FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Cooray, A Calanog, J Wardlow, JL Bock, J Bridge, C Burgarella, D Bussmann, RS Casey, CM Clements, D Conley, A Farrah, D Fu, H Gavazzi, R Ivison, RJ La Porte, N Lo Faro, B Ma, B Magdis, G Oliver, SJ Osage, WA Perez-Fournon, I Riechers, D Rigopoulou, D Scott, D Viero, M Watson, D AF Cooray, Asantha Calanog, Jae Wardlow, Julie L. Bock, J. Bridge, C. Burgarella, D. Bussmann, R. S. Casey, C. M. Clements, D. Conley, A. Farrah, D. Fu, H. Gavazzi, R. Ivison, R. J. La Porte, N. Lo Faro, B. Ma, Brian Magdis, G. Oliver, S. J. Osage, W. A. Perez-Fournon, I. Riechers, D. Rigopoulou, D. Scott, Douglas Viero, M. Watson, D. TI HerMES: THE REST-FRAME UV EMISSION AND A LENSING MODEL FOR THE z=6.34 LUMINOUS DUSTY STARBURST GALAXY HFLS3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; galaxies: starburst; gravitational lensing: strong; infrared: galaxies; submillimeter: galaxies ID STAR-FORMING GALAXIES; HUBBLE-SPACE-TELESCOPE; HIGH-REDSHIFT GALAXIES; SUBMILLIMETER GALAXIES; PHOTOMETRIC REDSHIFTS; SUPERNOVA 1987A; LENSED GALAXIES; MOLECULAR GAS; DEEP FIELD; HERSCHEL AB We discuss the rest-frame ultraviolet emission from the starbursting galaxy HFLS3 at a redshift of 6.34. The galaxy was discovered in Herschel/SPIRE data due to its red color in the submillimeter wavelengths from 250 to 500 m. Keck/NIRC2 K-s-band adaptive optics imaging data showed two potential near-IR counterparts near HFLS3. Previously, the northern galaxy was taken to be in the foreground at z = 2.1, while the southern galaxy was assumed to be HFLS3' s near-IR counterpart. The recently acquired Hubble/WFC3 and Advanced Camera for Surveys (ACS) imaging data show conclusively that both optically bright galaxies are in the foreground at z < 6. A new lensing model based on the Hubble imaging data and the millimeter-wave continuum emission yields a magnification factor of 2.2 +/- 0.3, with a 95% confidence upper limit on the magnification of 3.5. When corrected for lensing, the instantaneous star formation rate is 1320M(circle dot) yr(-1), with the 95% confidence lower limit around 830M(circle dot) yr(-1). The dust and stellar masses of HFLS3 from the same spectral energy distribution (SED) models are at the level of 3x10(8) M-circle dot and similar to 5x10(10) M-circle dot, respectively, with large systematic uncertainties on assumptions related to the SED model. With Hubble/WFC3 images, we also find diffuse near-IR emission about 0.5 arcsec (similar to 3 kpc) to the southwest of HFLS3 that remains undetected in the ACS imaging data. The emission has a photometric redshift consistent with either z similar to 6 or a dusty galaxy template at z similar to 2. C1 [Cooray, Asantha; Calanog, Jae; Casey, C. M.; Ma, Brian; Osage, W. A.; Viero, M.] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA. [Wardlow, Julie L.; Watson, D.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Bock, J.; Bridge, C.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Burgarella, D.] Aix Marseille Univ, Lab Astrophys Marseille, CNRS, F-13013 Marseille, France. [Bussmann, R. S.; Riechers, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Clements, D.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Conley, A.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA UCB 389, Boulder, CO 80309 USA. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Fu, H.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Gavazzi, R.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Ivison, R. J.] European So Observ, D-85748 Garching, Germany. [Ivison, R. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [La Porte, N.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Lo Faro, B.] Aix Marseille Univ, CNRS, Lab Astrophys Marseille, F-13388 Marseille, France. [Magdis, G.; Rigopoulou, D.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Oliver, S. J.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Perez-Fournon, I.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. RP Cooray, A (reprint author), Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA. RI Magdis, Georgios/C-7295-2014; Wardlow, Julie/C-9903-2015; Watson, Darach/E-4521-2015; Ivison, R./G-4450-2011; OI Magdis, Georgios/0000-0002-4872-2294; Wardlow, Julie/0000-0003-2376-8971; Watson, Darach/0000-0002-4465-8264; Ivison, R./0000-0001-5118-1313; Scott, Douglas/0000-0002-6878-9840; Casey, Caitlin/0000-0002-0930-6466 FU NASA from the Space Telescope Science Institute [HST-GO-13045]; NASA [NAS 5-26555]; NSF [AST-1313319]; Danish National Research Foundation; Science and Technology Facilities Council [ST/I000976/1]; CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA) FX Financial support for this work was provided by NASA through grant HST-GO-13045 from the Space Telescope Science Institute, which is operated by Associated Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Additional support for A.C., W.O., J.C., J.L.W., and C.M.C. was from NSF with AST-1313319. We thank E. da Cunha for help with Magphys. Dark Cosmology Centre is funded by the Danish National Research Foundation (J.L.W. and D. W.). S.O. acknowledges support from the Science and Technology Facilities Council [grant No. ST/I000976/1]. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM(France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). The data presented in this paper will be released through the Herschel Database in Marseille HeDaM (hedam.oamp.fr/HerMES). NR 47 TC 20 Z9 20 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 JUL 20 PY 2014 VL 790 IS 1 AR 40 DI 10.1088/0004-637X/790/1/40 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800040 ER PT J AU Drlica-Wagner, A Gomez-Vargas, GA Hewitt, JW Linden, T Tibaldo, L AF Drlica-Wagner, Alex Gomez-Vargas, German A. Hewitt, John W. Linden, Tim Tibaldo, Luigi TI SEARCHING FOR DARK MATTER ANNIHILATION IN THE SMITH HIGH-VELOCITY CLOUD SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; gamma rays: general; gamma rays: ISM; ISM: clouds ID LARGE-AREA TELESCOPE; GAMMA-RAY EMISSION; MILKY-WAY; CO SURVEY; GALAXY; CONSTRAINTS; GAS; PROPAGATION; CATALOG; MODELS AB Recent observations suggest that some high-velocity clouds may be confined by massive dark matter halos. In particular, the proximity and proposed dark matter content of the Smith Cloud make it a tempting target for the indirect detection of dark matter annihilation. We argue that the Smith Cloud may be a better target than some Milky Way dwarf spheroidal satellite galaxies and use gamma-ray observations from the Fermi Large Area Telescope to search for a dark matter annihilation signal. No significant gamma-ray excess is found coincident with the Smith Cloud, and we set strong limits on the dark matter annihilation cross section assuming a spatially extended dark matter profile consistent with dynamical modeling of the Smith Cloud. Notably, these limits exclude the canonical thermal relic cross section (similar to 3 x 10(-26) cm(3) s(-1)) for dark matter masses less than or similar to 30 GeV annihilating via the b (b) over bar or tau(+)tau(-) channels for certain assumptions of the dark matter density profile; however, uncertainties in the dark matter content of the Smith Cloud may significantly weaken these constraints. C1 [Drlica-Wagner, Alex] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA. [Gomez-Vargas, German A.] Pontificia Univ Catolica Chile, Dept Fis, Santiago 4860, Chile. [Gomez-Vargas, German A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Hewitt, John W.] Univ Maryland, CRESST, Baltimore, MD 21250 USA. [Hewitt, John W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Linden, Tim] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Tibaldo, Luigi] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, Stanford, CA 94305 USA. [Tibaldo, Luigi] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. RP Drlica-Wagner, A (reprint author), Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, POB 500, Batavia, IL 60510 USA. RI Gomez-Vargas, German/C-7138-2015 FU NASA Fermi Guest Investigator Program [61330]; NASA through Einstein Postdoctoral Award [PF3-140110]; Conicyt Anillo [ACT1102]; Spanish MICINN's Consolider-Ingenio 2010 Programme [MultiDark CSD2009-00064, FPA2012-34694]; Department of Energy Office of Science Graduate Fellowship Program (DOE SCGF) [DE-AC05-06OR23100]; National Aeronautics and Space Administration and the Department of Energy in the United States; Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan; K.A. Wallenberg Foundation; Swedish Research Council and the Swedish National Space Board in Sweden FX We would like to thank Luca Baldini, Seth Digel, Guolaugur Johannesson, and Miguel Sanchez-Conde for helpful discussions. This project is partially supported by the NASA Fermi Guest Investigator Program Cycle 6 No. 61330. T.L. is supported by NASA through Einstein Postdoctoral Award No. PF3-140110. The work of G.A.G.V. was supported by Conicyt Anillo grant ACT1102 and the Spanish MICINN's Consolider-Ingenio 2010 Programme under grant MultiDark CSD2009-00064 and grant FPA2012-34694. A.D.W. received partial support from the Department of Energy Office of Science Graduate Fellowship Program (DOE SCGF) administered by ORISE-ORAU under Contract No. DE-AC05-06OR23100.; The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K.A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. NR 48 TC 12 Z9 12 U1 2 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 JUL 20 PY 2014 VL 790 IS 1 AR 24 DI 10.1088/0004-637X/790/1/24 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800024 ER PT J AU Fox, OD Bostroem, KA Van Dyk, SD Filippenko, AV Fransson, C Matheson, T Cenko, SB Chandra, P Dwarkadas, V Li, WD Parker, AH Smith, N AF Fox, Ori D. Bostroem, K. Azalee Van Dyk, Schuyler D. Filippenko, Alexei V. Fransson, Claes Matheson, Thomas Cenko, S. Bradley Chandra, Poonam Dwarkadas, Vikram Li, Weidong Parker, Alex H. Smith, Nathan TI UNCOVERING THE PUTATIVE B-STAR BINARY COMPANION OF THE SN 1993J PROGENITOR SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; supernovae: general; supernovae: individual (SN 1993J) ID HUBBLE-SPACE-TELESCOPE; SUPERNOVA 1993J; RING NEBULA; SUPERGIANT PROGENITOR; IIB SUPERNOVA; LIGHT CURVES; SPECTRA; SPECTROSCOPY; PHOTOMETRY; EMISSION AB The Type IIb supernova (SN) 1993J is one of only a few stripped-envelope SNe with a progenitor star identified in pre-explosion images. SN IIb models typically invoke H envelope stripping by mass transfer in a binary system. For the case of SN 1993J, the models suggest that the companion grew to 22M(circle dot) and became a source of ultraviolet (UV) excess. Located in M81, at a distance of only 3.6 Mpc, SN 1993J offers one of the best opportunities to detect the putative companion and test the progenitor model. Previously published near-UV spectra in 2004 showed evidence for absorption lines consistent with a hot (B2 Ia) star, but the field was crowded and dominated by flux from the SN. Here we present Hubble Space Telescope Cosmic Origins Spectrograph and Wide-Field Camera 3 observations of SN 1993J from 2012, at which point the flux from the SN had faded sufficiently to potentially measure the UV continuum properties from the putative companion. The resulting UV spectrum is consistent with contributions from both a hot B star and the SN, although we cannot rule out line-of-sight coincidences. C1 [Fox, Ori D.; Filippenko, Alexei V.; Cenko, S. Bradley; Li, Weidong; Parker, Alex H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Bostroem, K. Azalee] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Van Dyk, Schuyler D.] CALTECH, Pasadena, CA 91125 USA. [Fransson, Claes] Stockholm Univ, Oskar Klein Ctr, Dept Astron, SE-10691 Stockholm, Sweden. [Matheson, Thomas] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Chandra, Poonam] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Dwarkadas, Vikram] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Fox, OD (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM ofox@berkeley.edu OI Fransson, Claes/0000-0001-8532-3594; Van Dyk, Schuyler/0000-0001-9038-9950 FU NASA [NAS5-26555]; NASA - STScI [GO-12531]; NSF [AST-1211916]; TABASGO Foundation; Christopher R. Redlich Fund; Swedish Research Council and National Space Board; W.M. Keck Foundation FX (Observed -Model)/Error Normalized Probability That x2 Due to Chance (Q) This work is based on observations made with the NASA/ ESA Hubble Space Telescope, obtained from the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under NASA contract NAS5-26555. Financial support was provided by NASA through grant GO-12531 from STScI, NSF grant AST-1211916, the TABASGO Foundation, and the Christopher R. Redlich Fund. The research by C.F. is supported by the Swedish Research Council and National Space Board. We are grateful to the STScI Help Desk for their assistance with the HST data. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W.M. Keck Foundation. We thank the staff of the Keck Observatory, together with Kelsey Clubb, WeiKang Zheng, and Adam Miller, for their assistance with the observations. Selma de Mink provided enlightening discussions. NR 50 TC 25 Z9 25 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2014 VL 790 IS 1 AR 17 DI 10.1088/0004-637X/790/1/17 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800017 ER PT J AU Haas, M Leipski, C Barthel, P Wilkes, BJ Vegetti, S Bussmann, RS Willner, SP Westhues, C Ashby, MLN Chini, R Clements, DL Fassnacht, CD Horesh, A Klaas, U Koopmans, LVE Kuraszkiewicz, J Lagattuta, DJ Meisenheimer, K Stern, D Wylezalek, D AF Haas, Martin Leipski, Christian Barthel, Peter Wilkes, Belinda J. Vegetti, Simona Bussmann, R. Shane Willner, S. P. Westhues, Christian Ashby, Matthew L. N. Chini, Rolf Clements, David L. Fassnacht, Christopher D. Horesh, Assaf Klaas, Ulrich Koopmans, Leon V. E. Kuraszkiewicz, Joanna Lagattuta, David J. Meisenheimer, Klaus Stern, Daniel Wylezalek, Dominika TI 3C 220.3: A RADIO GALAXY LENSING A SUBMILLIMETER GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: individual (3C 220.3); gravitational lensing: strong; radio continuum: galaxies; submillimeter: galaxies ID SPITZER-SPACE-TELESCOPE; COLD DARK-MATTER; GRAVITATIONAL-LENS; ARRAY CAMERA; MISSION; MASS; SPECTROMETER; PERFORMANCE; POPULATION; B2045+265 AB Herschel Space Observatory photometry and extensive multiwavelength follow-up have revealed that the powerful radio galaxy (PRG) 3C 220.3 at z = 0.685 acts as a gravitational lens for a background submillimeter galaxy (SMG) at z = 2.221. At an observed wavelength of 1 mm, the SMG is lensed into three distinct images. In the observed near infrared, these images are connected by an arc of similar to 1 ''.8 radius forming an Einstein half-ring centered near the radio galaxy. In visible light, only the arc is apparent. 3C 220.3 is the only known instance of strong galaxy-scale lensing by a PRG not located in a galaxy cluster and therefore it offers the potential to probe the dark matter content of the radio galaxy host. Lens modeling rejects a single lens, but two lenses centered on the radio galaxy host A and a companion B, separated by 1 ''.5, provide a fit consistent with all data and reveal faint candidates for the predicted fourth and fifth images. The model does not require an extended common dark matter halo, consistent with the absence of extended bright X-ray emission on our Chandra image. The projected dark matter fractions within the Einstein radii of A (1 ''.02) and B (0 ''.61) are about 0.4 +/- 0.3 and 0.55 +/- 0.3. The mass to i-band light ratios of A and B, M/L-i similar to 8 +/- 4 M-circle dot L-circle dot(-1), appear comparable to those of radio-quiet lensing galaxies at the same redshift in the CfA-Arizona Space Telescope LEns Survey, Lenses Structure and Dynamics, and Strong Lenses in the Legacy Survey samples. The lensed SMG is extremely bright with observed f (250 mu m) = 440 mJy owing to a magnification factor mu similar to 10. The SMG spectrum shows luminous, narrow Civ lambda 1549 angstrom emission, revealing that the SMG houses a hidden quasar in addition to a violent starburst. Multicolor image reconstruction of the SMG indicates a bipolar morphology of the emitted ultraviolet (UV) light suggestive of cones through which UV light escapes a dust-enshrouded nucleus. C1 [Haas, Martin; Westhues, Christian; Chini, Rolf] Ruhr Univ Bochum, Inst Astron, Bochum, Germany. [Leipski, Christian; Klaas, Ulrich; Meisenheimer, Klaus] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Barthel, Peter; Koopmans, Leon V. E.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. [Wilkes, Belinda J.; Bussmann, R. Shane; Willner, S. P.; Ashby, Matthew L. N.; Kuraszkiewicz, Joanna] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vegetti, Simona] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Chini, Rolf] Univ Catolica Norte, Antofagasta, Chile. [Clements, David L.] Univ London Imperial Coll Sci Technol & Med, London, England. [Fassnacht, Christopher D.] Univ Calif Davis, Davis, CA 95616 USA. [Horesh, Assaf] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Lagattuta, David J.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Lagattuta, David J.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW 2016, Australia. [Stern, Daniel; Wylezalek, Dominika] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Wylezalek, Dominika] European So Observ, Garching, Germany. RP Haas, M (reprint author), Ruhr Univ Bochum, Inst Astron, Postfach 102148, Bochum, Germany. EM haas@astro.rub.de RI Horesh, Assaf/O-9873-2016 OI Horesh, Assaf/0000-0002-5936-1156 NR 50 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2014 VL 790 IS 1 AR 46 DI 10.1088/0004-637X/790/1/46 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800046 ER PT J AU Kelly, PL Fox, OD Filippenko, AV Cenko, SB Prato, L Schaefer, G Shen, KJ Zheng, WK Graham, ML Tucker, BE AF Kelly, Patrick L. Fox, Ori D. Filippenko, Alexei V. Cenko, S. Bradley Prato, Lisa Schaefer, Gail Shen, Ken J. Zheng, WeiKang Graham, Melissa L. Tucker, Brad E. TI CONSTRAINTS ON THE PROGENITOR SYSTEM OF THE TYPE Ia SUPERNOVA 2014J FROM PRE-EXPLOSION HUBBLE SPACE TELESCOPE IMAGING SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: symbiotic; supernovae: general; supernovae: individual (SN 2014J) ID NOVA RS OPHIUCHI; WHITE-DWARF MODELS; X-RAY; RECURRENT NOVAE; 1985 OUTBURST; RED GIANT; SYMBIOTIC STARS; HOST GALAXIES; EVOLUTION; MASS AB We constrain the properties of the progenitor system of the highly reddened Type Ia supernova (SN Ia) 2014J in Messier 82 (M82; d approximate to 3.5 Mpc). We determine the supernova (SN) location using Keck-II K-band adaptive optics images, and we find no evidence for flux from a progenitor system in pre-explosion near-ultraviolet through near-infrared Hubble Space Telescope (HST) images. Our upper limits exclude systems having a bright red giant companion, including symbiotic novae with luminosities comparable to that of RS Ophiuchi. While the flux constraints are also inconsistent with predictions for comparatively cool He-donor systems (T less than or similar to 35,000 K), we cannot preclude a system similar to V445 Puppis. The progenitor constraints are robust across a wide range of RV and AV values, but significantly greater values than those inferred from the SN light curve and spectrum would yield proportionally brighter luminosity limits. The comparatively faint flux expected from a binary progenitor system consisting of white dwarf stars would not have been detected in the pre-explosion HST imaging. Infrared HST exposures yield more stringent constraints on the luminosities of very cool (T < 3000 K) companion stars than was possible in the case of SN Ia 2011fe. C1 [Kelly, Patrick L.; Fox, Ori D.; Filippenko, Alexei V.; Shen, Ken J.; Zheng, WeiKang; Graham, Melissa L.; Tucker, Brad E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Prato, Lisa] Lowell Observ, Flagstaff, AZ 86001 USA. [Schaefer, Gail] Georgia State Univ, Mt Wilson Observ, CHARA Array, Mt Wilson, CA 91023 USA. [Tucker, Brad E.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. RP Kelly, PL (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM pkelly@astro.berkeley.edu FU Christopher R. Redlich Fund; TABASGO Foundation; Gary and Cynthia Bengier; NSF [AST-1211916]; NASA from the Space Telescope Science Institute [AR-12623, AR-12850]; AURA, Inc., under NASA [NAS 5-26555]; NASA through Einstein Postdoctoral Fellowship [PF1-120088]; Smithsonian Astrophysical Observatory for NASA [NAS8-03060]; W. M. Keck Foundation FX We greatly appreciate the critical contribution of observing time from Vithal Tilvi, Nicola Mehrtens, Casey Papovich, and Mark Dickinson that enabled us to complete the Keck AO imaging, as well as their encouragement and helpful suggestions on the manuscript. We thank Michael Liu, Shriharsh Tendulkar, Yi Cao, and Trent Dupuy for generously providing details of their NIRC2 AO observations to aid our team in deciding whether any further imaging could be helpful. Correspondence with both Matthew Darnley and G. C. Anupama was also useful. A.V.F.'s group at UC Berkeley has received generous financial assistance from the Christopher R. Redlich Fund, the TABASGO Foundation, Gary and Cynthia Bengier, and NSF grant AST-1211916. This work was also supported by NASA grants AR-12623 and AR-12850 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. K.J.S. is supported by NASA through Einstein Postdoctoral Fellowship grant number PF1-120088 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060.; Some of the data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to NASA through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We recognize the Hawaiian community for the opportunity to conduct these observations from the summit of Mauna Kea. NR 75 TC 31 Z9 31 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 JUL 20 PY 2014 VL 790 IS 1 AR 3 DI 10.1088/0004-637X/790/1/3 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800003 ER PT J AU Kreckel, K Armus, L Groves, B Lyubenova, M Diaz-Santos, T Schinnerer, E Appleton, P Croxall, KV Dale, DA Hunt, LK Beirao, P Bolatto, AD Calzetti, D Meyer, JD Draine, BT Hinz, J Kennicutt, RC Meidt, S Murphy, EJ Smith, JDT Tabatabaei, FS Walter, F AF Kreckel, K. Armus, L. Groves, B. Lyubenova, M. Diaz-Santos, T. Schinnerer, E. Appleton, P. Croxall, K. V. Dale, D. A. Hunt, L. K. Beirao, P. Bolatto, A. D. Calzetti, D. Meyer, J. Donovan Draine, B. T. Hinz, J. Kennicutt, R. C. Meidt, S. Murphy, E. J. Smith, J. D. T. Tabatabaei, F. S. Walter, F. TI A FAR-IR VIEW OF THE STARBURST-DRIVEN SUPERWIND IN NGC 2146 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies: individual (NGC 2146); galaxies: starburst; infrared: ISM; ISM: kinematics and dynamics ID STAR-FORMING GALAXIES; ULTRALUMINOUS INFRARED GALAXIES; INTEGRAL FIELD SPECTROSCOPY; POTSDAM MULTIAPERTURE SPECTROPHOTOMETER; LYMAN BREAK GALAXIES; HERSCHEL-PACS; MOLECULAR OUTFLOWS; NEARBY GALAXIES; INTERSTELLAR CARBON; ELLIPTIC GALAXIES AB NGC 2146, a nearby luminous infrared galaxy, presents evidence for outflows along the disk minor axis in all gas phases (ionized, neutral atomic, and molecular). We present an analysis of the multi-phase, starburst-driven superwind in the central 5 kpc as traced in spatially resolved spectral line observations, using far-IR Herschel PACS spectroscopy, to probe the effects on the atomic and ionized gas, and optical integral field spectroscopy to examine the ionized gas through diagnostic line ratios. We observe an increased similar to 250 km s(-1) velocity dispersion in the [O I] 63 mu m, [O III] 88 mu m, [N II] 122 mu m, and [C II] 158 mu m fine-structure lines that is spatially coincident with high excitation gas above and below the disk. We model this with a slow similar to 200 km s(-1) shock and trace the superwind to the edge of our field of view 2.5 kpc above the disk. We present new SOFIA 37 mu m observations to explore the warm dust distribution, and detect no clear dust entrainment in the outflow. The stellar kinematics appear decoupled from the regular disk rotation seen in all gas phases, consistent with a recent merger event disrupting the system. We consider the role of the superwind in the evolution of NGC 2146 and speculate on the evolutionary future of the system. Our observations of NGC 2146 in the far-IR allow an unobscured view of the wind, crucial for tracing the superwind to the launching region at the disk center, and provide a local analog for future ALMA observations of outflows in high-redshift systems. C1 [Kreckel, K.; Groves, B.; Lyubenova, M.; Schinnerer, E.; Meidt, S.; Tabatabaei, F. S.; Walter, F.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Armus, L.; Diaz-Santos, T.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Appleton, P.] CALTECH, IPAC, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. [Croxall, K. V.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Dale, D. A.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Hunt, L. K.] INAF Osservatorio Astros Arcetri, I-50125 Florence, Italy. [Beirao, P.] Observ Paris, F-75014 Paris, France. [Bolatto, A. D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Bolatto, A. D.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Bolatto, A. D.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Calzetti, D.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Meyer, J. Donovan] Natl Radio Astron Observ, Charlottesville, VA 22901 USA. [Draine, B. T.] Princeton Univ Observ, Princeton, NJ 08544 USA. [Hinz, J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Hinz, J.] MMT Observ, Tucson, AZ 85721 USA. [Kennicutt, R. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Murphy, E. J.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Smith, J. D. T.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. RP Kreckel, K (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM kreckel@mpia.de RI Kreckel, Kathryn/C-3468-2012; OI Appleton, Philip/0000-0002-7607-8766; Kreckel, Kathryn/0000-0001-6551-3091; Hunt, Leslie/0000-0001-9162-2371; Schinnerer, Eva/0000-0002-3933-7677 FU DFG Priority Program 1573 [GR 3948/1-1, SCHI 536/8-1]; National Science Foundation [AST-0955836]; Cottrell Scholar award from the Research Corporation for Science Advancement; DFG [TA 801/1-1]; BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain); Universities Space Research Association, Inc. (USRA), under NASA [NAS2-97001]; Deutsches SOFIA Institut (DSI) under DLR [50 OK 0901] FX We thank the referee for helpful comments. K. K. acknowledges the support of grants GR 3948/1-1 and SCHI 536/8-1 from the DFG Priority Program 1573, "The Physics of the Interstellar Medium." A.D.B. acknowledges support from the National Science Foundation through grant AST-0955836, as well as a Cottrell Scholar award from the Research Corporation for Science Advancement. The National Radio Astronomy Observatory is a facility of the National Science Foundation Operated under cooperative agreement by Associated Universities, Inc. F. T. acknowledges the DFG grant TA 801/1-1.; This work is based on observations made with Herschel. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain).; Based in part on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). SOFIA is jointly operated by the Universities Space Research Association, Inc. (USRA), under NASA contract NAS2-97001, and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901 to the University of Stuttgart. NR 99 TC 7 Z9 7 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2014 VL 790 IS 1 AR 26 DI 10.1088/0004-637X/790/1/26 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800026 ER PT J AU Kucera, TA Gilbert, HR Karpen, JT AF Kucera, T. A. Gilbert, H. R. Karpen, J. T. TI MASS FLOWS IN A PROMINENCE SPINE AS OBSERVED IN EUV SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: filaments; prominences ID SOLAR PROMINENCES; ABSORPTION FEATURES; HYDROMAGNETIC INTERIOR; EVOLUTION; FILAMENT; CORONA; DYNAMICS; SDO/AIA; REGION; MODEL AB We analyze a quiescent prominence observed by the Solar Dynamics Observatory's Atmospheric Imaging Assembly (AIA) with a focus on mass and energy flux in the spine, measured using Lyman continuum absorption. This is the first time this type of analysis has been applied with an emphasis on individual features and fluxes in a quiescent prominence. The prominence, observed on 2010 September 28, is detectable in most AIA wavebands in absorption and/or emission. Flows along the spine exhibit horizontal bands 5 ''-10 '' wide and kinetic energy fluxes on the order of a few times 10(5) erg s(-1)cm(-2), consistent with quiet sun coronal heating estimates. For a discrete moving feature we estimate a mass of a few times 10(11) g. We discuss the implications of our derived properties for a model of prominence dynamics, the thermal non-equilibrium model. C1 [Kucera, T. A.; Gilbert, H. R.; Karpen, J. T.] NASA GSFC, Greenbelt, MD 20771 USA. RP Kucera, TA (reprint author), NASA GSFC, Greenbelt, MD 20771 USA. OI Kucera, Therese/0000-0001-9632-447X FU NASA's Living with a Star Targeted Research and Technology program FX The authors thank Karin Muglach for helpful comments on the manuscript. This work was funded by NASA's Living with a Star Targeted Research and Technology program. AIA data are courtesy of NASA's SDO and the AIA science team. The SECCHI data from NASA's STEREO mission are produced by an international consortium of the NRL, LMSAL, and NASA GSFC (USA), RAL and Univ. Birmingham (UK), MPS (Germany), CSL (Belgium), and IOTA and IAS (France). NR 42 TC 0 Z9 0 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 JUL 20 PY 2014 VL 790 IS 1 AR 68 DI 10.1088/0004-637X/790/1/68 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800068 ER PT J AU Rigby, JR Bayliss, MB Gladders, MD Sharon, K Wuyts, E Dahle, H AF Rigby, J. R. Bayliss, M. B. Gladders, M. D. Sharon, K. Wuyts, E. Dahle, H. TI ON THE LACK OF CORRELATION BETWEEN Mg II 2796, 2803 angstrom AND Ly alpha EMISSION IN LENSED STAR-FORMING GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: star formation; gravitational lensing: strong; ISM: jets and outflows; techniques: spectroscopic ID RCSGA 032727-132609; SPECTROSCOPY; OUTFLOWS; ABSORPTION; SPECTRA; BRIGHT; Z=1.7 AB We examine the Mg II 2796, 2803, Ly alpha, and nebular line emission in five bright star-forming galaxies at 1.66 < z < 1.91 that have been gravitationally lensed by foreground galaxy clusters. All five galaxies show prominent Mg II emission and absorption in a P Cygni profile. We find no correlation between the equivalent widths of Mg II and Lya emission. The Mg II emission has a broader range of velocities than do the nebular emission line profiles; the Mg II emission is redshifted with respect to systemic by 100-200 km s(-1). When present, Ly alpha is even more redshifted. The reddest components of Mg II and Ly alpha emission have tails to 500-600 km s(-1), implying a strong outflow. The lack of correlation in the Mg II and Ly alpha equivalent widths, the differing velocity profiles, and the high ratios of Mg II to nebular line fluxes together suggest that the bulk of Mg II emission does not ultimately arise as nebular line emission, but may instead be reprocessed stellar continuum emission. C1 [Rigby, J. R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Bayliss, M. B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bayliss, M. B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gladders, M. D.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Gladders, M. D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Sharon, K.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Wuyts, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Dahle, H.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. RP Rigby, JR (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. RI Rigby, Jane/D-4588-2012 OI Rigby, Jane/0000-0002-7627-6551 FU Carnegie Observatories, U. Michigan; Carnegie Observatories, U. Chicago; Harvard-Smithsonian Center for Astrophysics FX This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. Magellan time for this project was granted by the Carnegie Observatories, U. Michigan, U. Chicago, and the Harvard-Smithsonian Center for Astrophysics. NR 22 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2014 VL 790 IS 1 AR 44 DI 10.1088/0004-637X/790/1/44 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800044 ER PT J AU Staguhn, JG Kovacs, A Arendt, RG Benford, DJ Decarli, R Dwek, E Fixsen, DJ Hilton, GC Irwin, KD Jhabvala, CA Karim, A Leclercq, S Maher, SF Miller, TM Moseley, SH Sharp, EH Walter, F Wollack, EJ AF Staguhn, Johannes G. Kovacs, Attila Arendt, Richard G. Benford, Dominic J. Decarli, Roberto Dwek, Eli Fixsen, Dale J. Hilton, Gene C. Irwin, Kent D. Jhabvala, Christine A. Karim, Alexander Leclercq, Samuel Maher, Stephen F. Miller, Timothy M. Moseley, S. Harvey Sharp, Elmer H. Walter, Fabian Wollack, Edward J. TI THE GISMO TWO-MILLIMETER DEEP FIELD IN GOODS-N SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; galaxies: luminosity function, mass function; galaxies: photometry; galaxies: starburst; infrared: galaxies ID SCUBA SUPER-MAP; MU-M OBSERVATIONS; SUBMILLIMETER GALAXIES; LUMINOSITY FUNCTIONS; INFRARED PROPERTIES; STAR-FORMATION; NUMBER COUNTS; NORTH FIELD; 1 MM; TELESCOPE AB We present deep continuum observations using the GISMO camera at a wavelength of 2 mm centered on the Hubble Deep Field in the GOODS-N field. These are the first deep field observations ever obtained at this wavelength. The 1 sigma sensitivity in the innermost similar to 4' of the 7' diameter map is similar to 135 mu Jy beam(-1), a factor of three higher in flux/beam sensitivity than the deepest available SCUBA 850 mu m observations, and almost a factor of four higher in flux/beam sensitivity than the combined MAMBO/AzTEC 1.2 mm observations of this region. Our source extraction algorithm identifies 12 sources directly, and another 3 through correlation with known sources at 1.2 mm and 850 m. Five of the directly detected GISMO sources have counterparts in the MAMBO/AzTEC catalog, and four of those also have SCUBA counterparts. HDF850.1, one of the first blank-field detected submillimeter galaxies, is now detected at 2 mm. The median redshift of all sources with counterparts of known redshifts is (z) over tilde = 2.91 +/- 0.94. Statistically, the detections are most likely real for five of the seven 2 mm sources without shorter wavelength counterparts, while the probability for none of them being real is negligible. C1 [Staguhn, Johannes G.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. [Staguhn, Johannes G.; Arendt, Richard G.; Benford, Dominic J.; Dwek, Eli; Fixsen, Dale J.; Jhabvala, Christine A.; Maher, Stephen F.; Miller, Timothy M.; Moseley, S. Harvey; Sharp, Elmer H.; Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Kovacs, Attila] CALTECH, Pasadena, CA 91125 USA. [Kovacs, Attila] Univ Minnesota, Inst Astrophys, Minneapolis, MN 55455 USA. [Arendt, Richard G.] Univ Maryland, CRESST, Baltimore, MD 21250 USA. [Decarli, Roberto; Walter, Fabian] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Fixsen, Dale J.] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Hilton, Gene C.; Irwin, Kent D.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Irwin, Kent D.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Karim, Alexander] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Karim, Alexander] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Leclercq, Samuel] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Maher, Stephen F.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Sharp, Elmer H.] Global Sci & Technol Inc, Greenbelt, MD 20770 USA. RP Staguhn, JG (reprint author), Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA. RI Kovacs, Attila/C-1171-2010; Wollack, Edward/D-4467-2012; Benford, Dominic/D-4760-2012; OI Kovacs, Attila/0000-0001-8991-9088; Wollack, Edward/0000-0002-7567-4451; Benford, Dominic/0000-0002-9884-4206; Arendt, Richard/0000-0001-8403-8548 FU INSU/CNRS (France); MPG (Germany); IGN (Spain); NSF ATI grants [1020981, 1106284] FX We would like to thank Carsten Kramer, Santiago Navarro, David John, Albrecht Sievers, and the entire IRAM Granada staff for their support during the instrument installation and observations. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). This work was supported through NSF ATI grants 1020981 and 1106284. NR 49 TC 9 Z9 9 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2014 VL 790 IS 1 AR 77 DI 10.1088/0004-637X/790/1/77 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0SK UT WOS:000338836800077 ER PT J AU Gall, C Hjorth, J Watson, D Dwek, E Maund, JR Fox, O Leloudas, G Malesani, D Day-Jones, AC AF Gall, Christa Hjorth, Jens Watson, Darach Dwek, Eli Maund, Justyn R. Fox, Ori Leloudas, Giorgos Malesani, Daniele Day-Jones, Avril C. TI Rapid formation of large dust grains in the luminous supernova 2010j1 SO NATURE LA English DT Article ID LARGE-MAGELLANIC-CLOUD; IIN SUPERNOVA; SN 2010JL; INFRARED-EMISSION; INTERSTELLAR DUST; SHOCK BREAKOUT; MASSIVE STARS; MILKY-WAY; RADIATION; HERSCHEL AB The origin of dust in galaxies is still a mystery(1-4). The majority of the refractory elements are produced in supernova explosions, but it is unclear how and where dust grains condense and grow, and how they avoid destruction in the harsh environments of star-forming galaxies. The recent detection of 0.1 to 0.5 solar masses of dust in nearby supernova remnants(5-7) suggests in situ dust formation, while other observations reveal very little dust in supernovae in the first few years after explosion(1,8,10). Observations of the spectral evolution of the bright SN 2010j1 have been interpreted as pre-existing dust(11), dust formationlz(12,13) or no dust at all(14). Here we report the rapid (40 to 240 days) formation of dust in its dense circumstellar medium. The wavelength-dependent extinction of this dust reveals the presence of very large (exceeding one micrometre) grains, which resist destruction(15). At later times (500 to 900 days), the near-infrared thermal emission shows an accelerated growth in dust mass, marking the transition of the dust source from the circumstellar medium to the ejecta. This provides the link between the early and late dust mass evolution in supernovae with dense circumstellar media. C1 [Gall, Christa] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Gall, Christa; Hjorth, Jens; Watson, Darach; Maund, Justyn R.; Leloudas, Giorgos; Malesani, Daniele] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Gall, Christa; Dwek, Eli] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Maund, Justyn R.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Fox, Ori] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Leloudas, Giorgos] Stockholm Univ, Dept Phys, Oskar Klein Ctr, Albanova Univ Ctr, S-10691 Stockholm, Sweden. [Day-Jones, Avril C.] Univ Chile, Dept Astron, Santiago, Chile. RP Gall, C (reprint author), Aarhus Univ, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. EM cgall@phys.au.dk RI Hjorth, Jens/M-5787-2014; Watson, Darach/E-4521-2015; Gall, Christa/P-7630-2016; OI Hjorth, Jens/0000-0002-4571-2306; Watson, Darach/0000-0002-4465-8264; Gall, Christa/0000-0002-8526-3963; Maund, Justyn/0000-0003-0733-7215 FU ESO Telescopes at the La Silla paranal Observatory [084.C-0315(D), 087.C-0456(A)]; NASA Postdoctoral Program (NPP); Danish Agency for Science and Technology and Innovation; Swedish Research Council [623-2011-7117]; Proyecto Basal [PB06]; Joint Committee ESO-Government Chile; Danish National Research Foundation FX We thank L. Christensen and T. Frederiksen for advice on data reduction with the X-shooter pipeline and M. Stritzinger and R. Arendt for discussions. RESEARCH This investigation is based on observations made with ESO Telescopes at the La Silla paranal Observatory under programme ID numbers 084.C-0315(D) and 087.C-0456(A). C.G. was supported from the NASA Postdoctoral Program (NPP) and acknowledges funding provided by the Danish Agency for Science and Technology and Innovation. G.L. is supported by the Swedish Research Council through grant number 623-2011-7117. A.C.D.-J. is supported by the Proyecto Basal PB06 (CATA), and partially supported by the Joint Committee ESO-Government Chile. The Dark Cosmology Centre is funded by the Danish National Research Foundation. NR 47 TC 36 Z9 37 U1 0 U2 8 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD JUL 17 PY 2014 VL 511 IS 7509 BP 326 EP + DI 10.1038/nature13558 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AL2YR UT WOS:000338992200030 PM 25030169 ER PT J AU Winslow, RM Johnson, CL Anderson, BJ Gershman, DJ Raines, JM Lillis, RJ Korth, H Slavin, JA Solomon, SC Zurbuchen, TH Zuber, MT AF Winslow, Reka M. Johnson, Catherine L. Anderson, Brian J. Gershman, Daniel J. Raines, Jim M. Lillis, Robert J. Korth, Haje Slavin, James A. Solomon, Sean C. Zurbuchen, Thomas H. Zuber, Maria T. TI Mercury's surface magnetic field determined from proton-reflection magnetometry SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID LUNAR-PROSPECTOR; ELECTRON REFLECTOMETER; MESSENGER AB Solar wind protons observed by the MESSENGER spacecraft in orbit about Mercury exhibit signatures of precipitation loss to Mercury's surface. We apply proton-reflection magnetometry to sense Mercury's surface magnetic field intensity in the planet's northern and southern hemispheres. The results are consistent with a dipole field offset to the north and show that the technique may be used to resolve regional-scale fields at the surface. The proton loss cones indicate persistent ion precipitation to the surface in the northern magnetospheric cusp region and in the southern hemisphere at low nightside latitudes. The latter observation implies that most of the surface in Mercury's southern hemisphere is continuously bombarded by plasma, in contrast with the premise that the global magnetic field largely protects the planetary surface from the solar wind. C1 [Winslow, Reka M.; Johnson, Catherine L.] Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V5Z 1M9, Canada. [Johnson, Catherine L.] Planetary Sci Inst, Tucson, AZ USA. [Anderson, Brian J.; Korth, Haje] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Gershman, Daniel J.; Raines, Jim M.; Slavin, James A.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Gershman, Daniel J.] NASA, Geospace Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD USA. [Lillis, Robert J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 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. [Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. RP Winslow, RM (reprint author), Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V5Z 1M9, Canada. EM rwinslow@eos.ubc.ca RI Lillis, Robert/A-3281-2008; Slavin, James/H-3170-2012 OI Lillis, Robert/0000-0003-0578-517X; Slavin, James/0000-0002-9206-724X FU NASA [NAS5-97271, NASW-00002]; MESSENGER Participating Scientist grant [NNX11AB84G]; Natural Sciences and Engineering Research Council of Canada 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. C. L. J. is supported by the MESSENGER Participating Scientist grant NNX11AB84G. R. M. W. and C. L. J. acknowledge support from the Natural Sciences and Engineering Research Council of Canada. MESSENGER data are available on the Planetary Data System (https://pds.jpl.nasa.gov). NR 23 TC 7 Z9 7 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUL 16 PY 2014 VL 41 IS 13 BP 4463 EP 4470 DI 10.1002/2014GL060258 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AN0SW UT WOS:000340295300008 ER PT J AU Plane, JMC Feng, W Dawkins, E Chipperfield, MP Hoffner, J Janches, D Marsh, DR AF Plane, J. M. C. Feng, W. Dawkins, E. Chipperfield, M. P. Hoeffner, J. Janches, D. Marsh, D. R. TI Resolving the strange behavior of extraterrestrial potassium in the upper atmosphere SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID LIDAR MEASUREMENTS; CHEMICAL-MODEL; MESOSPHERIC NA; CHEMISTRY; SODIUM; KINETICS; LITHIUM; METALS; NAHCO3; LAYER AB It has been known since the 1960s that the layers of Na and K atoms, which occur between 80 and 105 km in the Earth's atmosphere as a result of meteoric ablation, exhibit completely different seasonal behavior. In the extratropics Na varies annually, with a pronounced wintertime maximum and summertime minimum. However, K varies semiannually with a small summertime maximum and minima at the equinoxes. This contrasting behavior has never been satisfactorily explained. Here we use a combination of electronic structure and chemical kinetic rate theory to determine two key differences in the chemistries of K and Na. First, the neutralization of K+ ions is only favored at low temperatures during summer. Second, cycling between K and its major neutral reservoir KHCO3 is essentially temperature independent. A whole atmosphere model incorporating this new chemistry, together with a meteor input function, now correctly predicts the seasonal behavior of the K layer. C1 [Plane, J. M. C.; Feng, W.] Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England. [Feng, W.; Dawkins, E.; Chipperfield, M. P.] Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England. [Hoeffner, J.] Leibniz Inst Atmospher Phys, Kuhlungsborn, Germany. [Janches, D.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. [Marsh, D. R.