terms such as "climate change" are more likely to be effective with a wider farmer audience. C1 [Arbuckle, J. G., Jr.; Morton, L. W.] Iowa State Univ, Ames, IA 50011 USA. [Hobbs, J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Loy, A.] Lawrence Univ, Appleton, WI 54912 USA. [Prokopy, L. S.] Purdue Univ, Dept Forestry & Nat Resources, W Lafayette, IN 47907 USA. [Tyndall, J.] Iowa State Univ, Dept Nat Resources Ecol & Management, Ames, IA USA. RP Arbuckle, JG (reprint author), Iowa State Univ, Ames, IA 50011 USA. OI Loy, Adam/0000-0002-5780-4611 NR 62 TC 7 Z9 7 U1 5 U2 35 PU SOIL WATER CONSERVATION SOC PI ANKENY PA 945 SW ANKENY RD, ANKENY, IA 50023-9723 USA SN 0022-4561 EI 1941-3300 J9 J SOIL WATER CONSERV JI J. Soil Water Conserv. PD NOV-DEC PY 2014 VL 69 IS 6 BP 505 EP 516 DI 10.2489/jswc.69.6.505 PG 12 WC Ecology; Soil Science; Water Resources SC Environmental Sciences & Ecology; Agriculture; Water Resources GA AT6BY UT WOS:000345025000014 ER PT J AU Mu, XD Meissner, S Meissner, H Yu, AW AF Mu, Xiaodong Meissner, Stephanie Meissner, Helmuth Yu, Anthony W. TI High efficiency Yb:YAG crystalline fiber-waveguide lasers SO OPTICS LETTERS LA English DT Article ID SINGLE-MODE OPERATION; DIODE; AMPLIFIER AB A laser diode (LD) cladding pumped single-mode 1030 nm laser has been demonstrated, in an adhesive-free bonded 40 mu m core Yb:YAG crystalline fiber waveguide (CFW). A laser output power of 13.2 W at a wavelength of 1.03 mu m has been achieved, for an input pump power of 39.5 W. The corresponded laser efficiency is 33.4%. The laser beam quality is confirmed to be near diffraction-limited, with a measured M-2 = 1.02. A LD core pumped single-clad Yb:YAG CFW laser has also been demonstrated with a top-hat laser beam profile, with a laser output power of 28 W and a slope efficiency of 78%. (C) 2014 Optical Society of America. C1 [Mu, Xiaodong; Meissner, Stephanie; Meissner, Helmuth] Onyx Opt Inc, Dublin, CA 94568 USA. [Yu, Anthony W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Mu, XD (reprint author), Onyx Opt Inc, 6551 Sierra Lane, Dublin, CA 94568 USA. EM xmu@onyxoptics.com RI Chen, Ru/A-5105-2015 FU NASA SBIR [NNX13CG12P] FX This Letter was partially supported by NASA SBIR contract NNX13CG12P. NR 21 TC 5 Z9 5 U1 1 U2 12 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 EI 1539-4794 J9 OPT LETT JI Opt. Lett. PD NOV 1 PY 2014 VL 39 IS 21 BP 6331 EP 6334 DI 10.1364/OL.39.006331 PG 4 WC Optics SC Optics GA AT5MA UT WOS:000344985900062 PM 25361347 ER PT J AU Tang, H Dubayah, R Brolly, M Ganguly, S Zhang, G AF Tang, Hao Dubayah, Ralph Brolly, Matthew Ganguly, Sangram Zhang, Gong TI Large-scale retrieval of leaf area index and vertical foliage profile from the spaceborne waveform lidar (GLAS/ICESat) SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Lidar; LAI; Vertical foliage profile; GLAS; Landsat ID DECIDUOUS FORESTS; SPECIES RICHNESS; LASER ALTIMETER; VEGETATION; LANDSAT; LAI; FRACTION; HEIGHT; COVER; TOPOGRAPHY AB Leaf area index (LAI) and canopy vertical profiles are important descriptors of ecosystem structure. The Geoscience Laser Altimeter System (GLAS) on board ICESat (Ice, Cloud, and land Elevation Satellite) provided three-dimensional observations that can be used to derive these canopy structure parameters globally. While several canopy height products have been produced globally from GLAS, no comparable data sets for LAI and canopy profiles exist across large areas. In this study we develop a physically based method of retrieving LAI and vertical foliage profiles (VFPs) from GLAS observations over the entire state of California, USA. This method refines lidar derived LAI and VFP through a recursive analysis of GLAS waveforms using ancillary data obtained from existing remote sensing products. Those supplemental inputs include canopy clumping index derived from POLDER, 500 m land cover type and 1 km LAI data derived from MODIS. Implementation of our method created state-level LAI and VFP data for the existing GIAS transects over California. We then analyzed the variability of LAI and VFP data sets across environmental gradients and as a function of land cover type and elevation. Both LAI and VFP showed strong variability across elevational gradients and among land cover types. We compared our results at the scale of GLAS footprints with an LAI map derived from Landsat (at 30 m) and found moderate agreement (r(2) = 034, bias = 0.26, RMSD (Root Mean Square Difference) = 1.85) between the two. In particular, Landsat LAI not only appeared to saturate relative to GLAS LAI at around LAI = 5, but also showed an overestimation for LAI less than about 2. Best agreement between the two LAI data sets was shown to occur in areas with slope less than 20 degrees. Results from our study suggest the possibility of retrieving global LAI and VFP data from GIAS data and the potential for synergetic observation of lidar and passive optical remote sensing data such as Landsat. (C) 2014 Elsevier Inc. All rights reserved. C1 [Tang, Hao; Dubayah, Ralph] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Brolly, Matthew] Univ Brighton, Sch Environm & Technol, Brighton BN2 4AT, E Sussex, England. [Ganguly, Sangram; Zhang, Gong] Bay Area Environm Res Inst, West Sonoma, CA USA. [Ganguly, Sangram; Zhang, Gong] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Tang, H (reprint author), Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. RI Tang, Hua/K-4948-2016; OI Tang, Hua/0000-0002-6685-6165; Brolly, Matthew/0000-0002-3576-9675 FU NASA [NNX12AK07G]; Earth And Space Science Graduate Fellowship [NNX12AN43H] FX This work was funded by NASA under grant NNX12AK07G (Dubayah) and an Earth And Space Science Graduate Fellowship NNX12AN43H (Dubayah/Tang). We thank Maosheng Zhao and Qing Ying for their help in processing MODIS data. We also thank the NSIDC (National Snow & Ice Data Center) User Services for the help on data acquisition and NASA Earth Exchange (NEX) for computing resources. NR 57 TC 14 Z9 16 U1 7 U2 35 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD NOV PY 2014 VL 154 SI SI BP 8 EP 18 DI 10.1016/j.rse.2014.08.007 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AT8SI UT WOS:000345201900002 ER PT J AU Guillevic, PC Biard, JC Hulley, GC Privette, JL Hook, SJ Olioso, A Gottsche, FM Radocinski, R Roman, MO Yu, YY Csiszar, I AF Guillevic, Pierre C. Biard, James C. Hulley, Glynn C. Privette, Jeffrey L. Hook, Simon J. Olioso, Albert Goettsche, Frank M. Radocinski, Robert Roman, Miguel O. Yu, Yunyue Csiszar, Ivan TI Validation of Land Surface Temperature products derived from the Visible Infrared Imaging Radiometer Suite (VIIRS) using ground-based and heritage satellite measurements SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Land Surface Temperature; VIIRS; Validation; MODIS; Ground-based measurements ID TRACK SCANNING RADIOMETER; RADIATION BUDGET NETWORK; BROAD-BAND EMISSIVITY; LAKE TAHOE; MODIS DATA; ASTER; ALGORITHM; SURFRAD; VEGETATION; MODEL AB Thermal infrared satellite observations of the Earth's surface are widely used to retrieve Land Surface Temperature (LST) and monitor LST changes around the world. Since January 2012, the Visible Infrared Imaging Radiometer Suite (VIIRS) onboard the Suomi National Polar-Orbiting Partnership (S-NPP) has provided daily observations of LST with a spatial resolution of 750 m at nadir. Comparison of the standard VIIRS LST product with the equivalent daily standard product from the Moderate Resolution Imaging Spectroradiometer (MODIS) collection-5 and with ground-based measurements over vegetated and inland water surfaces showed good agreement Analysis indicated the accuracy and precision of the VIIRS product over these cover types was 02 K and 2.0 K respectively provided the analyses included appropriate compensation for any spatial heterogeneity in LST within the validation site. However, comparisons between in situ LST and the VIIRS and MODIS LST over arid and semi-arid regions indicate both satellite products significantly underestimate the LST, and the VIIRS algorithm can have large errors in the retrieved LST over areas of high atmospheric water vapor. Errors of up to 4 K were observed over semi-arid and arid areas due to incorrect characterization of emissivity, and differences of up to 15 K were observed over areas with high atmospheric water content between the VIIRS LST and matching MODIS LST. (C) 2014 Elsevier Inc. All rights reserved. C1 [Guillevic, Pierre C.; Hulley, Glynn C.; Hook, Simon J.; Radocinski, Robert] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Biard, James C.] N Carolina State Univ, Cooperat Inst Climate & Satellites, Asheville, NC USA. [Biard, James C.; Privette, Jeffrey L.] NOAA, Natl Climat Data Ctr, Asheville, NC USA. [Olioso, Albert] INRA, EMMAH, Avignon, France. [Goettsche, Frank M.] Karlsruhe Inst Technol, D-76021 Karlsruhe, Germany. [Roman, Miguel O.] NASA, Goddard Space Flight Ctr, Terr Informat Syst Lab, Greenbelt, MD 20771 USA. [Yu, Yunyue; Csiszar, Ivan] NOAA, Ctr Satellite Applicat & Res, College Pk, MD 20740 USA. RP Guillevic, PC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM pierre.c.guillevic@jpl.nasa.gov RI Csiszar, Ivan/D-2396-2010; Yu, Yunyue/F-5636-2010; Biard, James/E-5593-2014; Roman, Miguel/D-4764-2012; Gottsche, Frank-Michael/A-7362-2013; Hook, Simon/D-5920-2016; Privette, Jeffrey/G-7807-2011; OI Biard, James/0000-0002-2952-2828; Roman, Miguel/0000-0003-3953-319X; Gottsche, Frank-Michael/0000-0001-5836-5430; Hook, Simon/0000-0002-0953-6165; Privette, Jeffrey/0000-0001-8267-9894; Olioso, Albert/0000-0001-8342-9272 FU Cooperative Institute for Climate and Satellites-North Carolina - Joint Polar Satellite System program [NA09NES4400006]; National Oceanic and Atmospheric Administration (NOAA)'s Climate Data Record project; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA; National Aeronautic and Space Administration (NASA); European Organization for the Exploitation of Meteorological Satellites (EUMETSAT) FX The research described in this paper was carried out at (1) the Cooperative Institute for Climate and Satellites-North Carolina under Cooperative Agreement NA09NES4400006 supported by the Joint Polar Satellite System program, and by the National Oceanic and Atmospheric Administration (NOAA)'s Climate Data Record project, and at (2) the Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, under contract with the National Aeronautic and Space Administration (NASA). The VIIRS data are distributed by the NOAA's Comprehensive large Array-Data Stewardship System (CLASS, http://www.class.ncdc.noaa.gov). The MODIS data used in the study are distributed by the NASA Earth Observing System Data and Information System (http://earthdata.nasa.gov). The in situ data from Gobabeb, Namibia, were collected within the context of the LSA-SAF ( http://landsaf.ipma.pt), a project funded by the European Organization for the Exploitation of Meteorological Satellites (EUMETSAT). The authors would like to thank Dr. Zhengming Wan from University of Santa Barbara, CA, USA, Dr. John Augustine from NOAA's Earth System Research Laboratory, Boulder, CO, USA and Dr. Alain Sei from Northrop Grumman Aerospace Systems, Redondo Beach, CA, USA for their scientific support regarding MODIS, SURFRAD and VIIRS products. NR 71 TC 18 Z9 20 U1 0 U2 42 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 2014 VL 154 SI SI BP 19 EP 37 DI 10.1016/j.rse.2014.08.013 PG 19 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AT8SI UT WOS:000345201900003 ER PT J AU Miernecki, M Wigneron, JP Lopez-Baeza, E Kerr, Y De Jeu, R De Lannoy, GJM Jackson, TJ O'Neill, PE Schwank, M Moran, RF Bircher, S Lawrence, H Mialon, A Al Bitar, A Richaume, P AF Miernecki, Maciej Wigneron, Jean-Pierre Lopez-Baeza, Ernesto Kerr, Yann De Jeu, Richard De Lannoy, Gabrielle J. M. Jackson, Thomas J. O'Neill, Peggy E. Schwank, Mike Fernandez Moran, Roberto Bircher, Simone Lawrence, Heather Mialon, Arnaud Al Bitar, Ahmad Richaume, Philippe TI Comparison of SMOS and SMAP soil moisture retrieval approaches using tower-based radiometer data over a vineyard field SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE SMOS; SMAP; Soil moisture retrieval; ELBARA; Valencia Anchor Station ID VEGETATION OPTICAL DEPTH; L-MEB MODEL; PASSIVE MICROWAVE OBSERVATIONS; POLARIZATION DIFFERENCE INDEX; DATA ASSIMILATION SYSTEM; CROP FIELDS; AMSR-E; EMISSION; CALIBRATION; BIOMASS AB The objective of this study was to compare several approaches to soil moisture (SM) retrieval using L-band microwave radiometry. The comparison was based on a brightness temperature (T-B) data set acquired since 2010 by the L-band radiometer ELBARA-II over a vineyard field at the Valencia Anchor Station (VAS) site. ELBARA-II, provided by the European Space Agency (ESA) within the scientific program of the SMOS (Soil Moisture and Ocean Salinity) mission, measures multiangular T-B data at horizontal and vertical polarization for a range of incidence angles (30 degrees-60 degrees). Based on a three year data set (2010-2012), several SM retrieval approaches developed for spaceborne missions including AMSR-E (Advanced Microwave Scanning Radiometer for EOS), SMAP (Soil Moisture Active Passive) and SMOS were compared. The approaches include: the Single Channel Algorithm (SCA) for horizontal (SCA-H) and vertical (SCA-V) polarizations, the Dual Channel Algorithm (DCA), the Land Parameter Retrieval Model (LPRM) and two simplified approaches based on statistical regressions (referred to as 'Mattar' and 'Saleh'). Time series of vegetation indices required for three of the algorithms (SCA-H, SCA-V and 'Mattar') were obtained from MODIS observations. The SM retrievals were evaluated against reference SM values estimated from a multiangular 2-Parameter inversion approach. As no in situ SM data was used, the evaluation made here is relative to the use of this specific reference data set. The results obtained with the current base line algorithms developed for SMAP (SCA-H and -V) are in very good agreement with the 'reference' SM data set derived from the multi-angular observations (R-2 approximate to 0.90, RMSE varying between 0.035 and 0.056 m(3)/m(3) for several retrieval configurations). This result showed that provided the relationship between vegetation optical depth and a remotely-sensed vegetation index can be calibrated, the SCA algorithms can provide results very close to those obtained from multi-angular observations in this study area. The approaches based on statistical regressions provided similar results and the best accuracy was obtained with the 'Saleh' methods based on either bi-angular or bipolarization observations (R-2 approximate to 0.93, RMSE 0.035 m(3)/m(3)). The LPRM and DCA algorithms were found to be slightly less successful in retrieving the 'reference' SM time series (R-2 approximate to 0.75, RMSE 0.055 m(3)/m(3)). However, the two above approaches have the great advantage of not requiring any model calibrations previous to the SM retrievals. (C) 2014 Elsevier Inc. All rights reserved. C1 [Miernecki, Maciej] Univ Hamburg, Ctr Marine & Atmospher Sci ZMAW, Hamburg, Germany. [Wigneron, Jean-Pierre] INRA, Bordeaux Sci Agro, UMR ISPA 1391, F-33140 Villenave Dornon, France. [Lopez-Baeza, Ernesto; Fernandez Moran, Roberto] Univ Valencia, Fac Phys, E-46100 Valencia, Spain. [Kerr, Yann; Bircher, Simone; Mialon, Arnaud; Al Bitar, Ahmad; Richaume, Philippe] Univ Toulouse 3, CNRS, IRD, Ctr Etud Spatiales BIOsphere,CESBIO CNES, F-31062 Toulouse, France. [De Jeu, Richard] Vrije Univ Amsterdam, Dept Earth Sci, Amsterdam, Netherlands. [De Lannoy, Gabrielle J. M.; O'Neill, Peggy E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Jackson, Thomas J.] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA. [Schwank, Mike] Gamma Remote Sensing, CH-3073 Gumlingen, Switzerland. [Schwank, Mike] Swiss Fed Res Inst WSL, CH-8903 Birmensdorf, Switzerland. [Lawrence, Heather] European Ctr Medium Range Weather Forecasts ECMWF, Reading, Berks, England. RP Wigneron, JP (reprint author), INRA, Bordeaux Sci Agro, UMR ISPA 1391, F-33140 Villenave Dornon, France. EM wigneron@bordeaux.inra.fr OI Al Bitar, Ahmad/0000-0002-1756-1096 FU TOSCA program of CNES (Centre National d'Etudes Spatiales, France); Spanish National Program on Space Research [MIDAS-5, ESP2007-65667-C04-03, MIDAS-6, AYA2010-22062-C05-03]; ESA (European Space Agency) FX This study received financial support from the TOSCA program of CNES (Centre National d'Etudes Spatiales, France), the Spanish National Program on Space Research (MIDAS-5, ESP2007-65667-C04-03, and MIDAS-6, AYA2010-22062-C05-03, Projects) and ESA (European Space Agency) in the framework of the cal/val activities of the SMOS mission. The MODIS MOD13Q1 data were obtained through the online Data Pool at the NASA Land Processes Distributed Active Archive Center (LP DAAC), USGS/Earth Resources Observation and Science (EROS) Center, Sioux Falls, South Dakota (http://lpdaac.usgs.gov/get_data). The CATDS data were obtained from the "Centre Aval de Traitement des Donnees SMOS" (CATDS), operated for the "Centre National d'Etudes Spatiales" (CNES, France) by IFREMER (Brest, France). NR 62 TC 2 Z9 3 U1 3 U2 31 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 2014 VL 154 SI SI BP 89 EP 101 DI 10.1016/j.rse.2014.08.002 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AT8SI UT WOS:000345201900008 ER PT J AU Veraverbeke, S Stavros, EN Hook, SJ AF Veraverbeke, Sander Stavros, E. Natasha Hook, Simon J. TI Assessing fire severity using imaging spectroscopy data from the Airborne Visible/Infrared Imaging Spectrometer (AVIRIS) and comparison with multispectral capabilities SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Fire severity; EnMAP; HyspIRI; PRISMA; Hyperspectral; Wildland fire; Forest fire; AVIRIS; OLI; Weighted multiple endmember spectral mixture analysis (wMESMA) ID SPECTRAL MIXTURE ANALYSIS; 2007 PELOPONNESE WILDFIRES; ADJUSTED VEGETATION INDEX; BURN SEVERITY; LANDSAT DATA; ENDMEMBER VARIABILITY; HYPERSPECTRAL IMAGERY; URBAN-ENVIRONMENT; MISSION; FOREST AB Fire severity, the degree of environmental change caused by a fire, is traditionally assessed by broadband spectral indices, such as the differenced Normalized Burn Ratio (dNBR) from Landsat imagery. Here, we used an alternative indicator, the burned fraction derived from spectral mixture analysis (SMA), to evaluate and compare the performance for assessing fire severity of broadband and narrowband imaging spectroscopy (IS) data in the visible to shortwave infrared (VSWIR, 035-2.5 mu m). We used the band specifications of the broadband Operational Land Imager (OLI) and the narrowband Airborne Visible/Infrared Imaging Spectrometer (AVIRIS). We integrated two techniques to account for endmember variability in the unmixing process, spectral weighting and iterative unmixing, in a model referred to as weighted multiple endmember SMA (wMESMA). Based on a separability index, we evaluated the separability between the different ground components, or endmembers, that comprise post-fire environments (char, green vegetation (CV), non-photosynthetic vegetation (NPV) and substrate). We found that the near infrared region (0.7-1.3 mu m) had the highest discriminatory power, followed by the shortwave infrared 2 (SWIR2, 2-2.4 mu m), SWIR1 (1.5-1.7 mu m) and visible (0.35-0.7 mu m) regions. Individual narrowbands did not substantially outperform individual broadbands, however, the higher data dimensionality of IS resulted in significantly improved post-fire fractional cover and burned fraction estimates compared to multispectral data. Multispectral data captured a fair amount of the variability in fire severity conditions as represented by the different fractional cover estimates of the endmembers in both a multispectral narrow- and broadband scenario, however, fractional cover estimates derived from IS data using all viable bands were significantly better. This demonstrated the benefits of IS over traditional multispectral data to assess fire severity and also showed that the additional information gain was the result of higher data dimensionality and not because of certain narrowbands capturing narrow spectral features. In addition, we found that the burned fraction derived from all viable AVIRIS bands over a fire in California, USA, was highly correlated with two field measures of fire severity (Geo Composite Burn Index: R-2 = 0.86, and the percentage black trees and shrubs: R-2 = 0.65). Formal quantification of potential improvements of IS over multispectral methods is important with the advent of upcoming spaceborne IS missions (e.g. the Environmental Mapping and Analysis Program and Hyperspectral Infrared Imager). Our analysis showed that IS data when combined with advanced analysis techniques significantly improved fire severity assessments. The improvements of using IS data require higher computational cost and advanced processing, thus multispectral data might still suit the needs of certain applications such as rapid fire damage assessments and global analysis of spatio-temporal fire severity patterns. (C) 2014 Elsevier Inc. All rights reserved. C1 [Veraverbeke, Sander] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Veraverbeke, Sander; Stavros, E. Natasha; Hook, Simon J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Veraverbeke, S (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, 2224 Croul Hall, Irvine, CA 92697 USA. EM Sander.Veraverbeke@ucl.edu; Natasha.Stavros@jpl.nasa.gov; Simon.J.Hook@jpl.nasa.gov RI Hook, Simon/D-5920-2016; Veraverbeke, Sander/H-2301-2012 OI Hook, Simon/0000-0002-0953-6165; Veraverbeke, Sander/0000-0003-1362-5125 FU NASA grant for Interdisciplinary Research in Earth Science [NNX10AL14G] FX We would like to thank Sarah Lundeen for transferring the AVIRIS data and providing the AVIRIS signal-to-noise ratios. Julia Barsi is gratefully acknowledged for providing the OLI spectral response functions and signal-to-noise ratios. We gratefully thank several colleagues at the Jet Propulsion Laboratory (Glenn Sellar, Rob Green, Robert Staehle, David Thompson, David Schimel, Marc Simard, Justin Boland among others) for fostering the analysis presented in this paper. We also would like to thank the anonymous reviewers for their useful suggestions to improve the manuscript. Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The work was funded by a NASA grant for Interdisciplinary Research in Earth Science (NNX10AL14G). Copyright 2014 California Institute of Technology. Government sponsorship acknowledged. NR 80 TC 8 Z9 8 U1 3 U2 36 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD NOV PY 2014 VL 154 SI SI BP 153 EP 163 DI 10.1016/j.rse.2014.08.019 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AT8SI UT WOS:000345201900013 ER PT J AU Lagomasino, D Price, RM Whitman, D Campbell, PKE Melesse, A AF Lagomasino, David Price, Rene M. Whitman, Dean Campbell, Petya K. E. Melesse, Assefa TI Estimating major ion and nutrient concentrations in mangrove estuaries in Everglades National Park using leaf and satellite reflectance SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Water quality; Spectral reflectance; Mangroves; Everglades; Landsat; NDVI; Remote sensing ID SPECTRAL REFLECTANCE; RHIZOPHORA-MANGLE; FLORIDA BAY; HYPERSPECTRAL DATA; SOUTH FLORIDA; PLANT STRESS; FOOD WEBS; VEGETATION; GROWTH; RIVER AB Coastal mangrove ecosystems are under duress worldwide because of urban development, sea-level rise, and climate change, processes that are capable of changing the salinity and nutrient concentration of the water utilized by the mangroves. This study correlates long-term water chemistry in mangrove environments, located in Everglades National Park, with mangrove spectral reflectance measurements made at both the leaf and canopy scales. Spectral reflectance measurements were collected using a handheld spectrometer for leaf-level measurements and Landsat 5TM data for regional coverage. Leaf-level reflectance data were collected from three mangrove species (i.e., red, black and white mangroves) across two regions; a tall mangrove (similar to 18 m) and dwarf mangrove (1-2 m) region. The reflectance data were then used to calculate a wide variety of biophysical reflectance indices (e.g., NDVI, EVI, SAVI) to determine signs of stress. Discrete, quarterly water samples from the surface water, groundwater, and pore water (20 and 85 cm depths) and daily autonomous surface water samples were collected at each site and analyzed for major anions (Cl- and SO42-), cations (Na+, K+, Mg2+, and Ca2+), total nitrogen (TN) and total phosphorus (TP). Mangrove sites that exhibited the highest salinity and ionic concentrations in the surface and subsurface water also had the lowest near-infrared reflectance at both the leaf and satellite levels. Seasonal reflectance responses were measured in the near-infrared (NIR) wavelengths at both the leaf and canopy scales and were strongly correlated with nutrient and ionic concentrations in the surface and subsurface water, even though there was no significant separability between the three mangrove species. Study sites that experienced the greatest variability in surface and subsurface water ionic concentrations also exhibited the greatest fluctuations in NIR spectral reflectance. Landsat 5TM images were able to detect tall and dwarf mangroves by the differences in spectral indices (e.g., NDVI, NDWI, and EVI) because of the variability in the background conditions amongst the environments. In addition, Landsat 5TM images spanning 16 years (1993-2009) were successfully used to estimate the seasonal variability in ionic concentrations in the surface water across the Florida Coastal mangrove ecotone. This study has shown that water chemistry can be estimated indirectly by measuring the change in spectral response at the leaf- or satellite-scale. Furthermore, the results of this research may be extrapolated to similar coastal mangrove systems throughout the Caribbean and world-wide wherever red, black, and white mangroves occur. (C) 2014 Elsevier Inc. All rights reserved. C1 [Lagomasino, David; Price, Rene M.; Whitman, Dean; Melesse, Assefa] Florida Int Univ, Dept Earth & Environm, Miami, FL 33199 USA. [Lagomasino, David; Price, Rene M.] Southeast Environm Res Ctr, Miami, FL USA. [Campbell, Petya K. E.] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. [Campbell, Petya K. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lagomasino, D (reprint author), Univ Space Res Assoc, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM david.lagomasino@nasa.gov RI Campbell, Petya/L-7486-2013; Lagomasino, David/P-8413-2015; Melesse, Assefa/F-9931-2013 OI Campbell, Petya/0000-0002-0505-4951; Lagomasino, David/0000-0003-4008-5363; Melesse, Assefa/0000-0003-4724-9367 FU National Science Foundation through the Florida Coastal Everglades Long-Term Ecological Research program [DBI-0620409, DEB-1237517]; National Aeronautics and Space Administration's Water Science of Coupled Aquatic Processes in Ecosystems from Space (WaterSCAPES) University Research Center program [NNX-10AQ13A]; Everglades National Park [P11AT50508]; Florida Education Fund McKnight Dissertation Year Fellowship FX This material was supported directly by the National Science Foundation through the Florida Coastal Everglades Long-Term Ecological Research program under Grant Nos. DBI-0620409 and DEB-1237517 and the from the National Aeronautics and Space Administration's Water Science of Coupled Aquatic Processes in Ecosystems from Space (WaterSCAPES) University Research Center program under Grant No. NNX-10AQ13A. Additional support was provided by Everglades National Park (Grant No. P11AT50508) and the Florida Education Fund McKnight Dissertation Year Fellowship. The Field Spec Handheld and Field Spec 3 spectroradiometers used in this study were provided by the Goetz Instrument Support Program hosted by Analytical Spectral Devices, Inc. (ASD). This is SERC contribution number 685. NR 98 TC 5 Z9 5 U1 9 U2 50 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 2014 VL 154 SI SI BP 202 EP 218 DI 10.1016/j.rse.2014.08.022 PG 17 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AT8SI UT WOS:000345201900017 ER PT J AU Pahlevan, N Lee, ZP Wei, JW Schaaf, CB Schott, JR Berk, A AF Pahlevan, Nima Lee, Zhongping Wei, Jianwei Schaaf, Crystal B. Schott, John R. Berk, Alexander TI On-orbit radiometric characterization of OLI (Landsat-8) for applications in aquatic remote sensing SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE OLI; Landsat-8; Coastal/inland waters; Radiometric calibration; Ocean color ID OCEAN COLOR SENSORS; AEROSOL OPTICAL-THICKNESS; WATER-LEAVING RADIANCE; ATMOSPHERIC CORRECTION; BIDIRECTIONAL REFLECTANCE; MULTIPLE-SCATTERING; CROSS-CALIBRATION; SEAWIFS; SATELLITE; PRODUCTS AB Landsat-8 carries two separate sensors, namely the Operational Land Imager (OLI) and the Thermal Infrared Radiometer Suite (TIRS), that image the earth surface throughout the visible and thermal portions of the spectrum. Compared to Landsat heritage sensors, the OLI has enhanced features, which include its 12-bit radiometric resolution and the addition of a band centered at 443 nm. The dramatically improved data quality/quantity expands existing applications of Landsat imagery in aquatic sciences from the retrieval of bio-geochemical properties, such as near-surface concentrations of chlorophyll-a (CHL) and total suspended solids (TSS), to benthic mapping. This study offers analysis of OLI's absolute radiometric performance over bodies of water using benchmark observations, namely the top-of-atmosphere (TOA) ocean color observations and marine in situ radiometric measurements. Sensor-to-sensor comparisons are performed to derive gain factors (g(1)) from near-concurrent observations in TOA radiance and reflectance domains. The gains in the radiance domain were further validated/adjusted by determining a second set of gains (g(2)) via analysis of OLI-derived water-leaving radiance, i.e., L-w(lambda), against in situ measurements made either at the Ocean Color AErosol RObotic NETwork (AERONET-OC) sites or during field campaigns. The analyses yield the OLI calibration uncertainties that need to be accounted for when studying aquatic environments. It was found that, for the visible and near-infrared channels, the OLI radiometric responses, on average, are well in agreement (< 2 % discrepancies) with the TOA radiances estimated by ocean color satellites or those predicted by models based on measurements of aquatic and atmospheric properties. However, the TOA radiance at the new 443-nm band is found to be, on average, 3.4 % larger than the reference observations. The inter-sensor comparisons in the reflectance domain, however, indicated slightly different results with the OLI responses being low in the blue bands. To enhance the retrieval accuracy of aquatic-science products from OLI datasets, sets of temporally averaged gains (radiance and reflectance) are derived and recommended for use prior to the retrieval of in-water products. (C) 2014 Elsevier Inc. All rights reserved. C1 [Pahlevan, Nima; Lee, Zhongping; Wei, Jianwei; Schaaf, Crystal B.] Univ Massachusetts, Sch Environm, Boston, MA 02125 USA. [Pahlevan, Nima] NASA, Goddard Space Flight Ctr, Terr Informat Syst Lab, Greenbelt, MD 20771 USA. [Pahlevan, Nima] Sigma Space Corp, Lanham, MD 20706 USA. [Schott, John R.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA. [Berk, Alexander] Spectral Sci Inc, Burlington, MA 01803 USA. RP Pahlevan, N (reprint author), NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA. EM nima.pahlevan@nasa.gov RI wei, Jianwei/E-8031-2016; OI wei, Jianwei/0000-0002-6872-3534; Pahlevan, Nima/0000-0002-5454-5212 FU Air Force Research Laboratories [AFRL-FA8718-05-C-0077]; USGS award [G11PS00422]; NOAA STAR [DG-133E-13-SE-1669]; Spectral Sciences, Inc. FX The authors are grateful to Steven Greb with the Department of Natural Resources of Wisconsin and Roy Armstrong with the University of Puerto Rico, Department of Marine Sciences for their support and assistance during the field campaigns. We would like to thank Giuseppe Zibordi, Susanne Kratzer, Bill Gibson, Alan Weidemann, Brent Holben, Heidi Sosik, Hui Feng, Burton Jones and Curtiss Davis, the principle investigators of the AERONET-OC stations as well as the National Aeronautics and Space Administration for providing data through the AERONET program: http://aeronet.gsfc.nasa.gov. We also would like to thank Fred Hawes with Spectral Sciences Inc. for his code for generating Legendre polynomials from aerosol phase functions, Brian Markham and the Landsat Cal/Val Team for their support and their insights on OL1 calibration, James Storey with NASA GSFC for providing OLI's angle calculator code, Bryan Franz and Sean Bailey with NASA OBPG for their sharing of initial OLI vicarious calibration results, NASA MCST/VCST for providing calibrated MODISA/VIIRS data, Wei Shi and Lide Jiang with NOAA/STAR for the discussions of SNPP-VIIRS, Peter Ma with the Terrestrial Information Systems Lab at NASA GSFC for helping with the graphics, hit Kuster with the Estonian Marine Institute for sharing his field measurements, and Robert Arnone and Sherwin Ladner with the Naval Research Laboratory for sharing their efforts on SNPP-VIIRS validations. The authors appreciate the support by Jeff Dusenberry with the high-performance computing center at the University of Massachusetts Boston. Alexander Berk also acknowledges the IRAD support from Spectral Sciences, Inc. and support from the Air Force Research Laboratories under Contract No. AFRL-FA8718-05-C-0077. Nima Pahlevan, Crystal Schaaf, and Zhongping Lee were supported in part by USGS award G11PS00422. The field campaigns exercised in this study were, in part, supported by NOAA STAR under contract No. DG-133E-13-SE-1669. NR 60 TC 33 Z9 34 U1 4 U2 47 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 2014 VL 154 SI SI BP 272 EP 284 DI 10.1016/j.rse.2014.08.001 PG 13 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AT8SI UT WOS:000345201900023 ER PT J AU Duncanson, LI Cook, BD Hurtt, GC Dubayah, RO AF Duncanson, L. I. Cook, B. D. Hurtt, G. C. Dubayah, R. O. TI An efficient, multi-layered crown delineation algorithm for mapping individual tree structure across multiple ecosystems SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE LiDAR; Forest; Individual tree structure; Crown delineation; Carbon ID LIDAR DATA; BASAL AREA; AIRBORNE LIDAR; DATA FUSION; BIOMASS; FOREST; EXTRACTION; IMAGERY; HEIGHT; VOLUME AB Deriving individual tree information from discrete return, small footprint LiDAR data may improve forest aboveground biomass estimates, and provide tree-level information that is important in many ecological studies. Several crown delineation algorithms have been developed to extract individual tree information from LiDAR point clouds or rasterized canopy height models (CHM), but many of these algorithms have difficulty discriminating between overlapping crowns, and also may fail to detect understory trees. Our approach uses a watershed-based delineation of a CHM, which is subsequently refined using the LiDAR point cloud. Individual tree detection was validated with stem mapped field data from the Smithsonian Environmental Research Center (SERC), Maryland, and on a plot and stand level through comparisons of stem density and basal area to delineated metrics at both SERC and a study area in the Sierra Nevada, California. For individual tree detection, the algorithm correctly identified 70% of dominant trees, 58% of codominant trees, 35% of intermediate trees and 21% of suppressed trees at SERC. The algorithm had difficulty distinguishing between crowns of small, dense understory trees of approximately the same height. Delineated crown volume alone explained 53% and 84% of the variability in basal area at the SERC and Sierra Nevada sites, respectively. The algorithm produced crown area distributions comparable to diameter at breast height (DBH) size class distributions observed in the field in both study sites. The algorithm detected understory crowns better in the conifer-dominated Sierra Nevada site than in the closed-canopy deciduous site in Maryland. The ability for the algorithm to reproduce both accurate tree size distributions and individual crown geometries in two dissimilar and complex forests suggests great promise for applicability to a wide range of forest systems. (C) 2014 Elsevier Inc. All rights reserved. C1 [Duncanson, L. I.; Hurtt, G. C.; Dubayah, R. O.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Cook, B. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Duncanson, LI (reprint author), Univ Maryland, Dept Geog Sci, 2181 Lefrak Hall, College Pk, MD 20742 USA. EM lduncans@umd.edu FU NASA Earth and Space Science Fellowship program [016324-001]; Natural Sciences and Engineering Research Council of Canada (NSERC), Postgraduate Graduate Scholarship D3 FX The authors gratefully acknowledge the NASA Earth and Space Science Fellowship program (grant number 016324-001), and the Natural Sciences and Engineering Research Council of Canada (NSERC), Postgraduate Graduate Scholarship D3, for funding this work. Thank you to the Smithsonian Environmental Research Center and SIGEO program for provision of field data. Specific thanks go to Dr. Geoffrey Parker for data provision and helpful comments on this manuscript. The algorithm was run on the Pleiades supercomputer at NASA Ames through the NASA Earth Exchange (NEX) program. NEX represents a new platform for the Earth science community that provides a mechanism for scientific collaboration and knowledge sharing. NEX combines state-of-the-art supercomputing, Earth system modeling, workflow management, NASA remote sensing data feeds, and a knowledge sharing platform to deliver a complete work environment in which users can explore and analyze large datasets, run modeling codes, collaborate on new or existing projects, and quickly share results among the Earth Science communities. Additional thanks go to Dr. Matthew Brolly, Dr. Naiara Pinto, Dr. Anu Swatatran, Dr. James Kellner, Dr. Jackie Rosette, Justin Fisk, Katelyn Dolan, Benjamin Stewart, the members of the Global Ecology Lab and all those who collected the field data. NR 23 TC 32 Z9 31 U1 11 U2 48 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 2014 VL 154 SI SI BP 378 EP 386 DI 10.1016/j.rse.2013.07.044 PG 9 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AT8SI UT WOS:000345201900032 ER PT J AU Montesano, PM Nelson, RF Dubayah, RO Sun, G Cook, BD Ranson, KJR Raesset, EN Kharuk, V AF Montesano, P. M. Nelson, R. F. Dubayah, R. O. Sun, G. Cook, B. D. Ranson, K. J. R. Raesset, E. N. Kharuk, V. TI The uncertainty of biomass estimates from LiDAR and SAR across a boreal forest structure gradient SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Taiga; Tundra; Ecotone; Lidar; Sar; Uncertainty; Boreal; Forest; Biomass ID MULTISENSOR LIDAR; AIRBORNE LIDAR; CLIMATE-CHANGE; VEGETATION; CARBON; ERRORS; AREA; BACKSCATTER; ECOSYSTEMS; LANDSCAPE AB In this study, we examined the uncertainty of aboveground live biomass (AGB) estimates based on light detection and ranging (LiDAR) and synthetic aperture radar (SAR) measurements distributed across a low-biomass vegetation structure gradient from forest to non-forest in boreal-like ecosystems. The conifer-dominant structure gradient was compiled from ground data amassed from multiple field expeditions in central Maine (USA), Aurskog (Norway), and across central Siberia (Russia). Single variable empirical models were built to model AGB from remote sensing metrics. Using these models, we calculated a root mean square error (RMSE) and a 95% confidence interval (CI) of the RMSE from the difference between the remote sensing AGB predictions and the ground reference AGB estimates within AGB intervals across a 0-100 Mg ha(-1) boreal forest structure gradient. The results show that the error in AGB predictions (RMSE) and the error uncertainty (the CI) from LiDAR and SAR change across a forest gradient. The errors of airborne LiDAR and SAR metrics and spaceborne LiDAR platforms show a general trend of reduced relative errors as AGB magnitudes increase, particularly from 0 to 60 Mg ha(-1). Empirical models relating spaceborne metrics to AGB and estimates of spaceborne LiDAR error uncertainty demonstrate the difficulty of characterizing differences in AGB at the site-level with current spaceborne sensors, particularly below 80 Mg ha(-1) with less than 50-100% error. (C) 2014 Elsevier Inc. All rights reserved. C1 [Montesano, P. M.; Dubayah, R. O.; Sun, G.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Montesano, P. M.] Sigma Space Corp, Lanham, MD 20706 USA. [Nelson, R. F.; Cook, B. D.; Ranson, K. J. R.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. [Raesset, E. N.] Norwegian Univ Life Sci, Dept Ecol & Nat Resource Management, NO-1432 As, Norway. [Kharuk, V.] Russian Acad Sci, Siberian Branch, Sukachev Inst Forest, Krasnoyarsk 660036, Russia. RP Montesano, PM (reprint author), Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. EM paul.m.montesano@nasa.gov RI Ranson, Kenneth/G-2446-2012; Beckley, Matthew/D-4547-2013 OI Ranson, Kenneth/0000-0003-3806-7270; NR 68 TC 13 Z9 13 U1 7 U2 43 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 2014 VL 154 SI SI BP 398 EP 407 DI 10.1016/j.rse.2014.01.027 PG 10 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AT8SI UT WOS:000345201900034 ER PT J AU Leake, JE DeVore, CR Thayer, JP Burns, AG Crowley, G Gilbert, HR Huba, JD Krall, J Linton, MG Lukin, VS Wang, W AF Leake, J. E. DeVore, C. R. Thayer, J. P. Burns, A. G. Crowley, G. Gilbert, H. R. Huba, J. D. Krall, J. Linton, M. G. Lukin, V. S. Wang, W. TI Ionized Plasma and Neutral Gas Coupling in the Sun's Chromosphere and Earth's Ionosphere/Thermosphere SO SPACE SCIENCE REVIEWS LA English DT Review DE Sun; Ionosphere; Thermosphere; Chromosphere ID FARLEY-BUNEMAN INSTABILITY; RAYLEIGH-TAYLOR INSTABILITY; GENERAL-CIRCULATION MODEL; EQUATORIAL SPREAD F; SOLAR-TYPE STARS; ALFVEN WAVES; MAGNETIC-FIELDS; QUIET-SUN; NUMERICAL SIMULATIONS; FILAMENTARY STRUCTURE AB We review physical processes of ionized plasma and neutral gas coupling in the weakly ionized, stratified, electromagnetically-permeated regions of the Sun's chromosphere and Earth's ionosphere/thermosphere. Using representative models for each environment we derive fundamental descriptions of the coupling of the constituent parts to each other and to the electric and magnetic fields, and we examine the variation in magnetization of the components. Using these descriptions we compare related phenomena in the two environments, and discuss electric currents, energy transfer and dissipation. We present examples of physical processes that occur in both atmospheres, the descriptions of which have previously been conducted in contrasting paradigms, that serve as examples of how the chromospheric and ionospheric communities can further collaborate. We also suggest future collaborative studies that will help improve our understanding of these two different atmospheres, which while sharing many similarities, also exhibit large disparities in key quantities. C1 [Leake, J. E.] George Mason Univ, Fairfax, VA 22030 USA. [Huba, J. D.; Krall, J.; Linton, M. G.; Lukin, V. S.] Naval Res Lab, Washington, DC 20375 USA. [DeVore, C. R.; Gilbert, H. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Thayer, J. P.] Univ Colorado, Boulder, CO 80309 USA. [Burns, A. G.; Wang, W.] NCAR, Boulder, CO 80307 USA. [Crowley, G.] Atmospher & Space Technol Res Associates, Boulder, CO 80301 USA. RP Leake, JE (reprint author), George Mason Univ, Fairfax, VA 22030 USA. EM jleake@gmu.edu RI DeVore, C/A-6067-2015; Burns, Alan/L-1547-2013; Wang, Wenbin/G-2596-2013; THAYER, JEFFREY P./B-7264-2016 OI DeVore, C/0000-0002-4668-591X; Wang, Wenbin/0000-0002-6287-4542; THAYER, JEFFREY P./0000-0001-7127-8251 FU NASA's Living with a Star (LWS) Targeted Research and Technology (TRT) program; NASA's "Living with a Star" Targeted Research and Technology program "Plasma-Neutral Gas Coupling in the Chromosphere and Ionosphere"; National Science Foundation FX This work was supported by NASA's Living with a Star (LWS) Targeted Research and Technology (TR&T) program. Numerical simulations were performed under a grant of computer time from the Department of Defense (DoD) High Performance Computing (HPC) program. The Authors thank the anonymous referees who contributed significantly to the improvement of this manuscript.; This work was funded by NASA's "Living with a Star" Targeted Research and Technology program "Plasma-Neutral Gas Coupling in the Chromosphere and Ionosphere". Numerical simulations were performed using a grant of computer time from the DoD High Performance Computing Program. NCAR is sponsored by the National Science Foundation. NR 151 TC 11 Z9 11 U1 0 U2 16 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD NOV PY 2014 VL 184 IS 1-4 BP 107 EP 172 DI 10.1007/s11214-014-0103-1 PG 66 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AU0NJ UT WOS:000345319600004 ER PT J AU Niezrecki, C Avitabile, P Chen, JL Sherwood, J Lundstrom, T LeBlanc, B Hughes, S Desmond, M Beattie, A Rumsey, M Klute, SM Pedrazzani, R Werlink, R Newman, J AF Niezrecki, Christopher Avitabile, Peter Chen, Julie Sherwood, James Lundstrom, Troy LeBlanc, Bruce Hughes, Scott Desmond, Michael Beattie, Alan Rumsey, Mark Klute, Sandra M. Pedrazzani, Renee Werlink, Rudy Newman, John TI Inspection and monitoring of wind turbine blade-embedded wave defects during fatigue testing SO STRUCTURAL HEALTH MONITORING-AN INTERNATIONAL JOURNAL LA English DT Article DE Digital image correlation; shearography; fiber-optic sensing; damage detection; composites; wind turbine blade; defect AB The research presented in this article focuses on a 9-m CX-100 wind turbine blade, designed by a team led by Sandia National Laboratories and manufactured by TPI Composites Inc. The key difference between the 9-m blade and baseline CX-100 blades is that this blade contains fabric wave defects of controlled geometry inserted at specified locations along the blade length. The defect blade was tested at the National Wind Technology Center at the National Renewable Energy Laboratory using a schedule of cycles at increasing load level until failure was detected. Researchers used digital image correlation, shearography, acoustic emission, fiber-optic