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. RP Plane, JMC (reprint author), Univ Leeds, Sch Chem, Leeds LS2 9JT, W Yorkshire, England. EM j.m.c.plane@leeds.ac.uk RI Marsh, Daniel/A-8406-2008; Janches, Diego/D-4674-2012; FENG, WUHU/B-8327-2008; Chipperfield, Martyn/H-6359-2013; Plane, John/C-7444-2015 OI Marsh, Daniel/0000-0001-6699-494X; Janches, Diego/0000-0001-8615-5166; FENG, WUHU/0000-0002-9907-9120; Chipperfield, Martyn/0000-0002-6803-4149; Plane, John/0000-0003-3648-6893 FU UK Natural Environment Research Council (NERC) [NE/G019487/1]; European Research Council [291332-CODITA] FX This work was supported by the UK Natural Environment Research Council (NERC grant NE/G019487/1) and the European Research Council (project 291332-CODITA). The data required for the rate coefficient calculations described in the paper are in Table S1 of the supporting information. Additional figures S1-S3, referred to in the text, are also included in the supporting information. NR 32 TC 13 Z9 13 U1 5 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 JUL 16 PY 2014 VL 41 IS 13 BP 4753 EP 4760 DI 10.1002/2014GL060334 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AN0SW UT WOS:000340295300044 ER PT J AU Emory, AE Demoz, B Vermeesch, K Hicks, M AF Emory, Amber E. Demoz, Belay Vermeesch, Kevin Hicks, Micheal TI Double bright band observations with high-resolution vertically pointing radar, lidar, and profilers SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MELTING LAYER; PRECIPITATION; CLOUDS; SYSTEM AB On 11 May 2010, an elevated temperature inversion associated with an approaching warm front produced two melting layers simultaneously, which resulted in two distinct bright bands as viewed from the ER-2 Doppler radar system, a vertically pointing, coherent X band radar located in Greenbelt, MD. Due to the high temporal resolution of this radar system, an increase in altitude of the melting layer of approximately 1.2 km in the time span of 4 min was captured. The double bright band feature remained evident for approximately 17 min, until the lower atmosphere warmed enough to dissipate the lower melting layer. This case shows the relatively rapid evolution of freezing levels in response to an advancing warm front over a 2 h time period and the descent of an elevated warm air mass with time. Although observations of double bright bands are somewhat rare, the ability to identify this phenomenon is important for rainfall estimation from spaceborne sensors because algorithms employing the restriction of a radar bright band to a constant height, especially when sampling across frontal systems, will limit the ability to accurately estimate rainfall. C1 [Emory, Amber E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Demoz, Belay] Howard Univ, Dept Phys & Astron, Washington, DC 20059 USA. [Vermeesch, Kevin] Sci Syst & Applicat Inc, Lanham, MD USA. [Hicks, Micheal] Natl Weather Serv, Sterling, VA USA. RP Emory, AE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM amber.emory@nasa.gov RI Demoz, Belay/N-4130-2014 FU NASA under the University Research Centers (URC); NOAA Center for Atmospheric Studies FX The authors would like to thank Gerald Heymsfield, Lin Tian, and Everette Joseph for fruitful and informative discussions about this case. The authors would also like to thank Kevin Witt from the Sterling, VA NWS forecast office for help with the forecast discussion and the Maryland Department of the Environment for the 915 MHz profiler data. The instruments operated at the Howard University Beltsville site are funded by NASA under the University Research Centers (URC) and NOAA Center for Atmospheric Studies. NR 27 TC 0 Z9 0 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 16 PY 2014 VL 119 IS 13 AR 2013JD020063 DI 10.1002/2013JD020063 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN2IK UT WOS:000340408000026 ER PT J AU Glantz, P Bourassa, A Herber, A Iversen, T Karlsson, J Kirkevag, A Maturilli, M Seland, O Stebel, K Struthers, H Tesche, M Thomason, L AF Glantz, Paul Bourassa, Adam Herber, Andreas Iversen, Trond Karlsson, Johannes Kirkevag, Alf Maturilli, Marion Seland, Oyvind Stebel, Kerstin Struthers, Hamish Tesche, Matthias Thomason, Larry TI Remote sensing of aerosols in the Arctic for an evaluation of global climate model simulations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OPTICAL DEPTH RETRIEVAL; EARTH SYSTEM MODEL; SEA-SALT AEROSOLS; CHEMICAL-COMPOSITION; AIR-POLLUTION; STRATOSPHERIC AEROSOL; LAGRANGIAN EXPERIMENT; LIGHT-SCATTERING; WIND-SPEED; NY-ALESUND AB In this study Moderate Resolution Imaging Spectroradiometer (MODIS) Aqua retrievals of aerosol optical thickness (AOT) at 555 nm are compared to Sun photometer measurements from Svalbard for a period of 9 years. For the 642 daily coincident measurements that were obtained, MODIS AOT generally varies within the predicted uncertainty of the retrieval over ocean (Delta AOT = +/- 0.03 +/- 0.05 . AOT). The results from the remote sensing have been used to examine the accuracy in estimates of aerosol optical properties in the Arctic, generated by global climate models and from in situ measurements at the Zeppelin station, Svalbard. AOT simulated with the Norwegian Earth System Model/Community Atmosphere Model version 4 Oslo global climate model does not reproduce the observed seasonal variability of the Arctic aerosol. The model overestimates clear-sky AOT by nearly a factor of 2 for the background summer season, while tending to underestimate the values in the spring season. Furthermore, large differences in all-sky AOT of up to 1 order of magnitude are found for the Coupled Model Intercomparison Project phase 5 model ensemble for the spring and summer seasons. Large differences between satellite/ground-based remote sensing of AOT and AOT estimated from dry and humidified scattering coefficients are found for the subarctic marine boundary layer in summer. C1 [Glantz, Paul; Tesche, Matthias] Stockholm Univ, Dept Appl Environm Sci, S-10691 Stockholm, Sweden. [Bourassa, Adam] Univ Saskatchewan, Inst Space & Atmospher Studies, Saskatoon, SK S7N 0W0, Canada. [Herber, Andreas; Maturilli, Marion] Alfred Wegener Inst Polar & Marine Res, Bremerhaven, Germany. [Iversen, Trond] ECMWF, Reading, Berks, England. [Iversen, Trond; Kirkevag, Alf; Seland, Oyvind] Norwegian Meteorol Inst, Oslo, Norway. [Karlsson, Johannes] Stockholm Univ, Dept Meteorol, S-10691 Stockholm, Sweden. [Stebel, Kerstin] Norwegian Inst Air Res, Oslo, Norway. [Struthers, Hamish] Linkoping Univ, Natl Supercomp Ctr, Linkoping, Sweden. [Thomason, Larry] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Glantz, P (reprint author), Stockholm Univ, Dept Appl Environm Sci, S-10691 Stockholm, Sweden. EM paul.glantz@itm.su.se RI Stebel, Kerstin/F-6465-2013; Maturilli, Marion/A-4344-2017; OI Stebel, Kerstin/0000-0002-6935-7564; Maturilli, Marion/0000-0001-6818-7383; Tesche, Matthias/0000-0003-0096-4785 FU Swedish Research Council for the Environment, Agricultural Sciences and Spatial Planning (FORMAS); Norwegian Space Center [JOP.12.12.2]; PM-VRAE project; Research Council of Norway through the EarthClim project [207711/E10]; Research Council of Norway through NOTUR/NorStore project; EU project PEGASOS; EU project ACCESS FX We thank the PIs of the AERONET sites used in this study for maintaining their stations. We acknowledge the MODIS mission scientists and associated NASA personnel for the production of the data used in this research effort. The authors are also thankful for the use of ECMWF data sets. We acknowledge the World Climate Research Programme's Working Group on Coupled Modeling, which is responsible for CMIP, and we thank the climate modeling groups for producing and making their model output available. The work was financed through research grants from the Swedish Research Council for the Environment, Agricultural Sciences and Spatial Planning (FORMAS). Furthermore, we thank the Norwegian Space Center for funding NILU received for the SatMonAir project (NSC nr: JOP.12.12.2), as well as the funding MET Norway received through the PM-VRAE project. T. Iversen, A. Kirkevag, and O. Seland were supported by the Research Council of Norway through the EarthClim (207711/E10) and NOTUR/NorStore projects, and through the EU projects PEGASOS and ACCESS. We thank the CRAICC project for their work on initiating cooperation on Nordic Arctic climate modeling and measurements. The authors are very thankful for the use of in situ aerosol data that are measured by the Department of Applied Environmental Science (ITM) at Stockholm University. The authors would like to thank Ulla Wideqvist at ITM for useful suggestions. Finally, we also want to thank three anonymous reviewers for their valuable comments. NR 98 TC 2 Z9 2 U1 3 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 16 PY 2014 VL 119 IS 13 AR 2013JD021279 DI 10.1002/2013JD021279 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN2IK UT WOS:000340408000024 ER PT J AU Manzini, E Karpechko, AY Anstey, J Baldwin, MP Black, RX Cagnazzo, C Calvo, N Charlton-Perez, A Christiansen, B Davini, P Gerber, E Giorgetta, M Gray, L Hardiman, SC Lee, YY Marsh, DR McDaniel, BA Purich, A Scaife, AA Shindell, D Son, SW Watanabe, S Zappa, G AF Manzini, E. Karpechko, A. Yu. Anstey, J. Baldwin, M. P. Black, R. X. Cagnazzo, C. Calvo, N. Charlton-Perez, A. Christiansen, B. Davini, Paolo Gerber, E. Giorgetta, M. Gray, L. Hardiman, S. C. Lee, Y-Y Marsh, D. R. McDaniel, B. A. Purich, A. Scaife, A. A. Shindell, D. Son, S-W Watanabe, S. Zappa, G. TI Northern winter climate change: Assessment of uncertainty in CMIP5 projections related to stratosphere-troposphere coupling SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ET-AL. 2011; CIRCULATION RESPONSE; TEMPERATURE RESPONSE; WEATHER REGIMES; OZONE RECOVERY; WAVE DRAG; PART I; VARIABILITY; ATLANTIC; MODELS AB Future changes in the stratospheric circulation could have an important impact on northern winter tropospheric climate change, given that sea level pressure (SLP) responds not only to tropospheric circulation variations but also to vertically coherent variations in troposphere-stratosphere circulation. Here we assess northern winter stratospheric change and its potential to influence surface climate change in the Coupled Model Intercomparison Project-Phase 5 (CMIP5) multimodel ensemble. In the stratosphere at high latitudes, an easterly change in zonally averaged zonal wind is found for the majority of the CMIP5 models, under the Representative Concentration Pathway 8.5 scenario. Comparable results are also found in the 1% CO2 increase per year projections, indicating that the stratospheric easterly change is common feature in future climate projections. This stratospheric wind change, however, shows a significant spread among the models. By using linear regression, we quantify the impact of tropical upper troposphere warming, polar amplification, and the stratospheric wind change on SLP. We find that the intermodel spread in stratospheric wind change contributes substantially to the intermodel spread in Arctic SLP change. The role of the stratosphere in determining part of the spread in SLP change is supported by the fact that the SLP change lags the stratospheric zonally averaged wind change. Taken together, these findings provide further support for the importance of simulating the coupling between the stratosphere and the troposphere, to narrow the uncertainty in the future projection of tropospheric circulation changes. C1 [Manzini, E.; Giorgetta, M.] Max Planck Inst Meteorol, D-20146 Hamburg, Germany. [Karpechko, A. Yu.] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. [Anstey, J.; Gray, L.] Univ Oxford, Dept Phys, Oxford, England. [Baldwin, M. P.] Univ Exeter, Coll Engn Math & Phys Sci, Exeter, Devon, England. [Black, R. X.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Cagnazzo, C.] CNR, Ist Sci Atmosfera & Clima, Rome, Italy. [Calvo, N.] Univ Complutense Madrid, Dept Fis Tierra 2, Madrid, Spain. [Charlton-Perez, A.] Univ Reading, Dept Meteorol, Reading, Berks, England. [Christiansen, B.] Danish Meteorol Inst, Copenhagen, Denmark. [Davini, Paolo] CNR, Ist Sci Atmosfera & Clima, Turin, Italy. [Gerber, E.] NYU, Courant Inst Math Sci, New York, NY USA. [Hardiman, S. C.; Scaife, A. A.] Met Off Hadley Ctr, Exeter, Devon, England. [Lee, Y-Y] Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA. [Marsh, D. R.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [McDaniel, B. A.] Kennesaw State Univ, Dept Biol & Phys, Kennesaw, GA USA. [Purich, A.] CSIRO Marine & Atmospher Res, Aspendale, Vic, Australia. [Shindell, D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Son, S-W] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea. [Watanabe, S.] Japan Agcy Marine Earth Sci & Technol, Yokohama, Kanagawa, Japan. [Zappa, G.] Univ Reading, Natl Ctr Atmospher Sci, Reading, Berks, England. RP Manzini, E (reprint author), Max Planck Inst Meteorol, Bundesstr 55, D-20146 Hamburg, Germany. EM elisa.manzini@mpimet.mpg.de RI Marsh, Daniel/A-8406-2008; Cagnazzo, Chiara/C-7194-2015; Son, Seok-Woo /A-8797-2013; Shindell, Drew/D-4636-2012; Black, Robert/L-8522-2014; Watanabe, Shingo/L-9689-2014; OI Marsh, Daniel/0000-0001-6699-494X; Watanabe, Shingo/0000-0002-2228-0088; CALVO FERNANDEZ, NATALIA/0000-0001-6213-1864; cagnazzo, chiara/0000-0002-2054-0448; Christiansen, Bo/0000-0003-2792-4724; Charlton-Perez, Andrew/0000-0001-8179-6220 FU EC COMBINE [GA 226520]; Academy of Finland [259537]; Joint DECC/Defra Met Office Hadley Centre Climate Programme [GA01101]; NSF under the U.S. CLIVAR program; Office of Polar Programs; Office of Science (BER) of the U.S. Department of Energy; National Science Foundation [ARC-1107384]; UK Natural Environment Research Council (NERC); National Centre for Atmospheric Science (NCAS); Korea Meteorological Administration Research and Development Program [CATER 2012-3065]; U.S. NSF [AGS-1264195]; National Science Foundation; Spanish Ministry of Science and Innovation (MCINN) through the MATRES [CGL2012-34221]; NERC under the TEMPEST project 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 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. We are grateful to Thomas Birner and Lorenzo Polvani for providing comments to an earlier version of the manuscript. Evgeny Volodin, John Wilson, and Seiji Yukimoto are kindly acknowledged to have provided the residual vertical velocity diagnostic. We thank Judith Perlwitz, John Scinocca, Michael Sigmond, Hauke Schmidt, and the anonymous reviewers for their constructive reviews and suggestions. E. M. and S. C. H. were partially supported by the EC COMBINE project (GA 226520). A.Y.K. was funded by the Academy of Finland, grant 259537. A. A. S. and S. C. H. were supported by the Joint DECC/Defra Met Office Hadley Centre Climate Programme (GA01101). M. P. B. was funded by NSF under the U.S. CLIVAR program and the Office of Polar Programs. The research efforts of R. X. B., B. A. M., and Y.-Y.L. were supported by the Office of Science (BER) of the U.S. Department of Energy and by the National Science Foundation grant, ARC-1107384. J.A. and L.J.G. were funded by the UK Natural Environment Research Council (NERC) and National Centre for Atmospheric Science (NCAS). S. W. S. was funded by the Korea Meteorological Administration Research and Development Program under grant CATER 2012-3065. E. P. G. was supported by the U.S. NSF, grant AGS-1264195. NCAR is sponsored by the National Science Foundation. N.C. was supported by the Spanish Ministry of Science and Innovation (MCINN) through the MATRES (CGL2012-34221). G.Z. was funded by NERC under the TEMPEST project. NR 49 TC 29 Z9 29 U1 2 U2 42 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 16 PY 2014 VL 119 IS 13 AR 2013JD021403 DI 10.1002/2013JD021403 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN2IK UT WOS:000340408000013 ER PT J AU Matsui, T Santanello, J Shi, JJ Tao, WK Wu, D Peters-Lidard, C Kemp, E Chin, M Starr, D Sekiguchi, M Aires, F AF Matsui, T. Santanello, J. Shi, J. J. Tao, W-K. Wu, D. Peters-Lidard, C. Kemp, E. Chin, M. Starr, D. Sekiguchi, M. Aires, F. TI Introducing multisensor satellite radiance-based evaluation for regional Earth System modeling SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID LAND-SURFACE-TEMPERATURE; SINGLE-SCATTERING PROPERTIES; CLOUD MICROPHYSICS PARAMETERIZATION; NONSPHERICAL ICE PARTICLES; AEROSOL OPTICAL-PROPERTIES; DATA ASSIMILATION SYSTEM; SPLIT-WINDOW ALGORITHM; M GOES-12 IMAGERY; PASSIVE-MICROWAVE; MULTIPLE-SCATTERING AB Earth System modeling has become more complex, and its evaluation using satellite data has also become more difficult due to model and data diversity. Therefore, the fundamental methodology of using satellite direct measurements with instrumental simulators should be addressed especially for modeling community members lacking a solid background of radiative transfer and scattering theory. This manuscript introduces principles of multisatellite, multisensor radiance-based evaluation methods for a fully coupled regional Earth System model: NASA-Unified Weather Research and Forecasting (NU-WRF) model. We use a NU-WRF case study simulation over West Africa as an example of evaluating aerosol-cloud-precipitation-land processes with various satellite observations. NU-WRF-simulated geophysical parameters are converted to the satellite-observable raw radiance and backscatter under nearly consistent physics assumptions via the multisensor satellite simulator, the Goddard Satellite Data Simulator Unit. We present varied examples of simple yet robust methods that characterize forecast errors and model physics biases through the spatial and statistical interpretation of various satellite raw signals: infrared brightness temperature (Tb) for surface skin temperature and cloud top temperature, microwave Tb for precipitation ice and surface flooding, and radar and lidar backscatter for aerosol-cloud profiling simultaneously. Because raw satellite signals integrate many sources of geophysical information, we demonstrate user-defined thresholds and a simple statistical process to facilitate evaluations, including the infrared-microwave-based cloud types and lidar/radar-based profile classifications. C1 [Matsui, T.; Santanello, J.; Shi, J. J.; Tao, W-K.; Wu, D.; Peters-Lidard, C.; Kemp, E.; Chin, M.; Starr, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Matsui, T.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Shi, J. J.] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21239 USA. [Wu, D.; Kemp, E.] Sci Syst & Applicat Inc, Lanham, MD USA. [Sekiguchi, M.] Tokyo Univ Marine Sci & Technol, Fac Marine Technol, Tokyo, Japan. [Aires, F.] Estellus, Paris, France. RP Matsui, T (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Toshihisa.Matsui-1@nasa.gov RI Peters-Lidard, Christa/E-1429-2012; Measurement, Global/C-4698-2015; Chin, Mian/J-8354-2012; Santanello, Joseph/D-4438-2012 OI Peters-Lidard, Christa/0000-0003-1255-2876; Santanello, Joseph/0000-0002-0807-6590 FU NASA Modeling and Analysis Prediction (MAP) program FX The work has been supported under NASA Modeling and Analysis Prediction (MAP) program (D. Considine at NASA HQ). is also made to T. Lee at NASA HQ, the NASA Goddard Space Flight Center, and the NASA Ames Research Center for computer resources used for our calculations. Thanks to the anonymous reviewers for improving the manuscript. NR 143 TC 6 Z9 6 U1 2 U2 22 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 16 PY 2014 VL 119 IS 13 AR 2013JD021424 DI 10.1002/2013JD021424 PG 26 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN2IK UT WOS:000340408000040 ER PT J AU Oreopoulos, L Cho, N Lee, D Kato, S Huffman, GJ AF Oreopoulos, Lazaros Cho, Nayeong Lee, Dongmin Kato, Seiji Huffman, George J. TI An examination of the nature of global MODIS cloud regimes SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID TROPICAL WESTERN PACIFIC; WEATHER STATES; PRECIPITATION PRODUCTS; TEMPERATURE; SENSITIVITY; CLIMATOLOGY; ISCCP; GPCP AB We introduce global cloud regimes (previously also referred to as "weather states") derived from cloud retrievals that use measurements by the Moderate Resolution Imaging Spectroradiometer (MODIS) instrument aboard the Aqua and Terra satellites. The regimes are obtained by applying clustering analysis on joint histograms of retrieved cloud top pressure and cloud optical thickness. By employing a compositing approach on data sets from satellites and other sources, we examine regime structural and thermodynamical characteristics. We establish that the MODIS cloud regimes tend to form in distinct dynamical and thermodynamical environments and have diverse profiles of cloud fraction and water content. When compositing radiative fluxes from the Clouds and the Earth's Radiant Energy System instrument and surface precipitation from the Global Precipitation Climatology Project, we find that regimes with a radiative warming effect on the atmosphere also produce the largest implied latent heat. Taken as a whole, the results of the study corroborate the usefulness of the cloud regime concept, reaffirm the fundamental nature of the regimes as appropriate building blocks for cloud system classification, clarify their association with standard cloud types, and underscore their distinct radiative and hydrological signatures. C1 [Oreopoulos, Lazaros; Cho, Nayeong; Lee, Dongmin; Huffman, George J.] NASA GSFC, Div Earth Sci, Greenbelt, MD 20771 USA. [Cho, Nayeong] USRA, Columbia, MD USA. [Lee, Dongmin] Morgan State Univ, GESTAR, Baltimore, MD 21239 USA. [Kato, Seiji] NASA LARC, Climate Sci Branch, Hampton, VA USA. RP Oreopoulos, L (reprint author), NASA GSFC, Div Earth Sci, Greenbelt, MD 20771 USA. EM Lazaros.Oreopoulos@nasa.gov RI Oreopoulos, Lazaros/E-5868-2012; Huffman, George/F-4494-2014 OI Oreopoulos, Lazaros/0000-0001-6061-6905; Huffman, George/0000-0003-3858-8308 FU NASA's Modeling Analysis and Prediction; CloudSat/CALIPSO; Science of Terra and Aqua programs FX Funding from NASA's Modeling Analysis and Prediction, CloudSat/CALIPSO, and the Science of Terra and Aqua programs is gratefully acknowledged. We would like to thank Robert Pincus and Steven Platnick for helpful discussions on ISCCP and MODIS cloud property retrieval differences and the reviewers for constructive suggestions that helped us greatly to improve the paper. Please contact the lead author for freely obtaining the MODIS cloud regime data used in this paper. NR 34 TC 7 Z9 7 U1 1 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 16 PY 2014 VL 119 IS 13 AR 2013JD021409 DI 10.1002/2013JD021409 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN2IK UT WOS:000340408000035 ER PT J AU Tosca, MG Diner, DJ Garay, MJ Kalashnikova, OV AF Tosca, M. G. Diner, D. J. Garay, M. J. Kalashnikova, O. V. TI Observational evidence of fire-driven reduction of cloud fraction in tropical Africa SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GENERAL-CIRCULATION MODEL; GLOBAL RADIATION BUDGET; DIURNAL CYCLE; AIR-POLLUTION; ABSORBING AEROSOLS; CONVECTIVE CLOUDS; CLIMATE RESPONSE; EQUATORIAL ASIA; SATELLITE DATA; TRACE GASES AB Anthopogenic savanna fires in sub-Saharan Africa emit smoke that affects cloudiness in the region. We measured the cloud response to fire aerosols using aerosol data from the Multi-angle Imaging SpectroRadiometer (MISR) and cloud fraction data from the morning and afternoon overpasses of the Moderate Resolution Imaging Spectroradiometer (MODIS) instrument. Considering the same cloud scene from the morning and afternoon satellite observations allowed us to observe the temporal relationship between clouds and aerosols. Level 2 data from 35 individual scenes during the fire season (December) between 2006 and 2010 were analyzed to quantify changes in MODIS cloud fraction from morning (10:30 A. M. local time) to afternoon (1:30 P. M. local time) in the presence of different morning aerosol burdens (from MISR). We controlled for the local meteorology by analyzing scenes from November, when fire activity and aerosol optical depth were low but cloud fraction and meteorological variables (boundary layer height, pressure, total column water vapor, temperature, and convective available potential energy) were similar to those of the fire season. High-fire-driven aerosol optical depth (AOD) was associated with reduced cloud fraction in both the raw and meteorologically normalized data. Fire aerosols reduced the relative cloud fraction in all sky conditions, but the effects were progressively larger in high-AOD conditions. These results may provide observational evidence of the semidirect cloud decimation effect in tropical regions and suggest a positive feedback loop between anthropogenic burning and cloudiness-where more aerosols lead to decreased clouds, increased surface exposure and drying, more fire, and thus more aerosols-which is consistent with previous studies linking smoke aerosols to reduced cloudiness and vice versa. C1 [Tosca, M. G.; Diner, D. J.; Garay, M. J.; Kalashnikova, O. V.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Tosca, MG (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM michael.g.tosca@jpl.nasa.gov RI Tosca, Michael/J-4908-2015 OI Tosca, Michael/0000-0003-1301-8341 FU National Aeronautics and Space Administration FX This work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We thank the MISR team for providing facilities and useful discussions. The MISR data were obtained from the NASA Langley Research Center Atmospheric Science Data Center (http://l0dup05.larc.nasa.gov/MISR/cgi-bin/MISR/main.cgi). The MODIS data were obtained from the Level 1 and Atmosphere Archive and Distribution System (http://modis.gsfc.nasa.gov/data/). NR 73 TC 9 Z9 9 U1 1 U2 19 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 16 PY 2014 VL 119 IS 13 DI 10.1002/2014JD021759 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN2IK UT WOS:000340408000038 ER PT J AU Zoghzoghy, FG Cohen, MB Said, RK Basilico, SS Blakeslee, RJ Inan, US AF Zoghzoghy, F. G. Cohen, M. B. Said, R. K. Basilico, S. S. Blakeslee, R. J. Inan, U. S. TI Lightning activity following the return stroke SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MULTIPLE GROUND CONTACTS; HIGH-SPEED VIDEO; ELECTRIC-FIELD; INTERFEROMETRIC OBSERVATIONS; CLOUD; FLASHES; THUNDERSTORMS; DISCHARGES; PULSES; SPACE AB Natural lightning is both frequent and variable and thus a good subject for statistical studies. A typical negative cloud-to-ground (CG) flash consists of multiple individual return strokes. The spatial and temporal distributions of various lightning events throughout the discharge provide a surrogate look inside the CG flash and offer insight into the underlying physical processes. In this study, we combine 8 years of National Lightning Detection Network (TM) (NLDN) and North Alabama Lightning Mapping Array (NALMA) data to compute the spatial and temporal distributions of (i) subsequent NLDN-reported return strokes and (ii) LMA-reported sources around NLDN-reported CG strokes. Subsequent strokes are separated into those with the same contact point as the first stroke and those flowing along new lightning channels. Statistically, the distribution of strokes along new channels evolves deterministically, with similar to 200 km/s propagation speed from the original channel, comparable to the speed of a stepped leader. This suggests that the -CG subsequent strokes forming new channels may be directly linked to the initial one by a propagating leader inside the cloud. We present LMA case studies and a multiyear analysis of NLDN-LMA data that support this behavior. Our results are supported by ground-truth measurements and video recordings from previous field studies. C1 [Zoghzoghy, F. G.; Basilico, S. S.; Inan, U. S.] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA. [Cohen, M. B.] Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. [Said, R. K.] Vaisala Inc, Boulder, CO USA. [Blakeslee, R. J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Inan, U. S.] Koc Univ, Dept Elect Engn, Istanbul, Turkey. RP Zoghzoghy, FG (reprint author), Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA. EM fadiz@stanford.edu OI Cohen, Morris/0000-0002-7920-5759 FU Defense Advanced Research Project Agency [HR0011-10-1-0058-P00001] FX This work is supported by the Defense Advanced Research Project Agency under grant HR0011-10-1-0058-P00001 to Stanford University with subcontract to the Georgia Institute of Technology. NLDN data are provided by Vaisala, Inc. (Ron Holle ron.holle@vaisala.com). The point of contact for NALMA data is Richard Blakeslee (rich.blakeslee@nasa.gov). NR 39 TC 0 Z9 0 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUL 16 PY 2014 VL 119 IS 13 DI 10.1002/2014JD021738 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN2IK UT WOS:000340408000033 ER PT J AU Keller, LP Berger, EL AF Keller, Lindsay P. Berger, Eve L. TI A transmission electron microscope study of Itokawa regolith grains SO EARTH PLANETS AND SPACE LA English DT Article DE Hayabusa; Itokawa; Space weathering; Irradiation; Micrometeorite impact; Solar flare tracks; Transmission electron microscopy ID ASTEROID SURFACES; ORIGIN AB Analyses of two olivine-rich particles from asteroid 25143 Itokawa returned by the Hayabusa mission (RA-QD02-0125 and RA-QD02-0211) show evidence for space weathering processes that occurred in the Itokawa regolith. Submicrometer impact-derived crystalline and glassy grains are observed adhering to the surfaces of the particles, including albite, orthopyroxene, olivine, augite, pyrrhotite, troilite, melt splashes, and melt spherules. Both particles are surrounded by 50- to 100-nm-thick disordered rims that are nanocrystalline, not amorphous, and compositionally similar to the grain cores. A pyrrhotite grain attached to RA-QD02-0125 also shows a disordered rim that is sulfur-depleted with nanophase Fe metal grains decorating the outermost surface. The structurally disordered rims on the Hayabusa particles likely result from atomic displacement damage from solar wind ions given the similarity of the rim thickness compared to the implantation depth of solar wind ions. The outermost few nanometers of the disordered rims are more Si-rich and Mg-and Fe-depleted relative to the cores of the grains and likely represent a minor accumulation of impact-generated vapors or sputter deposits. Nanophase Fe metal particles are present in the rim on RA-QD02-0211 but were not detected in the rim on RA-QD02-0125. Solar flare particle tracks are observed in RA-QD02-0211 but were not observed in RA-QD02-0125, suggesting short surface exposure times for the particles, on the order of approximately 103 to 104 years. This result implies that the optical effects of space weathering develop far more rapidly than was previously recognized. C1 [Keller, Lindsay P.] NASA, Lyndon B Johnson Space Ctr, Robert M Walker Lab Space Sci, Houston, TX 77058 USA. [Berger, Eve L.] NASA, Lyndon B Johnson Space Ctr, Jacobs JETS contract, GeoControl Syst Inc, Houston, TX 77058 USA. RP Keller, LP (reprint author), NASA, Lyndon B Johnson Space Ctr, Robert M Walker Lab Space Sci, Houston, TX 77058 USA. EM Lindsay.P.Keller@nasa.gov FU NASA Laboratory Analysis of Returned Samples (LARS) program FX This research was supported by a grant to LPK from the NASA Laboratory Analysis of Returned Samples (LARS) program. We gratefully acknowledge the samples allocated for this study from JAXA and the Hayabusa Curation Facility. NR 20 TC 9 Z9 9 U1 1 U2 10 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1880-5981 J9 EARTH PLANETS SPACE JI Earth Planets Space PD JUL 15 PY 2014 VL 66 AR 71 DI 10.1186/1880-5981-66-71 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AM4RJ UT WOS:000339842700002 ER PT J AU Keller, JM Balazs, GH Nilsen, F Rice, M Work, TM Jensen, BA AF Keller, Jennifer M. Balazs, George H. Nilsen, Frances Rice, Marc Work, Thierry M. Jensen, Brenda A. TI Investigating the Potential Role of Persistent Organic Pollutants in Hawaiian Green Sea Turtle Fibropapillomatosis SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID HUMAN BLOOD-PLASMA; CHELONIA-MYDAS; POLYCHLORINATED-BIPHENYLS; FLAME RETARDANTS; CARETTA-CARETTA; PCB METABOLITES; SPATIAL TRENDS; UNITED-STATES; WHOLE-BLOOD; ISLANDS AB It has been hypothesized for decades that environmental pollutants may contribute to green sea turtle fibropapillomatosis (FP), possibly through immunosuppression leading to greater susceptibility to the herpesvirus, the putative causative agent of this tumor-forming disease. To address this question, we measured concentrations of 164 persistent organic pollutants (POPs) and halogenated phenols in 53 Hawaiian green turtle (Chelonia mydas) plasma samples archived by the Biological and Environmental Monitoring and Archival of Sea Turtle Tissues (BEMAST) project at the National Institute of Standards and Technology Marine Environmental Specimen Bank. Four groups of turtles were examined: free-ranging turtles from Kiholo Bay (0% FP, Hawaii), Kailua Bay (low FP, 8%, Oahu), and Kapoho Bay (moderate FP, 38%, Hawaii) and severely tumored stranded turtles that required euthanasia (high FP, 100%, Main Hawaiian Islands). Four classes of POPs and seven halogenated phenols were detected in at least one of the turtles, and concentrations were low (often <200 pg/g wet mass). The presence of halogenated phenols in sea turtles is a novel discovery; their concentrations were higher than most man-made POPs, suggesting that the source of most of these compounds was likely natural (produced by the algal turtle diet) rather than metabolites of man-made POPs. None of the compounds measured increased in concentration with increasing prevalence of FP across the four groups of turtles, suggesting that these 164 compounds are not likely primary triggers for the onset of FP. However, the stranded, severely tumored, emaciated turtle group (n = 14) had the highest concentrations of POPs, which might suggest that mobilization of contaminants with lipids into the blood during late-stage weight loss could contribute to the progression of the disease. Taken together, these data suggest that POPs are not a major cofactor in causing the onset of FP. C1 [Keller, Jennifer M.; Nilsen, Frances] NIST, Div Chem Sci, Hollings Marine Lab, Charleston, SC 29412 USA. [Balazs, George H.] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96818 USA. [Nilsen, Frances; Jensen, Brenda A.] Hawaii Pacific Univ, Coll Nat & Computat Sci, Kaneohe, HI 96744 USA. [Rice, Marc] Hawaii Preparatory Acad, Sea Turtle Res Program, Kamuela, HI 96743 USA. [Work, Thierry M.] US Geol Survey, Natl Wildlife Hlth Ctr, Honolulu Field Stn, Honolulu, HI 96850 USA. RP Keller, JM (reprint author), NIST, Div Chem Sci, Hollings Marine Lab, Charleston, SC 29412 USA. EM jennifer.keller@noaa.gov RI Work, Thierry/F-1550-2015 OI Work, Thierry/0000-0002-4426-9090 NR 61 TC 10 Z9 11 U1 5 U2 60 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X EI 1520-5851 J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD JUL 15 PY 2014 VL 48 IS 14 BP 7807 EP 7816 DI 10.1021/es5014054 PG 10 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA AL6FH UT WOS:000339227500018 PM 24963745 ER PT J AU Kim, D Xavier, P Maloney, E Wheeler, M Waliser, D Sperber, K Hendon, H Zhang, CD Neale, R Hwang, YT Liu, HB AF Kim, Daehyun Xavier, Prince Maloney, Eric Wheeler, Matthew Waliser, Duane Sperber, Kenneth Hendon, Harry Zhang, Chidong Neale, Richard Hwang, Yen-Ting Liu, Haibo TI Process-Oriented MJO Simulation Diagnostic: Moisture Sensitivity of Simulated Convection SO JOURNAL OF CLIMATE LA English DT Article ID MADDEN-JULIAN OSCILLATION; TROPICAL INTRASEASONAL VARIABILITY; GENERAL-CIRCULATION MODELS; COUPLED EQUATORIAL WAVES; LARGE-SCALE MODELS; CUMULUS PARAMETERIZATION; CLIMATE MODELS; AGCM SIMULATIONS; ARAKAWA-SCHUBERT; CLOUD ENSEMBLE AB Process-oriented diagnostics for Madden-Julian oscillation (MJO) simulations are being developed to facilitate improvements in the representation of the MJO in weather and climate models. These process-oriented diagnostics are intended to provide insights into how parameterizations of physical processes in climate models should be improved for a better MJO simulation. This paper proposes one such process-oriented diagnostic, which is designed to represent sensitivity of simulated convection to environmental moisture: composites of a relative humidity (RH) profile based on precipitation percentiles. The ability of the RH composite diagnostic to represent the diversity of MJO simulation skill is demonstrated using a group of climate model simulations participating in phases 3 and 5 of the Coupled Model Intercomparison Project (CMIP3 and CMIP5). A set of scalar process metrics that captures the key physical attributes of the RH diagnostic is derived and their statistical relationship with indices that quantify the fidelity of the MJO simulation is tested. It is found that a process metric that represents the amount of lower-tropospheric humidity increase required for a transition from weak to strong rain regimes has a robust statistical relationship with MJO simulation skill. The results herein suggest that moisture sensitivity of convection is closely related to a GCM's ability to simulate the MJO. C1 [Kim, Daehyun; Liu, Haibo] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Xavier, Prince] Met Off Hadley Ctr, Exeter, Devon, England. [Maloney, Eric] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Wheeler, Matthew; Hendon, Harry] Ctr Australian Weather & Climate Res, Melbourne, Vic, Australia. [Waliser, Duane] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Sperber, Kenneth] Lawrence Livermore Natl Lab, PCMDI, Livermore, CA USA. [Zhang, Chidong] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. [Neale, Richard] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Hwang, Yen-Ting] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA. RP Kim, D (reprint author), Columbia Univ, Lamont Doherty Earth Observ, 61 Route 9W, Palisades, NY 10964 USA. EM dkim@ldeo.columbia.edu RI Hwang, Yen-Ting/P-8469-2014; Maloney, Eric/A-9327-2008; Sperber, Kenneth/H-2333-2012 OI Hwang, Yen-Ting/0000-0002-4084-1408; Maloney, Eric/0000-0002-2660-2611; FU NASA [NNX13AM18G, NNX13AQ50G]; Korea Meteorological Administration Research and Development Program [CATER 2013-3142]; Climate and Large-Scale Dynamics Program of the National Science Foundation [ATM-0832868, AGS-1025584]; Science and Technology Center for Multi-Scale Modeling of Atmospheric Processes [ATM-0425247]; National Oceanic and Atmospheric Administration [NA08OAR4320893, NA12OAR4310077]; U.S. Department of Commerce FX We thank anonymous reviewers for their constructive comments. DK is supported by NASA Grant NNX13AM18G and the Korea Meteorological Administration Research and Development Program under Grant CATER 2013-3142. EDM is supported by Climate and Large-Scale Dynamics Program of the National Science Foundation under Grants ATM-0832868 and AGS-1025584 and the Science and Technology Center for Multi-Scale Modeling of Atmospheric Processes, managed by Colorado State University, under Cooperative Agreement ATM-0425247. EDM is also supported by Award NA08OAR4320893 and NA12OAR4310077 from the National Oceanic and Atmospheric Administration, U.S. Department of Commerce, and NASA Grant NNX13AQ50G. The ERA-Interim data used in this study have been provided by the ECMWF data server. NR 76 TC 21 Z9 21 U1 0 U2 13 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 JUL 15 PY 2014 VL 27 IS 14 BP 5379 EP 5395 DI 10.1175/JCLI-D-13-00497.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AL4WJ UT WOS:000339135200010 ER PT J AU Jiang, XA Kubar, TL Wong, S Olson, WS Waliser, DE AF Jiang, Xianan Kubar, Terence L. Wong, Sun Olson, William S. Waliser, Duane E. TI Modulation of Marine Low Clouds Associated with the Tropical Intraseasonal Variability over the Eastern Pacific SO JOURNAL OF CLIMATE LA English DT Article ID MADDEN-JULIAN OSCILLATION; EARTHS RADIATION BUDGET; SEA-SURFACE TEMPERATURE; NORTH PACIFIC; BOREAL SUMMER; BOUNDARY-LAYER; CIRCULATION ANOMALIES; RADAR OBSERVATIONS; ERA-INTERIM; SATELLITE AB Owing to its profound influences on global energy balance, accurate representation of low cloud variability in climate models is an urgent need for future climate projection. In the present study, marine low cloud variability on intraseasonal time scales is characterized, with a particular focus over the Pacific basin during boreal summer and its association with the dominant mode of tropical intraseasonal variability (TISV) over the eastern Pacific (EPAC) intertropical convergence zone (ITCZ). Analyses indicate that, when anomalous TISV convection is enhanced over the elongated EPAC ITCZ, reduction of low cloud fraction (LCF) is evident over a vast area of the central North Pacific. Subsequently, when the enhanced TISV convection migrates to the northern part of the EPAC warm pool, a "comma shaped" pattern of reduced LCF prevails over the subtropical North Pacific, along with a pronounced reduction of LCF present over the southeast Pacific (SEPAC). Further analyses indicate that surface latent heat fluxes and boundary heights induced by anomalous low-level circulation through temperature advection and changes of total wind speed, as well as midlevel vertical velocity associated with the EPAC TISV, could be the most prominent factors in regulating the intraseasonal variability of LCF over the North Pacific. For the SEPAC, temperature anomalies at the top of the boundary inversion layer between 850 and 800 hPa play a critical role in the local LCF intraseasonal variations. Results presented in this study provide not only improved understanding of variability of marine low clouds and the underlying physics, but also a prominent benchmark in constraining and evaluating the representation of low clouds in climate models. C1 [Jiang, Xianan] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. [Jiang, Xianan; Kubar, Terence L.; Wong, Sun; Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kubar, Terence L.] Colorado State Univ, Ft Collins, CO 80523 USA. [Olson, William S.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. RP Jiang, XA (reprint author), CALTECH, Jet Prop Lab, MS 233-300,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM xianan@jifresse.ucla.edu FU NOAA MAPP Program [NA12OAR4310075]; NSF Climate and Large-Scale Dynamics Program [AGS-1228302]; NASA NEWS Program [NNX13AC40G]; National Aeronautics and Space Administration FX We thank the anonymous reviewers for their insightful comments on an earlier version of this manuscript. X.J. acknowledges support by the NOAA MAPP Program under Awards NA12OAR4310075, and the NSF Climate and Large-Scale Dynamics Program under Award AGS-1228302. W.O. and X.J. acknowledge support from the NASA NEWS Program under Award NNX13AC40G. 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. ISCCP surface heat flux data were provided by the WHOI OAFlux project (http://oaflux.whoi.edu). NR 52 TC 0 Z9 0 U1 4 U2 13 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 JUL 15 PY 2014 VL 27 IS 14 BP 5560 EP 5574 DI 10.1175/JCLI-D-13-00569.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AL4WJ UT WOS:000339135200021 ER PT J AU Koster, RD Walker, GK Collatz, GJ Thornton, PE AF Koster, R. D. Walker, G. K. Collatz, G. J. Thornton, P. E. TI Hydroclimatic Controls on the Means and Variability of Vegetation Phenology and Carbon Uptake SO JOURNAL OF CLIMATE LA English DT Article ID GENERAL-CIRCULATION MODEL; LAND-SURFACE; NORMALIZED DIFFERENCE; NDVI DATA; CLIMATE; ATMOSPHERE; WATER; BIOSPHERE; DATASET; SYSTEM AB Long-term, global offline (land only) simulations with a dynamic vegetation phenology model are used to examine the control of hydroclimate over vegetation-related quantities. First, with a control simulation, the model is shown to capture successfully (though with some bias) key observed relationships between hydroclimate and the spatial and temporal variations of phenological expression. In subsequent simulations, the model shows that (i) the global spatial variation of seasonal phenological maxima is controlled mostly by hydroclimate, irrespective of distributions in vegetation type; (ii) the occurrence of high interannual moisture-related phenological variability in grassland areas is determined by hydroclimate rather than by the specific properties of grassland; and (iii) hydroclimatic means and variability have a corresponding impact on the spatial and temporal distributions of gross primary productivity (GPP). C1 [Koster, R. D.; Walker, G. K.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Walker, G. K.] Sci Syst & Applicat Inc, Lanham, MD USA. [Collatz, G. J.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Thornton, P. E.] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. [Thornton, P. E.] Oak Ridge Natl Lab, Climate Change Sci Inst, Oak Ridge, TN 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; collatz, george/D-5381-2012; Thornton, Peter/B-9145-2012 OI Koster, Randal/0000-0001-6418-6383; Thornton, Peter/0000-0002-4759-5158 FU NASA Modeling, Analysis, and Prediction Program FX This research was supported by the NASA Modeling, Analysis, and Prediction Program. NR 46 TC 4 Z9 4 U1 0 U2 23 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 JUL 15 PY 2014 VL 27 IS 14 BP 5632 EP 5652 DI 10.1175/JCLI-D-13-00477.1 PG 21 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AL4WJ UT WOS:000339135200026 ER PT J AU Sejas, SA Cai, M Hu, AX Meehl, GA Washington, W Taylor, PC AF Sejas, Sergio A. Cai, Ming Hu, Aixue Meehl, Gerald A. Washington, Warren Taylor, Patrick C. TI Individual Feedback Contributions to the Seasonality of Surface Warming SO JOURNAL OF CLIMATE LA English DT Article ID GENERAL-CIRCULATION MODEL; GREENHOUSE-PLUS FEEDBACK; CLIMATE FEEDBACKS; SEA-ICE; POLAR AMPLIFICATION; ARCTIC TEMPERATURE; RADIATIVE-TRANSFER; CO2 CONCENTRATION; COUPLED MODELS; PART II AB Using the climate feedback response analysis method, the authors examine the individual contributions of the CO2 radiative forcing and climate feedbacks to the magnitude, spatial pattern, and seasonality of the transient surface warming response in a 1% yr(-1) CO2 increase simulation of the NCAR Community Climate System Model, version 4 (CCSM4). The CO2 forcing and water vapor feedback warm the surface everywhere throughout the year. The tropical warming is predominantly caused by the CO2 forcing and water vapor feedback, while the evaporation feedback reduces the warming. Most feedbacks exhibit noticeable seasonal variations; however, their net effect has little seasonal variation due to compensating effects, which keeps the tropical warming relatively invariant all year long. The polar warming has a pronounced seasonal cycle, with maximum warming in fall/winter and minimum warming in summer. In summer, the large cancelations between the shortwave and longwave cloud feedbacks and between the surface albedo feedback warming and the cooling from the ocean heat storage/dynamics feedback lead to a warming minimum. In polar winter, surface albedo and shortwave cloud feedbacks are nearly absent due to a lack of insolation. However, the ocean heat storage feedback relays the polar warming due to the surface albedo feedback from summer to winter, and the longwave cloud feedback warms the polar surface. Therefore, the seasonal variations in the cloud feedback, surface albedo feedback, and ocean heat storage/dynamics feedback, directly caused by the strong annual cycle of insolation, contribute primarily to the large seasonal variation of polar warming. Furthermore, the CO2 forcing and water vapor and atmospheric dynamics feedbacks add to the maximum polar warming in fall/winter. C1 [Sejas, Sergio A.; Cai, Ming] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA. [Hu, Aixue; Meehl, Gerald A.; Washington, Warren] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Taylor, Patrick C.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Sejas, SA (reprint author), Florida State Univ, Dept Earth Ocean & Atmospher Sci, Mail Code 4520,POB 3064520, Tallahassee, FL 32306 USA. EM sas07t@my.fsu.edu RI Hu, Aixue/E-1063-2013; Taylor, Patrick/D-8696-2015 OI Hu, Aixue/0000-0002-1337-287X; Taylor, Patrick/0000-0002-8098-8447 FU National Science Foundation [ATM-0833001]; DOE Office of Science Regional and Global Climate Modeling (RGCM) program [DE-SC0004974]; NOAA CPO/CPPA program [NA10OAR4310168]; NASA Living With a Star Program [NNX13AF91G]; Office of Science (BER), U.S. Department of Energy [DE-FC02-97ER62402]; National Science Foundation FX The authors are grateful for the insightful and constructive comments from the anonymous reviewers. This research was in part supported by research grants from the National Science Foundation (ATM-0833001), the DOE Office of Science Regional and Global Climate Modeling (RGCM) program (DE-SC0004974), the NOAA CPO/CPPA program (NA10OAR4310168), and the NASA Living With a Star Program (NNX13AF91G). Portions of this study were supported by the Office of Science (BER), U.S. Department of Energy, Cooperative Agreement DE-FC02-97ER62402, and the National Science Foundation. NR 42 TC 12 Z9 12 U1 1 U2 20 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD JUL 15 PY 2014 VL 27 IS 14 BP 5653 EP 5669 DI 10.1175/JCLI-D-13-00658.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AL4WJ UT WOS:000339135200027 ER PT J AU Gardner, JPA Bartz, RJ Brainard, RE Cohen, JD Dunbar, RB Garton, DW Powell, S AF Gardner, Jonathan P. A. Bartz, R. John Brainard, Russell E. Cohen, John D. Dunbar, Robert B. Garton, David W. Powell, Sam TI Conservation management options and actions: Putative decline of coral cover at Palmyra Atoll, Northern Line Islands, as a case study SO MARINE POLLUTION BULLETIN LA English DT Article DE Palmyra Atoll; Temperature; Sediment; Turbidity; Coral decline; Management options and actions ID CENTRAL PACIFIC-OCEAN; CLIMATE-CHANGE; STRESS-RESPONSE; PHOENIX ISLANDS; REEFS; IMPACTS; MUSSELS AB Localised loss of live coral cover at Palmyra Atoll (central Pacific Ocean) has been attributed to increased temperature and/or sedimentation arising from alterations made to the lagoon system. It has been hypothesised that a causeway spanning the lagoon hinders water circulation, resulting in warmer and/or more turbid water flowing towards a site of high coral cover and diversity (Coral Gardens). Analyses of a multi-site and multi-year data set revealed no differences in mean temperature or turbidity values on either side of the causeway and provided no evidence of significantly warmer or more turbid water at Coral Gardens. We conclude that the putative decline in live coral cover cannot be attributed to the presence of the causeway and that proposed management actions involving modification to the causeway cannot achieve the conservation outcomes suggested of them. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Gardner, Jonathan P. A.; Cohen, John D.; Powell, Sam] Victoria Univ Wellington, Ctr Marine Environm & Econ Res, Wellington 6140, New Zealand. [Bartz, R. John; Dunbar, Robert B.] Stanford Univ, Dept Environm Earth Syst Sci, Stanford, CA 94305 USA. [Brainard, Russell E.] NOAA, Coral Reef Ecosyst Div, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI USA. [Garton, David W.] Georgia Inst Technol, Sch Biol, Atlanta, GA 30332 USA. RP Gardner, JPA (reprint author), Victoria Univ Wellington, Ctr Marine Environm & Econ Res, POB 600, Wellington 6140, New Zealand. EM jonathan.gardner@vuw.ac.nz RI Gardner, Jonathan/M-3224-2016 NR 28 TC 1 Z9 1 U1 3 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0025-326X EI 1879-3363 J9 MAR POLLUT BULL JI Mar. Pollut. Bull. PD JUL 15 PY 2014 VL 84 IS 1-2 BP 182 EP 190 DI 10.1016/j.marpolbul.2014.05.013 PG 9 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA AL0GF UT WOS:000338804700034 PM 24889316 ER PT J AU Seubert, CR Stiles, LA Schaub, H AF Seubert, Carl R. Stiles, Laura A. Schaub, Hanspeter TI Effective Coulomb force modeling for spacecraft in Earth orbit plasmas SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Coulomb formation flight; Electrostatic force modeling; Plasma effective Debye length ID CHARGE CONTROL; 2-CRAFT AB Coulomb formation flight is a concept that utilizes electrostatic forces to control the separations of close proximity spacecraft. The Coulomb force between charged bodies is a product of their size, separation, potential and interaction with the local plasma environment. A fast and accurate analytic method of capturing the interaction of a charged body in a plasma is shown. The Debye-Huckel analytic model of the electrostatic field about a charged sphere in a plasma is expanded to analytically compute the forces. This model is fitted to numerical simulations with representative geosynchronous and low Earth orbit (GEO and LEO) plasma environments using an effective Debye length. This effective Debye length, which more accurately captures the charge partial shielding, can be up to 7 times larger at GEO, and as great as 100 times larger at LEO. The force between a sphere and point charge is accurately captured with the effective Debye length, as opposed to the electron Debye length solutions that have errors exceeding 50%. One notable finding is that the effective Debye lengths in LEO plasmas about a charged body are increased from centimeters to meters. This is a promising outcome, as the reduced shielding at increased potentials provides sufficient force levels for operating the electrostatically inflated membrane structures concept at these dense plasma altitudes. (C) 2014 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Seubert, Carl R.; Stiles, Laura A.; Schaub, Hanspeter] Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA. RP Seubert, CR (reprint author), Jet Prop Lab, M-S 198-326,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM carl.seubert@colorado.edu NR 40 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 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD JUL 15 PY 2014 VL 54 IS 2 BP 209 EP 220 DI 10.1016/j.asr.2014.04.005 PG 12 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA AL0OE UT WOS:000338825400007 ER PT J AU Frick, A Mogul, R Stabekis, P Conley, CA Ehrenfreund, P AF Frick, Andreas Mogul, Rakesh Stabekis, Pericles Conley, Catharine A. Ehrenfreund, Pascale TI Overview of current capabilities and research and technology developments for planetary protection SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Planetary protection; Human space exploration; Spacecraft sterilization; Planetary protection policy ID EXTREME CONDITIONS; HYDROGEN-PEROXIDE; OUTER-SPACE; DRY HEAT; SURVIVAL; BACTERIA AB The pace of scientific exploration of our solar system provides ever-increasing insights into potentially habitable environments, and associated concerns for their contamination by Earth organisms. Biological and organic-chemical contamination has been extensively considered by the COSPAR Panel on Planetary Protection (PPP) and has resulted in the internationally recognized regulations to which spacefaring nations adhere, and which have been in place for 40 years. The only successful Mars lander missions with system-level "sterilization" were the Viking landers in the 1970s. Since then different cleanliness requirements have been applied to spacecraft based on their destination, mission type, and scientific objectives. The Planetary Protection Subcommittee of the NASA Advisory Council has noted that a strategic Research & Technology Development (R&TD) roadmap would be very beneficial to encourage the timely availability of effective tools and methodologies to implement planetary protection requirements. New research avenues in planetary protection for ambitious future exploration missions can best be served by developing an over-arching program that integrates capability-driven developments with mission-driven implementation efforts. This paper analyzes the current status concerning microbial reduction and cleaning methods, recontamination control and bio-barriers, operational analysis methods, and addresses concepts for human exploration. Crosscutting research and support activities are discussed and a rationale for a Strategic Planetary Protection R&TD Roadmap is outlined. Such a roadmap for planetary protection provides a forum for strategic planning and will help to enable the next phases of solar system exploration. Published by Elsevier Ltd. on behalf of COSPAR. C1 [Frick, Andreas; Ehrenfreund, Pascale] George Washington Univ, Inst Space Policy, Washington, DC 20052 USA. [Mogul, Rakesh] Calif State Polytech Univ Pomona, Pomona, CA 91768 USA. [Stabekis, Pericles] Genex Syst Washington Off, Washington, DC USA. [Conley, Catharine A.] NASA Headquarters, Washington, DC 20546 USA. RP Conley, CA (reprint author), NASA Headquarters, 300 E St SW, Washington, DC 20546 USA. EM cassie.conley@nasa.gov FU NASA Astrobiology Institute FX The authors would like to thank the Planetary Protection Group at NASA JPL, Patricia Beauchamp, Gerhard Kminek, Margaret Race, and John Rummel for their support, guidance, and expertise in developing this overview, as well as the anonymous reviewers for thorough editorial corrections and thoughtful insights. P. E. acknowledges support from the NASA Astrobiology Institute. NR 56 TC 6 Z9 6 U1 3 U2 17 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 EI 1879-1948 J9 ADV SPACE RES JI Adv. Space Res. PD JUL 15 PY 2014 VL 54 IS 2 BP 221 EP 240 DI 10.1016/j.asr.2014.02.016 PG 20 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA AL0OE UT WOS:000338825400008 ER PT J AU Armytage, RMG Brandon, AD Peslier, AH Lapen, TJ AF Armytage, Rosalind M. G. Brandon, Alan D. Peslier, Anne H. Lapen, Thomas J. TI Osmium isotope evidence for Early to Middle Proterozoic mantle lithosphere stabilization and concomitant production of juvenile crust in Dish Hill, CA peridotite xenoliths SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID OCEANIC UPPER-MANTLE; HIGHLY SIDEROPHILE ELEMENTS; SW TURKEY IMPLICATIONS; RIO-GRANDE RIFT; RE-OS ISOTOPES; ABYSSAL PERIDOTITES; MELT EXTRACTION; TRACE-ELEMENT; ULTRAMAFIC INCLUSIONS; LHERZOLITE XENOLITHS AB The Os-187/Os-188 compositions in peridotite samples from the sub-continental lithospheric mantle (SCLM) can be used to constrain the timing of melt extraction and potentially test the link between large-scale mantle melting and juvenile crust production. The SCLM has often experienced a complex history such that some lithophile elements such as REEs (rare earth elements) in these rocks typically record overprinting during metasomatism. New Os-187/Os-188, major and trace element compositional data were obtained on sixteen Dish Hill peridotite xenoliths (California, USA) and are used to examine these issues. The samples show strong correlations between Os-187/Os-188 and indicators of melt depletion such as Lu abundance in clinopyroxene, modal abundance of clinopyroxene, bulk rock Al2O3 and the Cr# (Cr/(Cr vertical bar Al)) in spinel. These relationships indicate that metasomatism did not compromise the Os-187/Os-188 systematics. The data appear to form two melt depletion trends consistent with Re depletion model ages (T-RD) obtained from the two Al2O3 versus Os-187/Os-188 trends are 2.1 +/- 0.5 Ga and 1.3 +/- 0.3 Ga (+/- 95% conf.). It has been suggested that the SCLM under Dish Hill may be fragments of oceanic lithosphere emplaced as the result of Farallon plate subduction during the Late Cretaceous (Luffi et al., 2009). However, the strong melt depletion trends, major element compositions and Re-depletion ages are not consistent with the interpretation of this suite of xenoliths having an oceanic lithospheric origin. Rather, the 2.1 Ga age coincides with Nd model ages of 2-2.3 Ga (Bennett and DePaolo, 1987; Ramo and Calzia, 1998) for the overlying Mojavia crustal province. The 1.3 Ga age is consistent with large-scale A-type magmatism in the nearby region at this time that is purported to be the result of mantle plume melting processes. Therefore, data from this study point to the SCLM under Dish Hill being formed by two ancient mantle-melting events, which could be the result of interleaving SCLM at depth. These interpretations indicate that the primary mechanism of SCLM formation under Dish Hill was through stabilization following partial melting in the convecting mantle that also results in contemporaneous juvenile crust production. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Armytage, Rosalind M. G.; Brandon, Alan D.; Lapen, Thomas J.] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA. [Peslier, Anne H.] Jacobs Technol, JETS, Houston, TX 77058 USA. [Peslier, Anne H.] NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA. RP Armytage, RMG (reprint author), Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA. EM rarmytage@uh.edu FU NSF [EAR 1048583] FX A.D.B. acknowledges NSF award EAR 1048583 for funding this work. The Smithsonian is thanked for providing samples. Richard Walker of the University of Maryland is thanked for access to his mass spectrometer for measurements. Cin-Ty Lee of Rice University is likewise thanked for the use of his mass spectrometer for measurements. Claire McLeod is thanked for her helpful discussions during the writing of the manuscript. We would like to thank John Lassiter, James Day, and an anonymous reviewer for their very constructive and insightful reviews, which greatly improved the manuscript. We would also like to thank Janne Blichet-Toft for her editorial handling of the manuscript. NR 92 TC 5 Z9 5 U1 0 U2 20 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 JUL 15 PY 2014 VL 137 BP 113 EP 133 DI 10.1016/j.gca.2014.04.017 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AK4WD UT WOS:000338424000008 ER PT J AU Doucet, LS Peslier, AH Ionov, DA Brandon, AD Golovin, AV Goncharov, AG Ashchepkov, IV AF Doucet, Luc S. Peslier, Anne H. Ionov, Dmitri A. Brandon, Alan D. Golovin, Alexander V. Goncharov, Aleksey G. Ashchepkov, Igor V. TI High water contents in the Siberian cratonic mantle linked to metasomatism: An FTIR study of Udachnaya peridotite xenoliths SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID NOMINALLY ANHYDROUS MINERALS; ARCHEAN LITHOSPHERIC MANTLE; OCEANIC UPPER-MANTLE; RE-OS ISOTOPE; SOUTHERN AFRICA; EAST KIMBERLITE; TRACE-ELEMENTS; HIGH-PRESSURE; CONTINENTAL LITHOSPHERE; HIGH-TEMPERATURES AB The processes that control water distribution in nominally anhydrous minerals from peridotites are twofold. Melt depletion will remove water while metasomatism can potentially add water to these minerals. These processes can lead to a wide range of outcomes in water contents, which in turn could play a role in mantle rheology and long-term cratonic root stability. To examine these complexities, water concentrations in minerals from well-characterized peridotites from the Udachnaya kimberlite in the central Siberian craton were analyzed by FTIR. The peridotites span a complete top to bottom cross-section of typical cratonic lithospheric mantle (2-7 GPa and 700-1400 degrees C). Diffusion modeling of water content profiles across olivine grains shows that water loss during decompression is limited to the 100 mu m rims of olivines; the cores preserved their mantle water contents. Water contents range from 6 to 323 ppm wt H2O in olivine, 28-301 ppm H2O in orthopyroxene (opx), 100-272 ppm H2O in clinopyroxene (cpx) and 0-23 ppm H2O in garnet. Melting modeling cannot reproduce the high water contents of cratonic mantle peridotites and any potential partial melting trend must have been erased by later events. The water contents of minerals, however, are correlated with modal abundances of clinopyroxene and garnet, bulk rock FeO, TiO2 and SiO2 as well as with light and middle rare earth elements in clinopyroxene and garnet. These relationships are best interpreted as interaction of residual, melt-depleted peridotites with silicate melt, which produced modal and cryptic metasomatism. Importantly, the water enrichment in the Siberian cratonic mantle took place prior to kimberlite magmatism and eruption. Water addition by metasomatism occurred from pressures >4 GPa all the way to the base of the cratonic root below central Siberia, but was limited to shallower levels (<5 GPa) in the Kaapvaal cratonic lithosphere. The difference in olivine water contents at the deepest levels of the Kaapvaal (<5 ppm H2O) and Siberian (6-323 ppm H2O) cratonic roots may be linked to oxygen fugacity and resulting fluid speciation or, alternatively, to reaction with different metasomatic agents. Calculated viscosities for the deepest Udachnaya samples are similar to those inferred for the asthenosphere. If these xenoliths are representative of the deep cratonic lithosphere, water is not as important a parameter as previously thought in the strength of cratonic lithosphere, otherwise the cratonic root beneath Udachnaya would have been delaminated. Alternatively, the metasomatic xenoliths may not be representative of the Siberian cratonic root and kimberlites preferentially sample cratonic mantle lithosphere material located near, and metasomatized by, melt conduits, which served as channels for upward migration of water-rich melts and fluids including kimberlites. In that case, the cratonic root overall still may have relatively low water contents, which in addition to its less metasomatized (more refractory) and thereby buoyant nature, still play a role in making it strong enough to resist delamination by the surrounding asthenosphere. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Doucet, Luc S.; Ionov, Dmitri A.] Univ St Etienne, F-42023 St Etienne, France. [Doucet, Luc S.; Ionov, Dmitri A.] UMR CNRS 6524 Magmas & Volcans, F-42023 St Etienne, France. [Peslier, Anne H.] NASA, Lyndon B Johnson Space Ctr, Jacobs, Houston, TX 77058 USA. [Ionov, Dmitri A.] Univ Montpellier 2, Geosci Montpellier, F-34095 Montpellier, France. [Ionov, Dmitri A.] UMR CNRS 5243, F-34095 Montpellier, France. [Brandon, Alan D.] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77004 USA. [Golovin, Alexander V.; Ashchepkov, Igor V.] Russian Acad Sci, Siberian Branch, VS Sobolev Inst Geol & Mineral, Novosibirsk 630090, Russia. [Golovin, Alexander V.] Novosibirsk State Univ, Novosibirsk 630090, Russia. [Goncharov, Aleksey G.] St Petersbourg State Univ, Inst Earth Sci, St Petersbourg 1999034, Russia. RP Doucet, LS (reprint author), Univ Libre Bruxelles, Lab G Time, B-1050 Brussels, Belgium. EM ldoucet@ulb.ac.be RI Golovin, Alexander/A-7090-2014; Goncharov, Alexey/J-3017-2013; Ionov, Dmitri/E-5111-2010; Ashchepkov, Igor/O-2452-2013 OI Goncharov, Alexey/0000-0002-3766-5693; Ionov, Dmitri/0000-0002-5055-7339; Ashchepkov, Igor/0000-0003-3985-7661 FU Ministry of Education and Science of the Russian Federation; NSF [1118335, 1118388]; Russian Foundation for Basic Research [11-05-91060 PICS, 13-05-00439-a]; French CNRS (PICS) for collaboration with Russian Academy of Sciences [5812] FX Collette Guilbaud and Chantal Perrache are thanked for preparing grain mounts in St. Etienne. We thank D. Frost for providing the program for compution the fluid compositions and A. Sokol for comments on the earlier version of the manuscript. A.V.G. thanks the Ministry of Education and Science of the Russian Federation for support. This work was funded by NSF grants EAR #1118335 to A.H.P. and EAR #1118388 to A.D.B. Fieldwork at Udachnaya and xenolith studies were funded by the Russian Foundation for Basic Research (grants No. 11-05-91060 PICS and No. 13-05-00439-a) and the French CNRS (PICS grant No. 5812) for collaboration with Russian Academy of Sciences in 2011-2013. We are grateful for the constructive comments of two anonymous reviewers and of Kate Selway which helped greatly to improve the manuscript. Editorial handling by M. Norman and S. Weyer is highly appreciated. NR 206 TC 30 Z9 33 U1 5 U2 54 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 JUL 15 PY 2014 VL 137 BP 159 EP 187 DI 10.1016/j.gca.2014.04.011 PG 29 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AK4WD UT WOS:000338424000011 ER PT J AU Grundy, WM Benecchi, SD Porter, SB Noll, KS AF Grundy, W. M. Benecchi, S. D. Porter, S. B. Noll, K. S. TI The orbit of transneptunian binary Manwe and Thorondor and their upcoming mutual events SO ICARUS LA English DT Article DE Kuiper belt; Trans-neptunian objects; Hubble Space Telescope observations; Eclipses; Occultations ID KUIPER-BELT; DYNAMICAL EVOLUTION; MINOR PLANETS; SILA-NUNAM; OBJECTS; ECCENTRICITY; INCLINATION; COLOR AB A new Hubble Space Telescope observation of the 7:4 resonant transneptunian binary system (385446) Manwe has shown that, of two previously reported solutions for the orbit of its satellite Thorondor, the prograde one is correct. The orbit has a period of 110.18 +/- 0.02 days, semimajor axis of 6670 +/- 40 km, and an eccentricity of 0.563 +/- 0.007. It will be viewable edge-on from the inner Solar System during 2015-2017, presenting opportunities to observe mutual occultation and eclipse events. However, the number of observable events will be small, owing to the long orbital period and expected small sizes of the bodies relative to their separation. This paper presents predictions for events observable from Earth-based telescopes and discusses the associated uncertainties and challenges. (c) 2014 Elsevier Inc. All rights reserved. C1 [Grundy, W. M.; Porter, S. B.] Lowell Observ, Flagstaff, AZ 86001 USA. [Benecchi, S. D.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Porter, S. B.] Southwest Res Inst, Boulder, CO 80302 USA. [Noll, K. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Grundy, WM (reprint author), Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA. EM W.Grundy@lowell.edu OI Porter, Simon/0000-0003-0333-6055 FU NASA through Space Telescope Science Institute (STScI) FX This work is based on NASA/ESA Hubble Space Telescope program 13404. Support for this program was provided by NASA through a grant from the Space Telescope Science Institute (STScI), operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. We are especially grateful to Linda Dressel and Tony Roman at STScI for their help in designing and scheduling the observations. This manuscript benefited from insightful and constructive reviews by D. Ragozzine and J. Berthier whom we thank for their efforts. We also thank the creators and maintainers of the NASA/JPL NAIF/SPICE ephemeris system (http://naifjpl.nasa.gov/naif/), the Johnston archive (http://www.johnstonsarchive.net/astro/asteroidmoons.html), and Lowell Observatory's astorb.dat database and associated infrastructure (ftp://ftp.lowelLedu/pub/elgb/astorb.html). Finally, we thank the free and open source software communities for empowering us with key tools used to complete this project, notably Linux, the GNU tools, LibreOffice, Python, MariaDB, Evolution, and FVWM. NR 37 TC 0 Z9 0 U1 0 U2 1 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 JUL 15 PY 2014 VL 237 BP 1 EP 8 DI 10.1016/j.icarus.2014.04.021 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ3HF UT WOS:000337556400001 ER PT J AU Lorenz, RD Kirk, RL Hayes, AG Anderson, YZ Lunine, JI Tokano, T Turtle, EP Malaska, MJ Soderblom, JM Lucas, A Karatekin, O Wall, SD AF Lorenz, Ralph D. Kirk, Randolph L. Hayes, Alexander G. Anderson, Yanhua Z. Lunine, Jonathan I. Tokano, Tetsuya Turtle, Elizabeth P. Malaska, Michael J. Soderblom, Jason M. Lucas, Antoine Karatekin, Ozgur Wall, Stephen D. TI A radar map of Titan Seas: Tidal dissipation and ocean mixing through the throat of Kraken SO ICARUS LA English DT Article DE Titan, hydrology; Tides, solid body; Satellites, dynamics; Radio observations ID ONTARIO LACUS; HYDROCARBON LAKES; LIGEIA MARE; ATMOSPHERE; MODELS; ETHANE; WAVES; CYCLE AB We present a radar map of the Titan's seas, with bathymetry estimated as proportional to distance from the nearest shore. This naive analytic bathymetry, scaled to a recent radar sounding of Ligeia Mare, suggests a total liquid volume of 32,000 km(3), at the low end of estimates made in 2008 when mapping coverage was incomplete. We note that Kraken Mare has two principal basins, separated by a narrow (similar to 17 km wide, similar to 40 km long) strait we refer to as the 'throat'. Tidal currents in this strait may be dramatic (similar to 0.5 m/s), generating observable effects such as dynamic topography, whirlpools, and acoustic noise, much like tidal races on Earth such as the Corryvreckan off Scotland. If tidal flow through this strait is the dominant mixing process, the two basins take 20 Earth years to exchange their liquid inventory. Thus compositional differences over seasonal timescales may exist, but the composition of solutes (and thus evaporites) over Croll-Milankovich timescales should be homogenized. (c) 2014 Elsevier Inc. All rights reserved. C1 [Lorenz, Ralph D.; Turtle, Elizabeth P.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA. [Kirk, Randolph L.] US Geol Survey, Flagstaff, AZ 86001 USA. [Hayes, Alexander G.; Lunine, Jonathan I.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Anderson, Yanhua Z.; Malaska, Michael J.; Wall, Stephen D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tokano, Tetsuya] Univ Cologne, Inst Geophys & Meteorol, D-50923 Cologne, Germany. [Soderblom, Jason M.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Lucas, Antoine] Lab Anneaux Disques & Planetes, F-75013 Paris, France. [Karatekin, Ozgur] Royal Observ Belgium, B-1108 Brussels, Belgium. RP Lorenz, RD (reprint author), Johns Hopkins Univ, Appl Phys Lab, Dept Space, Johns Hopkins Rd, Laurel, MD 20723 USA. EM ralph.lorenz@jhuapl.edu RI Hayes, Alexander/P-2024-2014; Lucas, Antoine/A-9752-2009; Turtle, Elizabeth/K-8673-2012; Lorenz, Ralph/B-8759-2016; OI Hayes, Alexander/0000-0001-6397-2630; Lucas, Antoine/0000-0003-2192-4416; Turtle, Elizabeth/0000-0003-1423-5751; Lorenz, Ralph/0000-0001-8528-4644; Malaska, Michael/0000-0003-0064-5258 FU NASA Outer Planets Research program via grant "Physical Processes in Titan's Seas" [NNX13AK97G]; Cassini project grant "Cassini Radar Science Support" [NNX13AH14G] FX R.L. acknowledges the support of the NASA Outer Planets Research program via grant "Physical Processes in Titan's Seas" NNX13AK97G, as well as via Cassini project grant "Cassini Radar Science Support" NNX13AH14G. The Cassini/Huygens mission is a joint endeavor of NASA and ESA, as well as several European national agencies and is managed for NASA by the California Institute of Technology's Jet Propulsion Laboratory. We acknowledge stimulating discussions with the Cassini radar team. We thank Thomas Cornet and an anonymous reviewer for useful comments. NR 51 TC 14 Z9 15 U1 2 U2 19 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 15 PY 2014 VL 237 BP 9 EP 15 DI 10.1016/j.icarus.2014.04.005 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ3HF UT WOS:000337556400002 ER PT J AU Steele, LJ Lewis, SR Patel, MR Montmessin, F Forget, F Smith, MD AF Steele, Liam J. Lewis, Stephen R. Patel, Manish R. Montmessin, Franck Forget, Francois Smith, Michael D. TI The seasonal cycle of water vapour on Mars from assimilation of Thermal Emission Spectrometer data SO ICARUS LA English DT Article DE Mars, atmosphere; Mars, climate; Atmospheres, dynamics; Meteorology ID GENERAL-CIRCULATION MODEL; RADIO OCCULTATION MEASUREMENTS; WESTERN BOUNDARY CURRENTS; MARTIAN HYDROLOGIC-CYCLE; GLOBAL SURVEYOR; INTERANNUAL VARIABILITY; MGS-TES; VERTICAL-DISTRIBUTION; NORTHERN-HEMISPHERE; TRANSIENT EDDIES AB We present for the first time an assimilation of Thermal Emission Spectrometer (TES) water vapour column data into a Mars global climate model (MGCM). We discuss the seasonal cycle of water vapour, the processes responsible for the observed water vapour distribution, and the cross-hemispheric water transport. The assimilation scheme is shown to be robust in producing consistent reanalyses, and the global water vapour column error is reduced to around 2-4 pr mu m depending on season. Wave activity is shown to play an important role in the water vapour distribution, with topographically steered flows around the Hellas and Argyre basins acting to increase transport in these regions in all seasons. At high northern latitudes, zonal wavenumber 1 and 2 stationary waves during northern summer are responsible for spreading the sublimed water vapour away from the pole. Transport by the zonal wavenumber 2 waves occurs primarily to the west of Tharsis and Arabia Terra and, combined with the effects of western boundary currents, this leads to peak water vapour column abundances here as observed by numerous spacecraft. A net transport of water to the northern hemisphere over the course of one Mars year is calculated, primarily because of the large northwards flux of water vapour which occurs during the local dust storm around Ls = 240-260 degrees. Finally, outlying frost deposits that surround the north polar cap are shown to be important in creating the peak water vapour column abundances observed during northern summer. (C) 2014 Elsevier Inc. All rights reserved. C1 [Steele, Liam J.; Lewis, Stephen R.; Patel, Manish R.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Montmessin, Franck] IPSL, CNRS, Observat Spatiales LATMOS, Lab Atmospheres, F-78280 Guyancourt, France. [Forget, Francois] IPSL, CNRS, LMD, F-75252 Paris, France. [Smith, Michael D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Steele, LJ (reprint author), Open Univ, Dept Phys Sci, Walton Hall, Milton Keynes MK7 6AA, Bucks, England. EM liam.steele@open.ac.uk OI Lewis, Stephen/0000-0001-7237-6494 FU UK Science and Technology Facilities Council FX The authors thank Luca Montabone for his help with the assimilation scheme and David Kass for his suggestions which helped improve this paper. This work was funded by the UK Science and Technology Facilities Council. NR 74 TC 8 Z9 8 U1 3 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 JUL 15 PY 2014 VL 237 BP 97 EP 115 DI 10.1016/j.icarus.2014.04.017 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ3HF UT WOS:000337556400010 ER PT J AU Cleaves, HJ Neish, C Callahan, MP Parker, E Fernandez, FM Dworkin, JP AF Cleaves, H. James, II Neish, Catherine Callahan, Michael P. Parker, Eric Fernandez, Facundo M. Dworkin, Jason P. TI Amino acids generated from hydrated Titan tholins: Comparison with Miller-Urey electric discharge products SO ICARUS LA English DT Article DE Atmospheres, chemistry; Astrobiology; Titan; Organic chemistry; Prebiotic chemistry ID PREBIOTIC SYNTHESIS; EARLY EARTH; ORGANIC-CHEMISTRY; HYDROGEN-CYANIDE; OXIDATION-STATE; ICE ANALOGS; HYDROLYSIS; ATMOSPHERE; SURFACE; IMPACT AB Various analogues of Titan haze particles (termed 'tholins') have been made in the laboratory. In certain geologic environments on Titan, these haze particles may come into contact with aqueous ammonia (NH3) solutions, hydrolyzing them into molecules of astrobiological interest. A Titan tholin analogue hydrolyzed in aqueous NH3 at room temperature for 2.5 years was analyzed for amino acids using highly sensitive ultra-high performance liquid chromatography coupled with fluorescence detection and timeof-flight mass spectrometry (UHPLC-FD/ToF-MS) analysis after derivatization with a fluorescent tag. We compare here the amino acids produced from this reaction sequence with those generated from room temperature Miller-Urey (MU) type electric discharge reactions. We find that most of the amino acids detected in low temperature MU CH4/N-2/H2O electric discharge reactions are generated in Titan simulation reactions, as well as in previous simulations of Triton chemistry. This argues that many processes provide very similar mixtures of amino acids, and possibly other types of organic compounds, in disparate environments, regardless of the order of hydration. Although it is unknown how life began, it is likely that given reducing conditions, similar materials were available throughout the early Solar System and throughout the universe to facilitate chemical evolution. (C) 2014 The Authors. Published by Elsevier Inc. C1 [Cleaves, H. James, II] Tokyo Inst Technol, Earth Life Sci Inst, Minato Ku, Tokyo 152, Japan. [Cleaves, H. James, II] Inst Adv Study, Princeton, NJ 08540 USA. [Cleaves, H. James, II] Blue Marble Space Inst Sci, Washington, DC 20008 USA. [Cleaves, H. James, II; Parker, Eric; Fernandez, Facundo M.] Georgia Inst Technol, Ctr Chem Evolut, Atlanta, GA 30332 USA. [Neish, Catherine] Florida Inst Technol, Melbourne, FL 32901 USA. [Callahan, Michael P.; Dworkin, Jason P.] NASA Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Parker, Eric; Fernandez, Facundo M.] Georgia Inst Technol, Sch Chem & Biochem, Atlanta, GA 30332 USA. RP Cleaves, HJ (reprint author), Tokyo Inst Technol, Earth Life Sci Inst, Minato Ku, Tokyo 152, Japan. EM cleaves@elsi.jp RI Dworkin, Jason/C-9417-2012; OI Dworkin, Jason/0000-0002-3961-8997; Cleaves, Henderson/0000-0003-4101-0654 FU NASA Astrobiology Institute NPP fellowship; NSF; NSF Center for Chemical Evolution [CHE-1004570]; NASA Astrobiology Institute; Goddard Center for Astrobiology; NASA Astrobiology program FX H.J.C. would like to thank the Geophysical Laboratory of the Carnegie Institution of Washington and Mrs. Mary Wolf for assistance with literature searches, as well as support from a NASA Astrobiology Institute NPP fellowship for grant support. E.T.P., H.J.C. and F.M.F. acknowledge support from the NSF and NASA Astrobiology program under the NSF Center for Chemical Evolution, CHE-1004570. M.P.C. and J.P.D. acknowledge support from the NASA Astrobiology Institute and The Goddard Center for Astrobiology. NR 58 TC 4 Z9 4 U1 5 U2 58 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 JUL 15 PY 2014 VL 237 BP 182 EP 189 DI 10.1016/j.icarus.2014.04.042 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ3HF UT WOS:000337556400015 ER PT J AU de Pater, I Fletcher, LN Luscz-Cook, S DeBoer, D Butler, B Hammel, HB Sitko, ML Orton, G Marcus, PS AF de Pater, Imke Fletcher, Leigh N. Luscz-Cook, Statia DeBoer, David Butler, Bryan Hammel, Heidi B. Sitko, Michael L. Orton, Glenn Marcus, Philip S. TI Neptune's global circulation deduced from multi-wavelength observations SO ICARUS LA English DT Article DE Neptune, atmosphere; Infrared observations; Radio observations ID INFRARED-ABSORPTION-SPECTRA; GREAT RED SPOT; CLOUD STRUCTURE; ADAPTIVE OPTICS; VERTICAL STRUCTURE; ATMOSPHERIC CIRCULATION; VOYAGER MEASUREMENTS; RADIATIVE-TRANSFER; THERMAL STRUCTURE; KECK TELESCOPE AB We observed Neptune between June and October 2003 at near- and mid-infrared wavelengths with the 10-m W.M. Keck IL and I telescopes, respectively; and at radio wavelengths with the Very Large Array. Images were obtained at near-infrared wavelengths with NIRC2 coupled to the adaptive optics system in both broad- and narrow-band filters between 1.2 and 2.2 In the mid-infrared we imaged Neptune at wavelengths between 8 and 22 pm, and obtained slit-resolved spectra at 8-13 pm and 18-221.tm. At radio wavelengths we mapped the planet in discrete filters between 0.7 and 6 cm. We analyzed each dataset separately with a radiative-transfer program that is optimized for that particular wavelength regime. At southern midlatitudes the atmosphere appears to be cooler at mid-infrared wavelengths than anywhere else on the planet. We interpret this to be caused by adiabatic cooling due to air rising at midlatitudes at all longitudes from the upper troposphere up to;5,0.1 mbar levels. At nearinfrared wavelengths we find two distinct cloud layers at these latitudes: a relatively deep layer of clouds (presumably methane) in the troposphere at pressure levels P 300-z600 mbar, which we suggest to be caused by the large-scale upwelling and its accompanying adiabatic cooling and condensation of methane; and a higher, spatially intermittent, layer of clouds in the stratosphere at 20-30 mbar. The latitudes of these high clouds encompass an anticyclonic band of zonal flow, which suggests that they may be due to strong, but localized, vertical upwellings associated with local anticyclones, rather than plumes in convective (i.e., cyclonic) storms. Clouds at northern midlatitudes are located at the highest altitudes in the atmosphere, near 10 mbar. Neptune's south pole is considerably enhanced in brightness at both mid-infrared and radio wavelengths, i.e., from,,0.1 mbar levels in the stratosphere down to tens of bars in the troposphere. We interpret this to be due to subsiding motions from the stratosphere all the way down to the deep troposphere. The enhanced brightness observed at mid-infrared wavelengths is interpreted to be due to adiabatic heating by compression in the stratosphere, and the enhanced brightness temperature at radio wavelengths reveals that the subsiding air over the pole is very dry; the relative humidity of H2S over the pole is only 5% at altitudes above the NH4SH cloud at 40 bar. The low humidity region extends from the south pole down to latitudes of 66 S. This is near the same latitudes as the south polar prograde jet signifying the boundary of the polar vortex. We suggest that the South Polar Features (SPFs) at latitudes of 60-70 are convective storms, produced by baroclinic instabilities expected to be produced at latitudes near the south polar prograde jet. Taken together, our data suggest a global circulation pattern where air is rising above southern and northern midlatitudes, from the troposphere up well into the stratosphere, and subsidence of dry air over the pole and equator from the stratosphere down into the troposphere. We suggest that this pattern extends all the way from <0.1 mbar down to pressures of >40 bar. 2014 Elsevier Inc. All rights reserved. C1 [de Pater, Imke; DeBoer, David] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [de Pater, Imke] Delft Univ Technol, Fac Aerosp Engn, NL-2629 HS Delft, Netherlands. [de Pater, Imke] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Fletcher, Leigh N.] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England. [Butler, Bryan] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Hammel, Heidi B.] Assoc Univ Res Astron, Washington, DC 20005 USA. [Hammel, Heidi B.] Space Sci Inst, Boulder, CO 80301 USA. [Orton, Glenn] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Sitko, Michael L.] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA. [Luscz-Cook, Statia] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Marcus, Philip S.] Univ Calif Berkeley, Dept Mech Engn, Berkeley, CA 94720 USA. RP de Pater, I (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM imke@berkeley.edu RI Fletcher, Leigh/D-6093-2011 OI Fletcher, Leigh/0000-0001-5834-9588 FU W.M. Keck Foundation; National Science Foundation Science and Technology Center for Adaptive Optics; Kalbfleisch Postdoctoral Fellowship at the American Museum of Natural History; Royal Society Research Fellowship at the University of Oxford; NASA PATM [NNX10AB93G, NNX13AG56G]; [AST1009907] FX We thank L. Sromovsky and two anonymous referees for valuable comments to help improve our manuscript. Some of the data presented 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 has been supported in part by the National Science Foundation Science and Technology Center for Adaptive Optics, managed by the University of California at Santa Cruz under cooperative Agreement No. AST 9876783, and by NSF Grant AST0908575 to UC Berkeley. S.H.L.C. is supported by the Kalbfleisch Postdoctoral Fellowship at the American Museum of Natural History. L.N.F. is supported by a Royal Society Research Fellowship at the University of Oxford. P.S.M. is supported in part by AST1009907 and by NASA PATM grants NNX10AB93G and NNX13AG56G. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to conduct observations from this mountain. NR 100 TC 9 Z9 9 U1 3 U2 14 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 JUL 15 PY 2014 VL 237 BP 211 EP 238 DI 10.1016/j.icarus.2014.02.030 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ3HF UT WOS:000337556400018 ER PT J AU Edmonds, RM Murphy, JR Schofield, JT Heavens, NG AF Edmonds, Robert M. Murphy, J. R. Schofield, J. T. Heavens, N. G. TI Convective instabilities during Mars Climate Sounder's limb staring mode were overestimated SO ICARUS LA English DT Article DE Atmospheres, dynamics; Mars, atmosphere; Mars; Meteorology ID GRAVITY-WAVE; MARTIAN ATMOSPHERE; TURBULENCE; SPECTRA AB We report that the onset, and temporary cessation, of instabilities in MCS temperature profiles during MY 28 coincided with the initiation and cessation of limb staring operation, suggesting instrument operation was a factor in the identification of instabilities by Heavens et al. (Heavens et al. [2010]. Icarus, 208, 574-589). We demonstrate that the limb staring instrument operation during northern autumn of MY 28 can produce erroneous unstable lapse rates. (C) 2014 Elsevier Inc. All rights reserved. C1 [Edmonds, Robert M.; Murphy, J. R.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Schofield, J. T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Heavens, N. G.] Hampton Univ, Dept Atmospher & Planetary Sci, Hampton, VA 23669 USA. RP Edmonds, RM (reprint author), New Mexico State Univ, Dept Astron, POB 30001,MSC 4500, Las Cruces, NM 88003 USA. EM redmonds@nmsu.edu OI Heavens, Nicholas/0000-0001-7654-503X NR 18 TC 0 Z9 0 U1 1 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 JUL 15 PY 2014 VL 237 BP 415 EP 418 DI 10.1016/j.icarus.2014.04.034 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ3HF UT WOS:000337556400030 ER PT J AU Kotov, DV Yee, HC Panesi, M Prabhu, DK Wray, AA AF Kotov, Dmitry V. Yee, H. C. Panesi, Marco Prabhu, Dinesh K. Wray, Alan A. TI Computational challenges for simulations related to the NASA electric arc shock tube (EAST) experiments SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Article DE Numerical methods for problems with stiff source terms and discontinuities Hypersonic nonequilibrium electric arc shock tube simulations; Wrong propagation speed of discontinuities; Spurious numerics; High order simulations of hypersonic viscous flows ID STIFF SOURCE TERMS; COMPRESSIBLE EULER EQUATIONS; MULTISCALE VISCOUS FLOWS; OVERLAPPING GRID METHODS; II FLIGHT EXPERIMENT; HIGH-ORDER METHODS; NUMERICAL DISSIPATION; SUBCELL RESOLUTION; CAPTURING METHODS; MIXED STEADY AB The goal of this study is to gain some physical insights and an understanding of the computational challenges for the simulations related to the hypersonic nonequilibrium multi-species and multi-reaction experiments on the NASA Electric Arc Shock Tube (EAST). While experimental measurement does not provide any information about the radial structure of this type of flow, accurate and reliable numerical simulations can provide more insight into the physical structure of the flow to aid the design of atmospheric entry spacecrafts. The paper focuses on the spurious numerics which take place in numerical simulations of the subject physics containing stiff source terms and discontinuities. This paper is based on the knowledge gained from Yee et al. on simple reacting test cases(Yee et al. 2013, [9]) as a guide to reveal the computational challenges involved for such an extreme flow type. The results of the 1D and 2D EAST viscous and inviscid simulations using a simplified physical model are presented. The computation reveals, for the first time, that the 2D viscous model which contains both shocks and shears exhibits Tollmien-Schlichting-like instability complex patterns at the boundary layer. In addition to exhibiting spurious numerical behavior of wrong propagation speed of discontinuities by typical shock-capturing methods, there is improved understanding on the cause of numerical difficulties by previous investigators. One example is that the relative distance between the shocks and shear/contact is different from one grid spacing to another for each considered high order shock-capturing scheme. The results presented can provide insight on the numerical instability observed by previous investigations and future algorithm development for this type of extreme flow. Published by Elsevier Inc. C1 [Kotov, Dmitry V.] Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA. [Yee, H. C.; Prabhu, Dinesh K.; Wray, Alan A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Panesi, Marco] Univ Illinois, Dept Aerosp Engn, Urbana, IL 61801 USA. RP Yee, HC (reprint author), NASA, Ames Res Ctr, MS 258-5, Moffett Field, CA 94035 USA. EM dkotov@stanford.edu; helen.m.yee@nasa.gov; mpanesi@illinois.edu; dinesh.k.prabhu@nasa.gov; alan.a.wray@nasa.gov OI Prabhu, Dinesh/0000-0002-0550-2072 FU DOE/SciDAC SAP grant [DE-AI02-06ER25796]; NASA Fundamental Aeronautics (Hypersonics) program FX The support of the DOE/SciDAC SAP grant DE-AI02-06ER25796 is acknowledged. The work was performed by the first author as a postdoctoral fellow at the Center for Turbulence Research, Stanford University. Financial support from the NASA Fundamental Aeronautics (Hypersonics) program for the second, third, fourth and fifth authors is gratefully acknowledged. NR 45 TC 2 Z9 2 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 0021-9991 EI 1090-2716 J9 J COMPUT PHYS JI J. Comput. Phys. PD JUL 15 PY 2014 VL 269 BP 215 EP 233 DI 10.1016/j.jcp.2014.03.021 PG 19 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA AG5DL UT WOS:000335439300013 ER PT J AU Aveline, DC Strekalov, DV Yu, N AF Aveline, David C. Strekalov, Dmitry V. Yu, Nan TI Micro-slotted whispering gallery mode resonators for optomechanical applications SO APPLIED PHYSICS LETTERS LA English DT Article ID RAYLEIGH-SCATTERING; CAVITY; MICROSPHERES AB We present a study of augmented whispering gallery mode optical resonators that contain one or more narrow slots, through which the optical field exits the resonator's dielectric material and propagates in free space. We developed a theoretical model describing the micro-slotted resonator mode spectrum, and we find the theoretical results of the single-slot case are in close agreement with experimental observations. Furthermore, we examine a double-slot configuration that forms a cantilever-like partition within the circulating high-Q optical modes. The system exhibits high displacement sensitivity that could lead to optomechanical sensing applications. C1 [Aveline, David C.; Strekalov, Dmitry V.; Yu, Nan] CALTECH, Jet Prop Lab, Quantum Sci & Technol Grp, Pasadena, CA 91109 USA. RP Aveline, DC (reprint author), CALTECH, Jet Prop Lab, Quantum Sci & Technol Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM daveline@jpl.nasa.gov FU National Aeronautics and Space Administration; NASA's Center Innovation Fund 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, with NASA's Center Innovation Fund. The authors thank Lukas Baumgartel and Matthew Mecklenberg for helpful discussions and contributions. NR 15 TC 3 Z9 3 U1 2 U2 18 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 JUL 14 PY 2014 VL 105 IS 2 AR 021111 DI 10.1063/1.4890081 PG 4 WC Physics, Applied SC Physics GA AO2KU UT WOS:000341151400011 ER PT J AU Soibel, A Hill, CJ Keo, SA Hoglund, L Rosenberg, R Kowalczyk, R Khoshakhlagh, A Fisher, A Ting, DZY Gunapala, SD AF Soibel, Alexander Hill, Cory J. Keo, Sam A. Hoglund, Linda Rosenberg, Robert Kowalczyk, Robert Khoshakhlagh, Arezou Fisher, Anita Ting, David Z. -Y. Gunapala, Sarath D. TI Room temperature performance of mid-wavelength infrared InAsSb nBn detectors SO APPLIED PHYSICS LETTERS LA English DT Article ID PHOTODETECTORS; DESIGN AB In this work, we investigate the high temperature performance of mid-wavelength infrared InAsSb-AlAsSb nBn detectors with cut-off wavelengths near 4.5 mu m. The quantum efficiency of these devices is 35% without antireflection coatings and does not change with temperature in the 77-325 K temperature range, indicating potential for room temperature operation. The current generation of nBn detectors shows an increase of operational bias with temperature, which is attributed to a shift in the Fermi energy level in the absorber. Analysis of the device performance shows that operational bias and quantum efficiency of these detectors can be further improved. The device dark current stays diffusion limited in the 150 K-325 K temperature range and becomes dominated by generation-recombination processes at lower temperatures. Detector detectivities are D*(lambda) = 1 x 10(9) (cm Hz(0.5)/W) at T = 300 K and D*(lambda) = 5 x 10(9) (cm Hz(0.5)/W) at T = 250 K, which is easily achievable with a one stage TE cooler. (C) 2014 AIP Publishing LLC. C1 [Soibel, Alexander; Hill, Cory J.; Keo, Sam A.; Hoglund, Linda; Rosenberg, Robert; Kowalczyk, Robert; Khoshakhlagh, Arezou; Fisher, Anita; Ting, David Z. -Y.; Gunapala, Sarath D.] CALTECH, Jet Prop Lab, Pasadena, CA 91030 USA. RP Soibel, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91030 USA. RI Soibel, Alexander/A-1313-2007 NR 18 TC 19 Z9 19 U1 7 U2 34 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 JUL 14 PY 2014 VL 105 IS 2 AR 023512 DI 10.1063/1.4890465 PG 4 WC Physics, Applied SC Physics GA AO2KU UT WOS:000341151400084 ER PT J AU Panesi, M Munafo, A Magin, TE Jaffe, RL AF Panesi, M. Munafo, A. Magin, T. E. Jaffe, R. L. TI Nonequilibrium shock-heated nitrogen flows using a rovibrational state-to-state method SO PHYSICAL REVIEW E LA English DT Article ID POTENTIAL-ENERGY SURFACES; THERMAL RATE CONSTANTS; II FLIGHT EXPERIMENT; VIBRATIONAL-RELAXATION; HYPERSONIC FLOWS; THERMOCHEMICAL NONEQUILIBRIUM; ROTATIONAL RELAXATION; TRANSLATIONAL ENERGY; 3-BODY RECOMBINATION; ATOMIC NITROGEN AB A rovibrational collisional model is developed to study the internal energy excitation and dissociation processes behind a strong shock wave in a nitrogen flow. The reaction rate coefficients are obtained from the ab initio database of the NASA Ames Research Center. The master equation is coupled with a one-dimensional flow solver to study the nonequilibrium phenomena encountered in the gas during a hyperbolic reentry into Earth's atmosphere. The analysis of the populations of the rovibrational levels demonstrates how rotational and vibrational relaxation proceed at the same rate. This contrasts with the common misconception that translational and rotational relaxation occur concurrently. A significant part of the relaxation process occurs in non-quasi-steady-state conditions. Exchange processes are found to have a significant impact on the relaxation of the gas, while predissociation has a negligible effect. The results obtained by means of the full rovibrational collisional model are used to assess the validity of reduced order models (vibrational collisional and multitemperature) which are based on the same kinetic database. It is found that thermalization and dissociation are drastically overestimated by the reduced order models. The reasons of the failure differ in the two cases. In the vibrational collisional model the overestimation of the dissociation is a consequence of the assumption of equilibrium between the rotational energy and the translational energy. The multitemperature model fails to predict the correct thermochemical relaxation due to the failure of the quasi-steady-state assumption, used to derive the phenomenological rate coefficient for dissociation. C1 [Panesi, M.] Univ Illinois, Champaign, IL 61801 USA. [Munafo, A.; Magin, T. E.] von Karman Inst Fluid Dynam, B-1640 Rhode St Genese, Belgium. [Jaffe, R. L.