strain sensing, thermal imaging, and piezoelectric sensing as structural health monitoring techniques. This article provides a comparison of the sensing results of these different structural health monitoring approaches to detect the defects and track the resultant damage from the initial fatigue cycle to final failure. C1 [Niezrecki, Christopher; Avitabile, Peter; Chen, Julie; Sherwood, James; Lundstrom, Troy; LeBlanc, Bruce] Univ Massachusetts, Dept Mech Engn, Lowell, MA 01854 USA. [Hughes, Scott; Desmond, Michael] Natl Renewable Energy Lab, Golden, CO USA. [Beattie, Alan; Rumsey, Mark] Sandia Natl Labs, Albuquerque, NM 87185 USA. [Klute, Sandra M.; Pedrazzani, Renee] Luna Innovations Inc, Blacksburg, VA USA. [Werlink, Rudy] NASA, Kennedy Space Ctr, Merritt Isl, FL USA. [Newman, John] Laser Technol Inc, Norristown, PA USA. RP Niezrecki, C (reprint author), Univ Massachusetts, Lowell, MA 01854 USA. EM Christopher_Niezrecki@uml.edu FU US Department of Energy (DOE) [DE-EE001374]; US Department of Energy's National Nuclear Security Administration [DE-AC04-94AL85000] FX The authors appreciate the financial support for this work provided by the US Department of Energy (DOE) (DE-EE001374). Any opinions, findings, conclusions, or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of DOE. Sandia National Laboratories is a multi-program laboratory managed and operated by Sandia Corporation, a wholly owned subsidiary of Lockheed Martin Corporation, for the US Department of Energy's National Nuclear Security Administration under contract DE-AC04-94AL85000. NR 24 TC 6 Z9 7 U1 1 U2 27 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1475-9217 EI 1741-3168 J9 STRUCT HEALTH MONIT JI Struct. Health Monit. PD NOV PY 2014 VL 13 IS 6 BP 629 EP 643 DI 10.1177/1475921714532995 PG 15 WC Engineering, Multidisciplinary; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA AT9EQ UT WOS:000345231200007 ER PT J AU Sherwood, B AF Sherwood, Brent TI WHAT NEXT FOR HUMAN SPACE FLIGHT? SO ARCHITECTURAL DESIGN LA English DT Article AB Space travel is undergoing a significant period of transformation. While exploration in the last six decades has been driven by government-funded exploration by the major powers, the possibilities are now opening up for a Space Architecture that diversifies and caters for leisure, large-scale industrialization and permanent settlement. Experienced space architect Brent Sherwood brings into focus four potential futures for human space flight - experiencing, exploring, exploiting and settling. RP Sherwood, B (reprint author), Jet Prop Lab, Pasadena, CA 91109 USA. NR 7 TC 0 Z9 0 U1 2 U2 8 PU WILEY PERIODICALS, INC PI SAN FRANCISCO PA ONE MONTGOMERY ST, SUITE 1200, SAN FRANCISCO, CA 94104 USA SN 0003-8504 EI 1554-2769 J9 ARCHIT DESIGN JI Archit. Des. PD NOV-DEC PY 2014 VL 84 IS 6 SI SI BP 16 EP 19 DI 10.1002/ad.1827 PG 4 WC Architecture SC Architecture GA AT2ZB UT WOS:000344802200003 ER PT J AU Howe, AS AF Howe, A. Scott TI ARCHITECTURE FOR OTHER PLANETS SO ARCHITECTURAL DESIGN LA English DT Article AB Opportunities for Space Architecture are proliferating over time. As NASA architect and robotics engineer A Scott Howe, however, explains, a varied skill set is required to develop the right specialist expertise to become a space architect. Extreme environmental factors always have to be taken into consideration when designing for Space. These vary from lack of gravity, extreme variations in temperature and exposure to abrasive materials, such as lunar dust. Architects also need to develop an acute awareness of transportation systems and robotic constructions. It is, though, only with prototyping that designs, systems and materials can start to be tested. C1 CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. RP Howe, AS (reprint author), CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91125 USA. NR 5 TC 0 Z9 0 U1 0 U2 3 PU WILEY PERIODICALS, INC PI SAN FRANCISCO PA ONE MONTGOMERY ST, SUITE 1200, SAN FRANCISCO, CA 94104 USA SN 0003-8504 EI 1554-2769 J9 ARCHIT DESIGN JI Archit. Des. PD NOV-DEC PY 2014 VL 84 IS 6 SI SI BP 36 EP 39 DI 10.1002/ad.1830 PG 4 WC Architecture SC Architecture GA AT2ZB UT WOS:000344802200006 ER PT J AU Adams, C Jones, R AF Adams, Constance Jones, Rod TI ALPHA FROM THE INTERNATIONAL STYLE TO THE INTERNATIONAL SPACE STATION SO ARCHITECTURAL DESIGN LA English DT Article AB How has a Modernist predilection for the modular contributed to the design of Space Architecture? Leading space architects Constance Adams and Rod Jones highlight how by embracing a diligent modularity in the early 1980s, NASA initiated a design approach that has enabled replicability, flexibility and technological transparency, and has proved the International Space Station resilient in the face of multiple logistical, financial and political challenges. C1 [Adams, Constance] Synth Int, San Juan, PR 00919 USA. [Jones, Rod] NASA, Int Space Stn, Washington, DC USA. RP Adams, C (reprint author), Synth Int, San Juan, PR 00919 USA. NR 6 TC 1 Z9 1 U1 1 U2 3 PU WILEY PERIODICALS, INC PI SAN FRANCISCO PA ONE MONTGOMERY ST, SUITE 1200, SAN FRANCISCO, CA 94104 USA SN 0003-8504 EI 1554-2769 J9 ARCHIT DESIGN JI Archit. Des. PD NOV-DEC PY 2014 VL 84 IS 6 SI SI BP 70 EP 77 DI 10.1002/ad.1835 PG 8 WC Architecture SC Architecture GA AT2ZB UT WOS:000344802200011 ER PT J AU Cohen, MM AF Cohen, Marc M. TI BEING A SPACE ARCHITECT SO ARCHITECTURAL DESIGN LA English DT Article AB A space architect for NASA for over 25 years and now the founding principal of Astrotecture, Marc M Cohen highlights how Space Architecture as a discipline differentiates itself from architecture, its terrestrial cousin, by designing structures for the most extreme of environmental conditions. He discusses three design projects undertaken by Astrotecture and funded by NASA that emphasise the level of physical problem-solving involved in astronautical design. C1 [Cohen, Marc M.] NASA, Ames Res Ctr, Washington, DC 20546 USA. [Cohen, Marc M.] Space Stn Programme, Washington, DC USA. [Cohen, Marc M.] Northrop Grumman Aerosp Syst, Los Angeles, CA USA. [Cohen, Marc M.] Marc M Cohen Architect PC, Moffett Field, CA USA. RP Cohen, MM (reprint author), NASA, Ames Res Ctr, Washington, DC 20546 USA. NR 7 TC 0 Z9 0 U1 1 U2 1 PU WILEY PERIODICALS, INC PI SAN FRANCISCO PA ONE MONTGOMERY ST, SUITE 1200, SAN FRANCISCO, CA 94104 USA SN 0003-8504 EI 1554-2769 J9 ARCHIT DESIGN JI Archit. Des. PD NOV-DEC PY 2014 VL 84 IS 6 SI SI BP 78 EP 81 DI 10.1002/ad.1836 PG 4 WC Architecture SC Architecture GA AT2ZB UT WOS:000344802200012 ER PT J AU Losee, JP Miller, JA Peterson, WT Teel, DJ Jacobson, KC AF Losee, James P. Miller, Jessica A. Peterson, William T. Teel, David J. Jacobson, Kym C. TI Influence of ocean ecosystem variation on trophic interactions and survival of juvenile coho and Chinook salmon SO CANADIAN JOURNAL OF FISHERIES AND AQUATIC SCIENCES LA English DT Article ID NORTHERN CALIFORNIA CURRENT; COLUMBIA-RIVER; ONCORHYNCHUS-TSHAWYTSCHA; PACIFIC SALMON; PARASITE COMMUNITIES; MARINE SURVIVAL; HELMINTH-PARASITES; ILLEX-COINDETII; FEEDING ECOLOGY; JACK MACKEREL AB The community of trophically transmitted marine parasites of juvenile coho (Oncorhynchus kisutch) and Chinook (Oncorhynchus tshawytscha) salmon across 8 years (2002-2009) was related to indices of physical and biological ocean conditions and adult returns. When the biomass of lipid-poor, southern origin copepods in the coastal ocean was high during juvenile salmon outmigration from fresh water (April-June), yearling coho and Chinook salmon harbored a different trophically transmitted parasite fauna and exhibited lower survival compared with years when the southern copepod biomass was low. As copepods are key intermediate hosts in many marine parasite life cycles, these results support a trophic linkage between the copepod community and salmon prey. Interannual variation in the parasite community was correlated with survival of coho salmon (r = -0.67) measured 1 year later and adult returns of Upper Columbia River summer and fall Chinook salmon (r = -0.94) 3 years from the time of ocean entry. C1 [Losee, James P.] Washington Dept Fish & Wildlife, North Olympia, WA 98501 USA. [Losee, James P.; Miller, Jessica A.] Oregon State Univ, Coastal Oregon Marine Expt Stn, Dept Fisheries & Wildlife, Newport, OR 97365 USA. [Peterson, William T.; Jacobson, Kym C.] NOAA, Newport Res Stn, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. [Teel, David J.] NOAA, Manchester Res Stn, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Manchester, WA 98353 USA. RP Losee, JP (reprint author), 600 Capitol Way N, Olympia, WA 98501 USA. EM james.losee@dfw.wa.gov FU Bonneville Power Administration [00053808]; Oregon State University's Cooperative Institute for Marine Resources Studies; National Oceanic and Atmospheric Administration (NOAA); Mamie Markham Research Award; Neil Armantrout Scholarship from Oregon State University FX Bruce McCune assisted in data analysis, and the crew of the F/V Frosti and many scientists assisted in collection of samples at sea and in the lab. In particular, we thank Antonio Baptista, Jennifer Fisher, Cheryl Morgan, Jay Peterson, Joe Needoba, Tawnya Peterson, Laurie Weitkamp, David Kuligowski, Donald Van Doornik, Andrew Claiborne, Andrew Claxton, Mary Beth Rew, and Kate Losee. Funding for this study was provided by the Bonneville Power Administration (contract No. 00053808), Oregon State University's Cooperative Institute for Marine Resources Studies, the National Oceanic and Atmospheric Administration (NOAA), Mamie Markham Research Award, and the Neil Armantrout Scholarship from Oregon State University. We appreciate the helpful comments of anonymous reviewers on earlier versions of this manuscript. NR 72 TC 2 Z9 2 U1 2 U2 18 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA SN 0706-652X EI 1205-7533 J9 CAN J FISH AQUAT SCI JI Can. J. Fish. Aquat. Sci. PD NOV PY 2014 VL 71 IS 11 BP 1747 EP 1757 DI 10.1139/cjfas-2014-0043 PG 11 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA AT0CN UT WOS:000344604800014 ER PT J AU Cook, BI Smerdon, JE Seager, R Coats, S AF Cook, Benjamin I. Smerdon, Jason E. Seager, Richard Coats, Sloan TI Global warming and 21st century drying SO CLIMATE DYNAMICS LA English DT Article ID FUTURE CLIMATE-CHANGE; ELEVATED CO2; HYDROLOGICAL CYCLE; EXTREME-WEATHER; DROUGHT INDEX; GREAT-PLAINS; WATER; CARBON; EVAPOTRANSPIRATION; PRECIPITATION AB Global warming is expected to increase the frequency and intensity of droughts in the twenty-first century, but the relative contributions from changes in moisture supply (precipitation) versus evaporative demand (potential evapotranspiration; PET) have not been comprehensively assessed. Using output from a suite of general circulation model (GCM) simulations from phase 5 of the Coupled Model Intercomparison Project, projected twenty-first century drying and wetting trends are investigated using two offline indices of surface moisture balance: the Palmer Drought Severity Index (PDSI) and the Standardized Precipitation Evapotranspiration Index (SPEI). PDSI and SPEI projections using precipitation and Penman-Monteith based PET changes from the GCMs generally agree, showing robust cross-model drying in western North America, Central America, the Mediterranean, southern Africa, and the Amazon and robust wetting occurring in the Northern Hemisphere high latitudes and east Africa (PDSI only). The SPEI is more sensitive to PET changes than the PDSI, especially in arid regions such as the Sahara and Middle East. Regional drying and wetting patterns largely mirror the spatially heterogeneous response of precipitation in the models, although drying in the PDSI and SPEI calculations extends beyond the regions of reduced precipitation. This expansion of drying areas is attributed to globally widespread increases in PET, caused by increases in surface net radiation and the vapor pressure deficit. Increased PET not only intensifies drying in areas where precipitation is already reduced, it also drives areas into drought that would otherwise experience little drying or even wetting from precipitation trends alone. This PET amplification effect is largest in the Northern Hemisphere mid-latitudes, and is especially pronounced in western North America, Europe, and southeast China. Compared to PDSI projections using precipitation changes only, the projections incorporating both precipitation and PET changes increase the percentage of global land area projected to experience at least moderate drying (PDSI standard deviation of B-1) by the end of the twenty-first century from 12 to 30 %. PET induced moderate drying is even more severe in the SPEI projections (SPEI standard deviation of <=-1; 11 to 44 %), although this is likely less meaningful because much of the PET induced drying in the SPEI occurs in the aforementioned arid regions. Integrated accounting of both the supply and demand sides of the surface moisture balance is therefore critical for characterizing the full range of projected drought risks tied to increasing greenhouse gases and associated warming of the climate system. C1 [Cook, Benjamin I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Smerdon, Jason E.; Seager, Richard; Coats, Sloan] Lamont Doherty Earth Observ, Palisades, NY 10964 USA. RP Cook, BI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM benjamin.i.cook@nasa.gov RI Smerdon, Jason/F-9952-2011; Cook, Benjamin/H-2265-2012 FU NOAA award Global Decadal Hydroclimate Variability and Change [NA10 OAR431037]; DOE [DE-SC0005107]; NSF [AGS-1243204]; NOAA [NA10OAR4310137]; NASA FX We acknowledge the World Climate Research Programme's Working Group on Coupled Modelling, which is responsible for CMIP, and we thank the climate modeling groups (listed in Table 1 of this paper) for producing and making available their model output. For CMIP, the U. S. Department of Energy's Program for Climate Model Diagnosis and Intercomparison provides coordinating support and led development of software infrastructure in partnership with the Global Organization for Earth System Science Portals. All derived PDSI and SPEI fields are available for download from http://www.ldeo.columbia.edu/similar to jsmerdon/2014_clidyn_cooketal_supplement.html Haibo Liu and Naomi Henderson provided computational support at LDEO. RS and JES were supported in part by the NOAA award Global Decadal Hydroclimate Variability and Change (NA10 OAR431037). RS was also supported by DOE award DE-SC0005107. Further support came from NSF award AGS-1243204 and NOAA award NA10OAR4310137. BIC was supported by NASA. LDEO Publication number #7758. We thank two anonymous reviewers for comments that greatly improved the quality of this manuscript. NR 73 TC 70 Z9 74 U1 40 U2 175 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 EI 1432-0894 J9 CLIM DYNAM JI Clim. Dyn. PD NOV PY 2014 VL 43 IS 9-10 BP 2607 EP 2627 DI 10.1007/s00382-014-2075-y PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AS8DJ UT WOS:000344480100016 ER PT J AU Memarsadeghi, N McFadden, L AF Memarsadeghi, Nargess McFadden, Lucy TI NASA Computational Case Study: Where Is My Moon? SO COMPUTING IN SCIENCE & ENGINEERING LA English DT Article ID IRREGULAR SATELLITES; COMPLETENESS; LIMITS AB A moon or natural satellite is a celestial body that orbits a planet, dwarf planet, or an asteroid. Several reasons motivate discovering and studying moons of planetary bodies. Here, we learn how astronomers search for moons of planetary bodies or perform satellite search. In particular, we look for moons of Pluto using Hubble Space Telescope's data. C1 [Memarsadeghi, Nargess] NASA, Goddard Space Flight Ctr, Sci Data Syst Branch, Washington, DC 20546 USA. [McFadden, Lucy] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Washington, DC USA. RP Memarsadeghi, N (reprint author), NASA, Goddard Space Flight Ctr, Sci Data Syst Branch, Washington, DC 20546 USA. EM nargess.memarsadeghi@nasa.gov; lucyann.a.mcfadden@nasa.gov OI McFadden, Lucy/0000-0002-0537-9975 FU US National Science Foundation FX We thank Max Mutchler for helping us with the Hubble datasets used in this case study, and for answering our many questions about his past work on discovering Pluto's moons, Nix and Hydra. We're grateful to Henry Freudenreich for helping us with the resistant mean algorithm. We also thank David Skillman for his helpful comments and advice. We're grateful to Delaram Kahrobaei's students at New York City College of Technology (CUNY) during Spring 2012 for beta testing this case study. Students were supported by the "Emerging Scholar Fellowship," a US National Science Foundation grant awarded to Pamela Brown. NR 22 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA SN 1521-9615 EI 1558-366X J9 COMPUT SCI ENG JI Comput. Sci. Eng. PD NOV-DEC PY 2014 VL 16 IS 6 BP 92 EP 99 PG 8 WC Computer Science, Interdisciplinary Applications SC Computer Science GA AT3OM UT WOS:000344843900011 ER PT J AU E-Martin, Y R-Moreno, MD Smith, DE AF E-Martin, Yolanda R-Moreno, Maria D. Smith, David E. TI Progressive heuristic search for probabilistic planning based on interaction estimates SO EXPERT SYSTEMS LA English DT Article DE probabilistic planning; planning graphs; interaction; heuristic search AB Development of real planning and scheduling applications often requires the ability to handle uncertainty. Often this uncertainty is represented using probability information on the initial conditions and on the outcomes of actions. In this paper, we describe a novel probabilistic plan graph heuristic that computes information about the interaction between actions and between propositions. This information is used to find better relaxed plans and to compute their probability of success. This information guides a forward state space search for high probability, non-branching seed plans. These plans are then used in a planning and scheduling system that handles unexpected outcomes by runtime replanning. We briefly describe the heuristic, the search process, and the results on different domains from recent international planning competitions. We discuss the results of this study and some of the issues involved in advancing this work further. C1 [E-Martin, Yolanda] USRA, Mountain View, CA 94043 USA. [E-Martin, Yolanda; R-Moreno, Maria D.] Univ Alcala de Henares, Dept Automat, Madrid 28871, Spain. [Smith, David E.] NASA, Intelligent Syst Div, Ames Res Ctr, Moffett Field, CA 94035 USA. RP E-Martin, Y (reprint author), USRA, 615 Natl Ave,Suite 220, Mountain View, CA 94043 USA. EM yolanda@aut.uah.es; mdolores@aut.uah.es; david.smith@nasa.gov FU Junta de Comunidades de Castilla-La Mancha [PEII11-0079-8929]; Universities Space Research Association (USRA); NASA Ames Research Center; Spanish CDTI project COLSUVH FX This work has been partially funded by the Junta de Comunidades de Castilla-La Mancha project PEII11-0079-8929, the Universities Space Research Association (USRA), and the NASA Ames Research Center. The second author is funded by the Spanish CDTI project COLSUVH. NR 29 TC 1 Z9 1 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0266-4720 EI 1468-0394 J9 EXPERT SYST JI Expert Syst. PD NOV PY 2014 VL 31 IS 5 SI SI BP 421 EP 436 DI 10.1111/exsy.12037 PG 16 WC Computer Science, Artificial Intelligence; Computer Science, Theory & Methods SC Computer Science GA AT3PW UT WOS:000344847300005 ER PT J AU Graham, WM Gelcich, S Robinson, KL Duarte, CM Brotz, L Purcell, JE Madin, LP Mianzan, H Sutherland, KR Uye, S Pitt, KA Lucas, CH Bogeberg, M Brodeur, RD Condon, RH AF Graham, William M. Gelcich, Stefan Robinson, Kelly L. Duarte, Carlos M. Brotz, Lucas Purcell, Jennifer E. Madin, Laurence P. Mianzan, Hermes Sutherland, Kelly R. Uye, Shin-ichi Pitt, Kylie A. Lucas, Cathy H. Bogeberg, Molly Brodeur, Richard D. Condon, Rolert H. TI Linking human well-being and jellyfish: ecosystem services, impacts, and societal responses SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT LA English DT Review ID GELATINOUS ZOOPLANKTON; BIODIVERSITY; COASTAL; BLOOMS; OCEAN; GULF; SEA; ASSOCIATIONS; CALIFORNIA; WATERS AB Jellyfish are usually perceived as harmful to humans and are seen as "pests". This negative perception has hindered knowledge regarding their value in terms of ecosystem services. As humans increasingly modify and interact with coastal ecosystems, it is important to evaluate the benefits and costs of jellyfish, given that jellyfish bloom size, frequency, duration, and extent are apparently increasing in some regions of the world. Here we explore those benefits and costs as categorized by regulating, supporting, cultural, and provisioning ecosystem services. A geographical perspective of human vulnerability to jellyfish over four categories of human well-being (health care, food, energy, and freshwater production) is also discussed in the context of thresholds and trade-offs to enable social adaptation. Whereas beneficial services provided by jellyfish likely scale linearly with biomass (perhaps peaking at a saturation point), non-linear thresholds exist for negative impacts to ecosystem services. We suggest that costly adaptive strategies will outpace the beneficial services if jellyfish populations continue to increase in the future. C1 [Graham, William M.; Robinson, Kelly L.] Univ So Mississippi, Dept Marine Sci, Stennis Space Ctr, MS 39529 USA. [Gelcich, Stefan] Pontificia Univ Catolica Chile, Lab Int Cambio Global, Fac Ciencias Biol, Santiago, Chile. [Gelcich, Stefan] Pontificia Univ Catolica Chile, Ctr Appl Ecol & Sustainabil, Fac Ciencias Biol, Santiago, Chile. [Duarte, Carlos M.] Inst Mediterraneo Estudios Avanzaaos IMEDEA, Dept Global Change Res, Esporles, Spain. [Duarte, Carlos M.] Univ Western Australia, UWA Oceans Inst, Crawley, Australia. [Duarte, Carlos M.] Univ Western Australia, Sch Plant Biol, Crawley, Australia. [Brotz, Lucas] Univ British Columbia, Sea Us Project, Fisheries Ctr, Vancouver, BC V5Z 1M9, Canada. [Brotz, Lucas] Univ British Columbia, Dept Zool, Vancouver, BC V5Z 1M9, Canada. [Purcell, Jennifer E.] Shannon Point Marine Ctr, Anacortes, WA USA. [Madin, Laurence P.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. [Mianzan, Hermes] Inst Nacl Invest & Desarrollo Pesquero, Mar Del Plata, Buenos Aires, Argentina. [Sutherland, Kelly R.] Univ Oregon, Dept Biol, Eugene, OR 97403 USA. [Uye, Shin-ichi] Hiroshima Univ, Grad Sch Biosphere Sci, Higashihiroshima 724, Japan. [Pitt, Kylie A.] Griffith Univ, Australian Rivers Inst, Gold Coast, Australia. [Pitt, Kylie A.] Griffith Univ, Griffith Sch Environm, Gold Coast, Australia. [Lucas, Cathy H.] Univ Southampton, Natl Oceanog Ctr, Southampton, Hants, England. [Bogeberg, Molly] Dauphin Isl Sea Lab, Dauphin Isl, AL USA. [Brodeur, Richard D.] NOAA, Natl Marine Fisheries Serv, Newport, OR USA. [Condon, Rolert H.] Univ N Carolina, Dept Biol & Marine Biol, Wilmington, NC 28401 USA. RP Graham, WM (reprint author), Univ So Mississippi, Dept Marine Sci, Stennis Space Ctr, MS 39529 USA. EM monty.graham@usm.edu RI Duarte, Carlos M/A-7670-2013; Pitt, Kylie/N-7421-2014 OI Duarte, Carlos M/0000-0002-1213-1361; Pitt, Kylie/0000-0002-2292-2052 FU National Center for Ecological Analysis and Synthesis comes from National Science Foundation [DEB-94-21535]; University of California at Santa Barbara; State of California FX Funding for the National Center for Ecological Analysis and Synthesis comes from National Science Foundation Grant DEB-94-21535, the University of California at Santa Barbara, and the State of California. We thank S Piraino for suggested references. NR 57 TC 7 Z9 8 U1 13 U2 96 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1540-9295 EI 1540-9309 J9 FRONT ECOL ENVIRON JI Front. Ecol. Environ. PD NOV PY 2014 VL 12 IS 9 BP 515 EP 523 DI 10.1890/130298 PG 9 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA AT3PK UT WOS:000344846200016 ER PT J AU Nessel, JA Manning, RM AF Nessel, James A. Manning, Robert M. TI Derivation of Microwave Refractive Index Structure Constant (C-n(2)) of the Atmosphere From K-Band Interferometric Phase Measurements SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION LA English DT Article DE Antenna arrays; atmospheric propagation; interferometry; microwave propagation ID TURBULENCE; VARIABILITY; TROPOSPHERE; RADAR; DELAY AB Differential phase data has been collected using a site test interferometer (STI) at K-band for several years at various NASA ground station sites, including the NASA Deep Space Network (DSN) in Goldstone, CA, and the NASA Space Network (SN) sites in White Sands, NM, and Guam. An objective of this work is to characterize the site-dependent atmospheric phase stability to determine the viability of that site for arraying applications. A useful figure of merit to quantify this effect is the determination of the microwave refractive index structure constant, C-n(2), which is highly dependent on variations in the water vapor concentration of the troposphere. In this paper, a method is proposed to derive C-n(2) from a two-element site test interferometer utilizing temporal phase structure function information. In this way, a path-averaged C-n(2) at each ground station site is determined which can be used in the design and expected system performance of future Ka-band communication systems in an arrayed architecture. Statistical characterization of microwave C-n(2) indicates that a mean value of 2.04 x 10(-14), 2.08 x 10(-14) and 9.8 x 10(-13) is expected for Goldstone, CA, White Sands, NM, and Guam, respectively. C1 [Nessel, James A.; Manning, Robert M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Nessel, JA (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM james.a.nessel@nasa.gov; robert.m.manning@nasa.gov FU NASA's Space Communications and Navigation (SCaN) Program under the Human Exploration and Operations Mission Directorate (HEOMD) FX Manuscript received November 25, 2013; revised June 03, 2014; accepted July 16, 2014. Date of publication August 14, 2014; date of current version October 28, 2014. This work was supported in part by the NASA's Space Communications and Navigation (SCaN) Program under the Human Exploration and Operations Mission Directorate (HEOMD). NR 25 TC 0 Z9 1 U1 0 U2 12 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-926X EI 1558-2221 J9 IEEE T ANTENN PROPAG JI IEEE Trans. Antennas Propag. PD NOV PY 2014 VL 62 IS 11 BP 5590 EP 5598 DI 10.1109/TAP.2014.2347997 PG 9 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA AS9WI UT WOS:000344588900019 ER PT J AU Liao, L Meneghini, R Tokay, A AF Liao, Liang Meneghini, Robert Tokay, Ali TI Uncertainties of GPM DPR Rain Estimates Caused by DSD Parameterizations SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article DE Algorithms; Radars; Radar observations; Remote sensing ID DROP-SIZE DISTRIBUTION; POLARIMETRIC RADAR MEASUREMENTS; DUAL-WAVELENGTH RADAR; RETRIEVAL; DISTRIBUTIONS; ALGORITHM; MODEL; SHAPE AB A framework based on measured raindrop size distribution (DSD) data has been developed to assess uncertainties in DSD models employed in Ku- and Ka-band dual-wavelength radar retrievals. In this study, the rain rates and attenuation coefficients from DSD parameters derived by dual-wavelength algorithms are compared with those directly obtained from measured DSD spectra. The impact of the DSD gamma parameterizations on rain estimation from the Global Precipitation Measurement mission (GPM) Dual-Frequency Precipitation Radar (DPR) is examined for the cases of a fixed shape factor as well as for a constrained that is, a - relation (a relationship between the shape parameter and slope parameter of the gamma DSD)by using 11 Particle Size and Velocity (Parsivel) disdrometer measurements with a total number of about 50 000 one-minute spectra that were collected during the Iowa Flood Studies (IFloodS) experiment. It is found that the DPR-like dual-wavelength techniques provide fairly accurate estimates of rain rate and attenuation if a fixed- gamma DSD model is used, with the value of ranging from 3 to 6. Comparison of the results reveals that the retrieval errors from the - relations are generally small, with biases of less than +/- 10%, and are comparable to the results from a fixed- gamma model with equal to 3 and 6. The DSD evaluation procedure is also applied to retrievals in which a lognormal DSD model is used. C1 [Liao, Liang] Morgan State Univ, Goddard Earth Sci & Technol Ctr, Greenbelt, MD USA. [Meneghini, Robert; Tokay, Ali] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tokay, Ali] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. RP Liao, L (reprint author), NASA, Goddard Space Flight Ctr, Goddard Earth Sci Technol MSU, Code 612, Greenbelt, MD 20771 USA. EM liang.liao-1@nasa.gov RI Measurement, Global/C-4698-2015 FU NASA Headquarters under NASA's Precipitation Measurement Mission (PMM) [NNH12ZDA001N-PMM] FX This work is supported by Dr. R. Kakar of NASA Headquarters under NASA's Precipitation Measurement Mission (PMM) Grant NNH12ZDA001N-PMM. The authors also thank the IFloodS Science Team for providing Parsivel disdrometer data. NR 29 TC 10 Z9 10 U1 5 U2 10 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD NOV PY 2014 VL 53 IS 11 BP 2524 EP 2537 DI 10.1175/JAMC-D-14-0003.1 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AT4UL UT WOS:000344938500007 ER PT J AU Rabenhorst, S Whiteman, DN Zhang, DL Demoz, B AF Rabenhorst, S. Whiteman, D. N. Zhang, D. -L. Demoz, B. TI A Case Study of Mid-Atlantic Nocturnal Boundary Layer Events during WAVES 2006 SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article DE Downslope winds; Boundary layer; Diurnal effects; Jets; Mesoscale processes; Profilers; atmospheric ID LOW-LEVEL JET; SOUTHERN GREAT-PLAINS; RAMAN LIDAR MEASUREMENTS; WEAK WIND CONDITIONS; WATER-VAPOR; DOWNSLOPE WINDS; SLOPING TERRAIN; COMPLEX-TERRAIN; PART I; CLIMATOLOGY AB The Water Vapor Variability-Satellite/Sondes (WAVES) 2006 field campaign provided a contiguous 5-day period of concentrated high-resolution measurements to examine finescale boundary layer phenomena under the influence of a summertime subtropical high over the mid-Atlantic region that is characterized by complex geography. A holistic analytical approach to low-level wind observations was adopted to identify the low-level flow structures and patterns of evolution on the basis of airmass properties and origination. An analysis of the measurements and the other available observations is consistent with the classic depiction of the daytime boundary layer development but revealed a pronounced diurnal cycle that was categorized into three stages: (i) daytime growth of the convective boundary layer, (ii) flow intensification into a low-level jet regime after dusk, and (iii) interruption by a downslope wind regime after midnight. The use of the field campaign data allows for the differentiation of the latter two flow regimes by their directions with respect to the orientation of the Appalachian Mountains and their airmass origins. Previous studies that have investigated mountain flows and low-level jet circulations have focused on regions with overt geographic prominence, stark gradients, or frequent reoccurrences, whereby such meteorological phenomena exhibit a clear signature and can be easily isolated and diagnosed. The results of this study provide evidence that similar circulation patterns operate in nonclassic locations with milder topography and atmospheric gradients, such as the mid-Atlantic region. The new results have important implications for the understanding of the mountain-forced flows and some air quality problems during the nocturnal period. C1 [Rabenhorst, S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Whiteman, D. N.] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Lab, Greenbelt, MD 20771 USA. [Zhang, D. -L.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Demoz, B.] Howard Univ, Dept Phys & Astron, Washington, DC 20059 USA. RP Rabenhorst, S (reprint author), Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. EM sraben1@umbc.edu RI Zhang, Da-Lin/F-2634-2010 OI Zhang, Da-Lin/0000-0003-1725-283X FU NASA Atmospheric Composition Program; Aura Validation project FX This research was funded under the NASA Atmospheric Composition Program and occurred within the NASA GSFC Mesoscale Atmospheric Processes Laboratory. We acknowledge the Aura Validation project for funding the WAVES campaign. We thank Howard University and the Maryland Department of the Environment for use of their instrument data. NR 61 TC 0 Z9 0 U1 2 U2 9 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD NOV PY 2014 VL 53 IS 11 BP 2627 EP 2648 DI 10.1175/JAMC-D-13-0350.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AT4UL UT WOS:000344938500013 ER PT J AU Mark, S Scott, GBI Donoviel, DB Leveton, LB Mahoney, E Charles, JB Siegel, B AF Mark, Saralyn Scott, Graham B. I. Donoviel, Dorit B. Leveton, Lauren B. Mahoney, Erin Charles, John B. Siegel, Bette TI The Impact of Sex and Gender on Adaptation to Space: Executive Summary SO JOURNAL OF WOMENS HEALTH LA English DT Review ID MICROGRAVITY; ASTRONAUTS; RESPONSES; WOMEN; STRESS; EPIDEMIOLOGY; REACTIVATION; SPACEFLIGHT; POPULATION; RADIATION AB This review article is a compendium of six individual manuscripts, a Commentary, and an Executive Summary. This body of work is entitled "The Impact of Sex and Gender on Adaptation to Space" and was developed in response to a recommendation from the 2011 National Academy of Sciences Decadal Survey, "Recapturing a Future for Space Exploration: Life and Physical Sciences for a New Era," which emphasized the need to fully understand sex and gender differences in space. To ensure the health and safety of male and female astronauts during long-duration space missions, it is imperative to examine and understand the influences that sex and gender have on physiological and psychological changes that occur during spaceflight. In this collection of manuscripts, six workgroups investigated and summarized the current body of published and unpublished human and animal research performed to date related to sex- and gender-based differences in the areas of cardiovascular, immunological, sensorimotor, musculoskeletal, reproductive, and behavioral adaptations to human spaceflight. Each workgroup consisted of scientists and clinicians from academia, the National Aeronautics and Space Administration (NASA), and other federal agencies and was co-chaired by one representative from NASA and one from the external scientific community. The workgroups met via telephone and e-mail over 6 months to review literature and data from space- and ground-based studies to identify sex and gender factors affecting crew health. In particular, the Life Sciences Data Archive and the Lifetime Surveillance of Astronaut Health were extensively mined. The groups identified certain sex-related differences that impact the risks and the optimal medical care required by space-faring women and men. It represents innovative research in sex and gender-based biology that impacts those individuals that are at the forefront of space exploration. C1 [Mark, Saralyn; Mahoney, Erin; Siegel, Bette] NASA, Adv Explorat Syst Div, Human Explorat & Operat Mission Directorate, Washington, DC 20546 USA. [Mark, Saralyn] Yale Univ, Sch Med, New Haven, CT USA. [Mark, Saralyn] Georgetown Univ, Sch Med, Washington, DC USA. [Mark, Saralyn] DMI Inc, Bethesda, MD USA. [Scott, Graham B. I.] Baylor Coll Med, Dept Mol & Cellular Biol, Natl Space Biomed Res Inst, Houston, TX 77030 USA. [Scott, Graham B. I.; Donoviel, Dorit B.] Baylor Coll Med, Ctr Space Med, Houston, TX 77030 USA. [Donoviel, Dorit B.] Baylor Coll Med, Dept Pharmacol, Natl Space Biomed Res Inst, Houston, TX 77030 USA. [Leveton, Lauren B.] NASA, Human Res Program, Div Biomed Res & Engn Sci, Houston, TX USA. [Mahoney, Erin] Valador Inc, Herndon, VA USA. [Charles, John B.] NASA, Int Sci Off, Human Res Program, Houston, TX USA. RP Siegel, B (reprint author), NASA, Human Explorat & Operat Mission Directorate, 300 E St Southwest, Washington, DC 20546 USA. EM bette.siegel@nasa.gov FU NSBRI through NASA Cooperative Agreement NCC [9-58]; NASA Advanced Exploration Systems Division; NASA Johnson Space Center Human Research Program; Division of Biomedical Research and Environmental Sciences Division FX G. B. I. S. and D. B. D. are grateful for the support provided by NSBRI through NASA Cooperative Agreement NCC 9-58. B. S., E. M., and S. M. are grateful for the support provided by the NASA Advanced Exploration Systems Division. L. B. L. and J.B.C. are grateful for the support provided by the NASA Johnson Space Center Human Research Program and the Division of Biomedical Research and Environmental Sciences Division. NR 70 TC 6 Z9 6 U1 0 U2 5 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1540-9996 EI 1931-843X J9 J WOMENS HEALTH JI J. Womens Health PD NOV 1 PY 2014 VL 23 IS 11 BP 941 EP 947 DI 10.1089/jwh.2014.4914 PG 7 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Obstetrics & Gynecology; Women's Studies SC Public, Environmental & Occupational Health; General & Internal Medicine; Obstetrics & Gynecology; Women's Studies GA AT3XO UT WOS:000344868200009 PM 25401937 ER PT J AU Mark, S AF Mark, Saralyn TI The Impact of Sex and Gender on Adaptation to Space: Commentary SO JOURNAL OF WOMENS HEALTH LA English DT Editorial Material C1 NASA, Washington, DC 20546 USA. RP Mark, S (reprint author), NASA, 300 E St SW, Washington, DC 20546 USA. EM saralyn.mark@nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 2 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1540-9996 EI 1931-843X J9 J WOMENS HEALTH JI J. Womens Health PD NOV 1 PY 2014 VL 23 IS 11 BP 948 EP 949 DI 10.1089/jwh.2014.1515 PG 2 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Obstetrics & Gynecology; Women's Studies SC Public, Environmental & Occupational Health; General & Internal Medicine; Obstetrics & Gynecology; Women's Studies GA AT3XO UT WOS:000344868200010 PM 25401938 ER PT J AU Platts, SH Merz, CNB Barr, Y Fu, Q Gulati, M Hughson, R Levine, BD Mehran, R Stachenfeld, N Wenger, NK AF Platts, Steven H. Merz, C. Noel Bairey Barr, Yael Fu, Qi Gulati, Martha Hughson, Richard Levine, Benjamin D. Mehran, Roxana Stachenfeld, Nina Wenger, Nanette K. TI Effects of Sex and Gender on Adaptation to Space: Cardiovascular Alterations SO JOURNAL OF WOMENS HEALTH LA English DT Review ID DOWN BED REST; SIMULATED MICROGRAVITY; ORTHOSTATIC INTOLERANCE; CARDIAC ATROPHY; PSEUDOTUMOR CEREBRI; ENDOCRINE RESPONSES; BLOOD-FLOW; WOMEN; ARTERIES; MEN AB Sex and gender differences in the cardiovascular adaptation to spaceflight were examined with the goal of optimizing the health and safety of male and female astronauts at the forefront of space exploration. Female astronauts are more susceptible to orthostatic intolerance after space flight; the visual impairment intracranial pressure syndrome predominates slightly in males. Since spaceflight simulates vascular aging, sex-specific effects on vascular endothelium and thrombotic risk warrant examination as predisposing factors to atherosclerosis, important as the current cohort of astronauts ages. Currently, 20% of astronauts are women, and the recently selected astronaut recruits are 50% women. Thus there should be expectation that future research will reflect the composition of the overall population to determine potential benefits or risks. This should apply both to clinical studies and to basic science research. C1 [Platts, Steven H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77573 USA. [Merz, C. Noel Bairey] Cedars Sinai Med Ctr, Los Angeles, CA 90048 USA. [Barr, Yael] Univ Texas Med Branch, Galveston, TX 77555 USA. [Fu, Qi; Levine, Benjamin D.] Univ Texas SW Med Ctr Dallas, Dallas, TX 75390 USA. [Gulati, Martha] Ohio State Univ, Div Cardiol, Columbus, OH 43210 USA. [Hughson, Richard] Univ Waterloo, Waterloo, ON N2L 3G1, Canada. [Mehran, Roxana] Mt Sinai Sch Med, New York, NY USA. [Stachenfeld, Nina] Yale Univ, Sch Med, John B Pierce Lab, New Haven, CT USA. [Wenger, Nanette K.] Emory Univ, Sch Med, Atlanta, GA USA. RP Platts, SH (reprint author), NASA, Biomed Res & Environm Sci Div, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy,Mail Code SK3, Houston, TX 77573 USA. EM steven.platts-1@nasa.gov NR 53 TC 6 Z9 8 U1 2 U2 8 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1540-9996 EI 1931-843X J9 J WOMENS HEALTH JI J. Womens Health PD NOV 1 PY 2014 VL 23 IS 11 BP 950 EP 955 DI 10.1089/jwh.2014.4912 PG 6 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Obstetrics & Gynecology; Women's Studies SC Public, Environmental & Occupational Health; General & Internal Medicine; Obstetrics & Gynecology; Women's Studies GA AT3XO UT WOS:000344868200011 PM 25401939 ER PT J AU Kennedy, AR Crucian, B Huff, JL Klein, SL Morens, D Murasko, D Nickerson, CA Sonnenfeld, G AF Kennedy, Ann R. Crucian, Brian Huff, Janice L. Klein, Sabra L. Morens, David Murasko, Donna Nickerson, Cheryl A. Sonnenfeld, Gerald TI Effects of Sex and Gender on Adaptation to Space: Immune System SO JOURNAL OF WOMENS HEALTH LA English DT Review ID MICROBIAL CHARACTERIZATION; SPACEFLIGHT; REACTIVATION; ASTRONAUTS; RESPONSES; STATION; DISEASE AB This review is focused on sex and gender effects on immunological alterations occurring during space flight. Sex differences in immune function and the outcome of inflammatory, infectious, and autoimmune diseases are well documented. The work of the Immunology Workgroup identified numerous reasons why there could be sex and/or gender differences observed during and after spaceflight, but thus far, there has been very little investigation in this area of research. In most cases, this is due to either a low total number of subjects or the minimal number of female flight crew members available for these studies. Thus, the availability of a sufficient number of female subjects to enable statistical analysis of the data has been a limiting factor. As the inclusion of female crew members has increased in the recent past, such studies should be possible in the future. It is very difficult to obtain immunologic and infectious data in small animals that can be usefully extrapolated to humans undergoing spaceflight. Thus, it is recommended by the Immunology Workgroup that a greater emphasis be placed on studying astronauts themselves, with a focus on long-term evaluations of specific, known infectious risks. C1 [Kennedy, Ann R.] Univ Penn, Perelman Sch Med, Dept Radiat Oncol, Philadelphia, PA 19104 USA. [Crucian, Brian] NASA, Lyndon B Johnson Space Ctr, Human Hlth & Performance Directorate, Houston, TX 77058 USA. [Huff, Janice L.] Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA. [Klein, Sabra L.] Johns Hopkins Bloomberg Sch Publ Hlth, W Harry Feinstone Dept Mol Microbiol & Immunol, Baltimore, MD USA. [Morens, David] NIAID, Off Director, NIH, Bethesda, MD 20892 USA. [Murasko, Donna] Drexel Univ, Coll Arts & Sci, Dept Biol, Philadelphia, PA 19104 USA. [Nickerson, Cheryl A.] Arizona State Univ, Biodesign Inst, Tempe, AZ USA. [Sonnenfeld, Gerald] Clemson Univ, Sch Hlth Res, Dept Biol Sci, Greenville, SC USA. [Sonnenfeld, Gerald] Greenville Hlth Syst, Greenville, SC USA. RP Kennedy, AR (reprint author), Univ Penn, Perelman Sch Med, Dept Radiat Oncol, 195 John Morgan Bldg,3620 Hamilton Walk, Philadelphia, PA 19104 USA. EM akennedy@mail.med.upenn.edu NR 24 TC 5 Z9 5 U1 1 U2 9 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1540-9996 EI 1931-843X J9 J WOMENS HEALTH JI J. Womens Health PD NOV 1 PY 2014 VL 23 IS 11 BP 956 EP 958 DI 10.1089/jwh.2014.4913 PG 3 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Obstetrics & Gynecology; Women's Studies SC Public, Environmental & Occupational Health; General & Internal Medicine; Obstetrics & Gynecology; Women's Studies GA AT3XO UT WOS:000344868200012 PM 25401940 ER PT J AU Reschke, MF Cohen, HS Cerisano, JM Clayton, JA Cromwell, R Danielson, RW Hwang, EY Tingen, C Allen, JR Tomko, DL AF Reschke, Millard F. Cohen, Helen S. Cerisano, Jody M. Clayton, Janine A. Cromwell, Ronita Danielson, Richard W. Hwang, Emma Y. Tingen, Candace Allen, John R. Tomko, David L. TI Effects of Sex and Gender on Adaptation to Space: Neurosensory Systems SO JOURNAL OF WOMENS HEALTH LA English DT Review ID PRODUCT OTOACOUSTIC EMISSIONS; EMOTIONALLY INFLUENCED MEMORY; HEARING-LOSS; SELF-ORIENTATION; AGE; EPIDEMIOLOGY; POPULATION; VERTIGO AB Sex and gender differences have long been a research topic of interest, yet few studies have explored the specific differences in neurological responses between men and women during and after spaceflight. Knowledge in this field is limited due to the significant disproportion of sexes enrolled in the astronaut corps. Research indicates that general neurological and sensory differences exist between the sexes, such as those in laterality of amygdala activity, sensitivity and discrimination in vision processing, and neuronal cell death (apoptosis) pathways. In spaceflight, sex differences may include a higher incidence of entry and space motion sickness and of post-flight vestibular instability in female as opposed to male astronauts who flew on both short- and long-duration missions. Hearing and auditory function in crewmembers shows the expected hearing threshold differences between men and women, in which female astronauts exhibit better hearing thresholds. Longitudinal observations of hearing thresholds for crewmembers yield normal age-related decrements; however, no evidence of sex-related differences from spaceflight has been observed. The impact of sex and gender differences should be studied by making spaceflight accessible and flying more women into space. Only in this way will we know if increasingly longer-duration missions cause significantly different neurophysiological responses in men and women. C1 [Reschke, Millard F.] NASA, Dept Neurosci, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Cohen, Helen S.; Danielson, Richard W.] Baylor Coll Med, Dept Otolaryngol Head & Neck Surg, Houston, TX 77030 USA. [Cerisano, Jody M.; Hwang, Emma Y.] Wyle Sci Technol & Engn Grp, Houston, TX USA. [Clayton, Janine A.] NIH, Off Res Womens Hlth, Bethesda, MD 20892 USA. [Tingen, Candace] Natl Inst Minor Hlth & Hlth Dispar, NIH, Bethesda, MD USA. [Cromwell, Ronita] Univ Space Res Assoc, Houston, TX USA. [Allen, John R.] Natl Aeronaut & Space Adm NASA Headquarters, Human Explorat & Operat Mission Directorate, Washington, DC USA. [Tomko, David L.] Natl Aeronaut & Space Adm