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA. RP Panesi, M (reprint author), Univ Illinois, 104 S Wright St, Champaign, IL 61801 USA. RI Magin, Thierry/A-7533-2016 OI Magin, Thierry/0000-0002-4376-1518 FU University of Illinois Startup Grant; NASA's Space Technology/Hypersonics-Entry, Descent and Landing Project; Fundamental Fundamental Aeronautics Program/Hypersonics Project; European Research Council [259354] FX The authors have benefited from numerous discussions with D. W. Schwenke, G. Chaban, W. Huo, and Y. Liu at the NASA Ames Research Center. We gratefully acknowledge K. Schulz at The University of Texas at Austin for his help in substantially speeding up the code. Funding for this research was provided through a University of Illinois Startup Grant. R.L.J. acknowledges support from NASA's Space Technology/Hypersonics-Entry, Descent and Landing Project and Fundamental Fundamental Aeronautics Program/Hypersonics Project. A.M. and T.E.M. acknowledge support from the European Research Council Starting Grant No. 259354. NR 75 TC 27 Z9 27 U1 4 U2 21 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0045 EI 2470-0053 J9 PHYS REV E JI Phys. Rev. E PD JUL 14 PY 2014 VL 90 IS 1 AR 013009 DI 10.1103/PhysRevE.90.013009 PG 16 WC Physics, Fluids & Plasmas; Physics, Mathematical SC Physics GA AO3PU UT WOS:000341246400009 PM 25122371 ER PT J AU Lindeman, MA AF Lindeman, M. A. TI Resonator-bolometer theory, microwave read out, and kinetic inductance bolometers SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID THERMOMETER; DETECTORS; NOISE; BAND AB Kinetic inductance bolometers and calorimeters, each consisting of a kinetic inductance device suspended on a membrane and embedded in a resonant circuit, are being developed for applications such as planetary science, climate science, and X-ray spectroscopy. Arrays of these resonator-bolometers, each with a unique resonance frequency, are coupled to a single feedline, allowing many bolometers or calorimeters to be multiplexed using microwave read out. We derive coupled linear differential equations describing resonator-bolometers and means for calculating responses to signal and noise sources. By employing the bolometer matrix formalism, the model compactly describes the effects of demodulation, detuning, electrothermal feedback, resonator to feedline coupling, and bolometer sensitivity to changes in temperature and bias current. Based on this theory, estimates for the bolometer response to phonon noise, Johnson noise, and microwave bias quasiparticle generation noise are derived. The model is represented in terms of accessible parameters, most of which are measurable using a network analyzer. It is applicable to other types of devices such as dielectric bolometers or alternating current biased transition edge sensors and is readily extendible to more complex bolometers or to unsuspended kinetic inductance devices. (C) 2014 AIP Publishing LLC. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lindeman, MA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU NASA; National Aeronautics and Space Administration FX This research was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The author would like to thank Peter Day and Alan Kleinsasser for useful discussions. NR 27 TC 3 Z9 3 U1 2 U2 12 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-8979 EI 1089-7550 J9 J APPL PHYS JI J. Appl. Phys. PD JUL 14 PY 2014 VL 116 IS 2 AR 024506 DI 10.1063/1.4890018 PG 8 WC Physics, Applied SC Physics GA AN0II UT WOS:000340267600077 ER PT J AU Lee, KJ Bassa, CG Janssen, GH Karuppusamy, R Kramer, M Liu, K Perrodin, D Smits, R Stappers, BW van Haasteren, R Lentati, L AF Lee, K. J. Bassa, C. G. Janssen, G. H. Karuppusamy, R. Kramer, M. Liu, K. Perrodin, D. Smits, R. Stappers, B. W. van Haasteren, R. Lentati, L. TI Model-based asymptotically optimal dispersion measure correction for pulsar timing SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: statistical; pulsars: general ID MILLISECOND PULSARS; TIME VARIABILITY; SCATTERING; ARRAY; B1937+21; PACKAGE; TEMPO2 AB In order to reach the sensitivity required to detect gravitational waves, pulsar timing array experiments need to mitigate as much noise as possible in timing data. A dominant amount of noise is likely due to variations in the dispersion measure. To correct for such variations, we develop a statistical method inspired by the maximum likelihood estimator and optimal filtering. Our method consists of two major steps. First, the spectral index and amplitude of dispersion measure variations are measured via a time-domain spectral analysis. Second, the linear optimal filter is constructed based on the model parameters found in the first step, and is used to extract the dispersion measure variation waveforms. Compared to current existing methods, this method has better time resolution for the study of short time-scale dispersion variations, and generally produces smaller errors in waveform estimations. This method can process irregularly sampled data without any interpolation because of its time-domain nature. Furthermore, it offers the possibility to interpolate or extrapolate the waveform estimation to regions where no data are available. Examples using simulated data sets are included for demonstration. C1 [Lee, K. J.; Karuppusamy, R.; Kramer, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Bassa, C. G.; Janssen, G. H.; Smits, R.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Bassa, C. G.; Kramer, M.; Stappers, B. W.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Liu, K.] CNRS Univ Orleans, LPC2E, F-45071 Orleans 02, France. [Liu, K.] CNRS INSU, Stn Radioastron Nancay, Observ Paris, F-18330 Nancay, France. [Perrodin, D.] INAF Osservatorio Astron Cagliari, I-09047 Selargius, CA, Italy. [van Haasteren, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA. [Lentati, L.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. RP Lee, KJ (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM kjlee007@gmail.com RI Perrodin, Delphine/L-1916-2016 OI Perrodin, Delphine/0000-0002-1806-2483 FU ERC [227947]; National Natural Science Foundation of China [11373011]; NASA Einstein Fellowship [PF3-140116] FX KJL gratefully acknowledges support from the ERC Advanced Grant 'LEAP', Grant Agreement Number 227947 (PI: Michael Kramer) and from the National Natural Science Foundation of China (Grant No. 11373011). We thank Dan Stinebring for helpful discussions. RvH is supported by NASA Einstein Fellowship grant PF3-140116. NR 50 TC 16 Z9 16 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 11 PY 2014 VL 441 IS 4 BP 2831 EP 2844 DI 10.1093/mnras/stu664 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK9RP UT WOS:000338764700004 ER PT J AU Weinzirl, T Jogee, S Neistein, E Khochfar, S Kormendy, J Marinova, I Hoyos, C Balcells, M den Brok, M Hammer, D Peletier, RF Kleijn, GV Carter, D Goudfrooij, P Lucey, JR Mobasher, B Trentham, N Erwin, P Puzia, T AF Weinzirl, Tim Jogee, Shardha Neistein, Eyal Khochfar, Sadegh Kormendy, John Marinova, Irina Hoyos, Carlos Balcells, Marc den Brok, Mark Hammer, Derek Peletier, Reynier F. Kleijn, Gijs Verdoes Carter, David Goudfrooij, Paul Lucey, John R. Mobasher, Bahram Trentham, Neil Erwin, Peter Puzia, Thomas TI The HST/ACS Coma Cluster Survey - VII. Structure and assembly of massive galaxies in the centre of the Coma cluster SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: bulges; galaxies: clusters: Coma; galaxies: elliptical and lenticular; cD; galaxies: evolution; galaxies: formation; galaxies: structure ID HUBBLE-SPACE-TELESCOPE; DIGITAL-SKY-SURVEY; ON SPIRAL GALAXIES; COLD DARK-MATTER; INTRACLUSTER PLANETARY-NEBULAE; SURFACE-DENSITY PROFILES; STAR-FORMATION RATES; SURVEY IMAGING DATA; N-BODY SIMULATIONS; ELLIPTIC GALAXIES AB We constrain the assembly history of galaxies in the projected central 0.5 Mpc of the Coma cluster by performing structural decomposition on 69 massive (M-a 50% of SNe IIn have at least one pre-explosion outburst that is brighter than 3 x 10(7) L-circle dot taking place up to 1/3 yr prior to the SN explosion. The average rate of such precursor events during the year prior to the SN explosion is likely greater than or similar to 1 yr(-1), and fainter precursors are possibly even more common. Ignoring the two weakest precursors in our sample, the precursors rate we find is still on the order of one per year. We also find possible correlations between the integrated luminosity of the precursor and the SN total radiated energy, peak luminosity, and rise time. These correlations are expected if the precursors are mass-ejection events, and the early-time light curve of these SNe is powered by interaction of the SN shock and ejecta with optically thick circumstellar material. C1 [Ofek, Eran O.; Steinbok, Aviram; Arcavi, Iair; Gal-Yam, Avishay; Tal, David; Ben-Ami, Sagi; Yaron, Ofer] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Sullivan, Mark] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Shaviv, Nir J.] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Kulkarni, Shrinivas R.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Nugent, Peter E.; Bloom, Joshua S.; Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Kasliwal, Mansi M.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Laher, Russ; Surace, Jason] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Silverman, Jeffrey M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Ofek, EO (reprint author), Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. OI Sullivan, Mark/0000-0001-9053-4820; Gal-Yam, Avishay/0000-0002-3653-5598 FU W. M. Keck Foundation; Israeli Ministry of Science, ISF, Minerva, Weizmann-UK; I-CORE Program of the Planning and Budgeting Committee; Israel Science Foundation [1829/12]; Gary and Cynthia Bengier; Christopher R. Redlich Fund; Richard and Rhoda Goldman Fund; TABASGO Foundation; NSF [AST-1211916] FX E.O.O. thanks Orly Gnat and Ehud Nakar for many discussions. This paper is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We are grateful for excellent staff assistance at Palomar, Lick, and Keck Observatories. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful for support by a grant from the Israeli Ministry of Science, ISF, Minerva, Weizmann-UK and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation (grant no 1829/12). A.V.F.'s group at UC Berkeley has received generous financial assistance from Gary and Cynthia Bengier, the Christopher R. Redlich Fund, the Richard and Rhoda Goldman Fund, the TABASGO Foundation, and NSF grant AST-1211916. NR 85 TC 40 Z9 40 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 JUL 10 PY 2014 VL 789 IS 2 AR 104 DI 10.1088/0004-637X/789/2/104 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8JY UT WOS:000338674900013 ER PT J AU Tal, T Dekel, A Oesch, P Muzzin, A Brammer, GB van Dokkum, PG Franx, M Illingworth, GD Leja, J Magee, D Marchesini, D Momcheva, I Nelson, EJ Patel, SG Quadri, RF Rix, HW Skelton, RE Wake, DA Whitaker, KE AF Tal, Tomer Dekel, Avishai Oesch, Pascal Muzzin, Adam Brammer, Gabriel B. van Dokkum, Pieter G. Franx, Marijn Illingworth, Garth D. Leja, Joel Magee, Daniel Marchesini, Danilo Momcheva, Ivelina Nelson, Erica J. Patel, Shannon G. Quadri, Ryan F. Rix, Hans-Walter Skelton, Rosalind E. Wake, David A. Whitaker, Katherine E. TI OBSERVATIONS OF ENVIRONMENTAL QUENCHING IN GROUPS IN THE 11 GYR SINCE z=2.5: DIFFERENT QUENCHING FOR CENTRAL AND SATELLITE GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: groups: general; galaxies: star formation ID DIGITAL SKY SURVEY; HUBBLE-SPACE-TELESCOPE; SIMILAR-TO 2; EXTRAGALACTIC LEGACY SURVEY; STAR-FORMATION HISTORIES; LUMINOUS RED GALAXIES; DARK-MATTER HALOS; MASSIVE GALAXIES; STELLAR MASS; SPECTROSCOPIC SURVEY AB We present direct observational evidence for star formation quenching in galaxy groups in the redshift range 0 < z < 2.5. We utilize a large sample of nearly 6000 groups, selected by fixed cumulative number density from three photometric catalogs, to follow the evolving quiescent fractions of central and satellite galaxies over roughly 11 Gyr. At z similar to 0, central galaxies in our sample range in stellar mass from Milky Way/M31 analogs (M-star/M-circle dot = 6.5 x 10(10)) to nearby massive ellipticals (M-star/M-circle dot = 1.5 x 10(11)). Satellite galaxies in the same groups reach masses as low as twice that of the Large Magellanic Cloud (M-star/M-circle dot = 6.5 x 10(9)). Using statistical background subtraction, we measure the average rest-frame colors of galaxies in our groups and calculate the evolving quiescent fractions of centrals and satellites over seven redshift bins. Our analysis shows clear evidence for star formation quenching in group halos, with a different quenching onset for centrals and their satellite galaxies. Using halo mass estimates for our central galaxies, we find that star formation shuts off in centrals when typical halo masses reach between 10(12) and 10(13) M-circle dot, consistent with predictions from the halo quenching model. In contrast, satellite galaxies in the same groups most likely undergo quenching by environmental processes, whose onset is delayed with respect to their central galaxy. Although star formation is suppressed in all galaxies over time, the processes that govern quenching are different for centrals and satellites. While mass plays an important role in determining the star formation activity of central galaxies, quenching in satellite galaxies is dominated by the environment in which they reside. C1 [Tal, Tomer; Illingworth, Garth D.; Magee, Daniel] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Oesch, Pascal; van Dokkum, Pieter G.; Leja, Joel; Momcheva, Ivelina; Nelson, Erica J.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Muzzin, Adam; Franx, Marijn] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Brammer, Gabriel B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Marchesini, Danilo] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA. [Patel, Shannon G.; Quadri, Ryan F.] Carnegie Observ, Pasadena, CA 91101 USA. [Rix, Hans-Walter] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Skelton, Rosalind E.] S African Astron Observ, ZA-7935 Cape Town, South Africa. [Wake, David A.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Wake, David A.] 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. RP Tal, T (reprint author), Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. EM tal@ucolick.org RI Skelton, Rosalind/S-1845-2016; OI Skelton, Rosalind/0000-0001-7393-3336; Leja, Joel/0000-0001-6755-1315; Oesch, Pascal/0000-0001-5851-6649 FU NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1202667]; Alfred P. Sloan Foundation; Participating Institutions; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX We thank Guillermo Barro and Alis Deason for engaging discussions and for commenting on an early draft of the paper. T.T. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1202667.; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 102 TC 27 Z9 28 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 JUL 10 PY 2014 VL 789 IS 2 AR 164 DI 10.1088/0004-637X/789/2/164 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8JY UT WOS:000338674900073 ER PT J AU Titarchuk, L Seifina, E Shrader, C AF Titarchuk, Lev Seifina, Elena Shrader, Chris TI X-RAY SPECTRAL AND TIMING BEHAVIOR OF SCORPIUS X-1. SPECTRAL HARDENING DURING THE FLARING BRANCH SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion; accretion disks; radiation mechanisms: non-thermal; stars: neutron; X-rays: binaries ID QUASI-PERIODIC OSCILLATIONS; BOUNDARY-LAYER EMISSION; ACCRETING NEUTRON-STARS; COLOR-COLOR DIAGRAM; SOURCE GX 340+0; Z-TRACK; XTE J1701-462; ATOLL SOURCES; OBSERVATIONAL EVIDENCE; LUMINOUS LMXBS AB We present an analysis of the spectral and timing properties of X-ray emission from the Z-source Sco X-1 during its evolution between the horizontal (HB) and flaring (FB) branches observed with the Rossi X-ray Timing Explorer during the 1996-2002 period. We find that the broadband (3-250 keV) energy spectra during all spectral states can be adequately reproduced by a model, consisting of two Comptonized components and an iron line. We suggest that the seed photons of kT(s1) less than or similar to 0.7 keV coming from the disk and of temperature kT(s2) less than or similar to 1.8 keV coming from the neutron star (NS) are each upscattered by hot electrons of a "Compton cloud" (hereafter the Comptb1 and Comptb2 components, respectively, which are associated with the similarly subscripted parameters). The photon power-law index Gamma(2) is almost constant (Gamma(2) similar to 2) for all spectral states. In turn, Gamma(1) demonstrates a two-phase behavior with the spectral state: Gamma(1) is quasi-constant at the level Gamma(1) similar to 2 for the HB-NB and Gamma(1) is less than 2, namely in the range of 1.3 < Gamma(1) < 2, when the source traces the FB. We also detect a decrease kT(s2) from 1.8 keV to 0.7 keV during the FB. We interpret this apparent quasi-stability of the indices during the HB-NB in the framework of the model in which the spectrum is determined by the Comptonized thermal components. This effect established for the Comptonized spectral components of the Z-source Sco X-1 is similar to what was previously found in the atoll sources 4U 1728-34, GX 3+1 and 4U 1820-30 and the Z-source GX 340+0 through all spectral states. However, we interpret the index reduction phase detected during the FB in Sco X-1 within the framework of a model in which the spectrum at the FB is determined by high radiation pressure from the NS surface. C1 [Titarchuk, Lev] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy. [Titarchuk, Lev] George Mason Univ, Fairfax, VA 22030 USA. [Titarchuk, Lev] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. [Seifina, Elena] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. [Shrader, Chris] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Shrader, Chris] Univ Space Res Assoc, Columbia, MD 21044 USA. RP Titarchuk, L (reprint author), Univ Ferrara, Dipartimento Fis, Via Saragat 1, I-44122 Ferrara, Italy. EM titarchuk@fe.infn.it; seif@sai.msu.ru; Chris.R.Shrader@nasa.gov NR 60 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2014 VL 789 IS 2 AR 98 DI 10.1088/0004-637X/789/2/98 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8JY UT WOS:000338674900007 ER PT J AU Ade, PAR Akiba, Y Anthony, AE Arnold, K Atlas, M Barron, D Boettger, D Borrill, J Chapman, S Chinone, Y Dobbs, M Elleflot, T Errard, J Fabbian, G Feng, C Flanigan, D Gilbert, A Grainger, W Halverson, NW Hasegawa, M Hattori, K Hazumi, M Holzapfel, WL Hori, Y Howard, J Hyland, P Inoue, Y Jaehnig, GC Jaffe, A Keating, B Kermish, Z Keskitalo, R Kisner, T Le Jeune, M Lee, AT Linder, E Leitch, EM Lungu, M Matsuda, F Matsumura, T Meng, X Miller, NJ Morii, H Moyerman, S Myers, MJ Navaroli, M Nishino, H Paar, H Peloton, J Quealy, E Rebeiz, G Reichardt, CL Richards, PL Ross, C Schanning, I Schenck, DE Sherwin, B Shimizu, A Shimmin, C Shimon, M Siritanasak, P Smecher, G Spieler, H Stebor, N Steinbach, B Stompor, R Suzuki, A Takakura, S Tomaru, T Wilson, B Yadav, A Zahn, O AF Ade, P. A. R. Akiba, Y. Anthony, A. E. Arnold, K. Atlas, M. Barron, D. Boettger, D. Borrill, J. Chapman, S. Chinone, Y. Dobbs, M. Elleflot, T. Errard, J. Fabbian, G. Feng, C. Flanigan, D. Gilbert, A. Grainger, W. Halverson, N. W. Hasegawa, M. Hattori, K. Hazumi, M. Holzapfel, W. L. Hori, Y. Howard, J. Hyland, P. Inoue, Y. Jaehnig, G. C. Jaffe, A. Keating, B. Kermish, Z. Keskitalo, R. Kisner, T. Le Jeune, M. Lee, A. T. Linder, E. Leitch, E. M. Lungu, M. Matsuda, F. Matsumura, T. Meng, X. Miller, N. J. Morii, H. Moyerman, S. Myers, M. J. Navaroli, M. Nishino, H. Paar, H. Peloton, J. Quealy, E. Rebeiz, G. Reichardt, C. L. Richards, P. L. Ross, C. Schanning, I. Schenck, D. E. Sherwin, B. Shimizu, A. Shimmin, C. Shimon, M. Siritanasak, P. Smecher, G. Spieler, H. Stebor, N. Steinbach, B. Stompor, R. Suzuki, A. Takakura, S. Tomaru, T. Wilson, B. Yadav, A. Zahn, O. CA POLARBEAR Collaboration TI Measurement of the Cosmic Microwave Background Polarization Lensing Power Spectrum with the POLARBEAR Experiment SO PHYSICAL REVIEW LETTERS LA English DT Article ID SOUTH-POLE TELESCOPE; DAMPING TAIL; 20 GHZ; ANISOTROPIES AB Gravitational lensing due to the large-scale distribution of matter in the cosmos distorts the primordial cosmic microwave background (CMB) and thereby induces new, small-scale B-mode polarization. This signal carries detailed information about the distribution of all the gravitating matter between the observer and CMB last scattering surface. We report the first direct evidence for polarization lensing based on purely CMB information, from using the four-point correlations of even- and odd-parity E- and B-mode polarization mapped over similar to 30 square degrees of the sky measured by the POLARBEAR experiment. These data were analyzed using a blind analysis framework and checked for spurious systematic contamination using null tests and simulations. Evidence for the signal of polarization lensing and lensing B modes is found at 4.2 sigma(stat + sys) significance. The amplitude of matter fluctuations is measured with a precision of 27%, and is found to be consistent with the Lambda cold dark matter cosmological model. This measurement demonstrates a new technique, capable of mapping all gravitating matter in the Universe, sensitive to the sum of neutrino masses, and essential for cleaning the lensing B-mode signal in searches for primordial gravitational waves. C1 [Ade, P. A. R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF10 3XQ, S Glam, Wales. [Akiba, Y.; Hasegawa, M.; Hazumi, M.; Inoue, Y.; Shimizu, A.] Grad Univ Adv Studies, Miura Dist, Kanagawa 2400115, Japan. [Anthony, A. E.; Halverson, N. W.; Jaehnig, G. C.; Schenck, D. E.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Arnold, K.; Atlas, M.; Barron, D.; Boettger, D.; Elleflot, T.; Feng, C.; Keating, B.; Matsuda, F.; Moyerman, S.; Navaroli, M.; Paar, H.; Schanning, I.; Shimon, M.; Siritanasak, P.; Stebor, N.; Wilson, B.; Yadav, A.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Borrill, J.; Errard, J.; Keskitalo, R.; Kisner, T.] Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 92093 USA. [Borrill, J.; Errard, J.; Kisner, T.; Linder, E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Chapman, S.; Ross, C.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. [Chinone, Y.; Hasegawa, M.; Hattori, K.; Hazumi, M.; Hori, Y.; Matsumura, T.; Morii, H.; Takakura, S.; Tomaru, T.] KEK, High Energy Accelerator Org, Tsukuba, Ibaraki 3050801, Japan. [Chinone, Y.; Flanigan, D.; Holzapfel, W. L.; Howard, J.; Lee, A. T.; Lungu, M.; Meng, X.; Myers, M. J.; Quealy, E.; Reichardt, C. L.; Richards, P. L.; Sherwin, B.; Shimmin, C.; Steinbach, B.; Suzuki, A.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Dobbs, M.; Gilbert, A.] McGill Univ, Dept Phys, Montreal, PQ H3A 0G4, Canada. [Fabbian, G.; Le Jeune, M.; Peloton, J.; Stompor, R.] Univ Paris Diderot, CNRS, IN2P3, CEA Irfu,Obs Paris,Sorbonne Paris Cite, Paris, France. [Fabbian, G.] SISSA, Int Sch Adv Studies, I-34014 Trieste, Italy. [Flanigan, D.] Columbia Univ, New York, NY 10027 USA. [Grainger, W.] STFC, Rutherford Appleton Lab, Swindon SN2 1SZ, Wilts, England. [Halverson, N. W.; Schenck, D. E.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.; Jaehnig, G. C.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Hazumi, M.; Nishino, H.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. [Howard, J.] Univ Oxford, Dept Phys, Oxford OX1 2JD, England. [Hyland, P.] Austin Coll, Dept Phys, Sherman, TX 75090 USA. [Jaffe, A.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England. [Kermish, Z.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Lee, A. T.; Linder, E.; Spieler, H.; Zahn, O.] Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 92093 USA. [Leitch, E. M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Leitch, E. M.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Miller, N. J.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Quealy, E.] Napa Valley Coll, Dept Phys, Napa, CA 94558 USA. [Rebeiz, G.] Univ Calif San Diego, Dept Elect & Comp Engn, La Jolla, CA 92093 USA. [Sherwin, B.] Univ Calif Berkeley, Miller Inst Basic Res Sci, Berkeley, CA 94720 USA. [Shimon, M.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Smecher, G.] Three Speed Log Inc, Vancouver, BC V6A 2J8, Canada. [Takakura, S.] Osaka Univ, Toyonaka, Osaka 5600043, Japan. RP Feng, C (reprint author), Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. EM cfeng@physics.ucsd.edu RI Holzapfel, William/I-4836-2015; OI Fabbian, Giulio/0000-0002-3255-4695; Reichardt, Christian/0000-0003-2226-9169 FU Office of Science, Office of High Energy Physics, of the U.S. Department of Energy [DE-AC0205CH11231]; Department of Energy [DE-AC0205-CH11231]; National Science Foundation [AST-0618398, AST-1212230]; MEXT KAKENHI [21111002]; KEK Cryogenics Science Center; Natural Sciences and Engineering Research Council; Canadian Institute for Advanced Research; Miller Institute for Basic Research in Science; NASA Postdoctoral Program; Simons Foundation; Joan and Irwin Jacobs FX This work was supported by the Director, Office of Science, Office of High Energy Physics, of the U.S. Department of Energy under Contract No. DE-AC0205CH11231. The computational resources required for this work were accessed via the GlideinWMS [36] on the Open Science Grid [37]. This project used the CAMB and FFTW software packages. Calculations were performed on the Department of Energy Open Science Grid at the University of California, San Diego, the Central Computing System, owned and operated by the Computing Research Center at KEK, and the National Energy Research Scientific Computing Center, which is supported by the Department of Energy under Contract No. DE-AC0205-CH11231. The POLARBEAR project is funded by the National Science Foundation under Grants No. AST-0618398 and No. AST-1212230. The KEK authors were supported by MEXT KAKENHI Grant No. 21111002, and acknowledge support from KEK Cryogenics Science Center. The McGill authors acknowledge funding from the Natural Sciences and Engineering Research Council and Canadian Institute for Advanced Research. We thank Marc Kamionkowski and Kim Griest for useful discussions and comments. B. D. S. acknowledges support from the Miller Institute for Basic Research in Science, N. M. acknowledges support from the NASA Postdoctoral Program, and K. A. acknowledges support from the Simons Foundation. M. S. gratefully acknowledges support from Joan and Irwin Jacobs. All silicon wafer-based technology for POLARBEAR was fabricated at the UC Berkeley Nanolab. We are indebted to our Chilean team members, Nolberto Oyarce and Jose Cortes. The James Ax Observatory operates in the Parque Astronomico Atacama in Northern Chile under the auspices of the Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT). Finally, we would like to acknowledge the tremendous contributions by Huan Tran to the POLARBEAR project. NR 37 TC 40 Z9 40 U1 1 U2 9 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 JUL 9 PY 2014 VL 113 IS 2 AR 021301 DI 10.1103/PhysRevLett.113.021301 PG 7 WC Physics, Multidisciplinary SC Physics GA AK9JM UT WOS:000338743400002 PM 25062161 ER PT J AU Rao, CV Soler, J Katiyar, R Shojan, J West, WC Katiyar, RS AF Rao, Chitturi Venkateswara Soler, Jesse Katiyar, Rajesh Shojan, Jifi West, William C. Katiyar, Ram S. TI Investigations on Electrochemical Behavior and Structural Stability of Li1.2Mn0.54Ni0.13Co0.13O2 Lithium-Ion Cathodes via in-Situ and ex-Situ Raman Spectroscopy SO JOURNAL OF PHYSICAL CHEMISTRY C LA English DT Article ID POSITIVE-ELECTRODE MATERIALS; SOLUTION LI2MNO3-LIMO2 M; LI-ION; IRREVERSIBLE CAPACITY; COMPOSITE ELECTRODES; BATTERY CATHODE; LAYERED OXIDE; HIGH-VOLTAGE; OXYGEN LOSS; MN AB In the present work, we performed electrochemical measurements to investigate Li (de)intercalation behavior and Raman spectroscopic studies to understand structural changes during charge-discharge processes and verify the structural stability after electrochemical cycling of the AlPO4-coated Li1.2Mn0.54Ni0.13Co0.13O2 composite cathode. Physicochemical characterization techniques confirmed the well-crystalline layered composite nature of the prepared material. Electrochemical measurements indicated high discharge capacities of similar to 230 and 160 mAh/g at C/20 and 1C, respectively, with good cycling performance. In-situ Raman spectroscopic studies revealed extraction of lithium and oxide ions from the lattice followed by rearrangement of cations during the first cycle charging process and extraction of oxide ions followed by insertion of lithium ions back in the structure without any major change during the discharging process. Ex-situ Raman and microscopic measurements on the cathode before and after electrochemical cycling indicated the structural stability of the material. Studies performed on the AlPO4-coated composite cathode demonstrate the possibility of using it as next-generation cathode material for advanced lithium-ion batteries. C1 [Rao, Chitturi Venkateswara; Katiyar, Rajesh; Shojan, Jifi; Katiyar, Ram S.] Univ Puerto Rico, Dept Phys, San Juan, PR 00936 USA. [Rao, Chitturi Venkateswara; Katiyar, Rajesh; Shojan, Jifi; Katiyar, Ram S.] Univ Puerto Rico, Inst Funct Nanomat, San Juan, PR 00936 USA. [Soler, Jesse; West, William C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Rao, CV (reprint author), Univ Puerto Rico, Dept Phys, San Juan, PR 00936 USA. EM vrao.chitturi@ymail.com; rkatiyar@hpcf.upr.edu FU NASA-URC [NNX10AQ17A] FX Financial support from a NASA-URC (NNX10AQ17A) grant to the University of Puerto Rico is gratefully acknowledged. This work was partially carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA's Space Power Systems Program. NR 43 TC 23 Z9 23 U1 4 U2 49 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1932-7447 J9 J PHYS CHEM C JI J. Phys. Chem. C PD JUL 3 PY 2014 VL 118 IS 26 BP 14133 EP 14141 DI 10.1021/jp501777v PG 9 WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary SC Chemistry; Science & Technology - Other Topics; Materials Science GA AK8QR UT WOS:000338693600008 ER PT J AU Huynh, HT Wang, ZJ Vincent, PE AF Huynh, H. T. Wang, Z. J. Vincent, P. E. TI High-order methods for computational fluid dynamics: A brief review of compact differential formulations on unstructured grids SO COMPUTERS & FLUIDS LA English DT Review DE Discontinuous Galerkin; High-order methods; Conservation laws; Flux Reconstruction; Correction procedure using reconstruction ID NAVIER-STOKES EQUATIONS; DISCONTINUOUS GALERKIN METHOD; CHEBYSHEV MULTIDOMAIN METHOD; ADVECTION-DIFFUSION PROBLEMS; RECONSTRUCTION SCHEMES; COMPRESSIBLE FLOWS; CONSERVATION-LAWS; EULER EQUATIONS; TURBULENT FLOWS; EXTENSION AB Popular high-order schemes with compact stencils for Computational Fluid Dynamics (CFD) include Discontinuous Galerkin (DG), Spectral Difference (SD), and Spectral Volume (SV) methods. The recently proposed Flux Reconstruction (FR) approach or Correction Procedure using Reconstruction (CPR) is based on a differential formulation and provides a unifying framework for these high-order schemes. Here we present a brief review of recent progress in FR/CPR research as well as some pacing items and future challenges. Published by Elsevier Ltd. C1 [Huynh, H. T.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. [Wang, Z. J.] Univ Kansas, Dept Aerosp Engn, Lawrence, KS 66045 USA. [Vincent, P. E.] Univ London Imperial Coll Sci Technol & Med, Dept Aeronaut, London, England. RP Huynh, HT (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM huynh@grc.nasa.gov; zjw@ku.edu; p.vincent@imperial.ac.uk RI Vincent, Peter/B-9288-2011 FU Aeronautical Sciences Project of NASA; AFOSR [FA95501210286]; NASA [NNX12AK04A] FX The first author was supported by the Aeronautical Sciences Project of NASA. He wishes to thank Drs. James DeBonis and Seth Spiegel for their thorough reviews and numerous valuable suggestions. The second author has been supported by AFOSR under Grant FA95501210286 and NASA under Grant NNX12AK04A. NR 65 TC 20 Z9 20 U1 2 U2 23 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0045-7930 EI 1879-0747 J9 COMPUT FLUIDS JI Comput. Fluids PD JUL 2 PY 2014 VL 98 SI SI BP 209 EP 220 DI 10.1016/j.compfluid.2013.12.007 PG 12 WC Computer Science, Interdisciplinary Applications; Mechanics SC Computer Science; Mechanics GA AJ8VM UT WOS:000337986000016 ER PT J AU Hoyt, DP AF Hoyt, Diana P. TI Innovation as Usual SO RESEARCH-TECHNOLOGY MANAGEMENT LA English DT Book Review C1 [Hoyt, Diana P.] NASA, Washington, DC 20546 USA. RP Hoyt, DP (reprint author), NASA, Washington, DC 20546 USA. EM diana.hoyt@nasa.gov NR 1 TC 0 Z9 0 U1 1 U2 1 PU INDUSTRIAL RESEARCH INST, INC PI ARLINGTON PA 2300 CLARENDON BLVD, STE 400, ARLINGTON, VA 22201 USA SN 0895-6308 EI 1930-0166 J9 RES TECHNOL MANAGE JI Res.-Technol. Manage. PD JUL-AUG PY 2014 VL 57 IS 4 BP 60 EP 63 PG 2 WC Business; Engineering, Industrial; Management SC Business & Economics; Engineering GA AK0IB UT WOS:000338095000016 ER PT J AU Brentner, KS Morris, PJ Lopes, LV AF Brentner, Kenneth S. Morris, Philip J. Lopes, Leonard V. TI A Method for Predicting the Noise of a Tip-Jet Driven Rotor SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY LA English DT Article ID SOUND; GENERATION; MOTION AB The use of tip-jets to provide the torque to power rotor blades has long been considered as an alternate approach to a shaft-driven rotor system. However, large tip-jet exit velocities are needed to provide sufficient jet thrust to power the rotor; hence, these jets can generate very large noise levels when compared to the usual sources of rotating blade noise. This paper demonstrates a new approach to predict the noise from such a design. The prediction method uses a derivative of the SAE ARP876 (Revision D) code to compute the tip-jet noise and PSU-WOPWOP to compute the rotational noise. Noise predictions for the Fairey Rotodyne aircraft are compared with acoustic measurements to provide a limited validation of the noise prediction method. The prediction method is also demonstrated through a brief investigation of design constraints and their impact on the rotor noise levels. C1 [Brentner, Kenneth S.; Morris, Philip J.] Penn State Univ, University Pk, PA 16802 USA. [Lopes, Leonard V.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Brentner, KS (reprint author), Penn State Univ, University Pk, PA 16802 USA. EM ksbrentner@psu.edu NR 20 TC 0 Z9 0 U1 2 U2 3 PU AMER HELICOPTER SOC INC PI ALEXANDRIA PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA SN 0002-8711 EI 2161-6027 J9 J AM HELICOPTER SOC JI J. Am. Helicopter Soc. PD JUL PY 2014 VL 59 IS 3 AR 032004 DI 10.4050/JAHS.59.032004 PG 10 WC Engineering, Aerospace SC Engineering GA AS6HX UT WOS:000344365900005 ER PT J AU Juhasz, O Syal, M Celi, R Khromov, V Rand, O Ruzicka, GC Strawn, RC AF Juhasz, Ondrej Syal, Monica Celi, Roberto Khromov, Vladimir Rand, Omri Ruzicka, Gene C. Strawn, Roger C. TI Comparison of Three Coaxial Aerodynamic Prediction Methods Including Validation with Model Test Data SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY LA English DT Article ID NAVIER-STOKES; ROTOR; WAKE; FLIGHT AB The paper presents the application of three aerodynamic prediction methods, covering a wide spectrum of sophistication and computational efficiency, to a model-scale coaxial rotor with highly twisted blades. The first method is based on blade-element momentum theory. The second is based on a free-vortex wake model, and the third is a computational fluid dynamics analysis based on Navier-Stokes solutions on structured grids. The results are compared with experimental data from model rotor tests in hover. There is generally good agreement between theory and experiment for the quantities considered, namely rotor thrust, torque, and inflow, but the results from the three methods differ in several important details. The best approach to coaxial rotor aerodynamic analysis judiciously combines the three predictive capabilities depending on the level of detail desired and uses a more sophisticated approach to calibrate and correct a simpler one. C1 [Juhasz, Ondrej; Syal, Monica; Celi, Roberto] Univ Maryland, Dept Aerosp Engn, College Pk, MD 20742 USA. [Khromov, Vladimir; Rand, Omri] Technion Israel Inst Technol, Fac Aerosp Engn, IL-32000 Haifa, Israel. [Ruzicka, Gene C.; Strawn, Roger C.] US Army Aeroflightdynam Directorate AMRDEC, Ames Res Ctr, Moffett Field, CA USA. RP Juhasz, O (reprint author), Univ Maryland, Dept Aerosp Engn, College Pk, MD 20742 USA. EM ojuhasz2@umd.edu NR 28 TC 1 Z9 1 U1 1 U2 1 PU AMER HELICOPTER SOC INC PI ALEXANDRIA PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA SN 0002-8711 EI 2161-6027 J9 J AM HELICOPTER SOC JI J. Am. Helicopter Soc. PD JUL PY 2014 VL 59 IS 3 AR 032006 DI 10.4050/JAHS.59.032006 PG 14 WC Engineering, Aerospace SC Engineering GA AS6HX UT WOS:000344365900007 ER PT J AU Lee-Rausch, EM Biedron, RT AF Lee-Rausch, Elizabeth M. Biedron, Robert T. TI FUN3D Airloads Predictions for the Full-Scale UH-60A Airloads Rotor in a Wind Tunnel SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY LA English DT Article ID GRIDS AB An unsteady Reynolds-averaged Navier-Stokes solver for unstructured grids, FUN3D, is used to compute the rotor performance and airloads of the UH-60A Airloads Rotor in the National Full-Scale Aerodynamic Complex (NFAC) 40- x 80-ft Wind Tunnel. The flow solver is loosely coupled to a rotorcraft comprehensive code, CAMRAD-II, to account for trim and aeroelastic deflections. Computations are made for the 1-g level flight speed-sweep test conditions with the airloads rotor installed on the NFAC Large Rotor Test Apparatus (LRTA) and in the 40- x 80-ft wind tunnel to determine the influence of the test stand and wind tunnel walls on the rotor performance and airloads. Detailed comparisons are made between the results of the computational fluid dynamics/computational structural dynamics (CFD/CSD) simulations and the wind tunnel measurements. The computed trends in solidity-weighted propulsive force and power coefficient match the experimental trends over the range of advance ratios and are comparable to previously published results. Rotor performance and sectional airloads show little sensitivity to the modeling of the wind tunnel walls, which indicates that the rotor shaft-angle correction adequately compensates for the wall influence up to an advance ratio of 0.37. Sensitivity of the rotor performance and sectional airloads to the modeling of the rotor with the LRTA body/hub increases with advance ratio. The inclusion of the LRTA in the simulation slightly improves the comparison of rotor propulsive force between the computation and wind tunnel data but does not resolve the difference in the rotor power predictions at an advance ratio of 0.37. Despite a more precise knowledge of the rotor trim loads and flight condition, the level of comparison between the computed and measured sectional airloads/pressures at an advance ratio of 0.37 is comparable to the results previously published for the high-speed flight test condition. C1 [Lee-Rausch, Elizabeth M.; Biedron, Robert T.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Lee-Rausch, EM (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM e.lee-rausch@nasa.gov NR 20 TC 2 Z9 2 U1 1 U2 2 PU AMER HELICOPTER SOC INC PI ALEXANDRIA PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA SN 0002-8711 EI 2161-6027 J9 J AM HELICOPTER SOC JI J. Am. Helicopter Soc. PD JUL PY 2014 VL 59 IS 3 AR 032002 DI 10.4050/JAHS.59.032002 PG 19 WC Engineering, Aerospace SC Engineering GA AS6HX UT WOS:000344365900003 ER PT J AU Takahashi, MD Whalley, MS Fletcher, JW Moralez, E Ott, CR Olmstead, MG AF Takahashi, Marc D. Whalley, Matthew S. Fletcher, Jay W. Moralez, Ernesto, III Ott, Carl R. Olmstead, Michael G. TI Development and Flight Testing of a Flight Control Law for Autonomous Operations Research on the RASCAL JUH-60A SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY LA English DT Article AB A critical element of rotorcraft autonomy is a flight control system that can operate harmoniously with the various autonomy components that depend on it. This is particularly true for highly interactive components, such as obstacle field navigation (OFN), where the vehicle navigation course is constantly being altered as more terrain information is gathered. This paper describes the development, integration, and flight-testing of an autonomous flight control system (AFCS) on a JUH-60A research helicopter. Flight-test results include control law validation using frequency domain analysis and performance characteristics using both ADS-33E mission task elements and path-error measurements. These performance data are then used to configure a risk minimizing OFN algorithm with the AFCS. The integrated OFN algorithm and AFCS are demonstrated in flight by navigating autonomously through 23 mi of mountainous terrain. C1 [Takahashi, Marc D.; Whalley, Matthew S.; Fletcher, Jay W.; Moralez, Ernesto, III; Ott, Carl R.; Olmstead, Michael G.] US Army Aviat Dev Directorate AFDD, Ctr Dev & Engn, Res Dev & Engn Command, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Takahashi, MD (reprint author), US Army Aviat Dev Directorate AFDD, Ctr Dev & Engn, Res Dev & Engn Command, Ames Res Ctr, Moffett Field, CA 94035 USA. EM marc.d.takahashi.civ@mail.mil NR 21 TC 1 Z9 1 U1 0 U2 3 PU AMER HELICOPTER SOC INC PI ALEXANDRIA PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA SN 0002-8711 EI 2161-6027 J9 J AM HELICOPTER SOC JI J. Am. Helicopter Soc. PD JUL PY 2014 VL 59 IS 3 AR 032007 DI 10.4050/JAHS.59.032007 PG 13 WC Engineering, Aerospace SC Engineering GA AS6HX UT WOS:000344365900008 ER PT J AU Trujillo, E Molotch, NP AF Trujillo, Ernesto Molotch, Noah P. TI Snowpack regimes of the Western United States SO WATER RESOURCES RESEARCH LA English DT Article ID TELEMETRY SNOTEL DATA; PACIFIC-NORTHWEST; TRENDS; PRECIPITATION; TEMPERATURE; SNOWMELT; SNOWFALL; AMERICA; IMPACTS; EVENTS AB Snow accumulation and melt patterns play a significant role in the water, energy, carbon, and nutrient cycles in the montane environments of the Western United States. Recent studies have illustrated that changes in the snow/rainfall apportionments and snow accumulation and melt patterns may occur as a consequence of changes in climate in the region. In order to understand how these changes may affect the snow regimes of the region, the current characteristics of the snow accumulation and melt patterns must be identified. Here we characterize the snow water equivalent (SWE) curve formed by the daily SWE values at 766 snow pillow stations in the Western United States, focusing on several metrics of the yearly SWE curves and the relationships between the different metrics. The metrics are the initial snow accumulation and snow disappearance dates, the peak snow accumulation and date of peak, the length of the snow accumulation season, the length of the snowmelt season, and the snow accumulation and snowmelt slopes. Three snow regimes emerge from these results: a maritime, an intermountain, and a continental regime. The maritime regime is characterized by higher maximum snow accumulations reaching 300 cm and shorter accumulation periods of less than 220 days. Conversely, the continental regime is characterized by lower maximum accumulations below 200 cm and longer accumulation periods reaching over 260 days. The intermountain regime lies in between. The regions that show the characteristics of the maritime regime include the Cascade Mountains, the Klamath Mountains, and the Sierra Nevada Mountains. The intermountain regime includes the Eastern Cascades slopes and foothills, the Blue Mountains, Northern and Central basins and ranges, the Columbia Mountains/Northern Rockies, the Idaho Batholith, and the Canadian Rockies. Lastly, the continental regime includes the Middle and Southern Rockies, and the Wasatch and Uinta Mountains. The implications of snow regime classification are discussed in the context of possible changes in accumulation and melt patterns associated with regional warming. C1 [Trujillo, Ernesto] Ecole Polytech Fed Lausanne, Sch Architecture Civil & Environm Engn, Lab Cryospher Sci, Lausanne, Switzerland. [Trujillo, Ernesto; Molotch, Noah P.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. [Molotch, Noah P.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA. [Molotch, Noah P.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Trujillo, E (reprint author), Ecole Polytech Fed Lausanne, Sch Architecture Civil & Environm Engn, Lab Cryospher Sci, Lausanne, Switzerland. EM Ernesto.Trujillo@epfl.ch RI Trujillo, Ernesto/A-6890-2013; Molotch, Noah/C-8576-2009 OI Trujillo, Ernesto/0000-0001-9731-7482; FU NASA [NNX11AK35A]; NSF [EAR 1032295, EAR 1141764, EAR 1331828]; USDA [2012-67003-19802]; NOAA RISA Western Water Assessment FX This research was supported by NASA grant NNX11AK35A, NSF grants EAR 1032295, EAR 1141764, and EAR 1331828, USDA grant 2012-67003-19802, and the NOAA RISA Western Water Assessment. Part of NPM's contributions to this study was carried out on behalf of the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 33 TC 10 Z9 10 U1 4 U2 41 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 JUL PY 2014 VL 50 IS 7 BP 5611 EP 5623 DI 10.1002/2013WR014753 PG 13 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA AQ2QG UT WOS:000342632000014 ER PT J AU Nearing, G AF Nearing, Grey TI Comment on "A blueprint for process-based modeling of uncertain hydrological systems" by Alberto Montanari and Demetris Koutsoyiannis SO WATER RESOURCES RESEARCH LA English DT Editorial Material ID DATA ASSIMILATION; FILTER C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Nearing, G (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM grey.s.nearing@nasa.gov NR 30 TC 3 Z9 3 U1 1 U2 8 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 JUL PY 2014 VL 50 IS 7 BP 6260 EP 6263 DI 10.1002/2013WR014812 PG 4 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA AQ2QG UT WOS:000342632000050 ER PT J AU Meyfroidt, P Carlson, KM Fagan, ME Gutierrez-Velez, VH Macedo, MN Curran, LM DeFries, RS Dyer, GA Gibbs, HK Lambin, EF Morton, DC Robiglio, V AF Meyfroidt, Patrick Carlson, Kimberly M. Fagan, Matthew E. Gutierrez-Velez, Victor H. Macedo, Marcia N. Curran, Lisa M. DeFries, Ruth S. Dyer, George A. Gibbs, Holly K. Lambin, Eric F. Morton, Douglas C. Robiglio, Valentina TI Multiple pathways of commodity crop expansion in tropical forest landscapes SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE land use displacement; deforestation drivers; indirect land use change; agricultural intensification; land sparing; market integration ID LAND-USE CHANGE; BRAZILIAN AMAZON; AGRICULTURAL INTENSIFICATION; PROTECTED AREAS; SOUTHEAST-ASIA; DEFORESTATION; GLOBALIZATION; DISPLACEMENT; CULTIVATION; LIVELIHOODS AB Commodity crop expansion, for both global and domestic urban markets, follows multiple land change pathways entailing direct and indirect deforestation, and results in various social and environmental impacts. Here we compare six published case studies of rapid commodity crop expansion within forested tropical regions. Across cases, between 1.7% and 89.5% of new commodity cropland was sourced from forestlands. Four main factors controlled pathways of commodity crop expansion: (i) the availability of suitable forestland, which is determined by forest area, agroecological or accessibility constraints, and land use policies, (ii) economic and technical characteristics of agricultural systems, (iii) differences in constraints and strategies between small-scale and large-scale actors, and (iv) variable costs and benefits of forest clearing. When remaining forests were unsuitable for agriculture and/or policies restricted forest encroachment, a larger share of commodity crop expansion occurred by conversion of existing agricultural lands, and land use displacement was smaller. Expansion strategies of large-scale actors emerge from context-specific balances between the search for suitable lands; transaction costs or conflicts associated with expanding into forests or other state-owned lands versus smallholder lands; net benefits of forest clearing; and greater access to infrastructure in already-cleared lands. We propose five hypotheses to be tested in further studies: (i) land availability mediates expansion pathways and the likelihood that land use is displaced to distant, rather than to local places; (ii) use of already-cleared lands is favored when commodity crops require access to infrastructure; (iii) in proportion to total agricultural expansion, large-scale actors generate more clearing of mature forests than smallholders; (iv) property rights and land tenure security influence the actors participating in commodity crop expansion, the form of land use displacement, and livelihood outcomes; (v) intensive commodity crops may fail to spare land when inducing displacement. We conclude that understanding pathways of commodity crop expansion is essential to improve land use governance. C1 [Meyfroidt, Patrick] Catholic Univ Louvain, Georges Lemaitre Ctr Earth & Climate Res, Earth & Life Inst, Louvain La Neuve, Belgium. [Meyfroidt, Patrick] Fonds Rech Sci FNRS, Brussels, Belgium. [Carlson, Kimberly M.] Univ Minnesota, Inst Environm, St Paul, MN 55108 USA. [Fagan, Matthew E.; DeFries, Ruth S.