NASA Headquarters, Space Life & Phys Sci Res Div, Washington, DC USA. RP Reschke, MF (reprint author), NASA, Dept Neurosci, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. EM millard.f.reschke@nasa.gov NR 32 TC 5 Z9 5 U1 0 U2 3 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1540-9996 EI 1931-843X J9 J WOMENS HEALTH JI J. Womens Health PD NOV 1 PY 2014 VL 23 IS 11 BP 959 EP 962 DI 10.1089/jwh.2014.4908 PG 4 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Obstetrics & Gynecology; Women's Studies SC Public, Environmental & Occupational Health; General & Internal Medicine; Obstetrics & Gynecology; Women's Studies GA AT3XO UT WOS:000344868200013 PM 25401941 ER PT J AU Ploutz-Snyder, L Bloomfield, S Smith, SM Hunter, SK Templeton, K Bemben, D AF Ploutz-Snyder, Lori Bloomfield, Susan Smith, Scott M. Hunter, Sandra K. Templeton, Kim Bemben, Debra TI Effects of Sex and Gender on Adaptation to Space: Musculoskeletal Health SO JOURNAL OF WOMENS HEALTH LA English DT Review ID INDUCED BONE LOSS; BODY NEGATIVE-PRESSURE; MUSCLE-FIBER FUNCTION; BED-REST; NUTRITION COUNTERMEASURES; TREADMILL EXERCISE; SKELETAL-MUSCLE; SIMULATED MICROGRAVITY; RESISTANCE EXERCISE; CONCURRENT EXERCISE AB There is considerable variability among individuals in musculoskeletal response to long-duration spaceflight. The specific origin of the individual variability is unknown but is almost certainly influenced by the details of other mission conditions such as individual differences in exercise countermeasures, particularly intensity of exercise, dietary intake, medication use, stress, sleep, psychological profiles, and actual mission task demands. In addition to variations in mission conditions, genetic differences may account for some aspect of individual variability. Generally, this individual variability exceeds the variability between sexes that adds to the complexity of understanding sex differences alone. Research specifically related to sex differences of the musculoskeletal system during unloading is presented and discussed. C1 [Ploutz-Snyder, Lori] NASA, Univ Space Res Assoc, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Smith, Scott M.] NASA, Biomed Res & Environm Sci Div, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Bloomfield, Susan] Texas A&M Univ, Dept Kinesiol, College Stn, TX USA. [Hunter, Sandra K.] Marquette Univ, Milwaukee, WI 53233 USA. [Templeton, Kim] Univ Kansas, Med Ctr, Dept Orthoped Surg, Kansas City, KS 66103 USA. [Bemben, Debra] Univ Oklahoma, Dept Hlth & Exercise Sci, Norman, OK 73019 USA. RP Ploutz-Snyder, L (reprint author), NASA, Univ Space Res Assoc, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. EM lori.ploutz-snyder-1@nasa.gov NR 30 TC 8 Z9 10 U1 0 U2 2 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1540-9996 EI 1931-843X J9 J WOMENS HEALTH JI J. Womens Health PD NOV 1 PY 2014 VL 23 IS 11 BP 963 EP 966 DI 10.1089/jwh.2014.4910 PG 4 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Obstetrics & Gynecology; Women's Studies SC Public, Environmental & Occupational Health; General & Internal Medicine; Obstetrics & Gynecology; Women's Studies GA AT3XO UT WOS:000344868200014 PM 25401942 ER PT J AU Ronca, AE Baker, ES Bavendam, TG Beck, KD Miller, VM Tash, JS Jenkins, M AF Ronca, April E. Baker, Ellen S. Bavendam, Tamara G. Beck, Kevin D. Miller, Virginia M. Tash, Joseph S. Jenkins, Marjorie TI Effects of Sex and Gender on Adaptations to Space: Reproductive Health SO JOURNAL OF WOMENS HEALTH LA English DT Review ID PSYCHOSOCIAL STRESS; SLEEP-DEPRIVATION; URINARY RETENTION; GONADAL-STEROIDS; MALE RATS; ESTRADIOL; TESTOSTERONE; CONTRACEPTION; SPACEFLIGHT; OXYTOCIN AB In this report, sex/gender research relevant to reproduction on Earth, in conjunction with the extant human and animal observations in space, was used to identify knowledge gaps and prioritize recommendations for future sex- and gender-specific surveillance and monitoring of male and female astronauts. With overall increased durations of contemporary space missions, a deeper understanding of sex/gender effects on reproduction-related responses and adaptations to the space environment is warranted to minimize risks and insure healthy aging of the men and women who travel into space. C1 [Ronca, April E.] NASA, Space Biosci Res Branch, Ames Res Ctr, Mountain View, CA 94035 USA. [Ronca, April E.] Wake Forest Sch Med, Dept Obstet & Gynecol, Winston Salem, NC USA. [Ronca, April E.] Wake Forest Sch Med, Dept Neurobiol & Anat, Winston Salem, NC USA. [Ronca, April E.] Wake Forest Sch Med, Dept Mol Med & Translat Sci, Winston Salem, NC USA. [Baker, Ellen S.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Bavendam, Tamara G.] NIDDK, NIH, Bethesda, MD USA. [Beck, Kevin D.] Rutgers New Jersey Med Sch, Dept Neurol & Neurosci, Newark, NJ USA. [Miller, Virginia M.] Mayo Clin, Coll Med, Dept Physiol, Rochester, MN USA. [Miller, Virginia M.] Mayo Clin, Coll Med, Dept Surg, Rochester, MN USA. [Tash, Joseph S.] Univ Kansas, Med Ctr, Dept Mol & Integrat Physiol, Kansas City, KS 66103 USA. [Tash, Joseph S.] Univ Kansas, Med Ctr, Dept Urol, Kansas City, KS 66103 USA. [Tash, Joseph S.] Univ Kansas, Med Ctr, Interdisciplinary Ctr Male Contracept Res & Drug, Kansas City, KS 66103 USA. [Jenkins, Marjorie] Texas Tech Univ, Hlth Sci Ctr, Dept Internal Med, Laura W Bush Inst Womens Hlth, Amarillo, TX USA. [Jenkins, Marjorie] Texas Tech Univ, Hlth Sci Ctr, Rush Endowed Chair Excellence Gynecol Oncol, Amarillo, TX USA. RP Ronca, AE (reprint author), NASA, Space Biosci Res Branch, Ames Res Ctr, MS 236-7, Mountain View, CA 94035 USA. EM aronca@wakehealth.edu NR 69 TC 5 Z9 5 U1 1 U2 5 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1540-9996 EI 1931-843X J9 J WOMENS HEALTH JI J. Womens Health PD NOV 1 PY 2014 VL 23 IS 11 BP 967 EP 974 DI 10.1089/jwh.2014.4915 PG 8 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Obstetrics & Gynecology; Women's Studies SC Public, Environmental & Occupational Health; General & Internal Medicine; Obstetrics & Gynecology; Women's Studies GA AT3XO UT WOS:000344868200015 PM 25401943 ER PT J AU Jenniskens, P AF Jenniskens, Peter TI The Sutter's Mill Fall SO METEORITICS & PLANETARY SCIENCE LA English DT Letter C1 [Jenniskens, Peter] SETI Inst, Mountain View, CA 94043 USA. [Jenniskens, Peter] NASA, Ames Res Ctr, Washington, DC USA. RP Jenniskens, P (reprint author), SETI Inst, Mountain View, CA 94043 USA. NR 2 TC 0 Z9 0 U1 1 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD NOV PY 2014 VL 49 IS 11 BP 1987 EP 1988 DI 10.1111/maps.12343 PG 2 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AT1ZZ UT WOS:000344731500001 ER PT J AU Zolensky, M Mikouchi, T Fries, M Bodnar, R Jenniskens, P Yin, QZ Hagiya, K Ohsumi, K Komatsu, M Colbert, M Hanna, R Maisano, J Ketcham, R Kebukawa, Y Nakamura, T Matsuoka, M Sasaki, S Tsuchiyama, A Gounelle, M Le, L Martinez, J Ross, K Rahman, Z AF Zolensky, Michael Mikouchi, Takashi Fries, Marc Bodnar, Robert Jenniskens, Peter Yin, Qing-zhu Hagiya, Kenji Ohsumi, Kazumasa Komatsu, Mutsumi Colbert, Matthew Hanna, Romy Maisano, Jessie Ketcham, Richard Kebukawa, Yoko Nakamura, Tomoki Matsuoka, Moe Sasaki, Sho Tsuchiyama, Akira Gounelle, Matthieu Le, Loan Martinez, James Ross, Kent Rahman, Zia TI Mineralogy and petrography of C asteroid regolith: The Sutter's Mill CM meteorite SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID 162173 1999 JU3; CARBONACEOUS CHONDRITE; THERMAL METAMORPHISM; PONDED DEPOSITS; LITHIC CLASTS; 433-EROS; FEATURES; TARGET; TYPE-2; EROS AB Based upon our characterization of three separate stones by electron and X-ray beam analyses, computed X-ray microtomography, Raman microspectrometry, and visible-IR spectrometry, Sutter's Mill is a unique regolith breccia consisting mainly of various CM lithologies. Most samples resemble existing available CM2 chondrites, consisting of chondrules and calcium-aluminum-rich inclusion (CAI) set within phyllosilicate-dominated matrix (mainly serpentine), pyrrhotite, pentlandite, tochilinite, and variable amounts of Ca-Mg-Fe carbonates. Some lithologies have witnessed sufficient thermal metamorphism to transform phyllosilicates into fine-grained olivine, tochilinite into troilite, and destroy carbonates. One finely comminuted lithology contains xenolithic materials (enstatite, Fe-Cr phosphides) suggesting impact of a reduced asteroid (E or M class) onto the main Sutter's Mill parent asteroid, which was probably a C class asteroid. One can use Sutter's Mill to help predict what will be found on the surfaces of C class asteroids such as Ceres and the target asteroids of the OSIRIS-REx and Hayabusa 2 sample return missions (which will visit predominantly primitive asteroids). C class asteroid regolith may well contain a mixture of hydrated and thermally dehydrated indigenous materials as well as a significant admixture of exogenous material would be essential to the successful interpretation of mineralogical and bulk compositional data. C1 [Zolensky, Michael; Fries, Marc] NASA, ARES, Johnson Space Ctr, Houston, TX 77058 USA. [Mikouchi, Takashi] Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, Tokyo 1130033, Japan. [Bodnar, Robert] Virginia Tech, Dept Geosci, Blacksburg, VA 24061 USA. [Jenniskens, Peter] SETI Inst, Mountain View, CA 94043 USA. [Yin, Qing-zhu] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. [Hagiya, Kenji] Univ Hyogo, Grad Sch Life Sci, Kamigori, Hyogo 6781297, Japan. [Ohsumi, Kazumasa] JASRI, Sayo, Hyogo 6795198, Japan. [Komatsu, Mutsumi] Waseda Univ, Shinjuku Ku, Tokyo 1698050, Japan. [Colbert, Matthew; Hanna, Romy; Maisano, Jessie; Ketcham, Richard] Univ Texas Austin, High Resolut Xray CT Facil, Austin, TX 78712 USA. [Kebukawa, Yoko] Hokkaido Univ, Sapporo, Hokkaido 0600810, Japan. [Nakamura, Tomoki; Matsuoka, Moe] Tohoku Univ, Grad Sch Sci, Sendai, Miyagi 9808578, Japan. [Sasaki, Sho] Osaka Univ, Grad Sch Sci, Toyonaka, Osaka 5600043, Japan. [Tsuchiyama, Akira] Kyoto Univ, Div Earth & Planetary Sci, Sakyo Ku, Kyoto 6068502, Japan. [Gounelle, Matthieu] Museum Natl Hist Nat, F-70005 Paris, France. [Le, Loan; Martinez, James; Ross, Kent; Rahman, Zia] ESCG Jacobs, Houston, TX 77058 USA. RP Zolensky, M (reprint author), NASA, ARES, Johnson Space Ctr, Houston, TX 77058 USA. EM michael.e.zolensky@nasa.gov RI Yin, Qing-Zhu/B-8198-2009; Ketcham, Richard/B-5431-2011 OI Yin, Qing-Zhu/0000-0002-4445-5096; Ketcham, Richard/0000-0002-2748-0409 FU NASA Cosmochemistry Program; NASA NEO Observation Program FX We thank Mr. Charles Farley for setting up and calibrating the Raman microprobe and for assisting with Raman analyses at Virginia Tech. Reviews of the first version of this paper by Neyda Abreu and an anonymous person greatly improved the text. MZ and QZY acknowledge support from the NASA Cosmochemistry Program. PJ is supported by the NASA NEO Observation Program. NR 52 TC 8 Z9 8 U1 3 U2 21 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD NOV PY 2014 VL 49 IS 11 BP 1997 EP 2016 DI 10.1111/maps.12386 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AT1ZZ UT WOS:000344731500003 ER PT J AU Nuevo, M Sandford, SA Flynn, GJ Wirick, S AF Nuevo, Michel Sandford, Scott A. Flynn, George J. Wirick, Susan TI Mid-infrared study of stones from the Sutter's Mill meteorite SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID INTERPLANETARY DUST PARTICLES; INFRARED TRANSMISSION SPECTRA AB The Sutter's Mill meteorite fell in northern California on April 22, 2012. Several fragments of the meteorite were recovered, some of them shortly after the fall, others several days later after a heavy rainstorm. In this work, we analyzed several samples of four fragments. SM2, SM12, SM20, and SM30. from the Sutter's Mill meteorite with two infrared (IR) microscopes operating in the 4000-650 cm(-1) (2.5-15.4 mu m) range. Spectra show absorption features associated with minerals such as olivines, phyllosilicates, carbonates, and possibly pyroxenes, as well as organics. Spectra of specific minerals vary from one particle to another within a given stone, and even within a single particle, indicating a nonuniform mineral composition. Infrared features associated with aliphatic CH2 and CH3 groups associated with organics are also seen in several spectra. However, the presence of organics in the samples studied is not clear because these features overlap with carbonate overtone bands. Finally, other samples collected within days after the rainstorm show evidence for bacterial terrestrial contamination, which indicates how quickly meteorites can be contaminated on such small scales. C1 [Nuevo, Michel; Sandford, Scott A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Nuevo, Michel] SETI Inst, Mountain View, CA 94043 USA. [Flynn, George J.] SUNY Coll Plattsburgh, Dept Phys, Plattsburgh, NY 12901 USA. [Wirick, Susan] Univ Chicago, Ctr Adv Radiat Sources, Chicago, IL 60637 USA. RP Sandford, SA (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA. EM Scott.A.Sandford@nasa.gov FU NASA [NNX10AR79G]; DOE [DE-AC02-98CH10886] FX The authors are grateful for grant support from the NASA Origins of Solar System and Astrobiology Programs (MN and SAS) and the NASA Exobiology program (GJF, no. NNX10AR79G). The authors are grateful for the opportunity to work with the Sutter's Mill Consortium and the samples provided by Peter Jenniskens. The authors are also grateful for assistance provided by M. McMahon and J. Hellgeth for the measurements made at the Thermo-Fisher Scientific Inc. facility in San Jose, California. The other measurements were conducted on the infrared Beamline U2b of the National Synchrotron Light Source (NSLS) at Brookhaven National Laboratory, Upton, New York. Use of the NSLS was supported by DOE under contract no. DE-AC02-98CH10886. This paper benefited substantially from helpful reviews by A. Ruzicka, Y. Kebukawa, and an anonymous reviewer for which the authors are grateful. NR 9 TC 2 Z9 2 U1 1 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD NOV PY 2014 VL 49 IS 11 BP 2017 EP 2026 DI 10.1111/maps.12269 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AT1ZZ UT WOS:000344731500004 ER PT J AU Yesiltas, M Kebukawa, Y Peale, RE Mattson, E Hirschmugl, CJ Jenniskens, P AF Yesiltas, Mehmet Kebukawa, Yoko Peale, Robert E. Mattson, Eric Hirschmugl, Carol J. Jenniskens, Peter TI Infrared imaging spectroscopy with micron resolution of Sutter's Mill meteorite grains SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID DIFFUSE INTERSTELLAR-MEDIUM; INSOLUBLE ORGANIC-MATTER; CARBONACEOUS CHONDRITES; HYDROUS COMPONENTS; COMET 81P/WILD-2; SOLAR-SYSTEM; MICROSPECTROSCOPY; ASTEROIDS; STARDUST; ORIGIN AB Synchrotron-based Fourier transform infrared spectroscopy and Raman spectroscopy are applied with submicrometer spatial resolution to multiple grains of Sutter's Mill meteorite, a regolith breccia with CM1 and CM2 lithologies. The Raman and infrared active functional groups reveal the nature and distribution of organic and mineral components and confirm that SM12 reached higher metamorphism temperatures than SM2. The spatial distributions of carbonates and organic matter are negatively correlated. The spatial distributions of aliphatic organic matter and OH relative to the distributions of silicates in SM2 differ from those in SM12, supporting a hypothesis that the parent body of Sutter's Mill is a combination of multiple bodies with different origins. The high aliphatic CH2/CH3 ratios determined from band intensities for SM2 and SM12 grains are similar to those of IDPs and less altered carbonaceous chondrites, and they are significantly higher than those in other CM chondrites and diffuse ISM objects. C1 [Yesiltas, Mehmet; Peale, Robert E.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. [Kebukawa, Yoko] Yokohama Natl Univ, Fac Engn, Hodogaya Ku, Yokohama, Kanagawa 2408501, Japan. [Mattson, Eric; Hirschmugl, Carol J.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53211 USA. [Jenniskens, Peter] SETI Inst, Mountain View, CA 94043 USA. [Jenniskens, Peter] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Yesiltas, M (reprint author), Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. EM myesiltas@knights.ucf.edu FU Turkish government [1416]; University of Wisconsin-Madison; University of Wisconsin-Milwaukee; NSF MRI [0619759]; NSF CHE [1112433] FX We thank NASA Ames Research Center and the Sutter's Mill meteorite consortium for providing the meteorite samples. Mr. Yesiltas is primarily supported through Graduate Fellowship Program #1416 by the Turkish government. SRC is primarily funded by the University of Wisconsin-Madison with supplemental support from facility users and the University of Wisconsin-Milwaukee. IRENI beamline's construction and development was supported by NSF MRI award #0619759, and CJH is funded by NSF CHE award #1112433. We are also grateful to associate editor Dr. S. Sandford and the reviewers for constructive comments on this manuscript. NR 37 TC 6 Z9 6 U1 1 U2 9 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD NOV PY 2014 VL 49 IS 11 BP 2027 EP 2037 DI 10.1111/maps.12321 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AT1ZZ UT WOS:000344731500005 ER PT J AU Zhao, XC Lin, YT Yin, QZ Zhang, JC Hao, JL Zolensky, M Jenniskens, P AF Zhao, Xuchao Lin, Yangting Yin, Qing-Zhu Zhang, Jianchao Hao, Jialong Zolensky, Michael Jenniskens, Peter TI Presolar grains in the CM2 chondrite Sutter's Mill SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID SIC GRAINS; CARBONACEOUS CHONDRITE; ISOTOPIC COMPOSITIONS; SILICON-CARBIDE; MET 00426; QUE 99177; METEORITE; NUCLEOSYNTHESIS; CIRCUMSTELLAR; RECOVERY AB The Sutter's Mill (SM) carbonaceous chondrite is a regolith breccia, composed predominantly of CM2 clasts with varying degrees of aqueous alteration and thermal metamorphism. An investigation of presolar grains in four Sutter's Mill sections, SM43, SM51, SM2-4, and SM18, was carried out using NanoSIMS ion mapping technique. A total of 37 C-anomalous grains and one O-anomalous grain have been identified, indicating an abundance of 63 ppm for presolar C-anomalous grains and 2 ppm for presolar oxides. Thirty-one silicon carbide (SiC), five carbonaceous grains, and one Al-oxide (Al2O3) were confirmed based on their elemental compositions determined by C-N-Si and O-Si-Mg-Al isotopic measurements. The overall abundance of SiC grains in Sutter's Mill (55 ppm) is consistent with those in other CM chondrites. The absence of presolar silicates in Sutter's Mill suggests that they were destroyed by aqueous alteration on the parent asteroid. Furthermore, SM2-4 shows heterogeneous distributions of presolar SiC grains (12-54 ppm) in different matrix areas, indicating that the fine-grained matrix clasts come from different sources, with various thermal histories, in the solar nebula. C1 [Zhao, Xuchao; Lin, Yangting; Zhang, Jianchao; Hao, Jialong] Chinese Acad Sci, Inst Geol & Geophys, Key Lab Earths Deep Interior, Beijing 100029, Peoples R China. [Yin, Qing-Zhu] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. [Zolensky, Michael] NASA, ARES, Johnson Space Ctr, Houston, TX 77058 USA. [Jenniskens, Peter] SETI Inst, Mountain View, CA 94043 USA. [Jenniskens, Peter] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Lin, YT (reprint author), Chinese Acad Sci, Inst Geol & Geophys, Key Lab Earths Deep Interior, 19 Beituchengxi Rd, Beijing 100029, Peoples R China. EM linyt@mail.igcas.ac.cn RI Yin, Qing-Zhu/B-8198-2009; Lin, Yangting/A-8845-2015 OI Yin, Qing-Zhu/0000-0002-4445-5096; FU Natural Science Foundation of China [40830421, 41173075]; State Key Laboratory of Lithospheric Evolution (IGG-CAS) [Z201003] FX We thank Dr. Sen Hu for preparing the section of SM43. The manuscript has been significantly improved by the detailed and constructive reviews by J. Leitner; P. Heck; an anonymous reviewer; and the associate editor, C. Floss. This study was supported by the Natural Science Foundation of China (40830421, 41173075) and the State Key Laboratory of Lithospheric Evolution (IGG-CAS Grant Z201003). NR 24 TC 1 Z9 1 U1 1 U2 9 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD NOV PY 2014 VL 49 IS 11 BP 2038 EP 2046 DI 10.1111/maps.12289 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AT1ZZ UT WOS:000344731500006 ER PT J AU Sears, DW Beauford, R AF Sears, Derek W. Beauford, Robert TI The Sutter's Mill meteorite: Thermoluminescence data on thermal and metamorphic history SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID CM CARBONACEOUS CHONDRITES; NATURAL THERMOLUMINESCENCE; ANTARCTIC METEORITES; AQUEOUS ALTERATION; TERRESTRIAL AGES; LUMINESCENCE; ORBITS; ABLATION; SHOCK AB A piece of the Sutter's Mill meteorite, fragment SM2-1d, has been examined using thermoluminescence techniques to better understand its thermal and metamorphic history. The sample had very weak but easily measureable natural and induced thermoluminescence (TL) signals; the signal-to-noise ratio was better than 10. The natural TL was restricted to the high-temperature regions of the glow curve suggesting that the meteorite had been heated to approximately 300 degrees C within the time it takes for the TL signal to recover from a heating event, probably within the last 10 5 years. It is possible that this reflects heating during release from the parent body, close passage by the Sun, or heating during atmospheric passage. Of these three options, the least likely is the first, but the other possibilities are equally likely. It seems that temperatures of approximately 300 degrees C reached 5 or 6 mm into the meteorite, so that all but one of the small Sutter's Mill stones have been heated. The Dhajala normalized induced TL signal for SM2-1d is comparable to that of type 3.0 chondrites and is unlike normal CM chondrites, the class it most closely resembles, which do not have detectable TL sensitivity. The shape of the induced TL curve is comparable to other low-type ordinary, CV, and CO chondrites, in that it has a broad hummocky structure, but does not resemble any of them in detail. This suggests that Sutter's Mill is a unique, low-petrographic-type (3.0) chondrite. C1 [Sears, Derek W.] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Mountain View, CA 94035 USA. [Beauford, Robert] Univ Arkansas, Arkansas Ctr Space & Planetary Sci, Fayetteville, AR 72701 USA. RP Sears, DW (reprint author), NASA, Bay Area Environm Res Inst, Ames Res Ctr, Mail Stop N245-3, Mountain View, CA 94035 USA. EM derek.sears@nasa.gov NR 33 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD NOV PY 2014 VL 49 IS 11 BP 2047 EP 2055 DI 10.1111/maps.12259 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AT1ZZ UT WOS:000344731500007 ER PT J AU Burton, AS Glavin, DP Elsila, JE Dworkin, JP Jenniskens, P Yin, QZ AF Burton, Aaron S. Glavin, Daniel P. Elsila, Jamie E. Dworkin, Jason P. Jenniskens, Peter Yin, Qing-Zhu TI The amino acid composition of the Sutter's Mill CM2 carbonaceous chondrite SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID LARGE ENANTIOMERIC EXCESSES; TAGISH LAKE METEORITE; MURCHISON METEORITE; PRIMITIVE METEORITES; EXTRATERRESTRIAL NUCLEOBASES; ISOTOPIC ANALYSES; HYDROXY-ACIDS; PARENT BODY; DECOMPOSITION; HYDROCARBONS AB We determined the abundances and enantiomeric compositions of amino acids in Sutter's Mill fragment #2 (designated SM2) recovered prior to heavy rains that fell April 25-26, 2012, and two other meteorite fragments, SM12 and SM51, that were recovered postrain. We also determined the abundance, enantiomeric, and isotopic compositions of amino acids in soil from the recovery site of fragment SM51. The three meteorite stones experienced terrestrial amino acid contamination, as evidenced by the low D/L ratios of several proteinogenic amino acids. The D/L ratios were higher in SM2 than in SM12 and SM51, consistent with rain introducing additional L-amino acid contaminants to SM12 and SM51. Higher percentages of glycine, beta-alanine, and gamma-amino-n-butyric acid were observed in free form in SM2 and SM51 compared with the soil, suggesting that these free amino acids may be indigenous. Trace levels of D+L-beta-aminoisobutyric acid (beta-AIB) observed in all three meteorites are not easily explained as terrestrial contamination, as beta-AIB is rare on Earth and was not detected in the soil. Bulk carbon and nitrogen and isotopic ratios of the SM samples and the soil also indicate terrestrial contamination, as does compound-specific isotopic analysis of the amino acids in the soil. The amino acid abundances in SM2, the most pristine SM meteorite analyzed here, are approximately 20-fold lower than in the Murchison CM2 carbonaceous chondrite. This may be due to thermal metamorphism in the Sutter's Mill parent body at temperatures greater than observed for other aqueously altered CM2 meteorites. C1 [Burton, Aaron S.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Glavin, Daniel P.; Elsila, Jamie E.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Jenniskens, Peter] SETI Inst, Mountain View, CA 94043 USA. [Jenniskens, Peter] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Yin, Qing-Zhu] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. RP Burton, AS (reprint author), NASA, Johnson Space Ctr, 2101 Space Ctr Pkwy, Houston, TX 77058 USA. EM aaron.s.burton@nasa.gov RI Yin, Qing-Zhu/B-8198-2009; Elsila, Jamie/C-9952-2012; Glavin, Daniel/D-6194-2012; Dworkin, Jason/C-9417-2012 OI Yin, Qing-Zhu/0000-0002-4445-5096; Glavin, Daniel/0000-0001-7779-7765; Dworkin, Jason/0000-0002-3961-8997 FU NASA; National Aeronautics and Space Administration (NASA) Astrobiology Institute; Goddard Center for Astrobiology; NASA Cosmochemistry program FX A.S.B. was supported by a NASA Postdoctoral Program fellowship administered by Oak Ridge Associated Universities through a contract with NASA. D. P. G., J.E.E., and J.P.D. acknowledge funding support from the National Aeronautics and Space Administration (NASA) Astrobiology Institute and the Goddard Center for Astrobiology and the NASA Cosmochemistry and Exobiology Programs. Q.Z.Y. acknowledges support from NASA Cosmochemistry program. We thank G. Cooper and D. W. Sears for preparation of the SM2 and SM12 sample fragments used in this study, R. Patrinellis for making SM51 available for research and providing the soil sample from the collection site of SM51, and T. McCoy and L. Welzenbach for providing the sample of Murchison. NR 50 TC 7 Z9 7 U1 2 U2 20 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD NOV PY 2014 VL 49 IS 11 BP 2074 EP 2086 DI 10.1111/maps.12281 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AT1ZZ UT WOS:000344731500010 ER PT J AU Kebukawa, Y Zolensky, ME Kilcoyne, ALD Rahman, Z Jenniskens, P Cody, GD AF Kebukawa, Yoko Zolensky, Michael E. Kilcoyne, A. L. David Rahman, Zia Jenniskens, Peter Cody, George D. TI Diamond xenolith and matrix organic matter in the Sutter's Mill meteorite measured by C-XANES SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID RAY-ABSORPTION SPECTROSCOPY; INTERSTELLAR DIAMONDS; CHONDRITE; CARBON; FILMS; EXCITATION; RESOLUTION; POLYMERS; ORIGIN; PLASMA AB The Sutter's Mill (SM) meteorite fell in El Dorado County, California, on April 22, 2012. This meteorite is a regolith breccia composed of CM chondrite material and at least one xenolithic phase: oldhamite. The meteorite studied here, SM2 (subsample 5), was one of three meteorites collected before it rained extensively on the debris site, thus preserving the original asteroid regolith mineralogy. Two relatively large (10 mu m sized) possible diamond grains were observed in SM2-5 surrounded by fine-grained matrix. In the present work, we analyzed a focused ion beam (FIB) milled thin section that transected a region containing these two potential diamond grains as well as the surrounding fine-grained matrix employing carbon and nitrogen X-ray absorption near-edge structure (C-XANES and N-XANES) spectroscopy using a scanning transmission X-ray microscope (STXM) (Beamline 5.3.2 at the Advanced Light Source, Lawrence Berkeley National Laboratory). The STXM analysis revealed that the matrix of SM2-5 contains C-rich grains, possibly organic nanoglobules. A single carbonate grain was also detected. The C-XANES spectrum of the matrix is similar to that of insoluble organic matter (IOM) found in other CM chondrites. However, no significant nitrogen-bearing functional groups were observed with N-XANES. One of the possible diamond grains contains a Ca-bearing inclusion that is not carbonate. C-XANES features of the diamond-edges suggest that the diamond might have formed by the CVD process, or in a high-temperature and -pressure environment in the interior of a much larger parent body. C1 [Kebukawa, Yoko; Cody, George D.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. [Kebukawa, Yoko] Hokkaido Univ, Dept Nat Hist Sci, Sapporo, Hokkaido 0600810, Japan. [Zolensky, Michael E.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Kilcoyne, A. L. David] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA 94720 USA. [Rahman, Zia] Jacobs Sverdrup, Houston, TX 77058 USA. [Jenniskens, Peter] SETI Inst, Mountain View, CA 94043 USA. [Jenniskens, Peter] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Kebukawa, Y (reprint author), Yokohama Natl Univ, Fac Engn, Yokohama, Kanagawa 2408501, Japan. EM kebukawa@ynu.ac.jp RI Kilcoyne, David/I-1465-2013 FU Office of Science, Department of Energy [DE-AC02-05CH11231]; NASA; JSPS; NASA Ames Research Center FX We thank George Flynn, Monica Grady, Hikaru Yabuta, and the Associate Editor Christine Floss for their careful reviews and constructive comments. STXM-XANES data were acquired at beamline 5.3.2.2 at the ALS, which is supported by the Director of the Office of Science, Department of Energy, under Contract No. DE-AC02-05CH11231. We gratefully acknowledge support from NASA Astrobiology and Origins of the Solar System Programs. Y. K. gratefully acknowledges support through the JSPS Postdoctoral Fellowships. The Sutter's Mill recovery was supported by NASA Ames Research Center. NR 41 TC 2 Z9 2 U1 2 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD NOV PY 2014 VL 49 IS 11 BP 2095 EP 2103 DI 10.1111/maps.12312 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AT1ZZ UT WOS:000344731500012 ER PT J AU Famiglietti, JS AF Famiglietti, J. S. TI The global groundwater crisis SO NATURE CLIMATE CHANGE LA English DT Editorial Material ID WATER MANAGEMENT; DEPLETION; IRRIGATION; DROUGHT; BALANCE; GRACE; INDIA C1 [Famiglietti, J. S.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. [Famiglietti, J. S.] Univ Calif Irvine, Dept Earth Syst Sci, Dept Civil & Environm Engn, Irvine, CA 92697 USA. RP Famiglietti, JS (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM James.Famiglietti@jpl.nasa.gov NR 24 TC 92 Z9 94 U1 15 U2 111 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1758-678X EI 1758-6798 J9 NAT CLIM CHANGE JI Nat. Clim. Chang. PD NOV PY 2014 VL 4 IS 11 BP 945 EP 948 PG 5 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AT0AD UT WOS:000344598400011 ER EF