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY USA. [Gutierrez-Velez, Victor H.] Columbia Univ, Earth Inst, Ctr Environm Sustainabil, New York, NY USA. [Macedo, Marcia N.] Woods Hole Res Ctr, Falmouth, MA USA. [Curran, Lisa M.] Stanford Univ, Dept Anthropol, Stanford, CA 94305 USA. [Curran, Lisa M.] Stanford Univ, Woods Inst Environm, Stanford, CA 94305 USA. [Dyer, George A.] El Colegio Mexico, Mexico City, DF, Mexico. [Gibbs, Holly K.] Univ Wisconsin, Dept Geog, Madison, WI 53706 USA. [Gibbs, Holly K.] Univ Wisconsin, Nelson Inst Environm Studies, Madison, WI USA. [Lambin, Eric F.] Stanford Univ, Sch Earth Sci, Stanford, CA 94305 USA. [Lambin, Eric F.] Stanford Univ, Woods Inst, Stanford, CA 94305 USA. [Fagan, Matthew E.; Morton, Douglas C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Robiglio, Valentina] World Agroforestry Ctr ICRAF, Lima, Peru. ABT Associates Inc, Cambridge, MA 02138 USA. RP Meyfroidt, P (reprint author), Catholic Univ Louvain, Georges Lemaitre Ctr Earth & Climate Res, Earth & Life Inst, Louvain La Neuve, Belgium. EM patrick.meyfroidt@uclouvain.be RI Morton, Douglas/D-5044-2012; Gutierrez-Velez, Victor/B-6882-2012; Meyfroidt, Patrick/G-7768-2012; OI Meyfroidt, Patrick/0000-0002-1047-9794; Carlson, Kimberly/0000-0003-2162-1378 FU NASA [NNX08AU75H]; NSF [DG-1122492]; Gordon and Betty Moore Foundation; National Aeronautics and Space Administration (NASA); Norwegian Agency for Development Cooperation (Norad); United States Agency for International Development (USAID); Brazilian National Council for Scientific and Technological Development (CNPq); European Union through the FP 7 grant [226310]; US National Science Foundation under grant NSF [1125210] FX After the first author, authorship reflects the alphabetic listing of first authors of the original case studies, followed by an alphabetical listing of other co-authors. KMC was supported by NASA (NNX08AU75H), NSF (DG-1122492), and the Gordon and Betty Moore Foundation. Support for this research was provided by the National Aeronautics and Space Administration (NASA), the Norwegian Agency for Development Cooperation (Norad), the United States Agency for International Development (USAID), the Gordon and Betty Moore Foundation, the Brazilian National Council for Scientific and Technological Development (CNPq), and the European Union through the FP 7 grant 226310 REDD-Alert. Thanks to Roberto Porro, Doug White, Glenn Hyman, Konstantin Koenig for earlier discussions. Thanks to Erle Ellis and the entire GLOBE team for the help with the representativeness analysis. Assistance by the GLOBE project (http://globe.umbc.edu) was supported by the US National Science Foundation under grant NSF # 1125210. This study contributes to the Global Land Project. NR 75 TC 24 Z9 24 U1 12 U2 73 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 JUL PY 2014 VL 9 IS 7 AR 074012 DI 10.1088/1748-9326/9/7/074012 PG 13 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AP2AA UT WOS:000341873200013 ER PT J AU Zhang, F Wang, J Ichoku, C Hyer, EJ Yang, ZF Ge, C Su, SJ Zhang, XY Kondragunta, S Kaiser, JW Wiedinmyer, C da Silva, A AF Zhang, Feng Wang, Jun Ichoku, Charles Hyer, Edward J. Yang, Zhifeng Ge, Cui Su, Shenjian Zhang, Xiaoyang Kondragunta, Shobha Kaiser, Johannes W. Wiedinmyer, Christine da Silva, Arlindo TI Sensitivity of mesoscale modeling of smoke direct radiative effect to the emission inventory: a case study in northern sub-Saharan African region SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE fire emission inventory; Sahel and northern sub-Saharan African region; smoke radiative effect; mesoscale modeling; air quality ID TRANSPORT; AEROSOLS; AEROCOM; CLOUDS AB An ensemble approach is used to examine the sensitivity of smoke loading and smoke direct radiative effect in the atmosphere to uncertainties in smoke emission estimates. Seven different fire emission inventories are applied independently to WRF-Chem model (v3.5) with the same model configuration (excluding dust and other emission sources) over the northern sub-Saharan African (NSSA) biomass-burning region. Results for November and February 2010 are analyzed, respectively representing the start and end of the biomass burning season in the study region. For February 2010, estimates of total smoke emission vary by a factor of 12, but only differences by factors of 7 or less are found in the simulated regional (15 degrees W-42 degrees E, 13 degrees S-17 degrees N) and monthly averages of column PM2.5 loading, surface PM2.5 concentration, aerosol optical depth (AOD), smoke radiative forcing at the top-of-atmosphere and at the surface, and air temperature at 2 m and at 700 hPa. The smaller differences in these simulated variables may reflect the atmospheric diffusion and deposition effects to dampen the large difference in smoke emissions that are highly concentrated in areas much smaller than the regional domain of the study. Indeed, at the local scale, large differences (up to a factor of 33) persist in simulated smoke-related variables and radiative effects including semi-direct effect. Similar results are also found for November 2010, despite differences in meteorology and fire activity. Hence, biomass burning emission uncertainties have a large influence on the reliability of model simulations of atmospheric aerosol loading, transport, and radiative impacts, and this influence is largest at local and hourly-to-daily scales. Accurate quantification of smoke effects on regional climate and air quality requires further reduction of emission uncertainties, particularly for regions of high fire concentrations such as NSSA. C1 [Zhang, Feng; Wang, Jun; Yang, Zhifeng; Ge, Cui] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE 68588 USA. [Zhang, Feng] Chinese Acad Sci, Inst Atmospher Phys, Int Ctr Climate & Environm Sci, Beijing 100029, Peoples R China. [Ichoku, Charles; Hyer, Edward J.; da Silva, Arlindo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Naval Res Lab Monterey, Monterey, CA USA. [Su, Shenjian] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA. [Ge, Cui] Chinese Acad Sci, Inst Atmospher Phys, State Key Lab Atmospher Boundary Layer Phys & Atm, Beijing 100029, Peoples R China. [Zhang, Xiaoyang] S Dakota State Univ, Geospatial Sci Ctr Excellence, Brookings, SD USA. [Kondragunta, Shobha] NOAA, NESDIS, Ctr Satellite Applicat, Res Triangle Pk, NC USA. [Kaiser, Johannes W.] Kings Coll London, London WC2R 2LS, England. [Kaiser, Johannes W.] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England. [Kaiser, Johannes W.] Max Planck Inst Chem, D-55128 Mainz, Germany. [Wiedinmyer, Christine] Natl Ctr Atmospher Res, NCAR Earth Syst Lab, Div Atmospher Chem, Boulder, CO 80301 USA. RP Wang, J (reprint author), Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE 68588 USA. EM jwang7@unl.edu RI Hyer, Edward/E-7734-2011; Kaiser, Johannes/A-7057-2012; Kondragunta, Shobha/F-5601-2010; Ichoku, Charles/E-1857-2012; Ge, Cui/I-6353-2016; Wang, Jun/A-2977-2008 OI Hyer, Edward/0000-0001-8636-2026; Kaiser, Johannes/0000-0003-3696-9123; Kondragunta, Shobha/0000-0001-8593-8046; Ichoku, Charles/0000-0003-3244-4549; Ge, Cui/0000-0002-6182-6856; Wang, Jun/0000-0002-7334-0490 FU Science Missions Directorate of the National Aeronautics and Space Administration (NASA) as part of an Interdisciplinary Studies (IDS); NASA Air Quality Applied Science program; European Commission through the MACC-II project [283576]; EU Seventh Research Framework Programme; NCAR; US NSF Grant [121168]; National Science Foundation FX This research was supported by the Science Missions Directorate of the National Aeronautics and Space Administration (NASA) as part of an Interdisciplinary Studies (IDS) conducted through the Radiation Sciences Program managed by Hal B Maring. E J Hyer and J Wang also acknowledge the support from the NASA Air Quality Applied Science program managed by John A Haynes. J W Kaiser's contribution was funded by the European Commission through the MACC-II project, contract number 283576, under the EU Seventh Research Framework Programme. C Wiedinmyer would like to acknowledge support from NCAR and US NSF Grant # 121168. The National Center for Atmospheric Research is sponsored by the National Science Foundation. The authors thank Guido van der Werf for providing their emissions datasets, and gratefully acknowledge the Holland Computing Center of the University of Nebraska-Lincoln and their staff for their helpful efforts with modeling. NR 36 TC 11 Z9 11 U1 1 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 JUL PY 2014 VL 9 IS 7 AR 075002 DI 10.1088/1748-9326/9/7/075002 PG 14 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AP2AA UT WOS:000341873200022 ER PT J AU Dolecek, L Divsalar, D Sun, YZ Amiri, B AF Dolecek, Lara Divsalar, Dariush Sun, Yizeng Amiri, Behzad TI Non-Binary Protograph-Based LDPC Codes: Enumerators, Analysis, and Designs SO IEEE TRANSACTIONS ON INFORMATION THEORY LA English DT Article DE LDPC codes; nonbinary codes; protographs; weight enumerators; asymptotic analysis; pseudo-codewords; trapping sets; stopping sets; iterative decoding thresholds; EXIT chart analysis; finite-length code design ID PARITY-CHECK CODES; MINIMUM DISTANCE; FINITE-FIELDS; ENSEMBLES; CONSTRUCTION; LENGTHS; WEIGHT; BINARY AB This paper provides a comprehensive analysis of nonbinary low-density parity check (LDPC) codes built out of protographs. We consider both random and constrained edge-weight labeling, and refer to the former as the unconstrained nonbinary protograph-based LDPC codes (U-NBPB codes) and to the latter as the constrained nonbinary protograph-based LDPC codes (C-NBPB codes). Equipped with combinatorial definitions extended to the nonbinary domain, ensemble enumerators of codewords, trapping sets, stopping sets, and pseudocodewords are calculated. The exact enumerators are presented in the finite-length regime, and the corresponding growth rates are calculated in the asymptotic regime. An EXIT chart tool for computing the iterative decoding thresholds of protograph-based LDPC codes is presented, followed by several examples of finite-length U-NBPB and C-NBPB codes with high performance. Throughout this paper, we provide accompanying examples, which demonstrate the advantage of nonbinary protograph-based LDPC codes over their binary counterparts and over random constructions. The results presented in this paper advance the analytical toolbox of nonbinary graph-based codes. C1 [Dolecek, Lara; Sun, Yizeng; Amiri, Behzad] Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA. [Divsalar, Dariush] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Dolecek, L (reprint author), Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA. EM dolecek@ee.ucla.edu; divsalar@jpl.nasa.gov; sunyz@ucla.edu; amiri@ucla.edu FU Jet Propulsion Laboratory, California Institute of Technology through the National Aeronautics and Space Administration; National Science Foundation (NSF) through JPL [CCF-1161822, 82-17473]; NSF [CCF-1150212, CCF-1162501]; Advanced Storage Technology Consortium (ASTC) FX This work was supported in part by the Jet Propulsion Laboratory, California Institute of Technology, through the National Aeronautics and Space Administration, in part by the National Science Foundation (NSF) under Grant CCF-1161822 through JPL Task Plan 82-17473, in part by NSF under Grant CAREER CCF-1150212, in part by NSF under Grant CCF-1162501, and in part by the Advanced Storage Technology Consortium (ASTC). This paper was presented in part at the 2011 IEEE Military Communications Conference, 2011 and 2012 IEEE International Symposia on Information Theory, and 2011 and 2012 IEEE Information Theory Workshop. NR 62 TC 26 Z9 26 U1 1 U2 14 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9448 EI 1557-9654 J9 IEEE T INFORM THEORY JI IEEE Trans. Inf. Theory PD JUL PY 2014 VL 60 IS 7 BP 3913 EP 3941 DI 10.1109/TIT.2014.2316215 PG 29 WC Computer Science, Information Systems; Engineering, Electrical & Electronic SC Computer Science; Engineering GA AP3NG UT WOS:000341982200018 ER PT J AU Matthews, B Das, S Bhaduri, K Das, K Martin, R Oza, N AF Matthews, Bryan Das, Santanu Bhaduri, Kanishka Das, Kamalika Martin, Rodney Oza, Nikunj TI Discovering Anomalous Aviation Safety Events Using Scalable Data Mining Algorithms (vol 10, pg 467, 2013) SO JOURNAL OF AEROSPACE INFORMATION SYSTEMS LA English DT Correction C1 [Matthews, Bryan; Das, Santanu; Bhaduri, Kanishka; Das, Kamalika; Martin, Rodney; Oza, Nikunj] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Matthews, B (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 1 TC 0 Z9 0 U1 1 U2 4 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 1940-3151 EI 2327-3097 J9 J AEROSP INFORM SYST JI J. Aerosp. Inf. Syst. PD JUL PY 2014 VL 11 IS 7 BP 482 EP 482 DI 10.2514/1.I010211 PG 1 WC Engineering, Aerospace SC Engineering GA AP4RV UT WOS:000342066900006 ER PT J AU Carmona, A Pinte, C Thi, WF Benisty, M Menard, F Grady, C Kamp, I Woitke, P Olofsson, J Roberge, A Brittain, S Duchene, G Meeus, G Martin-Zaidi, C Dent, B Le Bouquin, JB Berger, JP AF Carmona, A. Pinte, C. Thi, W. F. Benisty, M. Menard, F. Grady, C. Kamp, I. Woitke, P. Olofsson, J. Roberge, A. Brittain, S. Duchene, G. Meeus, G. Martin-Zaidi, C. Dent, B. Le Bouquin, J. B. Berger, J. P. TI Constraining the structure of the transition disk HD 135344B (SAO 206462) by simultaneous modeling of multiwavelength gas and dust observations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE protoplanetary disks; stars: pre-main sequence; planets and satellites: formation; techniques: high angular resolution; techniques: interferometric; stars: individual: HD 135344B (SAO 206462) ID HERBIG AE/BE STARS; MAIN-SEQUENCE STARS; RADIATION THERMOCHEMICAL MODELS; YOUNG CIRCUMSTELLAR DISKS; INTERMEDIATE-MASS STARS; SPITZER-IRS SPECTRA; FAR-INFRARED LINES; VEGA-LIKE STARS; T-TAURI STARS; PROTOPLANETARY DISKS AB Context. Constraining the gas and dust disk structure of transition disks, particularly in the inner dust cavity, is a crucial step toward understanding the link between them and planet formation. HD 135344B is an accreting (pre-)transition disk that displays the CO 4.7 mu m emission extending tens of AU inside its 30 AU dust cavity. Aims. We constrain HD 135344B's disk structure from multi-instrument gas and dust observations. Methods. We used the dust radiative transfer code MCFOST and the thermochemical code ProDiMo to derive the disk structure from the simultaneous modeling of the spectral energy distribution (SED), VLT/CRIRES CO P(10) 4.75 mu m, Herschel/PACS [OI] 63 mu m, Spitzer/IRS, and JCMT (CO)-C-12 J = 3-2 spectra, VLTI/PIONIER H-band visibilities, and constraints from (sub)mm continuum interferometry and near-IR imaging. Results. We found a disk model able to describe the current gas and dust observations simultaneously. This disk has the following structure. (1) To simultaneously reproduce the SED, the near-IR interferometry data, and the CO ro-vibrational emission, refractory grains (we suggest carbon) are present inside the silicate sublimation radius (0.08 100 to account for the 870 pm continuum upper limit and the CO P(10) line flux, (5) The gas-to-dust ratio in the outer disk (30 30 cm. In the Bellingshausen, the thickest snow is found nearshore in both Octobers and is thickest next to the Abbot Ice Shelf. Snow depth is linearly related to freeboard when freeboards are low but diverge as the freeboard increases especially in the thicker/rougher ice of the western Weddell. We find correlations of 0.71-0.84 between snow depth and surface roughness suggesting preferential accumulation over deformed ice. Retrievals also seem to be related to radar backscatter through surface roughness. Snow depths reported here, generally higher than those from in situ records, suggest dissimilarities in sample populations. Implications of these differences on Antarctic sea ice thickness are discussed. C1 [Kwok, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Maksym, T.] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM ronald.kwok@jpl.nasa.gov RI Kwok, Ron/A-9762-2008 OI Kwok, Ron/0000-0003-4051-5896 NR 48 TC 12 Z9 13 U1 0 U2 3 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 JUL PY 2014 VL 119 IS 7 BP 4141 EP 4167 DI 10.1002/2014JC009943 PG 27 WC Oceanography SC Oceanography GA AN2LA UT WOS:000340415500007 ER PT J AU Lu, XM Hu, YX Trepte, C Zeng, S Churnside, JH AF Lu, Xiaomei Hu, Yongxiang Trepte, Charles Zeng, Shan Churnside, James H. TI Ocean subsurface studies with the CALIPSO spaceborne lidar SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID ATTENUATION COEFFICIENTS; OCEANOGRAPHIC LIDAR; SURFACE; WATER; PERFORMANCE; INFORMATION; SCATTERING; ALTIMETRY; SIGNALS; TAIL AB The primary objective of the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) mission is to study the climate impact of clouds and aerosols in the atmosphere. However, recent studies have demonstrated that CALIPSO also collects information about the ocean subsurface. The objective of this study is to estimate the ocean subsurface backscatter from CALIPSO lidar measurements. The effects of the lidar receiver's transient response on the attenuated backscatter were first removed in order to obtain the correct attenuated backscatter profile. The empirical relationship between sea surface lidar backscatter and wind speed was used to estimate the theoretical ocean surface backscatter. Then the two-way atmospheric transmittance was estimated as the ratio between the corrected ocean surface backscatter and the theoretical one. The ocean subsurface backscatter was finally derived from the subsurface attenuated backscatter divided by the two-way atmospheric transmittance. Significant relationships between integrated subsurface backscatter and chlorophyll-a concentration and between integrated subsurface backscatter and particulate organic carbon were found, which indicate a potential use of CALIPSO lidar to estimate global chlorophyll-a and particulate organic carbon concentrations. C1 [Lu, Xiaomei; Zeng, Shan] NASA, Langley Res Ctr, Postdoctoral Program, Hampton, VA 23665 USA. [Hu, Yongxiang; Trepte, Charles] NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23665 USA. [Churnside, James H.] NOAA, Earth Syst Res Lab, Boulder, CO USA. RP Hu, YX (reprint author), NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23665 USA. EM yongxiang.hu-1@nasa.gov RI Hu, Yongxiang/K-4426-2012; Churnside, James/H-4873-2013; Manager, CSD Publications/B-2789-2015 FU NASA FX This research was supported by Xiaomei Lu's appointment to the NASA Postdoctoral Program at the NASA Langley Research Center administered by Oak Ridge Associated University through a contract with NASA. She also thanks the Science Systems & Applications, Inc. (SSAI) in Hampton, VA for providing the office space and computer support. We would like to thank J. P. Matthews from Kyoto University and the anonymous reviewers for their substantial comments and suggestions that led to the improvement of this manuscript. CALIPSO data were obtained from NASA Langley Research Center Atmospheric Science Data Center (https://eosweb.larc.nasa.gov/HORDERBIN/HTML_Start.cgi). MODIS Aqua chlorophyll-a and POC concentrations were provided by the NASA Ocean Color Data Web (http://oceancolor.gsfc.nasa.gov). AMSR-E wind speed products were obtained from National Snow and Ice Data Center (NSIDC) Earth-Observing System Data Pool (ftp://n5eil01u.ecs.nsidc.org/SAN/AMSA/). The in situ diffuse attenuation data were from the NASA SeaBASS archive (http://seabass.gsfc.nasa.gov/). NR 33 TC 7 Z9 9 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 JUL PY 2014 VL 119 IS 7 BP 4305 EP 4317 DI 10.1002/2014JC009970 PG 13 WC Oceanography SC Oceanography GA AN2LA UT WOS:000340415500017 ER PT J AU Halekas, JS Poppe, AR McFadden, JP AF Halekas, J. S. Poppe, A. R. McFadden, J. P. TI The effects of solar wind velocity distributions on the refilling of the lunar wake: ARTEMIS observations and comparisons to one-dimensional theory SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID IN-CELL SIMULATIONS; PLASMA EXPANSION; VACUUM; FIELD; MOON; SPACECRAFT AB The lunar plasma wake refills from all directions, with processes operating both parallel and perpendicular to the magnetic field. The resulting wake structure depends sensitively on the properties of the flowing plasma, including the form of the ion and electron velocity distributions. In this manuscript, we discuss theoretical approximations for the refilling of the lunar wake along the magnetic field. While an often-used treatment for the parallel refilling assumes cold ions, one can derive solutions for arbitrary ion velocity distributions. Similarly, though the most tractable theory utilizes Maxwellian electrons, one can derive solutions for other types of distributions. We discuss the theoretical framework for various one-dimensional solutions, spanning the full range from cold-ion theories to gas-dynamic solutions, and utilizing both Maxwellian and kappa electron distributions. We compare these solutions to ARTEMIS observations of the lunar wake, for time periods with appropriate plasma parameters. We also present cases that reveal the inherent limitations of one-dimensional approximations, including those related to electron anisotropies and those related to perpendicular processes associated with both fluid flow and ion gyro-motion. C1 [Halekas, J. S.; Poppe, A. R.; McFadden, J. P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Halekas, J. S.; Poppe, A. R.] NASA, Ames Res Ctr, Solar Syst Explorat Res Virtual Inst, Moffett Field, CA 94035 USA. RP Halekas, JS (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM jazzman@ssl.berkeley.edu OI Halekas, Jasper/0000-0001-5258-6128 FU NASA's Solar System Exploration Research Virtual Institute [SSERVI-2014-096]; LADEE Guest Investigator program through NASA Grant [NNX13A071G]; NASA [NAS5-02099] FX We thank NASA's Solar System Exploration Research Virtual Institute (number SSERVI-2014-096) and the LADEE Guest Investigator program through NASA Grant NNX13A071G for support and also thank ISSI for hosting a workshop that inspired part of this work. We acknowledge NASA contract NAS5-02099 and V. Angelopoulos for use of data from ARTEMIS, and specifically K. H. Glassmeier, U. Auster, and W. Baumjohann for the use of FGM data. ARTEMIS data are publicly available at http://artemis.ssl.berkeley.edu and NASA's CDAWeb. NR 48 TC 4 Z9 4 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUL PY 2014 VL 119 IS 7 BP 5133 EP 5149 DI 10.1002/2014JA020083 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AN4HT UT WOS:000340549000003 ER PT J AU Alexander, RL O'Modhrain, S Roberts, DA Gilbert, JA Zurbuchen, TH AF Alexander, Robert L. O'Modhrain, Sile Roberts, D. Aaron Gilbert, Jason A. Zurbuchen, Thomas H. TI The bird's ear view of space physics: Audification as a tool for the spectral analysis of time series data SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SOLAR-WIND; MAGNETOSHEATH; STEREO AB The effective navigation, mining, and analysis of large time series data sets presents a recurring challenge throughout heliophysics. Audification, a specific form of auditory analysis commonly used in other fields of research (such as geoseismology), provides a promising technique for the evaluation of spectral features in long heliospheric time series data sets. Following a standard research methodology for the development of new analysis techniques, this paper presents a detailed case study in which audification was introduced into the working process of an experienced heliophysics research scientist and used for the identification and classification of features in high-resolution magnetometer data during a structured analysis task. Auditory evaluation successfully led to the detection of artificial, instrument-induced noise that was not previously observed by the scientist and also the identification of wave activity embedded within turbulent solar wind data. A follow-up interview indicated that the scientist continued using these auditory analysis methods in the assessment of every large data set during the 2 months after the study was completed. These findings indicate that audification can be valuable and enabling for researchers in forming a deeper understanding of both microstructures and macrostructures within large time series. Additionally, as both a standalone methodology and a supplement to visual analysis methods, audification can expedite certain stages of the data survey, analysis, and mining process and provide new qualitative insight into the spectral content of time-varying signals. C1 [Alexander, Robert L.; Gilbert, Jason A.; Zurbuchen, Thomas H.] Univ Michigan, Coll Engn, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Alexander, Robert L.] Univ Michigan, Coll Engn, Dept Design Sci, Ann Arbor, MI 48109 USA. [Alexander, Robert L.; O'Modhrain, Sile] Univ Michigan, Sch Mus Theatre & Dance, Dept Performing Arts Technol, Ann Arbor, MI 48109 USA. [Roberts, D. Aaron] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP Alexander, RL (reprint author), Univ Michigan, Coll Engn, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. EM robertalexandermusic@gmail.com RI Gilbert, Jason/I-9020-2012 OI Gilbert, Jason/0000-0002-3182-7014 FU NASA-Harriet G. Jenkins Predoctoral Fellowship Project (JPFP) award; California Institute of Technology through NASA [NNX13AH66G, 44A-1093998] FX R.L.A. has been supported, in part, by the NASA-Harriet G. Jenkins Predoctoral Fellowship Project (JPFP) award. T.H.Z. and J.A.G. have been supported, in part, by the California Institute of Technology through NASA grant NNX13AH66G with subcontract award 44A-1093998 to the University of Michigan. Deepest thanks to our participating research scientist for his large time investment and his invaluable insight at the center of this paper. We acknowledge the University of Michigan Design Science Program for supporting this collaborative research. R. L. A. also acknowledges helpful discussions with several individuals in the Solar and Heliospheric Research Group, the NASA Heliophysics Science Division, and A. McGowan. The data sets used in this paper are accessible through the CDAWeb data repository (maintained by NASA Goddard Space Flight Center); all audification examples can be accessed online through the University of Michigan's permanent data archive [Alexander, 2014b]. NR 45 TC 1 Z9 1 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 JUL PY 2014 VL 119 IS 7 BP 5259 EP 5271 DI 10.1002/2014JA020025 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AN4HT UT WOS:000340549000011 ER PT J AU Hwang, KJ Goldstein, ML Moore, TE Walsh, BM Baishev, DG Moiseyev, AV Shevtsov, BM Yumoto, K AF Hwang, K-J Goldstein, M. L. Moore, T. E. Walsh, B. M. Baishev, D. G. Moiseyev, A. V. Shevtsov, B. M. Yumoto, K. TI A tailward moving current sheet normal magnetic field front followed by an earthward moving dipolarization front SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CURRENT DISRUPTION; PARTICLE-ACCELERATION; SUBSTORM EXPANSION; GEOMAGNETIC TAIL; MAGNETOTAIL; DYNAMICS; EVENT; RECONNECTION; PROPAGATION; RESISTIVITY AB A case study is presented using measurements from the Cluster spacecraft and ground-based magnetometers that show a substorm onset propagating from the inner to outer plasma sheet. On 3 October 2005, Cluster, traversing an ion-scale current sheet at the near-Earth plasma sheet, detected a sudden enhancement of B-z, which was immediately followed by a series of flux rope structures. Both the local B-z enhancement and flux ropes propagated tailward. Approximately 5 min later, another B-z enhancement, followed by a large density decrease, was observed to rapidly propagate earthward. Between the two B-z enhancements, a significant removal of magnetic flux occurred, possibly resulting from the tailward moving B-z enhancement and flux ropes. In our scenario, this flux removal caused the magnetotail to be globally stretched so that the thinnest sheet formed tailward of Cluster. The thinned current sheet facilitated magnetic reconnection that quickly evolved from plasma sheet to lobe and generated the later earthward moving dipolarization front (DF) followed by a reduction in density and entropy. Ground magnetograms located near the meridian of Cluster's magnetic foot points show two-step bay enhancements. The positive bay associated with the first B-z enhancement indicates that the substorm onset signatures propagated from the inner to the outer plasma sheet, consistent with the Cluster observation. The more intense bay features associated with the later DF are consistent with the earthward motion of the front. The event suggests that current disruption signatures that originated in the near-Earth current sheet propagated tailward, triggering or facilitating midtail reconnection, thereby preconditioning the magnetosphere for a later strong substorm enhancement. C1 [Hwang, K-J; Goldstein, M. L.; Moore, T. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hwang, K-J] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA. [Walsh, B. M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Baishev, D. G.; Moiseyev, A. V.] Russian Acad Sci, Siberian Branch, Yu G Shafer Inst Cosmophys Res & Aeron, Yakutsk, Russia. [Shevtsov, B. M.] Russian Acad Sci, Far East Branch, Inst Cosmophys Res & Radio Wave Propagat, Paratunka, Russia. [Yumoto, K.] Kyushu Univ, Int Ctr Space Weather Sci & Educ, Fukuoka 812, Japan. [Yumoto, K.] Kyushu Univ, Dept Earth & Planetary Sci, Fukuoka 812, Japan. RP Hwang, KJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Kyoung-Joo.Hwang@nasa.gov RI Walsh, Brian/C-4899-2016; OI Walsh, Brian/0000-0001-7426-5413; Baishev, Dmitry/0000-0002-0229-5792 FU NASA's Magnetospheric Multiscale Mission Interdisciplinary Science (MMS/IDS) grant; Cluster mission; SB RAS [106]; RFBR [12-05-98522, 13-05-00363]; NASA [NNH12ZDA001N-GEO] FX K.J.H. and M. L. G. were supported, in part, by NASA's Magnetospheric Multiscale Mission Interdisciplinary Science (MMS/IDS) grant to the Goddard Space Flight Center and by the Cluster mission. T. E. M. participated with support from the MMS Mission. This work was partly supported by SB RAS project 106 and RFBR grant 12-05-98522 and RFBR grant 13-05-00363 (MAV). K.J.H. was supported, in part, by NASA grant NNH12ZDA001N-GEO. K.J.H. appreciates useful comments by H. Kawano. NR 50 TC 6 Z9 6 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 JUL PY 2014 VL 119 IS 7 BP 5316 EP 5327 DI 10.1002/2013JA019657 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AN4HT UT WOS:000340549000017 ER PT J AU Kozyra, JU Liemohn, MW Cattell, C De Zeeuw, D Escoubet, CP Evans, DS Fang, X Fok, MC Frey, HU Gonzalez, WD Hairston, M Heelis, R Lu, G Manchester, WB Mende, S Paxton, LJ Rastaetter, L Ridley, A Sandanger, M Soraas, F Sotirelis, T Thomsen, MW Tsurutani, BT Verkhoglyadova, O AF Kozyra, J. U. Liemohn, M. W. Cattell, C. De Zeeuw, D. Escoubet, C. P. Evans, D. S. Fang, X. Fok, M-C Frey, H. U. Gonzalez, W. D. Hairston, M. Heelis, R. Lu, G. Manchester, W. B. Mende, S. Paxton, L. J. Rastaetter, L. Ridley, A. Sandanger, M. Soraas, F. Sotirelis, T. Thomsen, M. W. Tsurutani, B. T. Verkhoglyadova, O. TI Solar filament impact on 21 January 2005: Geospace consequences SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID GREAT MAGNETIC STORM; DENSE-PLASMA SHEET; IONOSPHERIC ELECTRIC-FIELDS; LATITUDE BOUNDARY-LAYER; NEAR-EARTH MAGNETOTAIL; GLOBAL MHD SIMULATION; RICE CONVECTION MODEL; LATENT-HEAT RELEASE; 1-2 SEPTEMBER 1859; ART. NO. 1151 AB On 21 January 2005, a moderate magnetic storm produced a number of anomalous features, some seen more typically during superstorms. The aim of this study is to establish the differences in the space environment from what we expect (and normally observe) for a storm of this intensity, which make it behave in some ways like a superstorm. The storm was driven by one of the fastest interplanetary coronal mass ejections in solar cycle 23, containing a piece of the dense erupting solar filament material. The momentum of the massive solar filament caused it to push its way through the flux rope as the interplanetary coronal mass ejection decelerated moving toward 1 AU creating the appearance of an eroded flux rope (see companion paper by Manchester et al. (2014)) and, in this case, limiting the intensity of the resulting geomagnetic storm. On impact, the solar filament further disrupted the partial ring current shielding in existence at the time, creating a brief superfountain in the equatorial ionosphere-an unusual occurrence for a moderate storm. Within 1 h after impact, a cold dense plasma sheet (CDPS) formed out of the filament material. As the interplanetary magnetic field (IMF) rotated from obliquely to more purely northward, the magnetotail transformed from an open to a closed configuration and the CDPS evolved from warmer to cooler temperatures. Plasma sheet densities reached tens per cubic centimeter along the flanks-high enough to inflate the magnetotail in the simulation under northward IMF conditions despite the cool temperatures. Observational evidence for this stretching was provided by a corresponding expansion and intensification of both the auroral oval and ring current precipitation zones linked to magnetotail stretching by field line curvature scattering. Strong Joule heating in the cusps, a by-product of the CDPS formation process, contributed to an equatorward neutral wind surge that reached low latitudes within 1-2 h and intensified the equatorial ionization anomaly. Understanding the geospace consequences of extremes in density and pressure is important because some of the largest and most damaging space weather events ever observed contained similar intervals of dense solar material. C1 [Kozyra, J. U.; Liemohn, M. W.; De Zeeuw, D.; Manchester, W. B.; Ridley, A.] Univ Michigan, AOSS Dept, Ann Arbor, MI 48109 USA. [Cattell, C.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Escoubet, C. P.] ESA, Noordwijk, Netherlands. [Fang, X.] Univ Colorado Boulder, LASP, Boulder, CO USA. [Fok, M-C] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Frey, H. U.; Mende, S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Gonzalez, W. D.] INPE, Sao Jose Dos Campos, Brazil. [Hairston, M.; Heelis, R.] Univ Texas Dallas, William B Hanson Ctr Space Sci, Richardson, TX 75083 USA. [Lu, G.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Paxton, L. J.; Sotirelis, T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Rastaetter, L.] GSFC, Community Coordinated Modeling Ctr, Greenbelt, MD USA. [Sandanger, M.; Soraas, F.] Univ Bergen, Dept Phys & Technol, Birkeland Ctr Space Sci, Bergen, Norway. [Thomsen, M. W.] Los Alamos Natl Lab, Los Alamos, NM USA. [Tsurutani, B. T.; Verkhoglyadova, O.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Kozyra, JU (reprint author), Univ Michigan, AOSS Dept, Ann Arbor, MI 48109 USA. EM jukozyra@umich.edu RI Liemohn, Michael/H-8703-2012; Lu, Gang/A-6669-2011; Paxton, Larry/D-1934-2015; Rastaetter, Lutz/D-4715-2012; Manchester, Ward/I-9422-2012; Fang, Xiaohua/C-2773-2008; Ridley, Aaron/F-3943-2011 OI Sandanger, Marit Irene/0000-0002-9696-3527; Cattell, Cynthia/0000-0002-3805-320X; Hairston, Marc/0000-0003-4524-4837; Frey, Harald/0000-0001-8955-3282; Liemohn, Michael/0000-0002-7039-2631; Paxton, Larry/0000-0002-2597-347X; Rastaetter, Lutz/0000-0002-7343-4147; Fang, Xiaohua/0000-0002-6584-2837; Verkhoglyadova, Olga/0000-0002-9295-9539; Ridley, Aaron/0000-0001-6933-8534 FU NASA [NAG5-10297, NAG-10850, NNX10AQ34G, NNX09AI04G]; NSF [ATM-0090165, ATM 0903596]; NASA USPI-GOCE project [1549222]; NASA Heliophysics Guest Investigators program [NNH09AK621]; National Science Foundation FX The authors would like to thank the sources of funding for this study: NASA grants NAG5-10297 and NAG-10850, NNX10AQ34G, NNX09AI04G, and NSF grants ATM-0090165 and ATM 0903596. A portion of this research was performed at the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. The work at NCAR was supported in part by the NASA USPI-GOCE project under subcontract 1549222 and by the NASA Heliophysics Guest Investigators program under grant NNH09AK621. NCAR is sponsored by the National Science Foundation. Helpful discussions with A. F. Nagy and G. Rostoker are gratefully acknowledged. The authors would also like to thank all of their data providers. Simulations used in this work are available through the Community Coordinated Modeling Center's run archive at http://ccmc.gsfc.nasa.gov/results/index.php under the identifiers Derek_Andeweg_111608_1 and Derek Andeweg_111608_2, and runs with outputs at a 1 min cadence (Derek_Andeweg_111608_1a and Derek Andeweg_111608_2a) are also available on request. Special thanks is given to the developers of the VISBARD visualization software, the CSEM team for use of the SWMF global models, and the developers of the Virtual Modeling Repository (VMR). The ACE, TIMED GUVI, IMAGE HENA, IMAGE FUV, NOAA, LANL MPA, and FAST satellite observations used in this analysis were freely available through OMNIWeb (http://omniweb.gsfc.nasa.gov), CDAWeb (http://cdaweb.gsfc.nasa.gov/cdaweb/), and NASA's Heliophysics Virtual Observatories (http://hpde.gsfc.nasa.gov/hpde_data_access.html). Reprocessed ACE solar wind parameters during intervals of high background radiation during the 21-22 January 2005 storm were provided by Ruth Skoug (LANL) and Heather Elliott (SwRI). Primary access to the DMSP SSJ data was through the APL DMSP data server at http://sd-www.jhuapl.edu/Aurora/spectrogram/index.html, and to the DMSP SSIES data through a data server at the University of Texas at Dallas at http://cindispace.utdallas.edu/DMSP/. Double Star-1 datawere accessed through the Double Star Science Data Center at http://www.rssd. esa.int/index.php? project=DOUBLESTAR&page=data_ring and Cluster satellite data through the Cluster Active Archive at http://caa.estec.esa.int/caa/home.xml. NR 199 TC 6 Z9 6 U1 2 U2 15 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 JUL PY 2014 VL 119 IS 7 BP 5401 EP 5448 DI 10.1002/2013JA019748 PG 48 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AN4HT UT WOS:000340549000022 ER PT J AU Lyatskaya, S Khazanov, GV Zesta, E AF Lyatskaya, Sonya Khazanov, George V. Zesta, Eftyhia TI Interhemispheric field-aligned currents: Simulation results SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID HEIGHT-INTEGRATED CONDUCTIVITY; AURORAL PRECIPITATION POWER; CONJUGATE HEMISPHERES; HIGH-LATITUDES; MODEL; SUBSTORMS; JOULE; MAGNETOSPHERE; IONOSPHERE; SATELLITE AB We present simulation results of the 3-D magnetosphere-ionosphere current system including the Region 1 and Region 2 field-aligned currents, ionospheric currents, and interhemispheric field-aligned currents flowing between the northern and southern conjugate ionospheres in the case of asymmetry in ionospheric conductivities in two hemispheres. The model shows that the interhemispheric currents can be an important part of the global 3-D current system in high-latitude ionosphere, especially during summer-winter months, when in winter ionosphere they can be comparable and even exceed both Region 1 and Region 2 currents. An important feature of these interhemispheric currents is that they link together processes in two hemispheres, so that the currents observed in one hemisphere can provide us with information about the currents in the opposite hemisphere. Although the interhemispheric currents might play a notable role in the total 3-D current system, they have not been sufficiently studied yet. The study of the contribution from the interhemispheric currents into the total 3-D current system allows us to improve understanding and forecasting of geomagnetic, auroral, and ionospheric disturbances in two hemispheres. C1 [Lyatskaya, Sonya] Howard Community Coll, Columbia, MD 21044 USA. [Lyatskaya, Sonya; Khazanov, George V.; Zesta, Eftyhia] NASA GSFC, Greenbelt, MD USA. RP Lyatskaya, S (reprint author), Howard Community Coll, Columbia, MD 21044 USA. EM lyatsky@hotmail.com FU NSF Postdoctoral Fellowship, Office of Polar Programs, National Science Foundation [ANT-1204019] FX We greatly appreciate the help and many useful suggestions of Wladislaw Lyatsky. This study was fulfilled as a part of the NSF Postdoctoral Fellowship ANT-1204019 Office of Polar Programs, National Science Foundation. NR 60 TC 3 Z9 3 U1 0 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUL PY 2014 VL 119 IS 7 BP 5600 EP 5612 DI 10.1002/2013JA019558 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AN4HT UT WOS:000340549000033 ER PT J AU Imber, SM Slavin, JA Boardsen, SA Anderson, BJ Korth, H McNutt, RL Solomon, SC AF Imber, Suzanne M. Slavin, James A. Boardsen, Scott A. Anderson, Brian J. Korth, Haje McNutt, Ralph L., Jr. Solomon, Sean C. TI MESSENGER observations of large dayside flux transfer events: Do they drive Mercury's substorm cycle? SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID INTERPLANETARY MAGNETIC-FIELD; MAGNETOPAUSE STRUCTURE; EARTHS MAGNETOPAUSE; X-LINE; RECONNECTION; MAGNETOSPHERE; SIGNATURES; MODEL; INSTRUMENT; SPACECRAFT AB The large-scale dynamic behavior of Mercury's highly compressed magnetosphere is predominantly powered by magnetic reconnection, which transfers energy and momentum from the solar wind to the magnetosphere. The contribution of flux transfer events (FTEs) at the dayside magnetopause to the redistribution of magnetic flux in Mercury's magnetosphere is assessed with magnetic field data acquired in orbit about Mercury by the Magnetometer on the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft. FTEs with core fields greater than the planetary field just inside the magnetopause are prevalent at Mercury. Fifty-eight such large-amplitude FTEs were identified during February and May 2012, when MESSENGER sampled the subsolar magnetosheath. The orientation of each FTE was determined by minimum variance analysis, and the magnetic flux content of each was estimated using a force-free flux rope model. The average flux content of the FTEs was 0.06 MWb, and their durations imply a transient increase in the cross-polar cap potential of similar to 25 kV. For a substorm timescale of 2-3min, as indicated by magnetotail flux loading and unloading, the FTE repetition rate (10s) and average flux content (assumed to be 0.03 MWb) imply that FTEs contribute at least similar to 30% of the flux transport required to drive the Mercury substorm cycle. At Earth, in contrast, FTEs are estimated to contribute less than 2% of the substorm flux transport. This result implies that whereas at Earth, at which steady-state dayside reconnection is prevalent, multiple X-line dayside reconnection and associated FTEs at Mercury are a dominant forcing for magnetospheric dynamics. C1 [Imber, Suzanne M.; Slavin, James A.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Imber, Suzanne M.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Boardsen, Scott A.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. [Boardsen, Scott A.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Catonsville, MD USA. [Anderson, Brian J.; Korth, Haje; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DE USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. RP Imber, SM (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. EM si88@leicester.ac.uk RI McNutt, Ralph/E-8006-2010; Slavin, James/H-3170-2012 OI McNutt, Ralph/0000-0002-4722-9166; Slavin, James/0000-0002-9206-724X FU MESSENGER project; European Union [263325]; NASA [NASW-00002, NAS5-97271] FX S. M. Imber is supported by the MESSENGER project and the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement 263325. The MESSENGER project is supported by the NASA Discovery Program under contracts NASW-00002 to the Carnegie Institution of Washington and NAS5-97271 to The Johns Hopkins Applied Physics Laboratory. The data used in this study are available from the Planetary Data Center. NR 59 TC 17 Z9 17 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 JUL PY 2014 VL 119 IS 7 BP 5613 EP 5623 DI 10.1002/2014JA019884 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AN4HT UT WOS:000340549000034 ER PT J AU Morgan, DD Dieval, C Gurnett, DA Duru, F Dubinin, EM Franz, M Andrews, DJ Opgenoorth, HJ Ulusen, D Mitrofanov, I Plaut, JJ AF Morgan, D. D. Dieval, C. Gurnett, D. A. Duru, F. Dubinin, E. M. Fraenz, M. Andrews, D. J. Opgenoorth, H. J. Ulusen, D. Mitrofanov, I. Plaut, J. J. TI Effects of a strong ICME on the Martian ionosphere as detected by Mars Express and Mars Odyssey SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SOLAR-WIND CONDITIONS; NIGHTSIDE IONOSPHERE; CHARGED-PARTICLES; RADAR SOUNDINGS; MAGNETIC-FIELD; VENUS; VARIABILITY; DEPENDENCE; SPACECRAFT; EVENTS AB We present evidence of a substantial ionospheric response to a strong interplanetary coronal mass ejection (ICME) detected by the Mars Advanced Radar for Subsurface and Ionosphere Sounding (MARSIS) on board the Mars Express (MEX) spacecraft. A powerful ICME impacted the Martian ionosphere beginning on 5 June 2011, peaking on 6 June, and trailing off over about a week. This event caused a strong response in the charged particle detector of the High-Energy Neutron Detector (HEND) on board the Odyssey spacecraft. The ion mass spectrometer of the Analyzer of Space Plasmas and Energetic Atoms instrument on MEX detected an increase in background counts, simultaneous with the increase seen by HEND, due to the flux of solar energetic particles (SEPs) associated with the ICME. Local densities and magnetic field strengths measured by MARSIS and enhancements of 100 eV electrons denote the passing of an intense space weather event. Local density and magnetosheath electron measurements and remote soundings show compression of ionospheric plasma to lower altitudes due to increased solar wind dynamic pressure. MARSIS topside sounding of the ionosphere indicates that it is extended well beyond the terminator, to about 116 degrees solar zenith angle, in a highly disturbed state. This extension may be due to increased ionization due to SEPs and magnetosheath electrons or to plasma transport across the terminator. The surface reflection from both ionospheric sounding and subsurface modes of the MARSIS radar was attenuated, indicating increased electron content in the Mars ionosphere at low altitudes, where the atmosphere is dense. C1 [Morgan, D. D.; Dieval, C.; Gurnett, D. A.; Duru, F.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Dubinin, E. M.; Fraenz, M.] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany. [Andrews, D. J.; Opgenoorth, H. J.] Swedish Space Sci Inst, Uppsala, Sweden. [Ulusen, D.] Space Technol Res Inst, Ankara, Turkey. [Mitrofanov, I.] Russian Acad Sci, Space Sci Inst, Moscow, Russia. [Plaut, J. J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Morgan, DD (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. EM david-morgan@uiowa.edu RI Andrews, David/B-2591-2009 OI Andrews, David/0000-0002-7933-0322 FU International Space Science Institute (ISSI), Bern, CH, through the "Mars Induced Magnetosphere Team"; [1224107] FX We aknowledge support from the International Space Science Institute (ISSI), Bern, CH, through the "Mars Induced Magnetosphere Team," led by M. Lester. Data from Mars Express MARSIS AIS and ASPERA-3 ELS and IMA are available from the NASA Planetary Data System (PDS) Geosciences Node. Data from Odyssey Gamma Ray Spectrometer, High-Energy Neutron Detector, are also available from the NASA PDS Geosciences Node. This work was completed under contract 1224107 administered by the Jet Propulsion Laboratory. NR 56 TC 9 Z9 9 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 JUL PY 2014 VL 119 IS 7 BP 5891 EP 5908 DI 10.1002/2013JA019522 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AN4HT UT WOS:000340549000055 ER PT J AU Foley, S Fitzpatrick, G Briggs, MS Connaughton, V Tierney, D McBreen, S Dwyer, JR Chaplin, VL Bhat, PN Byrne, D Cramer, E Fishman, GJ Xiong, S Greiner, J Kippen, RM Meegan, CA Paciesas, WS Preece, RD von Kienlin, A Wilson-Hodge, C AF Foley, S. Fitzpatrick, G. Briggs, M. S. Connaughton, V. Tierney, D. McBreen, S. Dwyer, J. R. Chaplin, V. L. Bhat, P. N. Byrne, D. Cramer, E. Fishman, G. J. Xiong, S. Greiner, J. Kippen, R. M. Meegan, C. A. Paciesas, W. S. Preece, R. D. von Kienlin, A. Wilson-Hodge, C. TI Pulse properties of terrestrial gamma-ray flashes detected by the Fermi Gamma-Ray Burst Monitor SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID BREAKDOWN; AIR AB The Gamma-ray Burst Monitor (GBM) on board the Fermi Gamma-ray Space Telescope has triggered on over 300 terrestrial gamma-ray flashes (TGFs) since its launch in June 2008. With 14 detectors, GBM collects on average similar to 100 counts per triggered TGF, enabling unprecedented studies of the time profiles of TGFs. Here we present the first rigorous analysis of the temporal properties of a large sample of TGFs (278), including the distributions of the rise and fall times of the individual pulses and their durations. A variety of time profiles are observed with 19% of TGFs having multiple pulses separated in time and 31 clear cases of partially overlapping pulses. The effect of instrumental dead time and pulse pileup on the temporal properties are also presented. As the observed gamma ray pulse structure is representative of the electron flux at the source, TGF pulse parameters are critical to distinguish between relativistic feedback discharge and lightning leader models. We show that at least 67% of TGFs at satellite altitudes are significantly asymmetric. For the asymmetric pulses, the rise times are almost always shorter than the fall times. Those which are not are consistent with statistical fluctuations. The median rise time for asymmetric pulses is similar to 3 times shorter than for symmetric pulses while their fall times are comparable. The asymmetric shapes observed are consistent with the relativistic feedback discharge model when Compton scattering of photons between the source and Fermi is included, and instrumental effects are taken into account. C1 [Foley, S.; Fitzpatrick, G.; Tierney, D.; McBreen, S.; Byrne, D.] Univ Coll Dublin, Sch Phys, Belfield, Ireland. [Foley, S.; Greiner, J.; von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Briggs, M. S.; Connaughton, V.; Chaplin, V. L.; Bhat, P. N.; Xiong, S.; Preece, R. D.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. [Briggs, M. S.; Connaughton, V.; Preece, R. D.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Dwyer, J. R.; Cramer, E.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Fishman, G. J.] Jacobs Engn Inc, Huntsville, AL USA. [Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM USA. [Meegan, C. A.; Paciesas, W. S.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA. [Wilson-Hodge, C.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. RP Fitzpatrick, G (reprint author), Univ Coll Dublin, Sch Phys, Belfield, Ireland. EM Gerard.Fitzpatrick@ucdconnect.ie FU Irish Research Council for Science, Engineering and Technology; Marie Curie Actions under FP7; Irish Research Council; Fermi Guest Investigator Program; Science Foundation Ireland [09-RFP-AST-2400, 12/IP/1288]; DARPA [HR0011-1-10-1-0061] FX We thank the anonymous reviewers for their insightful comments. S. F. acknowledges the support of the Irish Research Council for Science, Engineering and Technology, cofunded by Marie Curie Actions under FP7. G. F. acknowledges the support of the Irish Research Council. The Fermi GBM Collaboration acknowledges support for GBM development, operations, and data analysis from NASA in the United States and from BMWi/DLR in Germany. M. S. B., V. C., and S. X. acknowledge support from the Fermi Guest Investigator Program. D. T. acknowledges support from Science Foundation Ireland under grant 09-RFP-AST-2400. S. M. B. acknowledges support from Science Foundation Ireland under grant 12/IP/1288. The work by J.D. has been supported in part by DARPA grant HR0011-1-10-1-0061. All GBM data used in this paper are available at http://fermi.gsfc.nasa.gov/ssc/data/access/gbm/. NR 35 TC 3 Z9 3 U1 0 U2 2 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 JUL PY 2014 VL 119 IS 7 BP 5931 EP 5942 DI 10.1002/2014JA019805 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AN4HT UT WOS:000340549000058 ER PT J AU de Muelenaere, S Frankl, A Haile, M Poesen, J Deckers, J Munro, N Veraverbeke, S Nyssen, J AF de Muelenaere, S. Frankl, A. Haile, M. Poesen, J. Deckers, J. Munro, N. Veraverbeke, S. Nyssen, J. TI HISTORICAL LANDSCAPE PHOTOGRAPHS FOR CALIBRATION OF LANDSAT LAND USE/COVER IN THE NORTHERN ETHIOPIAN HIGHLANDS SO LAND DEGRADATION & DEVELOPMENT LA English DT Article DE remote sensing; land use and land cover change; satellite imagery; Ethiopia; Tigray; terrestrial photographs ID CENTRAL PLATEAU REGION; COVER-CHANGE; CLASSIFICATION ACCURACY; SEDIMENT DEPOSITION; EROSION FEATURES; TIGRAY HIGHLANDS; STONE BUNDS; SOIL; DEGRADATION; IMPACT AB The combined effects of erosive rains, steep slopes and human land use have caused severe land degradation in the Ethiopian Highlands for several thousand years, but since the 1970s, however, land rehabilitation programmes have been established to try to reverse deterioration. In order to characterize and quantify the transformations in the north Ethiopian Highlands, a study was carried out over 8884 km(2) of the Tigray Highlands of northern Ethiopia. Using Landsat Multispectral Scanner and later Thematic Mapper imagery (1972, 1984/1986 and 2000), historical terrestrial photographs (1974-1975) and fieldwork (2008), we prepared land use and cover maps. For assessing the use of the historical terrestrial photographs, Landsat images from 1972 were classified using two different methods, namely conventional change detection (image differencing) and ground truthing (using the historical photographs of 1974-1975). Results show that the use of terrestrial photographs is promising, as the classification accuracy based on this method (Kappa coefficient 0.54) is better than the classification accuracy of the method based on image differencing (Kappa coefficient 0.46). Major land use and cover changes indicate the following: (1) a gradual but significant decline in bare ground (32 per cent in 1972 to 8 per cent in 2000); (2) a significant increase of bushland (25 to 43 per cent) and total forest area (including eucalypt plantations, 2.6 to 6.3 per cent); and (3) creation of numerous lakes and ponds. The dominant change trajectory (27 per cent of the study area) indicates a gradual or recent vegetation increase. These changes can be linked to the population growth and the introduction of land rehabilitation initiatives, complemented by growing awareness of land holders. Copyright (C) 2012 John Wiley & Sons, Ltd. C1 [de Muelenaere, S.; Frankl, A.; Nyssen, J.] Univ Ghent, Dept Geog, B-9000 Ghent, Belgium. [Haile, M.] Mekelle Univ, Dept Land Resource Management & Environm Protect, Mekelle, Ethiopia. [Poesen, J.; Deckers, J.] Katholieke Univ Leuven, Dept Earth & Environm Sci, B-3001 Heverlee, Belgium. [Munro, N.] Old Abbey Associates, Dirleton, East Lothian, Scotland. [Veraverbeke, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Nyssen, J (reprint author), Univ Ghent, Dept Geog, Krijgslaan 281-S8, B-9000 Ghent, Belgium. EM jan.nyssen@ugent.be RI Nyssen, Jan/B-8280-2009; frankl, amaury/J-5908-2012; Veraverbeke, Sander/H-2301-2012 OI Nyssen, Jan/0000-0002-2666-3860; Veraverbeke, Sander/0000-0003-1362-5125 FU Flemish Interuniversity Council (VLIR-UOS, Belgium); VLIR IUC Programme; Mekelle University; Belgian Science Policy's project 'Be-REDD-i' FX This research was partly funded by a travel grant of the Flemish Interuniversity Council (VLIR-UOS, Belgium) and supported by the VLIR IUC Programme with Mekelle University and the Belgian Science Policy's project 'Be-REDD-i'. Field assistants and local inhabitants contributed to the success of the fieldwork in Ethiopia. Ellen Meire's help and support during this research has been greatly appreciated. We sincerely thank Dr Tony Vanderstraeten for his methodological support in the remote sensing analysis. The useful suggestions by two anonymous reviewers and by Robert H. Webb are sincerely appreciated. NR 71 TC 17 Z9 17 U1 4 U2 14 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1085-3278 EI 1099-145X J9 LAND DEGRAD DEV JI Land Degrad. Dev. PD JUL-AUG PY 2014 VL 25 IS 4 BP 319 EP 335 DI 10.1002/ldr.2142 PG 17 WC Environmental Sciences; Soil Science SC Environmental Sciences & Ecology; Agriculture GA AN3NZ UT WOS:000340496500002 ER PT J AU Simpson, DG Vinas, AF AF Simpson, David G. Vinas, Adolfo F. TI NASA Computational Case Study: Modeling Planetary Magnetic and Gravitational Fields SO COMPUTING IN SCIENCE & ENGINEERING LA English DT Article AB In this case study, we model a planet's magnetic and gravitational fields using spherical harmonic functions. As an exercise, we analyze data on the Earth's magnetic field collected by NASA's MAGSAT spacecraft, and use it to derive a simple magnetic field model based on these spherical harmonic functions. C1 [Simpson, David G.; Vinas, Adolfo F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Simpson, DG (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM david.g.simpson@nasa.gov; adolfo.figueroa-vinas-1@nasa.gov NR 18 TC 0 Z9 0 U1 0 U2 2 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 JUL-AUG PY 2014 VL 16 IS 4 BP 73 EP 79 PG 7 WC Computer Science, Interdisciplinary Applications SC Computer Science GA AM7DU UT WOS:000340025700010 ER PT J AU Dacso, CC Johnson, CGH Read, ME AF Dacso, Clifford C. Johnson, Colonel Gregory H. Read, Michael E. TI Medical and Molecular Engineering SO IEEE PULSE LA English DT Editorial Material C1 [Dacso, Clifford C.] Baylor Coll Med, Houston, TX 77030 USA. [Dacso, Clifford C.] Inst Collaborat Hlth, Boston, MA USA. [Johnson, Colonel Gregory H.] Ctr Adv Sci Space, Huntsville, AL USA. [Read, Michael E.] NASA, ISS Natl Lab Off, Johnson Space Ctr, Los Angeles, CA USA. RP Dacso, CC (reprint author), Baylor Coll Med, Houston, TX 77030 USA. EM cdacso@bcm.edu NR 0 TC 0 Z9 0 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2154-2287 J9 IEEE PULSE JI IEEE Pulse PD JUL-AUG PY 2014 VL 5 IS 4 BP 12 EP 13 DI 10.1109/MPUL.2014.2321936 PG 2 WC Engineering, Biomedical SC Engineering GA AN0NL UT WOS:000340281200004 PM 25158338 ER PT J AU Roberts, MS AF Roberts, Michael S. TI Of Mice and Men SO IEEE PULSE LA English DT Article C1 [Roberts, Michael S.] Ctr Adv Sci Space, Nashville, TN USA. [Roberts, Michael S.] NASA, Washington, DC USA. RP Roberts, MS (reprint author), Ctr Adv Sci Space, Nashville, TN USA. EM mroberts@iss-casis.org NR 0 TC 0 Z9 0 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2154-2287 J9 IEEE PULSE JI IEEE Pulse PD JUL-AUG PY 2014 VL 5 IS 4 BP 42 EP 45 DI 10.1109/MPUL.2014.2321216 PG 4 WC Engineering, Biomedical SC Engineering GA AN0NL UT WOS:000340281200010 PM 25029681 ER PT J AU Smith, SM Zwart, SR Heer, M Hudson, EK Shackelford, L Morgan, JLL AF Smith, Scott M. Zwart, Sara R. Heer, Martina Hudson, Edgar K. Shackelford, Linda Morgan, Jennifer L. L. TI Men and Women in Space: Bone Loss and Kidney Stone Risk After Long-Duration Spaceflight SO JOURNAL OF BONE AND MINERAL RESEARCH LA English DT Article DE DXA; BIOCHEMICAL MARKERS OF BONE TURNOVER; EXERCISE; SEX DIFFERENCES; RENAL STONE RISK ID BED REST; NUTRITIONAL-STATUS; FLIGHT; BIOCHEMISTRY; EXERCISE; STATION; HUMANS; ASTRONAUTS; METABOLISM; MARKERS AB Bone loss, a key concern for long-duration space travelers, is typically considered a female issue. The number of women who have flown long-duration space missions is now great enough to allow a quantitative comparison of changes in bone and renal stone risk by sex. Participants were 42 astronauts (33 men and 9 women) on long-duration missions to the International Space Station. Bone mineral density (by dual-energy X-ray absorptiometry) and biochemical markers of bone metabolism (from blood and urine samples) were evaluated before and after flight. Data were analyzed in two groups, based on available resistance exercise equipment. Missions were 49 to 215 days in duration, flown between 2000 and 2012. The bone density response to spaceflight was the same for men and women in both exercise groups. The bone mineral density response to flight was the same for men and women, and the typical decrease in bone mineral density (whole body and/or regional) after flight was not observed for either sex for those using an advanced resistive exercise device. Biochemical markers of bone formation and resorption responded similarly in male and female astronauts. The response of urinary supersaturation risk to spaceflight was not significantly different between men and women, although risks were typically increased after flight in both groups, and risks were greater in men than in women before and after flight. The responses of men and women to spaceflight with respect to these measures of bone health were not different. c 2014 American Society for Bone and Mineral Research. C1 [Smith, Scott M.; Shackelford, Linda] NASA, Lyndon B Johnson Space Ctr, Human Hlth & Performance Directorate, Houston, TX 77058 USA. [Zwart, Sara R.] Univ Space Res Assoc, Div Space Life Sci, Houston, TX USA. [Heer, Martina] Univ Bonn, Inst Nutr Physiol, Bonn, Germany. [Hudson, Edgar K.] NASA, Lyndon B Johnson Space Ctr, JES Tech, Houston, TX 77058 USA. [Morgan, Jennifer L. L.] Oak Ridge Associated Univ, Houston, TX USA. [Morgan, Jennifer L. L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Smith, SM (reprint author), NASA, Lyndon B Johnson Space Ctr, Attn Mail Code SK3,2101 NASA Pkwy, Houston, TX 77058 USA. EM scott.m.smith@nasa.gov FU NASA Human Research Program; German Federal Ministry for Economics and Technology/DLR Forschung unter Weltraumbedingungen [50WB0931] FX This project was funded by the NASA Human Research Program and by a grant from the German Federal Ministry for Economics and Technology/DLR Forschung unter Weltraumbedingungen (50WB0931) to MH. NR 27 TC 18 Z9 21 U1 3 U2 16 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0884-0431 EI 1523-4681 J9 J BONE MINER RES JI J. Bone Miner. Res. PD JUL PY 2014 VL 29 IS 7 BP 1639 EP 1645 DI 10.1002/jbmr.2185 PG 7 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA AN0AO UT WOS:000340243600014 PM 24470067 ER PT J AU Nagol, JR Vermote, EF Prince, SD AF Nagol, Jyoteshwar R. Vermote, Eric F. Prince, Stephen D. TI Quantification of Impact of Orbital Drift on Inter-Annual Trends in AVHRR NDVI Data SO REMOTE SENSING LA English DT Article DE AVHRR; LTDR; NDVI; orbital drift; BRDF; MODIS; solar zenith angle ID DIFFERENCE VEGETATION INDEX; TIME-SERIES; PRODUCTS; MODIS AB The Normalized Difference Vegetation Index (NDVI) time-series data derived from Advanced Very High Resolution Radiometer (AVHRR) have been extensively used for studying inter-annual dynamics of global and regional vegetation. However, there can be significant uncertainties in the data due to incomplete atmospheric correction and orbital drift of the satellites through their active life. Access to location specific quantification of uncertainty is crucial for appropriate evaluation of the trends and anomalies. This paper provides per pixel quantification of orbital drift related spurious trends in Long Term Data Record (LTDR) AVHRR NDVI data product. The magnitude and direction of the spurious trends was estimated by direct comparison with data from MODerate resolution Imaging Spectrometer (MODIS) Aqua instrument, which has stable inter-annual sun-sensor geometry. The maps show presence of both positive as well as negative spurious trends in the data. After application of the BRDF correction, an overall decrease in positive trends and an increase in number of pixels with negative spurious trends were observed. The mean global spurious inter-annual NDVI trend before and after BRDF correction was 0.0016 and -0.0017 respectively. The research presented in this paper gives valuable insight into the magnitude of orbital drift related trends in the AVHRR NDVI data as well as the degree to which it is being rectified by the MODIS BRDF correction algorithm used by the LTDR processing stream. C1 [Nagol, Jyoteshwar R.; Prince, Stephen D.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Vermote, Eric F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Nagol, JR (reprint author), Univ Maryland, Dept Geog Sci, 2181 Samuel J LeFrak Hall, College Pk, MD 20742 USA. EM jnagol@umd.edu; eric.f.vermote@nasa.gov; sprince@umd.edu RI Nagol, Jyoteshwar/P-2026-2015 OI Nagol, Jyoteshwar/0000-0003-0497-7874 FU NASA Headquarters under NASA Earth and Space Science Fellowship Program [NNX07AN86H] FX This work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program-Grant "NNX07AN86H". NR 15 TC 5 Z9 5 U1 1 U2 8 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD JUL PY 2014 VL 6 IS 7 BP 6680 EP 6687 DI 10.3390/rs6076680 PG 8 WC Remote Sensing SC Remote Sensing GA AM7IE UT WOS:000340038700037 ER PT J AU Pearson, C Lim, T North, C Bendo, G Conversi, L Dowell, D Griffin, M Jin, T Laporte, N Papageorgiou, A Schulz, B Shupe, D Smith, AJ Xu, K AF Pearson, Chris Lim, Tanya North, Chris Bendo, George Conversi, Luca Dowell, Darren Griffin, Matt Jin, Terry Laporte, Nicolas Papageorgiou, Andreas Schulz, Bernhard Shupe, Dave Smith, Anthony J. Xu, Kevin TI SPIRE point source photometry: within the Herschel interactive processing environment (HIPE) SO EXPERIMENTAL ASTRONOMY LA English DT Article DE Herschel; SPIRE; Photometry; Calibration ID SOURCE EXTRACTION; CALIBRATION AB The different algorithms appropriate for point source photometry on data from the SPIRE instrument on-board the Herschel Space Observatory, within the Herschel Interactive Processing Environment (HIPE) are compared. Point source photometry of a large ensemble of standard calibration stars and dark sky observations is carried out using the 4 major methods within HIPE: SUSSEXtractor, DAOphot, the SPIRE Timeline Fitter and simple Aperture Photometry. Colour corrections and effective beam areas as a function of the assumed source spectral index are also included to produce a large number of photometric measurements per individual target, in each of the 3 SPIRE bands (250, 350, 500 mu m), to examine both the accuracy and repeatability of each of the 4 algorithms. It is concluded that for flux densities down to the level of 30mJy that the SPIRE Timeline Fitter is the method of choice. However, at least in the 250 and 350 mu m bands, all 4 methods provide photometric repeatability better than a few percent down to at approximately 100mJy. The DAOphot method appears in many cases to have a systematic offset of similar to 8 % in all SPIRE bands which may be indicative of a sub-optimal aperture correction. In general, aperture photometry is the least reliable method, i.e. largest scatter between observations, especially in the longest wavelength band. At the faintest fluxes, < 30mJy, SUSSEXtractor or DAOphot provide a better alternative to the Timeline Fitter. C1 [Pearson, Chris; Lim, Tanya] STFC Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England. [Pearson, Chris] Open Univ, Milton Keynes MK7 6AA, Bucks, England. [North, Chris; Griffin, Matt; Papageorgiou, Andreas] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, Wales. [Bendo, George] Univ Manchester, Sch Phys & Astron, UK ALMA Reg Ctr Node, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Conversi, Luca] ESA, ESAC, Herschel Sci Ctr, Madrid 28691, Spain. [Dowell, Darren] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Jin, Terry] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Laporte, Nicolas] Inst Astrofis Canarias, San Cristobal la Laguna 38205, Spain. [Schulz, Bernhard; Shupe, Dave; Xu, Kevin] NASA, IPAC, Herschel Sci Ctr, Pasadena, CA 91125 USA. [Smith, Anthony J.] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Smith, Anthony J.] Bluesky Spect, Lethbridge, AB, Canada. RP Pearson, C (reprint author), STFC Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England. EM chris.pearson@stfc.ac.uk FU CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA) FX The authors would like to thank the referee for providing valuable comments that improved the results of this paper. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). 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. NR 18 TC 6 Z9 6 U1 0 U2 1 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 JUL PY 2014 VL 37 IS 2 BP 175 EP 194 DI 10.1007/s10686-013-9351-4 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM4FA UT WOS:000339807300004 ER PT J AU Higgins, R Teyssier, D Borys, C Braine, J Comito, C Delforge, B Helmich, F Olberg, M Ossenkopf, V Pearson, J Shipman, R AF Higgins, Ronan Teyssier, David Borys, Colin Braine, Jonathan Comito, Claudia Delforge, Bertrand Helmich, Frank Olberg, Michael Ossenkopf, Volker Pearson, John Shipman, Russell TI The effect of sideband ratio on line intensity for Herschel/HIFI SO EXPERIMENTAL ASTRONOMY LA English DT Article DE HIFI; Herschel; Heterodyne; Calibration; Sideband ratio ID PERFORMANCE; INSTRUMENT; HIFI AB The Heterodyne Instrument for the Far Infrared (HIFI) on board the Herschel Space Observatory is composed of a set of fourteen double sideband mixers. We discuss the general problem of the sideband ratio (SBR) determination and the impact of an imbalanced sideband ratio on the line calibration in double sideband heterodyne receivers. The HIFI SBR is determined from a combination of data taken during pre-launch gas cell tests and in-flight. The results and some of the calibration artefacts discovered in the gas cell test data are presented here along with some examples of how these effects appear in science data taken in orbit. C1 [Higgins, Ronan; Comito, Claudia; Ossenkopf, Volker] Univ Cologne, Phys Inst 1, D-50937 Cologne, Germany. [Teyssier, David] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain. [Borys, Colin] CALTECH, Pasadena, CA 91125 USA. [Braine, Jonathan] Observ Bordeaux, LAB, F-33270 Floirac, France. [Delforge, Bertrand; Helmich, Frank; Shipman, Russell] Univ Groningen, Kapteyn Astron Inst, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Olberg, Michael] Chalmers Univ Technologym, Onsala Space Observ, S-43992 Onsala, Sweden. [Pearson, John] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Higgins, R (reprint author), Univ Cologne, Phys Inst 1, Zulpicher Str 77, D-50937 Cologne, Germany. EM higgins@ph1.uni-koeln.de NR 27 TC 4 Z9 4 U1 0 U2 5 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 JUL PY 2014 VL 37 IS 2 BP 433 EP 452 DI 10.1007/s10686-014-9382-5 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM4FA UT WOS:000339807300016 ER PT J AU Argus, DF Peltier, WR Drummond, R Moore, AW AF Argus, Donald F. Peltier, W. R. Drummond, R. Moore, Angelyn W. TI The Antarctica component of postglacial rebound model ICE-6G_C (VM5a) based on GPS positioning, exposure age dating of ice thicknesses, and relative sea level histories SO GEOPHYSICAL JOURNAL INTERNATIONAL LA English DT Article DE Satellite geodesy; Global change from geodesy; Glaciology; Dynamics of lithosphere and mantle; Antarctica ID GLACIAL ISOSTATIC-ADJUSTMENT; INTERGLACIAL CYCLE; MANTLE VISCOSITY; VICTORIA LAND; SPACE GEODESY; SHEET GROWTH; VM2 MODEL; GRACE; EARTH; BALANCE AB A new model of the deglaciation history of Antarctica over the past 25 kyr has been developed, which we refer to herein as ICE-6G_C (VM5a). This revision of its predecessor ICE-5G (VM2) has been constrained to fit all available geological and geodetic observations, consisting of: (1) the present day uplift rates at 42 sites estimated from GPS measurements, (2) ice thickness change at 62 locations estimated from exposure-age dating, (3) Holocene relative sea level histories from 12 locations estimated on the basis of radiocarbon dating and (4) age of the onset of marine sedimentation at nine locations along the Antarctic shelf also estimated on the basis of C-14 dating. Our new model fits the totality of these data well. An additional nine GPS-determined site velocities are also estimated for locations known to be influenced by modern ice loss from the Pine Island Bay and Northern Antarctic Peninsula regions. At the 42 locations not influenced by modern ice loss, the quality of the fit of postglacial rebound model ICE-6G_C (VM5A) is characterized by a weighted root mean square residual of 0.9 mm yr(-1). The Southern Antarctic Peninsula is inferred to be rising at 2 mm yr(-1), requiring there to be less Holocene ice loss there than in the prior model ICE-5G (VM2). The East Antarctica coast is rising at approximately 1 mm yr(-1), requiring ice loss from this region to have been small since Last Glacial Maximum. The Ellsworth Mountains, at the base of the Antarctic Peninsula, are inferred to be rising at 5-8 mm yr(-1), indicating large ice loss from this area during deglaciation that is poorly sampled by geological data. Horizontal deformation of the Antarctic Plate is minor with two exceptions. First, O'Higgins, at the tip of the Antarctic Peninsula, is moving southeast at a significant 2 mm yr(-1) relative to the Antarctic Plate. Secondly, the margins of the Ronne and Ross Ice Shelves are moving horizontally away from the shelf centres at an approximate rate of 0.8 mm yr(-1), in viscous response to the early Holocene unloading of ice from the current locations of the ice shelf centers. ICE-6G_C (VM5A) fits the horizontal observations well (wrms residual speed of 0.7 mm yr(-1)), there being no need to invoke any influence of lateral variation inmantle viscosity. ICE-6G_C (VM5A) differs in several respects from the recently published W12A model of Whitehouse et al. First, the upper-mantle viscosity in VM5a is 5 x 10(20) Pa s, half that in W12A. The VM5a profile, which is identical to that inferred on the basis of the Fennoscandian relaxation spectrum, North American relative sea level histories and Earth rotation constraints, when coupled with the revised ICE-6G_C deglaciation history, fits all of the available constraints. Secondly, the net contribution of Antarctica ice loss to global sea level rise is 13.6 m, 2/3 greater than the 8 m in W12A. Thirdly, ice loss occurs quickly from 12 to 5 ka, and the contribution to global sea level rise during Meltwater Pulse 1B (11.5 ka) is large (5 m), consistent with sedimentation constraints from cores from the Antarctica ice shelf. Fourthly, in ICE-6G_C there is no ice gain in the East Antarctica interior, as there is in W12A. Finally, the new model of Antarctic deglaciation reconciles the global constraint upon the global mass loss during deglaciation provided by the Barbados record of relative sea level history when coupled with the Northern Hemisphere counterpart of this new model. C1 [Argus, Donald F.; Moore, Angelyn W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Peltier, W. R.; Drummond, R.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. RP Argus, DF (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Donald.F.Argus@jpl.nasa.gov RI Peltier, William/A-1102-2008 FU NASA; NSERC [A9627]; NOAA [NA110AR4310101] FX We are grateful to Michael Heflin, Susan Owen, Shailen Desai and all members of JPL's GPS positioning team. We are grateful to Michael Craymer for sharing results from the Canadian Base Network. We thank Michael Bevis, Alessandro Capra, Luca Vittuari, Eugene Domack, Christoph Knoefel, Matt King, John Dawson, Michael Moore, Ryan Ruddick, Lars Sjoberg and Terry Wilson for sharing GPS Rinex files. We are grateful to reviewer Matt King for extensive insight and suggestions on the submitted manuscript. We are thankful also to two anonymous reviewers who helped improve the study. We acknowledge contribution from the International GPS Service, UNAVCO and SOPAC. Research by Argus and Moore was performed at Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Research by Peltier and Drummond at the University of Toronto is supported by NSERC Discovery Grant A9627 to WRP and by NOAA grant NA110AR4310101. The construction of models of glacial isostatic rebound at the University of Toronto has employed the SciNet facility for high performance computation, which is a component of the Compute Canada HPC platform. NR 92 TC 42 Z9 43 U1 4 U2 51 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0956-540X EI 1365-246X J9 GEOPHYS J INT JI Geophys. J. Int. PD JUL PY 2014 VL 198 IS 1 BP 537 EP 563 DI 10.1093/gji/ggu140 PG 27 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AM2YI UT WOS:000339717200038 ER PT J AU Smith, HD Mckay, CP Duncan, AG Sims, RC Anderson, AJ Grossl, PR AF Smith, Heather D. Mckay, Christopher P. Duncan, Andrew G. Sims, Ronald C. Anderson, Anne J. Grossl, Paul R. TI An instrument design for non-contact detection of biomolecules and minerals on Mars using fluorescence SO JOURNAL OF BIOLOGICAL ENGINEERING LA English DT Article ID LASER-INDUCED FLUORESCENCE; NATIVE FLUORESCENCE; RAMAN-SPECTROSCOPY; ORGANIC-MOLECULES; EMISSION LIFE; REMOTE RAMAN; EARLY EARTH; METEORITES; DELIVERY; SYSTEM AB We discuss fluorescence as a method to detect polycyclic aromatic hydrocarbons and other organic molecules, as well as minerals on the surface of Mars. We present an instrument design that is adapted from the ChemCam instrument which is currently on the Mars Science Lander Rover Curiosity and thus most of the primary components are currently flight qualified for Mars surface operations, significantly reducing development costs. The major change compared to ChemCam is the frequency multipliers of the 1064 nm laser to wavelengths suitable for fluorescence excitation (266 nm, 355 nm, and 532 nm). We present fluorescence spectrum for a variety of organics and minerals relevant to the surface of Mars. Preliminary results show minerals already known on Mars, such as perchlorate, fluoresce strongest when excited by 355 nm. Also we demonstrate that polycyclic aromatic hydrocarbons, such as those present in Martian meteorites, are highly fluorescent at wavelengths in the ultraviolet (266 nm, 355 nm), but not as much in the visible (532 nm). We conclude that fluorescence can be an important method for Mars applications and standoff detection of organics and minerals. The instrument approach described in this paper builds on existing hardware and offers high scientific return for minimal cost for future missions. C1 [Smith, Heather D.; Sims, Ronald C.] Utah State Univ, Dept Biol Engn, Logan, UT 84322 USA. [Smith, Heather D.; Mckay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Anderson, Anne J.] Utah State Univ, Dept Biol, Logan, UT 84322 USA. [Grossl, Paul R.] Utah State Univ, Dept Plants Soils & Climate, Logan, UT 84322 USA. RP Smith, HD (reprint author), Utah State Univ, Dept Biol Engn, Logan, UT 84322 USA. EM hdsmith@aggiemail.usu.edu FU NASA Planetary Protection Program; NASA Graduate Student Research Program; Planetary Protection Program FX The authors would like to thank Dr. Charlie Miller of the USU Biological and Irrigation Engineering department for use of the Shimadzu 1501 Fluorometer. Dr. John Shervais and Marlon Jean of the USU Geology Department for access to the mineralogy and petrology collection, and to Dr. Chris Lloyd for helpful discussions. CPM was supported through funding from the NASA Planetary Protection Program. HDS is grateful for the NASA Graduate Student Research Program and the Planetary Protection Program for funding this research. NR 39 TC 3 Z9 4 U1 5 U2 16 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1754-1611 J9 J BIOL ENG JI J. Biol. Eng. PD JUL 1 PY 2014 VL 8 AR 16 DI 10.1186/1754-1611-8-16 PG 14 WC Biochemical Research Methods; Biotechnology & Applied Microbiology SC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology GA AM4OA UT WOS:000339833400002 PM 25057291 ER PT J AU Louis, T Addison, GE Hasselfield, M Bond, JR Calabrese, E Das, S Devlin, MJ Dunkley, J Dunner, R Gralla, M Hajian, A Hincks, AD Hlozek, R Huffenberger, K Infante, L Kosowsky, A Marriage, TA Moodley, K Naess, S Niemack, MD Nolta, MR Page, LA Partridge, B Sehgal, N Sievers, JL Spergel, DN Staggs, ST Walter, BZ Wollack, EJ AF Louis, Thibaut Addison, Graeme E. Hasselfield, Matthew Bond, J. Richard Calabrese, Erminia Das, Sudeep Devlin, Mark J. Dunkley, Joanna Duenner, Rolando Gralla, Megan Hajian, Amir Hincks, Adam D. Hlozek, Renee Huffenberger, Kevin Infante, Leopoldo Kosowsky, Arthur Marriage, Tobias A. Moodley, Kavilan Naess, Sigurd Niemack, Michael D. Nolta, Michael R. Page, Lyman A. Partridge, Bruce Sehgal, Neelima Sievers, Jonathan L. Spergel, David N. Staggs, Suzanne T. Walter, Benjamin Z. Wollack, Edward J. TI The Atacama Cosmology Telescope: cross correlation with Planck maps SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE CMBR experiments; CMBR detectors; cosmological parameters from CMBR ID PROBE WMAP OBSERVATIONS; POWER SPECTRUM; MICROWAVE AB We present the temperature power spectrum of the Cosmic Microwave Background obtained by cross-correlating maps from the Atacama Cosmology Telescope (ACT) at 148 and 218 GHz with maps from the Planck satellite at 143 and 217 GHz, in two overlapping regions covering 592 square degrees. We find excellent agreement between the two datasets at both frequencies, quantified using the variance of the residuals between the ACT power spectra and the ACT x Planck cross-spectra. We use these cross-correlations to measure the calibration of the ACT data at 148 and 218 GHz relative to Planck, to 0.7% and 2% precision respectively. We find no evidence for anisotropy in the calibration parameter. We compare the Planck 353 GHz power spectrum with the measured amplitudes of dust and cosmic infrared background (CIB) of ACT data at 148 and 218 GHz. We also compare planet and point source measurements from the two experiments. C1 [Louis, Thibaut; Calabrese, Erminia; Dunkley, Joanna; Naess, Sigurd] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Addison, Graeme E.; Hincks, Adam D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada. [Hasselfield, Matthew; Hlozek, Renee; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Bond, J. Richard; Hajian, Amir; Nolta, Michael R.; Sievers, Jonathan L.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Das, Sudeep] Argonne Natl Lab, Lemont, IL 60439 USA. [Devlin, Mark J.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Duenner, Rolando; Infante, Leopoldo] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile. [Gralla, Megan; Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Marriage, Tobias A.; Niemack, Michael D.; Page, Lyman A.; Spergel, David N.; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Huffenberger, Kevin] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Moodley, Kavilan; Sievers, Jonathan L.] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa. [Niemack, Michael D.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA. [Partridge, Bruce; Walter, Benjamin Z.] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. [Sehgal, Neelima] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Louis, T (reprint author), Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. EM Thibaut.Louis@astro.ox.ac.uk RI Wollack, Edward/D-4467-2012; OI Wollack, Edward/0000-0002-7567-4451; Sievers, Jonathan/0000-0001-6903-5074; Huffenberger, Kevin/0000-0001-7109-0099 FU U.S. National Science Foundation [AST-0408698, AST-0965625]; Princeton University; University of Pennsylvania; Canada Foundation for Innovation (CFI); Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT); CFI under Compute Canada; CFI under Government of Ontario; CFI under Ontario Research Fund - Research Excellence; University of Toronto; ERC [259505]; NASA Office of Space Science; [PHY-0855887]; [PHY-1214379] FX This work was supported by the U.S. National Science Foundation through awards AST-0408698 and AST-0965625 for the ACT project, as well as awards PHY-0855887 and PHY-1214379. Funding was also provided by Princeton University, the University of Pennsylvania, and a Canada Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque Astronomico Atacama in northern Chile under the auspices of the Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT). 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. Funding from ERC grant 259505 supports JD, EC, SN and TL. We thank George Efstathiou and Duncan Hanson for discussions about the Planck data. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. NR 26 TC 6 Z9 6 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD JUL PY 2014 IS 7 AR 016 DI 10.1088/1475-7516/2014/07/016 PG 16 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AM4DL UT WOS:000339802700017 ER PT J AU Fryauf, DM Zhang, J Norris, KJ Leon, JJD Oye, MM Wei, M Kobayashi, NP AF Fryauf, David M. Zhang, Junce Norris, Kate J. Leon, Juan J. Diaz Oye, Michael M. Wei, Min Kobayashi, Nobuhiko P. TI Photoluminescence blue shift of indium phosphide nanowire networks with aluminum oxide coating SO PHYSICA STATUS SOLIDI-RAPID RESEARCH LETTERS LA English DT Article DE indium phosphide nanowire; atomic layer deposition; aluminum oxide; photoluminescence; Burstein-Moss shift ID DEPENDENT PHOTOLUMINESCENCE; INP NANOWIRES; SURFACE AB This paper describes our finding that optical properties of semiconductor nanowires were modified by depositing a thin layer of metal oxide. Indium phosphide nanowires were grown by metal organic chemical vapor deposition on silicon substrates with gold catalyst resulting in three-dimensional nanowire networks, and optical properties were obtained from the collective nanowire networks. The networks were coated with an aluminum oxide thin film deposited by plasma-enhanced atomic layer deposition. We studied the dependence of the peak wavelength of photoluminescence spectra on the thickness of the oxide coatings. A continuous blue shift in photoluminescence spectra was observed when the thickness of the oxide coating was increased. The observed blue shift is attributed to the Burstein-Moss effect due to increased carrier concentration in the nanowire cores caused by repulsion from intrinsic negative fixed charges located at the inner oxide surface. Samples were further characterized by scanning electron microscopy, Raman spectroscopy, transmission electron microscopy, and selective area diffractometry to better understand the physical mechanisms for the blue shift. (C) 2014 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Fryauf, David M.; Zhang, Junce; Norris, Kate J.; Leon, Juan J. Diaz; Oye, Michael M.; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, NASA, Ames Res Ctr, Adv Studies Labs, Moffett Field, CA 94035 USA. [Fryauf, David M.; Zhang, Junce; Norris, Kate J.; Leon, Juan J. Diaz; Oye, Michael M.; Wei, Min; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. [Wei, Min] Univ Elect Sci & Technol China, Sch Microelect & Solid Elect, Chengdu 610054, Peoples R China. RP Fryauf, DM (reprint author), Univ Calif Santa Cruz, NASA, Ames Res Ctr, Adv Studies Labs, Moffett Field, CA 94035 USA. EM dfryauf@ucsc.edu RI Kobayashi, Nobuhiko/E-3834-2012 FU National Science Foundation [DGE-0809125-006] FX We would like to thank Hewlett-Packard Labs (Palo Alto, California), for their assistance with ALD deposition. We would like to thank the MACS 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 material is based upon work supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-0809125-006. NR 27 TC 1 Z9 1 U1 1 U2 28 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 1862-6254 EI 1862-6270 J9 PHYS STATUS SOLIDI-R JI Phys. Status Solidi-Rapid Res. Lett. PD JUL PY 2014 VL 8 IS 7 BP 663 EP 667 DI 10.1002/pssr.201409008 PG 5 WC Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Materials Science; Physics GA AM2DF UT WOS:000339658600011 ER PT J AU Homer, ER Harris, MB Zirbel, SA Kolodziejska, JA Kozachkov, H Trease, BP Borgonia, JPC Agnes, GS Howell, LL Hofmann, DC AF Homer, Eric R. Harris, Matthew B. Zirbel, Shannon A. Kolodziejska, Joanna A. Kozachkov, Henry Trease, Brian P. Borgonia, John-Paul C. Agnes, Gregory S. Howell, Larry L. Hofmann, Douglas C. TI New Methods for Developing and Manufacturing Compliant Mechanisms Utilizing Bulk Metallic Glass SO ADVANCED ENGINEERING MATERIALS LA English DT Article ID FATIGUE; TOUGHNESS; BEHAVIOR; ALLOYS C1 [Homer, Eric R.; Harris, Matthew B.; Zirbel, Shannon A.; Howell, Larry L.] Brigham Young Univ, Dept Mech Engn, Provo, UT 84602 USA. [Kolodziejska, Joanna A.; Kozachkov, Henry; Hofmann, Douglas C.] CALTECH, Keck Lab Engn, Pasadena, CA 91125 USA. [Kolodziejska, Joanna A.; Kozachkov, Henry; Trease, Brian P.; Borgonia, John-Paul C.; Agnes, Gregory S.; Hofmann, Douglas C.] CALTECH, Jet Prop Lab, Engn & Sci Directorate, Pasadena, CA 91109 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Homer, ER (reprint author), Brigham Young Univ, Dept Mech Engn, Provo, UT 84602 USA. EM dch@jpl.nasa.gov RI Howell, Larry/A-6828-2008 OI Howell, Larry/0000-0001-8132-8822 FU National Aeronautics and Space Administration (NASA); Center Innovation Fund; NASA's Exploration Systems Mission Directorate [NNH10ZTT001N]; NASA's Office of Education [NNX13AB34A]; National Science Foundation; Air Force Office of Scientific Research through NSF [1240417] FX Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA) and funded through the Center Innovation Fund. This work was partially supported by NASA's Exploration Systems Mission Directorate under contract no. NNH10ZTT001N, NASA's Office of Education through contract no. NNX13AB34A, and the National Science Foundation and the Air Force Office of Scientific Research through NSF Grant No. 1240417. Supporting Information is available online from Wiley Online Library or from the author. NR 23 TC 11 Z9 11 U1 5 U2 30 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 1438-1656 EI 1527-2648 J9 ADV ENG MATER JI Adv. Eng. Mater. PD JUL PY 2014 VL 16 IS 7 BP 850 EP 856 DI 10.1002/adem.201300566 PG 7 WC Materials Science, Multidisciplinary SC Materials Science GA AL9CA UT WOS:000339436000002 ER PT J AU Tigelaar, DM Degges, MJ Chuang, K Hurwitz, FI Kuo, KK Scheiman, DA McCorkle, LS Quade, DJ Vivod, SL Splinter, S AF Tigelaar, Dean M. Degges, Matthew J. Chuang, Kathy Hurwitz, Frances I. Kuo, Kenneth K. Scheiman, Daniel A. McCorkle, Linda S. Quade, Derek J. Vivod, Stephanie L. Splinter, Scott TI Synthesis and Characterization of Hyperbranched Polyazomethine Ablators for Space Exploration Applications SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER LA English DT Article ID LIGHTWEIGHT CERAMIC ABLATORS; THERMAL-PROPERTIES; CHARRING ABLATORS; POLYMERS; DESIGN AB A novel series of ablative composites containing a hyperbranched polyazomethine synthesized inside a carbon fiber preform (HyPAZA) were prepared, which have similar density to phenolic impregnated carbon ablators (approximate to 0.3g/cc). A novel method of synthesizing strong hyperbranched polyazomethine thermosets has been developed, enabling polyazomethines to be studied in ablators for the first time. Several formulations of HyPAZA perform better than the phenolic impregnated carbon ablator in terms of polymer char yield, composite mechanical strength, CO2 laser ablation tests at heat fluxes of 550 and 1100W/cm2, and small-scale arcjet testing at a heat flux of 400W/cm2. Char yields of hyperbranched polyazomethines were as high as 79% at 1000 degrees C by thermogravimetric analysis. This is one of the highest char yields ever reported for a fully organic polymer. Some HyPAZA composites are over 10 times stronger than the carbon fiber preform, as determined by compression tests. Specimens were also tested in an arcjet facility at 400W/cm2. Several formulations exhibited better performance than the phenolic impregnated carbon ablator in terms of ablation rate by a factor of 1.2 to 1.7. In addition, HyPAZA composites impregnated with aerogel show a lower rate of increase of back wall temperature, and therefore a lower thermal conductivity. C1 [Tigelaar, Dean M.; Chuang, Kathy; McCorkle, Linda S.; Quade, Derek J.; Vivod, Stephanie L.] NASA, John H Glenn Res Ctr, Lewis Field, Polymers Branch, Cleveland, OH 44135 USA. [Degges, Matthew J.; Kuo, Kenneth K.] Penn State Univ, Dept Mech & Nucl Engn, State Coll, PA 16801 USA. [Hurwitz, Frances I.] NASA, John H Glenn Res Ctr, Lewis Field, Struct & Mat Div, Cleveland, OH 44135 USA. [Scheiman, Daniel A.] NASA, John H Glenn Res Ctr, Lewis Field, Cleveland, OH 44135 USA. [Splinter, Scott] NASA, Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA. RP Tigelaar, DM (reprint author), Ohio Aerosp Inst, Cleveland, OH 44142 USA. NR 22 TC 0 Z9 0 U1 4 U2 23 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0887-8722 EI 1533-6808 J9 J THERMOPHYS HEAT TR JI J. Thermophys. Heat Transf. PD JUL PY 2014 VL 28 IS 3 BP 401 EP 409 DI 10.2514/1.T4319 PG 9 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA AM1QK UT WOS:000339622500004 ER PT J AU Bourguet, FA Blanchette, CD Fischer, NO Jackson, PJ Hadi, MZ He, W Kay, BK Lam, KS Laurence, TA Rogers, Z Voss, JC Coleman, MA AF Bourguet, Feliza A. Blanchette, Craig D. Fischer, Nicholas O. Jackson, Paul J. Hadi, Masood Z. He, Wei Kay, Brian K. Lam, Kit S. Laurence, Ted A. Rogers, Zachary Voss, John C. Coleman, Matthew A. TI Cell-free Translation Systems For Biophysical And Biochemical Characterization Of Proteins And Protein Complexes SO PROTEIN SCIENCE LA English DT Meeting Abstract CT 28th Annual Symposium of the Protein-Society CY JUL 27-30, 2014 CL San Diego, CA SP Prot Soc, Bristol Myers Squibb, Lilly, Biochemistry C1 [Bourguet, Feliza A.; Blanchette, Craig D.; Fischer, Nicholas O.; Jackson, Paul J.; Coleman, Matthew A.] Lawrence Livermore Natl Lab, Biol & Biotechnol Div, Livermore, CA USA. [Hadi, Masood Z.] NASA, Ames Res Ctr, Mountain View, CA USA. [He, Wei; Lam, Kit S.; Rogers, Zachary] Univ Calif Davis, Ctr Biophoton, Sacramento, CA 95817 USA. [Kay, Brian K.] Univ Illinois, Chicago, IL USA. [Laurence, Ted A.] Lawrence Livermore Natl Lab, Condensed Matter & Mat Div, Livermore, CA USA. [Voss, John C.; Coleman, Matthew A.] Univ Calif Davis, Sacramento, CA 95817 USA. NR 0 TC 0 Z9 0 U1 1 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0961-8368 EI 1469-896X J9 PROTEIN SCI JI Protein Sci. PD JUL PY 2014 VL 23 SU 1 MA 06-368 BP 235 EP 236 PG 2 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA AM0OU UT WOS:000339545700358 ER PT J AU Rinehart, SA Rizzo, M Benford, DJ Fixsen, DJ Veach, TJ Dhabal, A Leisawitz, DT Mundy, LG Silverberg, RF Barry, RK Staguhn, JG Barclay, R Mentzell, JE Griffin, M Ade, PAR Pascale, E Klemencic, G Savini, G Juanola-Parramon, R AF Rinehart, S. A. Rizzo, M. Benford, D. J. Fixsen, D. J. Veach, T. J. Dhabal, A. Leisawitz, D. T. Mundy, L. G. Silverberg, R. F. Barry, R. K. Staguhn, J. G. Barclay, R. Mentzell, J. E. Griffin, M. Ade, P. A. R. Pascale, E. Klemencic, G. Savini, G. Juanola-Parramon, R. TI The Balloon Experimental Twin Telescope for Infrared Interferometry (BETTII): An Experiment for High Angular Resolution in the Far-Infrared SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID MILLIMETER; SPACE; LINE AB The Balloon Experimental Twin Telescope for Infrared Interferometry (BETTII) is a new balloon-borne far-infrared interferometer, being designed to provide spatially-resolved spectroscopy in the far infrared (30-90 mu m). The combination of an 8-meter baseline with a double-Fourier Michelson interferometer allows the identification and separation of closely-spaced astronomical sources, while also providing a low-resolution spectrum for each source. In this wavelength range, BETTII will provide subarcsecond angular resolution, a capability unmatched by other far-infrared facilities. This paper provides an overview of the entire design of the BETTII experiment, with a short discussion of the predicted performance on flight. C1 [Rinehart, S. A.; Rizzo, M.; Benford, D. J.; Fixsen, D. J.; Veach, T. J.; Dhabal, A.; Leisawitz, D. T.; Silverberg, R. F.; Barry, R. K.; Staguhn, J. G.; Barclay, R.; Mentzell, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rizzo, M.; Fixsen, D. J.; Dhabal, A.; Mundy, L. G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Veach, T. J.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. [Silverberg, R. F.] Univ Space Res Assoc, Columbia, MD USA. [Staguhn, J. G.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. [Griffin, M.; Ade, P. A. R.; Pascale, E.; Klemencic, G.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Savini, G.; Juanola-Parramon, R.] UCL, Dept Phys & Astron, Opt Sci Lab, London WC1E 6BT, England. RP Rinehart, SA (reprint author), NASA, Goddard Space Flight Ctr, Mail Code 665, Greenbelt, MD 20771 USA. EM Stephen.A.Rinehart@nasa.gov RI Benford, Dominic/D-4760-2012 OI Benford, Dominic/0000-0002-9884-4206 FU NASA Science Mission Directorate through the ROSES/APRA program; NASA's Goddard Space Flight Center; NASA; STFC PRD grant FX The material presented in this paper is based upon work supported by NASA Science Mission Directorate through the ROSES/APRA program, with additional support provided by NASA's Goddard Space Flight Center. Work by T. Veach was supported by an appointment to the NASA Postdoctoral Program at GSFC, administered by the Oak Ridge Associated Universities under contract with NASA. Contributions to this project were also made by a large number of undergraduate students, including: S. Gomillion, J. Doiron, S. Gore, B. Hoffman, W. Tierney, R. Curley, T. Kale, T. Handleton, S. Shapoval, M. Canaparro, D. Andrade, J. Stokes, C. Gibbons, S. Weinreich, J. Alcorn, A. Rau, S. Padder, P. Nehme, L. Oliviera, H. Spooner, C. Wagner, A. Cotto, N. Mihalko, Y. Okafor, P. Taraschi, J. Gibson, and Y. Huertes-Morales. The BETTII program at Cardiff University and UCL is supported by an STFC PRD grant. NR 34 TC 8 Z9 8 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 2014 VL 126 IS 941 BP 660 EP 673 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM1JQ UT WOS:000339602600005 ER PT J AU White, LM AF White, Lauren M. TI Comments and Replies Regarding "Putative Indigenous Carbon-Bearing Alteration Features in Martian Meteorite Yamato 000593,'' by LM White, EK Gibson, KL Thomas-Keprta, SJ Clemett, and DS McKay. Astrobiology, February 2014, 14(2):170-181 SO ASTROBIOLOGY LA English DT Letter C1 NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP White, LM (reprint author), NASA, Jet Prop Lab, Pasadena, CA 91109 USA. EM Lauren.Spencer@jpl.nasa.gov NR 0 TC 0 Z9 0 U1 0 U2 1 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 JUL PY 2014 VL 14 IS 7 BP 561 EP 561 PG 1 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AL8MT UT WOS:000339394000003 PM 25141381 ER PT J AU White, LM AF White, Lauren M. TI Comments and Replies Regarding "Putative Indigenous Carbon-Bearing Alteration Features in Martian Meteorite Yamato 000593,'' by LM White, EK Gibson, KL Thomas-Keprta, SJ Clemett, and DS McKay. Astrobiology, February 2014, 14(2):170-181 SO ASTROBIOLOGY LA English DT Letter ID VOLCANIC GLASS C1 NASA, Jet Prop Lab, Pasadena, CA 91109 USA. RP White, LM (reprint author), NASA, Jet Prop Lab, Pasadena, CA 91109 USA. EM Lauren.Spencer@jpl.nasa.gov NR 5 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 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD JUL PY 2014 VL 14 IS 7 BP 562 EP 562 PG 1 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AL8MT UT WOS:000339394000005 ER PT J AU Shelor, CP Dasgupta, PK Aubrey, A Davila, AF Lee, MC McKay, CP Liu, Y Noell, AC AF Shelor, C. Phillip Dasgupta, Purnendu K. Aubrey, Andrew Davila, Alfonso F. Lee, Michael C. McKay, Christopher P. Liu, Yan Noell, Aaron C. TI What Can In Situ Ion Chromatography Offer for Mars Exploration? SO ASTROBIOLOGY LA English DT Article DE Ion chromatography; Perchlorate (ClO4-); Mars soil; Oxychlorine species ID MERIDIANI-PLANUM; ORGANIC-MOLECULES; NITRATE DEPOSITS; MARTIAN SOIL; LANDING SITE; PERCHLORATE; ORIGIN; CHEMISTRY; RADIATION; MILK AB The successes of the Mars exploration program have led to our unprecedented knowledge of the geological, mineralogical, and elemental composition of the martian surface. To date, however, only one mission, the Phoenix lander, has specifically set out to determine the soluble chemistry of the martian surface. The surprising results, including the detection of perchlorate, demonstrated both the importance of performing soluble ion measurements and the need for improved instrumentation to unambiguously identify all the species present. Ion chromatography (IC) is the state-of-the-art technique for soluble ion analysis on Earth and would therefore be the ideal instrument to send to Mars. A flight IC system must necessarily be small, lightweight, low-power, and have low eluent consumption. We demonstrate here a breadboard system that addresses these issues by using capillary IC at low flow rates with an optimized eluent generator and suppressor. A mix of 12 ions known or plausible for the martian soil, including 4 (oxy) chlorine species, has been separated at flow rates ranging from 1 to 10 mu L/min, requiring as little as 200 psi at 1.0 mu L/min. This allowed the use of pneumatic displacement pumping from a pressurized aluminum eluent reservoir and the elimination of the high-pressure pump entirely (the single heaviest and most energy-intensive component). All ions could be separated and detected effectively from 0.5 to 100 mu M, even when millimolar concentrations of perchlorate were present in the same mixtures. C1 [Shelor, C. Phillip; Dasgupta, Purnendu K.] Univ Texas Arlington, Dept Chem & Biochem, Arlington, TX 76019 USA. [Aubrey, Andrew; Lee, Michael C.; Noell, Aaron C.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Davila, Alfonso F.] SETI Inst, Mountain View, CA USA. [McKay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Liu, Yan] Dionex Thermo Fisher, Res & Dev, Sunnyvale, CA USA. RP Dasgupta, PK (reprint author), Univ Texas Arlington, Dept Chem & Biochem, Arlington, TX 76019 USA. EM dasgupta@uta.edu RI Davila, Alfonso/A-2198-2013; OI Davila, Alfonso/0000-0002-0977-9909; Shelor, Charles/0000-0002-2318-9411 FU NASA [NNX11A066G, NNX12AD61G]; Thermo Fisher/Dionex; National Aeronautics and Space Administration through internal Research and Technology Development program FX P.K.D. acknowledges support from NASA (through NNX11A066G) and Thermo Fisher/Dionex. A. F. D. acknowledges support from NASA (through NNX12AD61G). A portion 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 and funded through the internal Research and Technology Development program. NR 67 TC 1 Z9 1 U1 2 U2 19 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD JUL PY 2014 VL 14 IS 7 BP 577 EP 588 DI 10.1089/ast.2013.1131 PG 12 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AL8MT UT WOS:000339394000008 PM 24963874 ER PT J AU Hull, CLH Plambeck, RL Kwon, W Bower, GC Carpenter, JM Crutcher, RM Fiege, JD Franzmann, E Hakobian, NS Heiles, C Houde, M Hughes, AM Lamb, JW Looney, LW Marrone, DP Matthews, BC Pillai, T Pound, MW Rahman, N Sandell, G Stephens, IW Tobin, JJ Vaillancourt, JE Volgenau, NH Wright, MCH AF Hull, Charles L. H. Plambeck, Richard L. Kwon, Woojin Bower, Geoffrey C. Carpenter, John M. Crutcher, Richard M. Fiege, Jason D. Franzmann, Erica Hakobian, Nicholas S. Heiles, Carl Houde, Martin Hughes, A. Meredith Lamb, James W. Looney, Leslie W. Marrone, Daniel P. Matthews, Brenda C. Pillai, Thushara Pound, Marc W. Rahman, Nurur Sandell, Goeran Stephens, Ian W. Tobin, John J. Vaillancourt, John E. Volgenau, N. H. Wright, Melvyn C. H. TI TADPOL: A 1.3 mm SURVEY OF DUST POLARIZATION IN STAR-FORMING CORES AND REGIONS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ISM: magnetic fields; magnetic fields; polarization; stars: formation; stars: magnetic field; stars: protostars ID YOUNG STELLAR OBJECTS; MAGNETIC-FIELD STRUCTURE; INFRARED DARK CLOUD; CLASS 0 PROTOSTAR; RADIO-CONTINUUM EMISSION; DRIVEN MOLECULAR OUTFLOW; LARGE PROPER MOTIONS; HERBIG-HARO OBJECTS; LOW-MASS PROTOSTARS; IRAS POINT SOURCES AB We present lambda 1.3 mm Combined Array for Research in Millimeter-wave Astronomy observations of dust polarization toward 30 star-forming cores and eight star-forming regions from the TADPOL survey. We show maps of all sources, and compare the similar to 2 ''.5 resolution TADPOL maps with similar to 20 '' resolution polarization maps from single-dish submillimeter telescopes. Here we do not attempt to interpret the detailed B-field morphology of each object. Rather, we use average B-field orientations to derive conclusions in a statistical sense from the ensemble of sources, bearing in mind that these average orientations can be quite uncertain. We discuss three main findings. (1) A subset of the sources have consistent magnetic field (B-field) orientations between large (similar to 20 '') and small (similar to 2 ''.5) scales. Those same sources also tend to have higher fractional polarizations than the sources with inconsistent large-to-small-scale fields. We interpret this to mean that in at least some cases B-fields play a role in regulating the infall of material all the way down to the similar to 1000 AU scales of protostellar envelopes. (2) Outflows appear to be randomly aligned with B-fields; although, in sources with low polarization fractions there is a hint that outflows are preferentially perpendicular to small-scale B-fields, which suggests that in these sources the fields have been wrapped up by envelope rotation. (3) Finally, even at similar to 2 ''.5 resolution we see the so-called polarization hole effect, where the fractional polarization drops significantly near the total intensity peak. All data are publicly available in the electronic edition of this article. C1 [Hull, Charles L. H.; Plambeck, Richard L.; Bower, Geoffrey C.; Heiles, Carl; Wright, Melvyn C. H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Hull, Charles L. H.; Plambeck, Richard L.; Bower, Geoffrey C.; Heiles, Carl; Wright, Melvyn C. H.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Kwon, Woojin] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Bower, Geoffrey C.] ASIAA, Hilo, HI 96720 USA. [Carpenter, John M.; Lamb, James W.; Pillai, Thushara] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Crutcher, Richard M.; Hakobian, Nicholas S.; Stephens, Ian W.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Franzmann, Erica] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada. [Houde, Martin] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Houde, Martin] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Hughes, A. Meredith] Wesleyan Univ, Dept Astron, Van Vleck Observ, Middletown, CT 06459 USA. [Marrone, Daniel P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Matthews, Brenda C.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. [Matthews, Brenda C.] Natl Res Council Canada, Victoria, BC V9E 2E7, Canada. [Pound, Marc W.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Pound, Marc W.] Univ Maryland, Lab Millimeter Wave Astron, College Pk, MD 20742 USA. [Rahman, Nurur] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa. [Sandell, Goeran] NASA, Ames Res Ctr, Univ Space Res Assoc, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Stephens, Ian W.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Tobin, John J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Volgenau, N. H.] Owens Valley Radio Observ, Combined Array Res Millimeter Wave, Big Pine, CA 93513 USA. RP Hull, CLH (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM chat@astro.berkeley.edu OI Marrone, Daniel/0000-0002-2367-1080 NR 276 TC 47 Z9 47 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUL PY 2014 VL 213 IS 1 AR 13 DI 10.1088/0067-0049/213/1/13 PG 48 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL6HO UT WOS:000339233400013 ER PT J AU Johnson, TJ Venter, C Harding, AK Guillemot, L Smith, DA Kramer, M Celik, O Den Hartog, PR Ferrara, EC Hou, X Lande, J Ray, PS AF Johnson, T. J. Venter, C. Harding, A. K. Guillemot, L. Smith, D. A. Kramer, M. Celik, O. Den Hartog, P. R. Ferrara, E. C. Hou, X. Lande, J. Ray, P. S. TI CONSTRAINTS ON THE EMISSION GEOMETRIES AND SPIN EVOLUTION OF GAMMA-RAY MILLISECOND PULSARS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE acceleration of particles; gamma rays: stars; pulsars: general ID LARGE-AREA TELESCOPE; HIGH-ENERGY EMISSION; NANCAY RADIO TELESCOPE; PHASE-RESOLVED SPECTRA; ANNULAR GAP MODEL; LIGHT CURVES; NEUTRON-STAR; CRAB PULSAR; X-RAY; GLOBULAR-CLUSTER AB Millisecond pulsars (MSPs) are a growing class of gamma-ray emitters. Pulsed gamma-ray signals have been detected from more than 40 MSPs with the Fermi Large Area Telescope (LAT). The wider radio beams and more compact magnetospheres of MSPs enable studies of emission geometries over a broader range of phase space than non-recycled radio-loud gamma-ray pulsars. We have modeled the gamma-ray light curves of 40 LAT-detected MSPs using geometric emission models assuming a vacuum retarded-dipole magnetic field. We modeled the radio profiles using a single-altitude hollow-cone beam, with a core component when indicated by polarimetry; however, for MSPs with gamma-ray and radio light curve peaks occurring at nearly the same rotational phase, we assume that the radio emission is co-located with the gamma rays and caustic in nature. The best-fit parameters and confidence intervals are determined using a maximum likelihood technique. We divide the light curves into three model classes, with gamma-ray peaks trailing (Class I), aligned (Class II), or leading (Class III) the radio peaks. Outer gap and slot gap (two-pole caustic) models best fit roughly equal numbers of Class I and II, while Class III are exclusively fit with pair-starved polar cap models. Distinguishing between the model classes based on typical derived parameters is difficult. We explore the evolution of the magnetic inclination angle with period and spin-down power, finding possible correlations. While the presence of significant off-peak emission can often be used as a discriminator between outer gap and slot gap models, a hybrid model may be needed. C1 [Johnson, T. J.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Venter, C.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa. [Harding, A. K.; Celik, O.; Ferrara, E. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Guillemot, L.] CNRS, LPCE UMR 6115, Lab Phys & Chim Environ, F-45071 Orleans, France. [Guillemot, L.] CNRS INSU, Obser Paris, Stn Radioastron Nancay, F-18330 Nancay, France. [Smith, D. A.] Univ Bordeaux 1, IN2P3 CNRS, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Kramer, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Kramer, M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Celik, O.] CRESST, Greenbelt, MD 20771 USA. [Celik, O.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Celik, O.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. [Celik, O.] Univ Maryland, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Den Hartog, P. R.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Den Hartog, P. R.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Lande, J.] Twitter Inc, San Francisco, CA 94103 USA. [Ray, P. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. RP Johnson, TJ (reprint author), Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. EM tyrel.j.johnson@gmail.com; Christo.Venter@nwu.ac.za; ahardingx@yahoo.com OI Ray, Paul/0000-0002-5297-5278; Venter, Christo/0000-0002-2666-4812 FU LAT; scientific data analysis; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France; Commonwealth Government; National Science Foundation [AST-1100968]; NASA [DPR S-15633-Y, 10-Fermi10-C4-0054, 09-FERMI309-0076]; South African National Research Foundation FX The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden.; Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France.; Our research used the radio profiles published in Abdo et al. (2013) and we gratefully acknowledge the efforts of radio astronomers in support of Fermi LAT pulsar science. The Parkes radio telescope is part of the Australia Telescope which is funded by the Commonwealth Government for operation as a National Facility managed by CSIRO. The Robert C. Byrd Green Bank Telescope (GBT) is operated by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The Arecibo Observatory is operated by SRI International under a cooperative agreement with the National Science Foundation (AST-1100968), and in alliance with Ana G. Mndez-Universidad Metropolitana, and the Universities Space Research Association. The Nan, cay Radio Observatory is operated by the Paris Observatory, associated with the French Centre National de la Recherche Scientifique (CNRS). The Westerbork Synthesis Radio Telescope is operated by Netherlands Foundation for Radio Astronomy, ASTRON.; Portions of this research performed at the Naval Research Laboratory are sponsored by NASA DPR S-15633-Y. C.V. is supported by the South African National Research Foundation. A.K.H. acknowledges support from NASA Astrophysics Theory grants and Fermi Guest Investigator grants 10-Fermi10-C4-0054 and 09-FERMI309-0076. NR 161 TC 20 Z9 20 U1 2 U2 5 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 JUL PY 2014 VL 213 IS 1 AR 6 DI 10.1088/0067-0049/213/1/6 PG 54 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL6HO UT WOS:000339233400006 ER PT J AU Garcia-Pando, CP Stanton, MC Diggle, PJ Trzaska, S Miller, RL Perlwitz, JP Baldasano, JM Cuevas, E Ceccato, P Yaka, P Thomson, MC AF Garcia-Pando, Carlos Perez Stanton, Michelle C. Diggle, Peter J. Trzaska, Sylwia Miller, Ron L. Perlwitz, Jan P. Baldasano, Jose M. Cuevas, Emilio Ceccato, Pietro Yaka, Pascal Thomson, Madeleine C. TI Soil Dust Aerosols and Wind as Predictors of Seasonal Meningitis Incidence in Niger SO ENVIRONMENTAL HEALTH PERSPECTIVES LA English DT Article ID MENINGOCOCCAL MENINGITIS; POISSON REGRESSION; WEST-AFRICA; MODEL; EPIDEMICS; OUTBREAKS; CLIMATE; DISEASE; BELT AB Background: Epidemics of meningococcal meningitis are concentrated in sub-Saharan Africa during the dry season, a period when the region is affected by the Harmattan, a dry and dusty northeasterly trade wind blowing from the Sahara into the Gulf of Guinea. Objectives: We examined the potential of climate-based statistical forecasting models to predict seasonal incidence of meningitis in Niger at both the national and district levels. Data and methods: We used time series of meningitis incidence from 1986 through 2006 for 38 districts in Niger. We tested models based on data that would be readily available in an operational framework, such as climate and dust, population, and the incidence of early cases before the onset of the meningitis season in January-May. Incidence was used as a proxy for immunological state, susceptibility, and carriage in the population. We compared a range of negative binomial generalized linear models fitted to the meningitis data. Results: At the national level, a model using early incidence in December and averaged November-December zonal wind provided the best fit (pseudo-R-2 = 0.57), with zonal wind having the greatest impact. A model with surface dust concentration as a predictive variable performed indistinguishably well. At the district level, the best spatiotemporal model included zonal wind, dust concentration, early incidence in December, and population density (pseudo-R-2 = 0.41). Conclusions: We showed that wind and dust information and incidence in the early dry season predict part of the year-to-year variability of the seasonal incidence of meningitis at both national and district levels in Niger. Models of this form could provide an early-season alert that wind, dust, and other conditions are potentially conducive to an epidemic. C1 [Garcia-Pando, Carlos Perez; Miller, Ron L.; Perlwitz, Jan P.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Garcia-Pando, Carlos Perez; Miller, Ron L.; Perlwitz, Jan P.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. [Stanton, Michelle C.; Diggle, Peter J.] Univ Lancaster, Lancaster Med Sch, Lancaster, England. [Stanton, Michelle C.] Univ Liverpool, Liverpool Sch Trop Med, Liverpool L3 5QA, Merseyside, England. [Diggle, Peter J.] Univ Liverpool, Dept Epidemiol & Populat Hlth, Liverpool L69 3BX, Merseyside, England. [Trzaska, Sylwia; Ceccato, Pietro; Thomson, Madeleine C.] Int Res Inst Climate & Soc, Palisades, NY USA. [Baldasano, Jose M.] Ctr Nacl Supercomputac, Barcelona Supercomp Ctr, Barcelona, Spain. [Cuevas, Emilio] Agencia Estatal Meteorol, Izana Atmospher Res Ctr, Tenerife, Spain. [Yaka, Pascal] Off Civil Aviat & Meteorol Gen Direct, Ouagadougou, Burkina Faso. [Thomson, Madeleine C.] Columbia Univ, Mailman Sch Publ Hlth, Dept Environm Hlth Sci, New York, NY USA. RP Garcia-Pando, CP (reprint author), 2880 Broadway, New York, NY 10025 USA. EM carlos.perezga@nasa.gov RI Miller, Ron/E-1902-2012; Cuevas, Emilio/L-2109-2013; OI Cuevas, Emilio/0000-0003-1843-8302; Perez Garcia-Pando, Carlos/0000-0002-4456-0697; Diggle, Peter/0000-0003-3521-5020 FU EI Cross-Cutting Initiative project: "Atmospheric aerosol impacts on health in sub-Saharan Africa"; NASA (National Aeronautics and Space Administration) ROSES (Research Opportunities in Space and Earth Sciences); European Global Monitoring for Environment and Security-Monitoring Atmospheric Composition and Climate (GMES-MACC) project FX This study was supported by the EI Cross-Cutting Initiative project: "Atmospheric aerosol impacts on health in sub-Saharan Africa," NASA (National Aeronautics and Space Administration) ROSES (Research Opportunities in Space and Earth Sciences) applications feasibility studies, and European Global Monitoring for Environment and Security-Monitoring Atmospheric Composition and Climate (GMES-MACC) project Working Package 3.1. NR 26 TC 16 Z9 16 U1 0 U2 16 PU US DEPT HEALTH HUMAN SCIENCES PUBLIC HEALTH SCIENCE PI RES TRIANGLE PK PA NATL INST HEALTH, NATL INST ENVIRONMENTAL HEALTH SCIENCES, PO BOX 12233, RES TRIANGLE PK, NC 27709-2233 USA SN 0091-6765 EI 1552-9924 J9 ENVIRON HEALTH PERSP JI Environ. Health Perspect. PD JUL PY 2014 VL 122 IS 7 BP 679 EP 686 DI 10.1289/ehp.1306640 PG 8 WC Environmental Sciences; Public, Environmental & Occupational Health; Toxicology SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Toxicology GA AL2AK UT WOS:000338928000017 ER PT J AU Chin, TM Vazquez-Cuervo, J Armstrong, EM AF Chin, Toshio Michael Vazquez-Cuervo, Jorge Armstrong, Edward M. TI On "Gridless" Interpolation and Subgrid Data Density SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article AB Nearest-neighbor gridding, binning, and bin-averaging procedures are performed routinely to map the irregularly sampled data onto a grid for data analysis and assimilation. Because these procedures are actually an interpolation procedure based on a piecewise constant function as the interpolation kernel, they tend to discard the subgrid locations of the data. Use of a locally continuous function for the interpolation kernel can preserve the subgrid location information in the data, at the cost of numerical sensitivity to the spatial variation in data density. This paper suggests a simple numerical procedure, based on a single correlation coefficient parameter, to eliminate such numerical sensitivity. C1 [Chin, Toshio Michael; Vazquez-Cuervo, Jorge; Armstrong, Edward M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Chin, TM (reprint author), CALTECH, Jet Prop Lab, M-S 238-600,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mike.chin@jpl.nasa.gov FU National Aeronautics and Space Administration (NASA) 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 (NASA), especially the Making Earth System Data Records for Use in Research Environments (MEaSUREs) program. NR 19 TC 0 Z9 0 U1 0 U2 0 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 JUL PY 2014 VL 31 IS 7 BP 1642 EP 1652 DI 10.1175/JTECH-D-13-00219.1 PG 11 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA AL4KQ UT WOS:000339102200014 ER PT J AU Fleming, IA Bottom, DL Jones, KK Simenstad, CA Craig, JF AF Fleming, I. A. Bottom, D. L. Jones, K. K. Simenstad, C. A. Craig, J. F. TI Resilience of anadromous and resident salmonid populations SO JOURNAL OF FISH BIOLOGY LA English DT Editorial Material ID ECO-EVOLUTIONARY DYNAMICS; LIFE-HISTORY; DIVERSITY; BIODIVERSITY; COMPLEXITY; FITNESS; FUTURE; SALAR; BETS C1 [Fleming, I. A.] Mem Univ Newfoundland, Fish Evolutionary Ecol Res Grp, St John, NF A1C 5S7, Canada. [Fleming, I. A.] Mem Univ Newfoundland, Dept Ocean Sci, St John, NF A1C 5S7, Canada. [Bottom, D. L.] NOAA, Fish Ecol Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. [Jones, K. K.] Oregon Dept Fish & Wildlife, Corvallis, OR 97333 USA. [Simenstad, C. A.] Univ Washington, Sch Aquat & Fishery Sci, Seattle, WA 98195 USA. RP Fleming, IA (reprint author), Mem Univ Newfoundland, Fish Evolutionary Ecol Res Grp, St John, NF A1C 5S7, Canada. RI Fleming, Ian/I-7217-2012 NR 39 TC 4 Z9 4 U1 3 U2 29 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-1112 EI 1095-8649 J9 J FISH BIOL JI J. Fish Biol. PD JUL PY 2014 VL 85 IS 1 SI SI BP 1 EP 7 DI 10.1111/jfb.12429 PG 7 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA AL2HE UT WOS:000338945800001 PM 24980458 ER PT J AU Craig, BE Simenstad, CA Bottom, DL AF Craig, B. E. Simenstad, C. A. Bottom, D. L. TI Rearing in natural and recovering tidal wetlands enhances growth and life-history diversity of Columbia Estuary tributary coho salmon Oncorhynchus kisutch population SO JOURNAL OF FISH BIOLOGY LA English DT Article DE habitat restoration; migration; nomad; Pacific salmon; resilience; scale pattern analysis ID JUVENILE CHINOOK SALMON; SCALE PATTERN-ANALYSIS; RIVER ESTUARY; OREGON; TSHAWYTSCHA; WASHINGTON; STEELHEAD; MIGRATION; MOVEMENT; SURVIVAL AB This study provides evidence of the importance of tributary tidal wetlands to local coho salmon Oncorhynchus kisutch populations and life-history diversity. Subyearling and, to a lesser extent, yearling O. kisutch life histories utilized various estuary habitats within the Grays River, a tidal freshwater tributary of the Columbia River estuary, including restoring emergent wetlands and natural forested wetlands. Migration timing data, size distributions, estuary residence and scale patterns suggest a predominance of subyearling migrant life histories, including several that involve extended periods of estuary rearing. Estuarine-rearing subyearling O. kisutch exhibited the greatest overall growth rates; the highest growth rates were seen in fish that utilized restoring emergent wetlands. These results contrast with studies conducted in the main-stem Columbia River estuary, which captured few O. kisutch, of which nearly all were hatchery-origin yearling smolts. Restoration and preservation of peripheral and tributary wetland habitats, such as those in the Grays River, could play an important role in the recovery of natural O. kisutch populations in the Columbia River and elsewhere. (C) 2014 The Fisheries Society of the British Isles C1 [Craig, B. E.; Simenstad, C. A.] Univ Washington, Sch Aquat & Fishery Sci, Seattle, WA 98195 USA. [Bottom, D. L.] NOAA, Fish Ecol Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. RP Craig, BE (reprint author), Washington Dept Fish & Wildlife, Mill Creek, WA 98012 USA. EM Bethany.Craig@dfw.wa.gov FU Bonneville Power Administration FX This research was made possible by funding from the Bonneville Power Administration. We thank the staff of the NOAA Fisheries Point Adams laboratory, the University of Washington Wetland Ecosystem Team and High Seas Lab, the Washington Department of Fish and Wildlife, the Columbia River Estuary Study Taskforce and numerous volunteers for support and field assistance. NR 58 TC 3 Z9 3 U1 4 U2 43 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-1112 EI 1095-8649 J9 J FISH BIOL JI J. Fish Biol. PD JUL PY 2014 VL 85 IS 1 SI SI BP 31 EP 51 DI 10.1111/jfb.12433 PG 21 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA AL2HE UT WOS:000338945800003 PM 24890886 ER PT J AU Jones, KK Cornwell, TJ Bottom, DL Campbell, LA Stein, S AF Jones, K. K. Cornwell, T. J. Bottom, D. L. Campbell, L. A. Stein, S. TI The contribution of estuary-resident life histories to the return of adult Oncorhynchus kisutch SO JOURNAL OF FISH BIOLOGY LA English DT Article DE life-history diversity; Oregon; otolith microchemistry; Salmon River; survival; winter habitat ID JUVENILE COHO SALMON; RIVER ESTUARY; OTOLITH MICROCHEMISTRY; HABITAT USE; OREGON; RESILIENCE; WASHINGTON; MOVEMENTS; MIGRATION; STREAMS AB This study evaluated estuarine habitat use, life-history composition, growth and survival of four successive broods of coho salmon Oncoryhnchus kisutch in Salmon River, Oregon, U. S. A. Subyearling and yearling O. kisutch used restored and natural estuarine wetlands, particularly in the spring and winter. Stream-reared yearling smolts spent an average of 2 weeks in the estuary growing rapidly before entering the ocean. Emergent fry also entered the estuary in the spring, and some resided in a tidal marsh throughout the summer, even as salinities increased to >20. A significant portion of the summer stream-resident population of juvenile O. kisutch migrated out of the catchment in the autumn and winter and used estuary wetlands and adjacent streams as alternative winter-rearing habitats until the spring when they entered the ocean as yearling smolts. Passive integrated transponder (PIT) tag returns and juvenile life-history reconstructions from otoliths of returning adults revealed that four juvenile life-history types contributed to the adult population. Estuarine-associated life-history strategies accounted for 20-35% of the adults returning to spawn in the four brood years, indicating that a sizable proportion of the total O. kisutch production is ignored by conventional estimates based on stream habitat capacity. Juvenile O. kisutch responses to the reconnection of previously unavailable estuarine habitats have led to greater life-history diversity in the population and reflect greater phenotypic plasticity of the species in the U. S. Pacific Northwest than previously recognized. (C) 2014 The Fisheries Society of the British Isles C1 [Jones, K. K.; Cornwell, T. J.; Stein, S.] Oregon Dept Fish & Wildlife, Corvallis, OR 97333 USA. [Bottom, D. L.] NOAA, Fish Ecol Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. [Campbell, L. A.] Washington Dept Fish & Wildlife, Olympia, WA 98501 USA. RP Jones, KK (reprint author), Oregon Dept Fish & Wildlife, Corvallis, OR 97333 USA. EM kim.jones@oregonstate.edu FU Oregon Watershed Enhancement Board (OWEB); Oregon Department of Fish and Wildlife; NOAA Fisheries FX We appreciate the research funding provided through the Oregon Watershed Enhancement Board (OWEB) and support from Oregon Department of Fish and Wildlife and NOAA Fisheries. The USFS has been responsible for extensive estuarine restoration within the Cascade Head Scenic Research Area, with assistance from OWEB. D. Welch and other personnel at the ODFW Salmon River hatchery and staff from Miami Corporation provided logistical support and access. L. Borgerson analysed the adult O. kisutch scales. J. Peterson of Oregon State University graciously evaluated the survival rates. Special thanks to L. Nguyen, S. Orlaineta and A. Claiborne from the Washington Department of Fish and Wildlife, Fish Ageing and Otolith Laboratories for otolith sample preparation. We gratefully acknowledge the contributions of field staff that operated the screw trap, conducted field surveys and collected otoliths. Thorough reviews provided by three anonymous referees improved the manuscript immensely. NR 58 TC 20 Z9 19 U1 4 U2 36 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-1112 EI 1095-8649 J9 J FISH BIOL JI J. Fish Biol. PD JUL PY 2014 VL 85 IS 1 SI SI BP 52 EP 80 DI 10.1111/jfb.12380 PG 29 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA AL2HE UT WOS:000338945800004 PM 24766645 ER PT J AU Johanos, TC Harting, AL Wurth, TA Baker, JD AF Johanos, Thea C. Harting, Albert L. Wurth, Tracy A. Baker, Jason D. TI Range-wide movement patterns of Hawaiian monk seals SO MARINE MAMMAL SCIENCE LA English DT Article ID ABUNDANCE; ISLANDS; DISEASE C1 [Johanos, Thea C.; Baker, Jason D.] NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96814 USA. [Harting, Albert L.] Harting Biol Consulting, Bozeman, MT 59715 USA. [Wurth, Tracy A.] Univ Hawaii, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA. RP Johanos, TC (reprint author), NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, 1601 Kapiolani Blvd, Honolulu, HI 96814 USA. EM thea.johanos-kam@noaa.gov NR 21 TC 2 Z9 2 U1 1 U2 31 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0824-0469 EI 1748-7692 J9 MAR MAMMAL SCI JI Mar. Mamm. Sci. PD JUL PY 2014 VL 30 IS 3 BP 1165 EP 1174 DI 10.1111/mms.12084 PG 10 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA AL4KM UT WOS:000339101800019 ER PT J AU Sears, DWG AF Sears, Derek W. G. TI Oral histories in meteoritics and planetary science-XXV: Vagn F. Buchwald SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID YORK IRON METEORITE; CAPE-YORK; CHEMICAL CLASSIFICATION; GE CONCENTRATIONS; CORROSION; MINERALOGY; PPM AB Vagn Buchwald (Fig. 1) was born in Copenhagen where he attended school and college. Then after 18 months of military service, he assumed a position at the Technical University of Copenhagen. A few years later, he was presented with a piece of the Cape York meteorite, which led to an interest in iron meteorites. Through a campaign of informed searching, Vagn found the 20 ton Agpalilik meteorite (part of the Cape York shower) on 31st July 1963 and by September 1967 had arranged its transport to Copenhagen. After sorting and describing the Danish collection, which included application of the Fe-Ni-P phase diagram to iron meteorite mineralogy, Vagn was invited to sort and describe other iron meteorite collections. This led to a 7 yr project to write his monumental Handbook of Iron Meteorites. Vagn spent 3 yr in the United States and visited most of the world's museums, the visit to Berlin being especially important since the war had left their iron meteorites in bad condition and without labels. During a further decade or more of iron meteorite research, he documented natural and anthropomorphic alterations experienced by iron meteorites, discovered five new minerals (roaldite, carlsbergite, akaganeite, hibbingite, and arupite); had a mineral (buchwaldite, NaCaPO4) and asteroid (3209 Buchwald 1982 BL1) named after him; and led expeditions to Chile, Namibia, and South Africa in search of iron meteorites and information on them. Vagn then turned his attention to archeological metal artifacts. This work resulted in many papers and culminated in two major books on the subject published in 2005 and 2008, after his retirement in 1998. Vagn Buchwald has received numerous Scandinavian awards and honors, and served as president of the Meteoritical Society in 1981-1982. C1 NASA, Ames Res Ctr, Bay Area Environm Res Inst, Space Sci & Astrobiol Div, Mountain View, CA 94035 USA. RP Sears, DWG (reprint author), NASA, Ames Res Ctr, Bay Area Environm Res Inst, Space Sci & Astrobiol Div, Mountain View, CA 94035 USA. EM derek.sears@nasa.gov FU NASA FX This interview was recorded on February 2nd and 3rd, 2014, in Gentofte, Copenhagen, and edited by the author and VFB. I am grateful to NASA for financial support and to Ed Scott, John Wasson, and Hazel Sears for reviews and Hazel also for proofing. NR 37 TC 0 Z9 0 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 JUL PY 2014 VL 49 IS 7 BP 1271 EP 1287 DI 10.1111/maps.12332 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AL5FQ UT WOS:000339159300009 ER PT J AU Noguchi, T Kimura, M Hashimoto, T Konno, M Nakamura, T Zolensky, ME Tsuchiyama, A Matsumoto, T Matsuno, J Okazaki, R Uesugi, M Karouji, Y Yada, T Ishibashi, Y Shirai, K Abe, M Okada, T AF Noguchi, T. Kimura, M. Hashimoto, T. Konno, M. Nakamura, T. Zolensky, M. E. Tsuchiyama, A. Matsumoto, T. Matsuno, J. Okazaki, R. Uesugi, M. Karouji, Y. Yada, T. Ishibashi, Y. Shirai, K. Abe, M. Okada, T. TI Sylvite and halite on particles recovered from 25143 Itokawa: A preliminary report SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID ORDINARY CHONDRITES; PARENT BODY; DUST PARTICLES; MONAHANS 1998; ENCELADUS; ASTEROIDS; REGOLITH; SURFACE; WATER; LINK AB We observed cross sectional ultra-thin sections near the surface of 12 particles recovered from the S-type asteroid Itokawa by the Hayabusa spacecraft in 2010, using spherical aberration-corrected STEM and conventional TEM. Although their mineralogy is almost identical to the equilibrated LL chondrites and therefore basically anhydrous, micrometer-to-submicrometer-sized sylvite was identified on the surface of Itokawa particle RA-QD02-0034. Separately, micrometer-sized halite was also identified on the surface of Itokawa particle RA-QD02-0129. Detailed inspection of the sample processing procedures at the JAXA's Planetary Materials Sample Curation Facility and textural observation of the sylvite and halite indicate that they were clearly present on two Itokawa particles before they were removed from Clean Chamber #2 at JAXA. However, there is no direct evidence for their extraterrestrial origin at present. If the sylvite and halite are extraterrestrial, their presence suggests that they may be more abundant on the surface of S-type asteroids than previously thought. C1 [Noguchi, T.] Kyushu Univ, Fac Arts & Sci, Nishi Ku, Fukuoka 8190395, Japan. [Kimura, M.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan. [Hashimoto, T.; Konno, M.] Hitachi High Technol Corp, Hitachinaka, Ibaraki 3128504, Japan. [Nakamura, T.] Tohoku Univ, Grad Sch Sci, Div Earth & Planetary Mat Sci, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Zolensky, M. E.] NASA, Johnson Space Ctr, ARES, Houston, TX 77058 USA. [Tsuchiyama, A.; Matsumoto, T.; Matsuno, J.] Kyoto Univ, Grad Sch Sci, Div Earth & Planetary Sci, Sakyo Ku, Kyoto 6068502, Japan. [Okazaki, R.] Kyushu Univ, Dept Earth & Planetary Sci, Fukuoka 8128581, Japan. [Uesugi, M.; Karouji, Y.; Yada, T.; Ishibashi, Y.; Shirai, K.; Abe, M.; Okada, T.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. RP Noguchi, T (reprint author), Kyushu Univ, Fac Arts & Sci, Nishi Ku, 744 Motooka, Fukuoka 8190395, Japan. EM tnoguchi@artsci.kyushu-u.ac.jp RI U-ID, Kyushu/C-5291-2016 FU JSPS KAKENHI [2424408]; NASA's Muses-CN Program FX We specially thank the Hayabusa project team for the sample return. We are grateful to Y. Suzuki, T. Sato, and H. Matsumoto for supporting STEM and FE-TEM observation at Hitachi High-technologies Corporation. T. Noguchi was supported by JSPS KAKENHI grant number 2424408. M. E. Zolensky was supported by NASA's Muses-CN Program. We would like to appreciate J. C. Bridges, an anonymous reviewer, and the AE for their constructive comments. NR 35 TC 1 Z9 1 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2014 VL 49 IS 7 BP 1305 EP 1314 DI 10.1111/maps.12333 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AL5FQ UT WOS:000339159300011 ER PT J AU Jeong, SJ Ho, CH Piao, SL Kim, J Ciais, P Lee, YB Jhun, JG Park, SK AF Jeong, Su-Jong Ho, Chang-Hoi Piao, Shilong Kim, Jinwon Ciais, Philippe Lee, Yun-Bok Jhun, Jong-Ghap Park, Seon Ki TI Effects of double cropping on summer climate of the North China Plain and neighbouring regions SO NATURE CLIMATE CHANGE LA English DT Article ID GLOBAL LAND-COVER; FOOD SECURITY; VARIABILITY; ATMOSPHERE; CROPLANDS; MONSOON; ASIA AB The North China Plain (NCP) is one of the most important agricultural regions in Asia and produces up to 50% of the cereal consumed in China each year(1,2). To meet increasing food demands without expanding croplands, annual agricultural practice in much of the NCP has changed from single to double cropping(3,4). The impact of double cropping on the regional climate, through biophysical feedbacks caused by changes in land surface conditions, remains largely unknown. Here we show that observed surface air temperatures during the inter-cropping season (June and July) are 0.40 degrees C higher over double cropping regions (DCRs) than over single cropping regions (SCRs), with increases in the daily maximum temperature as large as 1.02 degrees C. Using regional climate modelling, we attribute the higher temperatures in DCRs to reduced evapotranspiration during the inter-cropping period. The higher surface temperatures in June and July affect low-level circulation and, in turn, rainfall associated with the East Asian monsoon over the NCP and neighbouring countries. These findings suggest that double cropping in the NCP can amplify the magnitude of summertime climate changes over East Asia. C1 [Jeong, Su-Jong] CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA. [Ho, Chang-Hoi; Lee, Yun-Bok; Jhun, Jong-Ghap] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul 151747, South Korea. [Piao, Shilong] Peking Univ, Sino French Inst Earth Syst Sci, Coll Urban & Environm Sci, Beijing 100871, Peoples R China. [Piao, Shilong] Chinese Acad Sci, Inst Tibetan Plateau Res, Lab Alpine Ecol & Biodivers, Beijing 100101, Peoples R China. [Kim, Jinwon] Univ Calif Los Angeles, JIFRESSE, Los Angeles, CA 90095 USA. [Kim, Jinwon] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA. [Ciais, Philippe] CE lOrme Merisiers, CEA CNRS UVSQ, Lab Sci Climat & Environm, F-91191 Gif Sur Yvette, France. [Park, Seon Ki] Ewha Womans Univ, Dept Environm Sci & Engn, Seoul 120750, South Korea. [Park, Seon Ki] Ewha Womans Univ, Dept Atmospher Sci & Engn, Seoul 120750, South Korea. [Park, Seon Ki] Ewha Womans Univ, Ctr Climate Environm Change Predict Res, Seoul 120750, South Korea. RP Ho, CH (reprint author), Seoul Natl Univ, Sch Earth & Environm Sci, Seoul 151747, South Korea. EM hoch@cpl.snu.ac.kr RI Jeong, Su-Jong/J-4110-2014; Ho, Chang-Hoi/H-8354-2015 FU Korea Ministry of Environment as 'Climate Change Correspondence RD Program' [CATER 2012~2040, NRF 2009-0083527] FX This work was funded by the Korea Ministry of Environment as 'Climate Change Correspondence R&D Program', CATER 2012~2040, and NRF 2009-0083527. The funders had no role in the study design, data collection and analysis, decision to publish, or presentation of the manuscript. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 26 TC 10 Z9 12 U1 14 U2 61 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 JUL PY 2014 VL 4 IS 7 BP 615 EP 619 DI 10.1038/NCLIMATE2266 PG 5 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AL0SP UT WOS:000338837400029 ER PT J AU Mishchenko, MI Dlugach, ZM Zakharova, NT AF Mishchenko, Michael I. Dlugach, Zhanna M. Zakharova, Nadezhda T. TI Direct demonstration of the concept of unrestricted effective-medium approximation SO OPTICS LETTERS LA English DT Article ID PARTICLES; DERIVATION; INCLUSIONS; SCATTERING; DROPLETS; OPTICS AB The modified unrestricted effective-medium refractive index is defined as one that yields accurate values of a representative set of far-field scattering characteristics (including the scattering matrix) for an object made of randomly heterogeneous materials. We validate the concept of the modified unrestricted effective-medium refractive index by comparing numerically exact superposition T-matrix results for a spherical host randomly filled with a large number of identical small inclusions and Lorenz-Mie results for a homogeneous spherical counterpart. A remarkable quantitative agreement between the superposition T-matrix and Lorenz-Mie scattering matrices over the entire range of scattering angles demonstrates unequivocally that the modified unrestricted effective-medium refractive index is a sound (albeit still phenomenological) concept provided that the size parameter of the inclusions is sufficiently small and their number is sufficiently large. Furthermore, it appears that in cases when the concept of the modified unrestricted effective-medium refractive index works, its actual value is close to that predicted by the Maxwell-Garnett mixing rule. (C) 2014 Optical Society of America C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Dlugach, Zhanna M.] Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine. [Zakharova, Nadezhda T.] Trinnovim LLC, New York, NY 10025 USA. RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM michael.i.mishchenko@nasa.gov RI Mishchenko, Michael/D-4426-2012 FU NASA Remote Sensing Theory Program; National Academy of Sciences of Ukraine under the Main Astronomical Observatory GRAPE/GPU/GRID Computing Cluster Project; NASA Radiation Sciences Program FX We thank Li Liu for technical assistance and Daniel Mackowski and Gorden Videen for instructive discussions. This material is based upon work supported by the NASA Remote Sensing Theory Program managed by Lucia Tsaoussi and the NASA Radiation Sciences Program managed by Hal Maring. We also acknowledge support from the National Academy of Sciences of Ukraine under the Main Astronomical Observatory GRAPE/GPU/GRID Computing Cluster Project. NR 22 TC 14 Z9 14 U1 1 U2 9 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 JUL 1 PY 2014 VL 39 IS 13 BP 3935 EP 3938 DI 10.1364/OL.39.003935 PG 4 WC Optics SC Optics GA AL2CJ UT WOS:000338933200062 PM 24978775 ER PT J AU Hilker, T Hall, FG Coops, NC Black, AT Jassal, R Mathys, A Grant, N AF Hilker, Thomas Hall, Forrest G. Coops, Nicholas C. Black, Andrew T. Jassal, Rachhpal Mathys, Amanda Grant, Nicholas TI Potentials and limitations for estimating daytime ecosystem respiration by combining tower-based remote sensing and carbon flux measurements SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE GPP; Daytime fluxes; Q(10); Light-use efficiency; Multi-angular remote sensing; Amspec; Eddy-covariance; Ecosystem carbon flux; Ecosystem respiration ID LEAF-AREA INDEX; LIGHT-USE EFFICIENCY; EUROPEAN FORESTS; SOIL RESPIRATION; TEMPERATURE; DIOXIDE; CANOPY; PHOTOSYNTHESIS; REFLECTANCE; EXCHANGE AB Vegetation carbon uptake and respiration constitute the largest carbon cycle of the planet with an annual turnover in the order of 120 GT. Currently, neither ecosystem carbon uptake (through photosynthesis) nor ecosystem carbon release (through respiration) can be measured directly during the daytime. Instead, flux-tower measurements rely on nighttime respiration based on the assumption of zero carbon uptake which are then projected to daytime using an exponential relationship to soil temperature at shallow soil depth. As an alternative to this approach, R could possibly also be determined from combining daytime eddy covariance measurements of net ecosystem production (NEP) and spectral observations of gross primary production (GPP). In previous work, we have shown that multi-angular observations can be used to determine GPP from the absorbed photosynthetically active radiation (APAR) and spectrally obtained observations of light-use efficiency (epsilon). The difference of NEP and GPP suggests that daytime respiration is greater and more dynamic than conventional estimates derived from nighttime flux values. Our findings also suggest that an accelerated ecosystem metabolism results in an exponential increase in respiration which eventually diminishes net ecosystem production. Respiration was also closely related to air and soil temperature. We conclude that tower-level spectral measurements provide considerable new insights into ecosystem fluxes as they allow independent yet complementary measurements of different aspects of the carbon and energy cycle. (C) 2014 Elsevier Inc All rights reserved. C1 [Hilker, Thomas] Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA. [Hall, Forrest G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Coops, Nicholas C.; Mathys, Amanda] Univ British Columbia, Fac Forest Resources Mgmt, Vancouver, BC V6T 1Z4, Canada. [Black, Andrew T.; Jassal, Rachhpal; Grant, Nicholas] Univ British Columbia, Fac Land & Food Syst, Vancouver, BC V6T 1Z4, Canada. RP Hilker, T (reprint author), Oregon State Univ, Coll Forestry, 231 Peavy Hall, Corvallis, OR 97331 USA. EM thomas.hilker@oregonstate.edu RI Coops, Nicholas/J-1543-2012 OI Coops, Nicholas/0000-0002-0151-9037 FU Canadian Carbon Program (Canadian Foundation for Climate and Atmospheric Sciences (CFCAS); Natural Sciences and Engineering Research Council of Canada (NSERC); BIOCAP; NSERC-Accelerator grant FX Thank you to Zoran Nesic, Dominic Lessard, Andrew Hum and Rick Ketler from UBC Faculty of Land and Food Systems (LFS) for their assistance in technical design, installation, and maintenance of Amspec and Amspec II. Mathew Brown is thanked for analyzing the EC data. The quality control for the climate data at SOA was done by Alan Barr. This research was partially funded by the Canadian Carbon Program (Canadian Foundation for Climate and Atmospheric Sciences (CFCAS)), the Natural Sciences and Engineering Research Council of Canada (NSERC) and BIOCAP, and an NSERC-Accelerator grant to Coops. NR 45 TC 3 Z9 3 U1 0 U2 44 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 JUL PY 2014 VL 150 BP 44 EP 52 DI 10.1016/j.rse.2014.04.018 PG 9 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AL3OG UT WOS:000339037500004 ER PT J AU Liu, Y Hansen, M Gupta, G Malik, W Jung, Y AF Liu, Yi Hansen, Mark Gupta, Gautam Malik, Waqar Jung, Yoon TI Predictability impacts of airport surface automation SO TRANSPORTATION RESEARCH PART C-EMERGING TECHNOLOGIES LA English DT Article DE Airport surface operations; Gate holding; Automation; Predictability; Performance metrics ID TRAVEL-TIME PREDICTION; INFORMATION; UNCERTAINTY AB Past evaluations of airport surface operations automation technologies have focused on capacity utilization, delay mitigation and fuel efficiency impacts. Predictability, while recognized as an important operational performance goal, has received little attention. One reason could be that applicable predictability metrics have not been developed in the context of airport surface operations management. This research fills the gap by proposing metrics for predictability performance evaluation. Using results from a SARDA humanin-the-loop simulation conducted at NASA Ames' Future Flight Central, we present a comprehensive assessment of the predictability impacts of airport surface automation. A wide range of the impacts is considered, which includes variability in taxi-out time, predictability of take-off time and take-off sequence, entropy of the airfield state, and perceived predictability from users. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Liu, Yi; Hansen, Mark] Univ Calif Berkeley, Dept Civil & Environm Engn, Berkeley, CA 94720 USA. [Gupta, Gautam; Malik, Waqar] Univ Calif Santa Cruz, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Jung, Yoon] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Liu, Y (reprint author), Univ Calif Berkeley, Dept Civil & Environm Engn, 107 McLaughlin Hall, Berkeley, CA 94720 USA. EM liuyisha@berkeley.edu FU NASA Aligned Research Program Award FX The study is supported by NASA Aligned Research Program Award. We would like to thank Frank Ketcham, pilot with Delta Airlines, for his valuable comments on aircraft surface operations. We would also like to thank Victoria L. Dulchinos, Miwa Hayashi and Ty Hoang at NASA Ames Research Center for their support in the research process. Last but not least, special thanks go to Professor Rhonda Righter at University of California at Berkeley for her comments on Markov Chain process and Professor Yu Zhang at University of South Florida for her comments on taxi-out time regression analysis. NR 53 TC 2 Z9 2 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0968-090X J9 TRANSPORT RES C-EMER JI Transp. Res. Pt. C-Emerg. Technol. PD JUL PY 2014 VL 44 BP 128 EP 145 DI 10.1016/j.trc.2014.03.010 PG 18 WC Transportation Science & Technology SC Transportation GA AL3OC UT WOS:000339037100009 ER PT J AU Raghavan, RK Almes, K Goodin, DG Harrington, JA Stackhouse, PW AF Raghavan, Ram K. Almes, Kelli Goodin, Doug G. Harrington, John A., Jr. Stackhouse, Paul W., Jr. TI Spatially Heterogeneous Land Cover/Land Use and Climatic Risk Factors of Tick-Borne Feline Cytauxzoonosis SO VECTOR-BORNE AND ZOONOTIC DISEASES LA English DT Article DE Cytauxzoonosis; Feline; Geographical Information Systems (GIS); Geographically Weighted Regression (GWR); Multivariate logistic; Climate; Humidity; Diurnal Temperature Range (DTR); NASA ID GEOGRAPHICALLY WEIGHTED REGRESSION; UNITED-STATES; AMBLYOMMA-AMERICANUM; TRANSMISSION; TEMPERATURE; DISEASES; VECTOR; TULAREMIA; MISSOURI; IXODIDAE AB Background: Feline cytauxzoonosis is a highly fatal tick-borne disease caused by a hemoparasitic protozoan, Cytauxzoon felis. This disease is a leading cause of mortality for cats in the Midwestern United States, and no vaccine or effective treatment options exist. Prevention based on knowledge of risk factors is therefore vital. Associations of different environmental factors, including recent climate were evaluated as potential risk factors for cytauxzoonosis using Geographic Information Systems (GIS). Methods: There were 69 cases determined to be positive for cytauxzoonosis based upon positive identification of C. felis within blood film examinations, tissue impression smears, or histopathologic examination of tissues. Negative controls totaling 123 were selected from feline cases that had a history of fever, malaise, icterus, and anorexia but lack of C. felis within blood films, impression smears, or histopathologic examination of tissues. Additional criteria to rule out C. felis among controls were the presence of regenerative anemia, cytologic examination of blood marrow or lymph node aspirate, other causative agent diagnosed, or survival of 25 days or greater after testing. Potential environmental determinants were derived from publicly available sources, viz., US Department of Agriculture (soil attributes), US Geological Survey (land-cover/landscape, landscape metrics), and NASA (climate). Candidate variables were screened using univariate logistic models with a liberal p value (0.2), and associations with cytauxzoonosis were modeled using a global multivariate logistic model (p < 0.05). Spatial heterogeneity among significant variables in the study region was modeled using a geographically weighted regression (GWR) approach. Results: Total Edge Contrast Index (TECI), grassland-coverage, humidity conditions recorded during the 9th week prior to case arrival, and an interaction variable, "diurnal temperature range percent mixed forest area" were significant risk factors for cytauxzoonosis in the study region. TECI and grassland areas exhibited significant regional differences in their effects on cytauxzoonosis outcome, whereas others were uniform. Conclusions: Land-cover areas favorable for tick habitats and climatic conditions that favor the tick life cycle are strong risk factors for feline cytauxzoonosis. Spatial heterogeneity and interaction effects between land-cover and climatic variables may reveal new information when evaluating risk factors for vector-borne diseases. C1 [Raghavan, Ram K.; Almes, Kelli] Kansas State Univ, Coll Vet Med, Dept Diagnost Med Pathobiol, Kansas State Vet Diagnost Lab, Manhattan, KS 66506 USA. [Goodin, Doug G.; Harrington, John A., Jr.] Kansas State Univ, Dept Geog, Coll Arts & Sci, Manhattan, KS 66506 USA. [Stackhouse, Paul W., Jr.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Raghavan, RK (reprint author), Kansas State Vet Diagnost Lab, 1800 Denison Ave, Manhattan, KS 66506 USA. EM rkraghavan@vet.k-state.edu FU Kansas State Veterinary Diagnostic Laboratory (KSVDL); NASA Earth Science Directorate Applied Science Program FX This study was supported by the Kansas State Veterinary Diagnostic Laboratory (KSVDL). We thank James M. Hoell, SSAI at the NASA Langley Research Center, for his excellent help in providing methods to more easily access the POWER data used in the analyses. The NASA Langley Research Center POWER Project is funded through the NASA Earth Science Directorate Applied Science Program. NR 38 TC 4 Z9 4 U1 1 U2 36 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1530-3667 EI 1557-7759 J9 VECTOR-BORNE ZOONOT JI Vector-Borne Zoonotic Dis. PD JUL PY 2014 VL 14 IS 7 BP 486 EP 495 DI 10.1089/vbz.2013.1496 PG 10 WC Public, Environmental & Occupational Health; Infectious Diseases SC Public, Environmental & Occupational Health; Infectious Diseases GA AL8MO UT WOS:000339393500004 PM 24978652 ER PT J AU Cochran, P Huntington, OH Pungowiyi, C Tom, S Chapin, FS Huntington, HP Maynard, NG Trainor, SF AF Cochran, Patricia Huntington, Orville H. Pungowiyi, Caleb Tom, Stanley Chapin, F. Stuart, III Huntington, Henry P. Maynard, Nancy G. Trainor, Sarah F. TI Indigenous frameworks for observing and responding to climate change in Alaska (vol 120, pg 557, 2013) SO CLIMATIC CHANGE LA English DT Correction C1 [Cochran, Patricia] Alaska Native Sci Commiss, Anchorage, AK 99524 USA. [Huntington, Orville H.] Tanana Chiefs Conf, Wildlife & Parks, Fairbanks, AK 99701 USA. [Tom, Stanley] Newtok Village Council, Newtok, AK 99559 USA. [Chapin, F. Stuart, III] Univ Alaska Fairbanks, Inst Arctic Biol, Fairbanks, AK 99775 USA. [Maynard, Nancy G.] NASA, Goddard Space Flight Ctr, Cryospher Sci Branch, Greenbelt, MD 20771 USA. [Trainor, Sarah F.] Univ Alaska Fairbanks, Alaska Ctr Climate Assessment & Policy, Fairbanks, AK 99775 USA. RP Chapin, FS (reprint author), Univ Alaska Fairbanks, Inst Arctic Biol, Fairbanks, AK 99775 USA. EM terry.chapin@alaska.edu NR 1 TC 0 Z9 0 U1 1 U2 11 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0165-0009 EI 1573-1480 J9 CLIMATIC CHANGE JI Clim. Change PD JUL PY 2014 VL 125 IS 2 BP 279 EP 279 DI 10.1007/s10584-014-1187-z PG 1 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AK9XF UT WOS:000338781200013 ER PT J AU Ortega-Retuerta, E Fichot, CG Arrigo, KR Van Dijken, GL Joux, F AF Ortega-Retuerta, E. Fichot, C. G. Arrigo, K. R. Van Dijken, G. L. Joux, F. TI Response of marine bacterioplankton to a massive under-ice phytoplankton bloom in the Chukchi Sea (Western Arctic Ocean) SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY LA English DT Article DE Phytoplankton; Bacterioplankton; Dissolved organic matter; Temperature effects; Arctic Ocean ID BACTERIAL CARBON METABOLISM; DISSOLVED ORGANIC-MATTER; SOUTHERN-OCEAN; ANTARCTIC PENINSULA; MICROBIAL-GROWTH; LOW-TEMPERATURE; SPRING BLOOM; SUMMER; WATERS; RESPIRATION AB The activity of heterotrophic bacterioplankton and their response to changes in primary production in the Arctic Ocean is essential to understand biogenic carbon flows in the area. In this study, we explored the patterns of bacterial abundance (BA) and bacterial production (BP) in waters coinciding with a massive under-ice phytoplankton bloom in the Chukchi Sea in summer 2011, where chlorophyll a (chl a) concentrations were up to 38.9 mg m(-3). Contrary to our expectations, BA and BP did not show their highest values coinciding with the bloom. In fact, bacterial biomass was only 3.5% of phytoplankton biomass. Similarly, average DOC values were similar inside (average 57.2 +/- 3.1 mu M) and outside (average 64.3 +/- 4.8 mu M) the bloom patch. Regression analyses showed relatively weak couplings, in terms of slope values, between chl a or primary production and BA or BR Multiple regression analyses indicated that both temperature and chl a explained BA and BP variability in the Chukchi Sea. This temperature dependence was confirmed experimentally, as higher incubation temperatures (6.6 degrees C vs. 2.2 degrees C) enhanced BA and BP, with Q(10) values of BP up to 20.0. Together, these results indicate that low temperatures in conjunction with low dissolved organic matter release can preclude bacteria to efficiently process a higher proportion of carbon fixed by phytoplankton, with further consequences on the carbon cycling in the area. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Ortega-Retuerta, E.] CSIC, Inst Ciencias Mar, Barcelona, Spain. [Ortega-Retuerta, E.; Joux, F.] Univ Paris 06, Sorbonne Univ, UMR 7621, Lab Oceanog Microbienne,Observ Oceanol, F-66650 Banyuls Sur Mer, France. [Ortega-Retuerta, E.; Joux, F.] CNRS, UMR 7621, Lab Oceanog Microbienne, Observ Oceanol, F-66650 Banyuls Sur Mer, France. [Fichot, C. G.] Univ S Carolina, Marine Sci Program, Columbia, SC 29208 USA. [Fichot, C. G.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Arrigo, K. R.; Van Dijken, G. L.] Stanford Univ, Dept Environm Earth Syst Sci, Stanford, CA 94305 USA. RP Ortega-Retuerta, E (reprint author), CSIC, Inst Ciencias Mar, Barcelona, Spain. EM ortegaretuerta@icm.csic.es RI Joux, Fabien/F-8107-2010; Ortega-Retuerta, Eva/I-2432-2015 OI Ortega-Retuerta, Eva/0000-0003-0780-8347 FU Ocean Biology and Biogeochemistry Program; Cryosphere Science Program of the National Aeronautic and Space Administration [NNX10AF42G]; French National Research Agency [ANR-BLAN08-1 310980]; LEFE-CYBER programme; CNES TOSCA programme; Arctic Net; European Space Agency FX We thank the captain and crew of USCGC 'Healy' on the HLY1101 mission to the Chukchi Sea for their assistance in the field during the NASA ICESCAPE cruise, and S.R. Laney for his help with flow cytometric analyses. This work was supported by the Ocean Biology and Biogeochemistry Program and the Cryosphere Science Program of the National Aeronautic and Space Administration (NNX10AF42G to K. Arrigo) and by the French National Research Agency, under the Grant no. ANR-BLAN08-1 310980 to the MALINA project, the LEFE-CYBER and CNES TOSCA programmes, Arctic Net, and the European Space Agency. We thank two anonymous reviewers that helped improve the manuscript. NR 43 TC 4 Z9 5 U1 2 U2 42 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 JUL PY 2014 VL 105 BP 74 EP 84 DI 10.1016/j.dsr2.2014.03.015 PG 11 WC Oceanography SC Oceanography GA AL2TP UT WOS:000338978700006 ER PT J AU Loughner, CP Tzortziou, M Follette-Cook, M Pickering, KE Goldberg, D Satam, C Weinheimer, A Crawford, JH Knapp, DJ Montzka, DD Diskin, GS Dickerson, RR AF Loughner, Christopher P. Tzortziou, Maria Follette-Cook, Melanie Pickering, Kenneth E. Goldberg, Daniel Satam, Chinmay Weinheimer, Andrew Crawford, James H. Knapp, David J. Montzka, Denise D. Diskin, Glenn S. Dickerson, Russell R. TI Impact of Bay-Breeze Circulations on Surface Air Quality and Boundary Layer Export SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID NONLOCAL CLOSURE-MODEL; SEA-BREEZE; CHESAPEAKE BAY; UNITED-STATES; PHOTOCHEMICAL SIMULATIONS; POLLUTANT TRANSPORT; IBERIAN PENINSULA; CARBON-MONOXIDE; CLIMATE-CHANGE; WEST-COAST AB Meteorological and air-quality model simulations are analyzed alongside observations to investigate the role of the Chesapeake Bay breeze on surface air quality, pollutant transport, and boundary layer venting. A case study was conducted to understand why a particular day was the only one during an 11-day ship-based field campaign on which surface ozone was not elevated in concentration over the Chesapeake Bay relative to the closest upwind site and why high ozone concentrations were observed aloft by in situ aircraft observations. Results show that southerly winds during the overnight and early-morning hours prevented the advection of air pollutants from the Washington, D.C., and Baltimore, Maryland, metropolitan areas over the surface waters of the bay. A strong and prolonged bay breeze developed during the late morning and early afternoon along the western coastline of the bay. The strength and duration of the bay breeze allowed pollutants to converge, resulting in high concentrations locally near the bay-breeze front within the Baltimore metropolitan area, where they were then lofted to the top of the planetary boundary layer (PBL). Near the top of the PBL, these pollutants were horizontally advected to a region with lower PBL heights, resulting in pollution transport out of the boundary layer and into the free troposphere. This elevated layer of air pollution aloft was transported downwind into New England by early the following morning where it likely mixed down to the surface, affecting air quality as the boundary layer grew. C1 [Loughner, Christopher P.; Tzortziou, Maria] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Loughner, Christopher P.; Tzortziou, Maria; Follette-Cook, Melanie; Pickering, Kenneth E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Follette-Cook, Melanie] Morgan State Univ, Baltimore, MD 21239 USA. [Goldberg, Daniel; Dickerson, Russell R.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Satam, Chinmay] Univ Maryland, Dept Chem & Biomol Engn, College Pk, MD 20742 USA. [Weinheimer, Andrew; Knapp, David J.; Montzka, Denise D.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Crawford, James H.; Diskin, Glenn S.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Loughner, CP (reprint author), NASA, Earth Syst Sci Interdisciplinary Ctr, GSFC, Code 614, Greenbelt, MD 20771 USA. EM christopher.p.loughner@nasa.gov RI Pickering, Kenneth/E-6274-2012; Dickerson, Russell/F-2857-2010; OI Dickerson, Russell/0000-0003-0206-3083; Loughner, Christopher/0000-0002-3833-2014 FU National Science Foundation FX The National Center for Atmospheric Research is sponsored by the National Science Foundation. NR 73 TC 13 Z9 14 U1 2 U2 31 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 JUL PY 2014 VL 53 IS 7 BP 1697 EP 1713 DI 10.1175/JAMC-D-13-0323.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AL0KY UT WOS:000338817000001 ER PT J AU Battaglia, A Tanelli, S Heymsfield, GM Tian, L AF Battaglia, Alessandro Tanelli, Simone Heymsfield, Gerald M. Tian, Lin TI The Dual Wavelength Ratio Knee: A Signature of Multiple Scattering in Airborne Ku-Ka Observations SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID RADAR MEASUREMENTS; MODEL DESCRIPTION; GPM PERSPECTIVE; PART II; ATTENUATION; CLOUDSAT; RAINFALL; RANGE AB Deep convective systems observed by the High Altitude Imaging Wind and Rain Airborne Profiler (HIWRAP) radar during the 2011 Midlatitude Continental Convective Clouds Experiment (MC3E) field campaign in Oklahoma provide the first evidence of multiple-scattering effects simultaneously at Ku and Ka band. One feature is novel and noteworthy: often, in correspondence to shafts with strong convection and when moving from the top of the cloud downward, the dual wavelength ratio (DWR) first increases as usual in Ku-Ka-band observations, but then it reaches a maximum and after that point it steadily decreases all the way to the surface, forming what will be hereinafter referred to as a knee. This DWR knee cannot be reproduced by single-scattering theory under almost any plausible cloud microphysical profile. On the other hand, it is explained straightforwardly with the help of multiple-scattering theory when simulations involving hail-bearing convective cores with large horizontal extents are performed. The DWR reduction in the lower troposphere (i.e., DWR increasing with altitude) is interpreted as the result of multiple-scattering pulse stretching caused by the highly diffusive hail layer positioned high up in the atmosphere, with Ka multiple scattering typically exceeding that occurring in the Ku channel. Since the effects of multiple scattering increase with increasing footprint size, if multiple-scattering effects are present in the aircraft measurements, they are likely to be more pronounced in the spaceborne dual-frequency Ku Ka radar observations, envisaged for the NASA Japan Aerospace Exploration Agency (JAXA) Global Precipitation Measurement (GPM) Mission, launched in February 2014. This notional study supports the idea that DWR knees will be observed by the GPM radar when overflying high-density ice shafts embedded in large convective systems and suggests that their explanation must not be sought in differential attenuation or differential Mie effects but via multiple-scattering effects. C1 [Battaglia, Alessandro] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Tanelli, Simone] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Heymsfield, Gerald M.; Tian, Lin] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tian, Lin] Morgan State Univ, Baltimore, MD 21239 USA. RP Battaglia, A (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. EM ab474@le.ac.uk RI Measurement, Global/C-4698-2015; OI Battaglia, Alessandro/0000-0001-9243-3484 FU NCEO Mission Support FX A portion of this work was funded by the NCEO Mission Support. A portion of this work (Tanelli) was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. This work was carried for the GPM mission under the Precipitation Measurement Missions program; support by Dr. Ramesh Kakar is gratefully acknowledged. The work performed by the engineering team led by Michael Coon, Lihua Li, Matthew McLinden, and Martin Perrine at Goddard made the measurements possible. NR 30 TC 6 Z9 6 U1 2 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 JUL PY 2014 VL 53 IS 7 BP 1790 EP 1808 DI 10.1175/JAMC-D-13-0341.1 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AL0KY UT WOS:000338817000007 ER PT J AU Wang, CP Luo, ZJ Chen, XH Zeng, XP Tao, WK Huang, XL AF Wang, Chunpeng Luo, Zhengzhao Johnny Chen, Xiuhong Zeng, Xiping Tao, Wei-Kuo Huang, Xianglei TI A Physically Based Algorithm for Non-Blackbody Correction of Cloud-Top Temperature and Application to Convection Study SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID RADIATIVE-TRANSFER MODEL; A-TRAIN; ICE; RETRIEVAL; MODIS; PRECIPITATION; MICROPHYSICS; SIMULATION; PRODUCTS; RADAR AB Cloud-top temperature (CTT) is an important parameter for convective clouds and is usually different from the 11-mu m brightness temperature due to non-blackbody effects. This paper presents an algorithm for estimating convective CTT by using simultaneous passive [Moderate Resolution Imaging Spectroradiometer (MODIS)] and active [CloudSat + Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO)] measurements of clouds to correct for the non-blackbody effect. To do this, a weighting function of the MODIS 11-mu m band is explicitly calculated by feeding cloud hydrometer profiles from CloudSat and CALIPSO retrievals and temperature and humidity profiles based on ECMWF analyses into a radiation transfer model. Among 16 837 tropical deep convective clouds observed by CloudSat in 2008, the averaged effective emission level (EEL) of the 11-mu m channel is located at optical depth similar to 0.72, with a standard deviation of 0,3. The distance between the EEL and cloud-top height determined by CloudSat is shown to be related to a parameter called cloud-top fuzziness (CTF), defined as the vertical separation between -30 and 10 dBZ of CloudSat radar reflectivity. On the basis of thee findings a relationship is then developed between the CTF and the difference between MODIS 11-mu m brightness temperature and physical CTT, the latter being the non-blackbody correction of CTT. Correction of the non-blackbody effect of CTT is applied to analyze convective cloud-top buoyancy. With this correction, about 70% of the convective cores observed by CloudSat in the height range of 6-10 km have positive buoyancy near cloud top, meaning clouds are still growing vertically, although their final fate cannot be determined by snapshot observations. C1 [Wang, Chunpeng; Chen, Xiuhong; Huang, Xianglei] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Luo, Zhengzhao Johnny] CUNY City Coll, Dept Earth & Atmospher Sci, New York, NY 10031 USA. [Luo, Zhengzhao Johnny] CUNY City Coll, NOAA, Cooperat Remote Sensing Sci & Technol Ctr, New York, NY 10031 USA. [Zeng, Xiping; Tao, Wei-Kuo] NASA, Goddard Space Flight Ctr, Mesoscale Atmospher Proc Lab, Greenbelt, MD 20771 USA. RP Wang, CP (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, 2455 Hayward St, Ann Arbor, MI 48109 USA. EM cpwang@umich.edu RI Huang, Xianglei/G-6127-2011; Chen, Xiuhong/P-4030-2014 OI Huang, Xianglei/0000-0002-7129-614X; FU NASA MAP project [NNX09AJ46G]; NASA CloudSat/CALIPSO Science Team [NNX10AM31G]; SEAC4RS Science Team [NNX12AC13G] FX The CloudSat data were obtained from the CloudSat Data Processing Center. The MODIS data were obtained from NASA Goddard DISC. The ECMWF interim data used in this study were obtained online (http://data.ecmwf.int/data/). We thank all three reviewers for their insightful and thorough comments, which greatly improved the clarity of the article. This research is supported by the NASA MAP project under Grant NNX09AJ46G awarded to the University of Michigan, the NASA CloudSat/CALIPSO Science Team under Grant NNX10AM31G, and the SEAC4RS Science Team under Grant NNX12AC13G, awarded to the City University of New York (CUNY). NR 45 TC 4 Z9 4 U1 0 U2 7 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 JUL PY 2014 VL 53 IS 7 BP 1844 EP 1857 DI 10.1175/JAMC-D-13-0331.1 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AL0KY UT WOS:000338817000010 ER PT J AU Kusaka, A Wollack, EJ Stevenson, TR AF Kusaka, Akito Wollack, Edward J. Stevenson, Thomas R. TI Angular and polarization response of multimode sensors with resistive-grid absorbers SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA A-OPTICS IMAGE SCIENCE AND VISION LA English DT Article ID CROSS-POLARIZATION; GRAVITY-WAVES; POLARIMETER; DETECTORS; SUBMILLIMETER; BOLOMETERS; INSTRUMENT; ARRAYS; PROBE; HORN AB High-sensitivity receiver systems with near-ideal polarization sensitivity are highly desirable for development of millimeter and submillimeter radio astronomy. Multimoded bolometers provide a unique solution to achieve such sensitivity, for which hundreds of single-mode sensors would otherwise be required. The primary concern in employing such multimoded sensors for polarimetery is the control of the polarization systematics. In this work, we examine the angular- and polarization-dependent absorption pattern of a thin resistive grid or membrane, which models an absorber used for a multimoded bolometer. The result shows that a freestanding thin resistive absorber with a surface resistivity of eta/2, where eta is the impedance of free space, attains a beam pattern with equal E- and H-plane responses, leading to zero cross-polarization. For a resistive-grid absorber, the condition is met when a pair of grids is positioned orthogonal to each other and both have a resistivity of eta/2. When a reflective backshort termination is employed to improve absorption efficiency, the cross-polar level can be suppressed below -30 dB if acceptance angle of the sensor is limited to less than or similar to 60 degrees. The small cross-polar systematics have even-parity patterns and do not contaminate the measurements of odd-parity polarization patterns, for which many of the recent instruments for cosmic microwave background are designed. Underlying symmetry that suppresses these cross-polar systematics is discussed in detail. The estimates and formalism provided in this work offer key tools in the design consideration of the instruments using the multimoded polarimeters. (C) 2014 Optical Society of America C1 [Kusaka, Akito] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Wollack, Edward J.; Stevenson, Thomas R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kusaka, A (reprint author), Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. EM akusaka@princeton.edu RI Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 FU Dicke Fellowship FX This work was done in the context of developing experimental projects using multimoded detectors, in particular MuSE and PIXIE. We thank the collaborators of these projects; especially we acknowledge D. J. Fixen, A. J. Kogut, S. S. Meyer, and S. T. Staggs for their insights and persistent encouragement. We thank L. A. Page and N. Jarosik for fruitful discussions. A. K. acknowledges the Dicke Fellowship. NR 58 TC 2 Z9 2 U1 3 U2 12 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1084-7529 EI 1520-8532 J9 J OPT SOC AM A JI J. Opt. Soc. Am. A-Opt. Image Sci. Vis. PD JUL 1 PY 2014 VL 31 IS 7 BP 1557 EP 1576 DI 10.1364/JOSAA.31.001557 PG 20 WC Optics SC Optics GA AL1IG UT WOS:000338878500025 PM 25121445 ER PT J AU Van Laerhoven, C Barnes, R Greenberg, R AF Van Laerhoven, C. Barnes, R. Greenberg, R. TI Tides, planetary companions, and habitability: habitability in the habitable zone of low-mass stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE astrobiology; celestial mechanics; planetary systems ID MAIN-SEQUENCE STARS; EXTRASOLAR GIANT PLANETS; TIDAL EVOLUTION; ALBEDO FEEDBACK; SYSTEM; SATELLITES; STABILITY; LIFETIMES; CLIMATE; LIMITS AB Earth-scale planets in the classical habitable zone (HZ) are more likely to be habitable if they possess active geophysics. Without a constant internal energy source, planets cool as they age, eventually terminating tectonic activity. Planets orbiting low-mass stars can be very old, due to the longevity of such stars, so they may be rendered sterile to life in this way. However, the presence of an outer companion could generate enough tidal heat in the HZ planet to prevent such cooling. The range of mass and orbital parameters for the companion that give adequate long-term heating of the inner HZ planet, while avoiding very early total desiccation, is probably substantial. We locate the ideal location for the outer of a pair of planets, under the assumption that the inner planet has the same incident flux as Earth, orbiting example stars: a generic late M dwarf (T-eff = 2670 K) and the M9V/L0 dwarf DEN1048. Thus discoveries of Earth-scale planets in the HZ zone of old small stars should be followed by searches for outer companion planets that might be essential for current habitability. C1 [Van Laerhoven, C.; Greenberg, R.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Barnes, R.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Barnes, R.] NASA, Virtual Planetary Lab, Seattle, WA 98195 USA. RP Van Laerhoven, C (reprint author), Univ Arizona, Dept Planetary Sci, 1629 E Univ Blvd, Tucson, AZ 85721 USA. EM c.vanlaerhoven@gmail.com FU NASA Earth and Space Science Fellowship program; NSF [AST-110882] FX CVL would like to acknowledge the NASA Earth and Space Science Fellowship program. RB would like to acknowledge NSF grant AST-110882, and the NASA Astrobiology Institute's Virtual Planetary Laboratory lead team. NR 38 TC 3 Z9 3 U1 0 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 1 PY 2014 VL 441 IS 3 BP 1888 EP 1898 DI 10.1093/mnras/stu685 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK9RE UT WOS:000338763600004 ER PT J AU Fernandez-Cobos, R Vielva, P Pietrobon, D Balbi, A Martinez-Gonzalez, E Barreiro, RB AF Fernandez-Cobos, R. Vielva, P. Pietrobon, D. Balbi, A. Martinez-Gonzalez, E. Barreiro, R. B. TI Searching for a dipole modulation in the large-scale structure of the Universe SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; large-scale structure of Universe ID MICROWAVE-ANISOTROPY-PROBE; HEMISPHERICAL POWER ASYMMETRY; DARK ENERGY CONSTRAINTS; EIS-NVSS SURVEY; BACKGROUND ANOMALIES; RADIO GALAXIES; SKY SURVEY; SPHERICAL WAVELETS; WMAP OBSERVATIONS; NON-GAUSSIANITY AB Several statistical anomalies in the cosmic microwave background (CMB) temperature anisotropies seem to defy the assumption of a homogeneous and isotropic universe. In particular, a dipole modulation has been detected both in WMAP and Planck data. We adapt the methodology proposed by Eriksen et al. on CMB data to galaxy surveys, tracing the large-scale structure. We analyse the National Radio Astronomy Observatory (NRAO) and Very Large Array (VLA) Sky Survey data at a resolution of similar to 2A degrees for three different flux thresholds: 2.5, 5.0 and 10.0 mJy, respectively. No evidence of a dipole modulation is found. This result suggests that the origin of the dipole asymmetry found in the CMB cannot be assigned to secondary anisotropies produced at redshifts around z = 1. However, it could still have been generated at redshifts higher or lower, such as the integrated Sachs-Wolfe effect produced by the local structures. Other all-sky surveys, like the infrared WISE catalogue, could help to explore with a high sensitivity a redshift interval closer than the one probed with NVSS. C1 [Fernandez-Cobos, R.; Vielva, P.; Martinez-Gonzalez, E.; Barreiro, R. B.] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain. [Fernandez-Cobos, R.] Univ Cantabria, Dept Fis Moderna, E-39005 Santander, Spain. [Pietrobon, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Balbi, A.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Balbi, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. RP Fernandez-Cobos, R (reprint author), Univ Cantabria, CSIC, Inst Fis Cantabria, Avda Castros S-N, E-39005 Santander, Spain. EM cobos@ifca.unican.es RI Vielva, Patricio/F-6745-2014; Barreiro, Rita Belen/N-5442-2014; Martinez-Gonzalez, Enrique/E-9534-2015 OI Vielva, Patricio/0000-0003-0051-272X; Barreiro, Rita Belen/0000-0002-6139-4272; Martinez-Gonzalez, Enrique/0000-0002-0179-8590 FU Spanish Ministerio de Economia y Competitividad [HI2008-0129, AYA2010-21766-C03-01, AYA2012-39475-C02-01, Consolider-Ingenio 2010 CSD2010-00064]; Spanish CSIC; European Social Fund FX We acknowledge partial financial support from the Spanish Ministerio de Economia y Competitividad Projects HI2008-0129, AYA2010-21766-C03-01, AYA2012-39475-C02-01 and Consolider-Ingenio 2010 CSD2010-00064. RFC thanks financial support from Spanish CSIC for a JAE-predoc fellowship, co-financed by the European Social Fund. We also acknowledge the computer resources, technical expertise and assistance provided by the Spanish Supercomputing Network (RES) node at Universidad de Cantabria. We also acknowledge the use of the NASA's HEASARC archive. The HEALPIX package (Gorski et al. 2005) and the COSMOMC code (Lewis & Bridle 2002) were used throughout the data analysis. NR 64 TC 10 Z9 10 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 1 PY 2014 VL 441 IS 3 BP 2392 EP 2397 DI 10.1093/mnras/stu749 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK9RE UT WOS:000338763600046 ER PT J AU Sprintall, J Gordon, AL Koch-Larrouy, A Lee, T Potemra, JT Pujiana, K Wijffels, SE AF Sprintall, Janet Gordon, Arnold L. Koch-Larrouy, Ariane Lee, Tong Potemra, James T. Pujiana, Kandaga Wijffels, Susan E. TI The Indonesian seas and their role in the coupled ocean-climate system SO NATURE GEOSCIENCE LA English DT Article ID WATER MASS TRANSFORMATION; TROPICAL INDIAN-OCEAN; MAKASSAR STRAIT; EL-NINO; THROUGHFLOW; PACIFIC; VARIABILITY; CIRCULATION; EXCHANGE; TRANSPORT AB The Indonesian seas represent the only pathway that connects different ocean basins in the tropics, and therefore play a pivotal role in the coupled ocean and climate system. Here, water flows from the Pacific to the Indian Ocean through a series of narrow straits. The throughflow is characterized by strong velocities at water depths of about 100 m, with more minor contributions from surface flow than previously thought. A synthesis of observational data and model simulations indicates that the temperature, salinity and velocity depth profiles of the Indonesian throughflow are determined by intense vertical mixing within the Indonesian seas. This mixing results in the net upwelling of thermocline water in the Indonesian seas, which in turn lowers sea surface temperatures in this region by about 0.5 degrees C, with implications for precipitation and air-sea heat flux. Moreover, the depth and velocity of the core of the Indonesian throughflow has varied with the El Nino/Southern Oscillation and Indian Ocean Dipole on interannual to decadal timescales. Specifically, the throughflow slows and shoals during El Nino events. Changes in the Indonesian throughflow alter surface and subsurface heat content and sea level in the Indian Ocean between 10 and 15 degrees S. We conclude that inter-ocean exchange through the Indonesian seas serves as a feedback modulating the regional precipitation and wind patterns. C1 [Sprintall, Janet] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Gordon, Arnold L.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Koch-Larrouy, Ariane] LEGOS, F-31401 Toulouse 9, France. [Lee, Tong] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Potemra, James T.] Univ Hawaii Manoa, SOEST IPRC, Honolulu, HI 96822 USA. [Pujiana, Kandaga] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA. [Pujiana, Kandaga] Inst Teknol Bandung, Fac Earth Sci & Technol, Bandung 40132, Indonesia. [Wijffels, Susan E.] CSIRO Marine & Atmospher Res, Hobart, Tas 7000, Australia. RP Sprintall, J (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. EM jsprintall@ucsd.edu RI Gordon, Arnold/H-1049-2011 OI Gordon, Arnold/0000-0001-6480-6095 FU National Aeronautics and Space Administration (NASA) [NNX13AO38G]; National Oceanic and Atmospheric Administration, US Department of Commerce [NA08OAR4320754]; Australian Climate Change Science Program FX The material is partially based on work supporting J.S. by the National Aeronautics and Space Administration (NASA) under award no. NNX13AO38G. A.L.G. is supported by NA08OAR4320754 from the National Oceanic and Atmospheric Administration, US Department of Commerce. The research was carried out in part by T.L. at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. S.E.W. was partly funded by the Australian Climate Change Science Program. NR 50 TC 28 Z9 28 U1 2 U2 51 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD JUL PY 2014 VL 7 IS 7 BP 487 EP 492 DI 10.1038/NGEO2188 PG 6 WC Geosciences, Multidisciplinary SC Geology GA AL0QV UT WOS:000338832700007 ER PT J AU Hofgartner, JD Hayes, AG Lunine, JI Zebker, H Stiles, BW Sotin, C Barnes, JW Turtle, EP Baines, KH Brown, RH Buratti, BJ Clark, RN Encrenaz, P Kirk, RD Le Gall, A Lopes, RM Lorenz, RD Malaska, MJ Mitchell, KL Nicholson, PD Paillou, P Radebaugh, J Wall, SD Wood, C AF Hofgartner, J. D. Hayes, A. G. Lunine, J. I. Zebker, H. Stiles, B. W. Sotin, C. Barnes, J. W. Turtle, E. P. Baines, K. H. Brown, R. H. Buratti, B. J. Clark, R. N. Encrenaz, P. Kirk, R. D. Le Gall, A. Lopes, R. M. Lorenz, R. D. Malaska, M. J. Mitchell, K. L. Nicholson, P. D. Paillou, P. Radebaugh, J. Wall, S. D. Wood, C. TI Transient features in a Titan sea SO NATURE GEOSCIENCE LA English DT Article ID METHANE CYCLE; RADAR; LAKES; ICE; SURFACE AB Titan's surface-atmosphere system bears remarkable similarities to Earth's, the most striking being an active, global methane cycle akin to Earth's water cycle(1,2). Like the hydrological cycle of Earth, Titan's seasonal methane cycle is driven by changes in the distribution of solar energy(2). The Cassini spacecraft, which arrived at Saturn in 2004 in the midst of northern winter and southern summer, has observed surface changes, including shoreline recession, at Titan's south pole3,4 and equator(5). However, active surface processes have yet to be confirmed in the lakes and seas in Titan's north polar region(6-8). As the 2017 northern summer solstice approaches, the onset of dynamic phenomena in this region is expected(6,7,9-12). Here we present the discovery of bright features in recent Cassini RADAR data that appeared in Titan's northern sea, Ligeia Mare, in July 2013 and disappeared in subsequent observations. We suggest that these bright features are best explained by the occurrence of ephemeral phenomena such as surface waves, rising bubbles, and suspended or floating solids. We suggest that our observations are an initial glimpse of dynamic processes that are commencing in the northern lakes and seas as summer nears in the northern hemisphere. C1 [Hofgartner, J. D.; Hayes, A. G.; Lunine, J. I.; Nicholson, P. D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Zebker, H.] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA. [Stiles, B. W.; Sotin, C.; Baines, K. H.; Buratti, B. J.; Lopes, R. M.; Malaska, M. J.; Mitchell, K. L.; Wall, S. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Barnes, J. W.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA. [Turtle, E. P.; Lorenz, R. D.] JHU Appl Phys Lab, Laurel, MD 20723 USA. [Brown, R. H.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Clark, R. N.] USGS Denver Fed Ctr, Denver, CO 80225 USA. [Encrenaz, P.] Observ Paris, F-75014 Paris, France. [Kirk, R. D.] USGS Astrogeol Ctr, Flagstaff, AZ 86001 USA. [Le Gall, A.] LATMOS UVSQ, F-78280 Paris, France. [Paillou, P.] Univ Bordeaux, F-33271 Bordeaux, France. [Radebaugh, J.] Brigham Young Univ, Dept Geol Sci, Provo, UT 84602 USA. [Wood, C.] Planetary Sci Inst, Tucson, AZ 85721 USA. RP Hofgartner, JD (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. EM jhofgartner@astro.cornell.edu RI Barnes, Jason/B-1284-2009; Hayes, Alexander/P-2024-2014; Turtle, Elizabeth/K-8673-2012; Lorenz, Ralph/B-8759-2016; Lopes, Rosaly/D-1608-2016; OI Barnes, Jason/0000-0002-7755-3530; Hayes, Alexander/0000-0001-6397-2630; Turtle, Elizabeth/0000-0003-1423-5751; Lorenz, Ralph/0000-0001-8528-4644; Lopes, Rosaly/0000-0002-7928-3167; Malaska, Michael/0000-0003-0064-5258 FU Cassini Project; Natural Sciences and Engineering Research Council of Canada; NASA [NNX13AG03G] FX J.D.H. gratefully acknowledges the Cassini RADAR and VIMS Teams for the data and the opportunity to lead the analysis and the Cassini Project and Natural Sciences and Engineering Research Council of Canada, Post Graduate Scholarship Program for financial support. A.G.H. was partially supported by NASA grant NNX13AG03G. A portion of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration. NR 24 TC 9 Z9 9 U1 0 U2 19 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD JUL PY 2014 VL 7 IS 7 BP 493 EP 496 DI 10.1038/NGEO2190 PG 4 WC Geosciences, Multidisciplinary SC Geology GA AL0QV UT WOS:000338832700008 ER PT J AU Ducluzeau, AL Schoepp-Cothenet, B Baymann, F Russell, MJ Nitschke, W AF Ducluzeau, Anne-Lise Schoepp-Cothenet, Barbara Baymann, Frauke Russell, Michael J. Nitschke, Wolfgang TI Free energy conversion in the LUCA: Quo vadis? SO BIOCHIMICA ET BIOPHYSICA ACTA-BIOENERGETICS LA English DT Review DE Evolution of bioenergetics; Last universal common ancestor; Quinone; Wood-Ljungdahl pathway; Sodium pumping ID COPPER OXYGEN REDUCTASES; MEMBRANE BIOENERGETICS; EVOLUTIONARY HISTORY; ATP SYNTHASE; NITRIC-OXIDE; HEME; ORIGIN; LIFE; HYDROGENASES; PHYLOGENY AB Living entities are unimaginable without means to harvest free energy from the environment, that is, without bioenergetics. The quest to understand the bioenergetic ways of early life therefore is one of the crucial elements to understand the emergence of life on our planet. Over the last few years, several mutually exclusive scenarios for primordial bioenergetics have been put forward, all of which are based on some sort of empirical observation, a remarkable step forward from the previous, essentially untestable, ab initio models. We here try to present and compare these scenarios while at the same time discuss their respective empirical weaknesses. The goal of this article is to harness crucial new expertise from the entire field by stimulating a larger part of the bioenergetics community to become involved in "origin-of-energy-metabolism" research. This article is part of a Special Issue entitled: 18th European Bioenergetic Conference. (C) 2013 Elsevier B.V. All rights reserved. C1 [Schoepp-Cothenet, Barbara; Baymann, Frauke; Nitschke, Wolfgang] Univ Aix Marseille, CNRS, Lab Bioenerget & Ingn Prot UMR AMU 7281, FR3479, F-13402 Marseille 20, France. [Russell, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ducluzeau, Anne-Lise] Univ Nebraska, Beadle Ctr, Lincoln, NE 68588 USA. RP Nitschke, W (reprint author), Univ Aix Marseille, CNRS, Lab Bioenerget & Ingn Prot UMR AMU 7281, FR3479, F-13402 Marseille 20, France. EM nitschke@imm.cnrs.fr OI Nitschke, Wolfgang/0000-0003-2084-3032 FU NASA [NNH06ZDA001N]; NASA Astrobiology Institute (Icy Worlds) FX We thank Fabrice Rappaport (Paris/France) as well as Shilpa Bali and Stuart J. Ferguson (Oxford/UK) for helpful comments and ideas. MJR's contribution was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration: with support by NASA Exobiology and Evolutionary Biology award (NNH06ZDA001N) and supported by the NASA Astrobiology Institute (Icy Worlds). NR 58 TC 6 Z9 6 U1 3 U2 25 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0005-2728 EI 0006-3002 J9 BBA-BIOENERGETICS JI Biochim. Biophys. Acta-Bioenerg. PD JUL PY 2014 VL 1837 IS 7 SI SI BP 982 EP 988 DI 10.1016/j.bbabio.2013.12.005 PG 7 WC Biochemistry & Molecular Biology; Biophysics SC Biochemistry & Molecular Biology; Biophysics GA AL0KE UT WOS:000338815000004 PM 24361840 ER PT J AU Landis, GA AF Landis, Geoffrey A. TI The Chatbot and the Drone SO COMMUNICATIONS OF THE ACM LA English DT Editorial Material C1 NASA, John Glenn Res Ctr, Cleveland, OH 44114 USA. RP Landis, GA (reprint author), NASA, John Glenn Res Ctr, Cleveland, OH 44114 USA. EM geoffrey.landis@nasa.gov NR 0 TC 0 Z9 0 U1 5 U2 9 PU ASSOC COMPUTING MACHINERY PI NEW YORK PA 2 PENN PLAZA, STE 701, NEW YORK, NY 10121-0701 USA SN 0001-0782 EI 1557-7317 J9 COMMUN ACM JI Commun. ACM PD JUL PY 2014 VL 57 IS 7 BP 112 EP 111 DI 10.1145/2631171 PG 2 WC Computer Science, Hardware & Architecture; Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA AK7RA UT WOS:000338624200025 ER PT J AU Levin, PS Kelble, CR Shuford, RL Ainsworth, C deReynier, Y Dunsmore, R Fogarty, MJ Holsman, K Howell, EA Monaco, ME Oakes, SA Werner, F AF Levin, Phillip S. Kelble, Christopher R. Shuford, Rebecca L. Ainsworth, Cameron deReynier, Yvonne Dunsmore, Rikki Fogarty, Michael J. Holsman, Kirstin Howell, Evan A. Monaco, Mark E. Oakes, Stephanie A. Werner, Francisco TI Guidance for implementation of integrated ecosystem assessments: a US perspective SO ICES JOURNAL OF MARINE SCIENCE LA English DT Article DE ecosystem-based management; ecosystem indicator; ecosystem risk; IEA; integrated ecosystem assessment; management strategy evaluation ID FISHERIES MANAGEMENT; INDICATORS; FRAMEWORK; FISH AB Ecosystem-based management (EBM) has emerged as a basic approach for managing human activities in marine ecosystems, with the aim of recovering and conserving marine ecosystems and the services they deliver. Integrated ecosystem assessments (IEAs) further the transition of EBM from principle to practice by providing an efficient, transparent means of summarizing the status of ecosystem components, screening and prioritizing potential risks, and evaluating alternative management strategies against a backdrop of environmental variability. In this paper, we draw upon lessons learned from the US National Oceanic and Atmospheric Administration's IEA programme to outline steps required for IEA implementation. We provide an overview of the conceptual framework for IEAs, the practical constraints that shape the structure of individual IEAs, and the uses and outcomes of IEAs in support of EBM. C1 [Levin, Phillip S.] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Seattle, WA 98115 USA. [Kelble, Christopher R.] NOAA, Off Ocean & Atmospher Res, Atlantic Oceanog & Meteorol Lab, Miami, FL USA. [Shuford, Rebecca L.; Oakes, Stephanie A.] Natl Marine Fisheries Serv, Off Sci & Technol, Silver Spring, MD USA. [Ainsworth, Cameron] Univ S Florida, St Petersburg, FL 33701 USA. [deReynier, Yvonne] NOAA, Natl Marine Fisheries Serv, Northwest Reg Off, Seattle, WA 98115 USA. [Dunsmore, Rikki] NOAA, Natl Ocean Serv, Natl Marine Sanctuary Program, Monterey Bay Natl Marine Sanctuary, Monterey, CA USA. [Fogarty, Michael J.] Natl Marine Fisheries Serv, Northeast Fisheries Sci Ctr, Woods Hole, MA 02543 USA. [Holsman, Kirstin] Univ Washington, Joint Inst Study Atmosphere & Ocean, Seattle, WA 98195 USA. [Howell, Evan A.] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI USA. [Monaco, Mark E.] NOAA, Natl Ocean Serv, Natl Ctr Coastal & Ocean Sci, Silver Spring, MD USA. [Werner, Francisco] Natl Marine Fisheries Serv, Southwest Fisheries Sci Ctr, La Jolla, CA 92038 USA. RP Levin, PS (reprint author), NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, 2725 Montlake Blvd E, Seattle, WA 98115 USA. EM phil.levin@noaa.gov RI Kelble, Christopher/A-8511-2008; OI Kelble, Christopher/0000-0003-0914-4134; Howell, Evan/0000-0001-9904-4633 NR 56 TC 23 Z9 23 U1 1 U2 35 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1054-3139 EI 1095-9289 J9 ICES J MAR SCI JI ICES J. Mar. Sci. PD JUL-AUG PY 2014 VL 71 IS 5 BP 1198 EP 1204 DI 10.1093/icesjms/fst112 PG 7 WC Fisheries; Marine & Freshwater Biology; Oceanography SC Fisheries; Marine & Freshwater Biology; Oceanography GA AK7TO UT WOS:000338630800021 ER PT J AU Han, JW Meyyappan, M AF Han, Jin-Woo Meyyappan, Meyya TI THE DEVICE MADE OF NOTHING The vacuum transistor could one day replace traditional silicon SO IEEE SPECTRUM LA English DT Article C1 [Han, Jin-Woo; Meyyappan, Meyya] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Han, JW (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 0 TC 3 Z9 3 U1 2 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9235 EI 1939-9340 J9 IEEE SPECTRUM JI IEEE Spectr. PD JUL PY 2014 VL 51 IS 7 BP 31 EP 35 PG 5 WC Engineering, Electrical & Electronic SC Engineering GA AK8HG UT WOS:000338667700008 ER PT J AU Devi, VM Benner, DC Sung, K Crawford, TJ Mantz, AW Smith, MAH AF Devi, V. Malathy Benner, D. Chris Sung, Keeyoon Crawford, Timothy J. Mantz, Arlan W. Smith, Mary Ann H. TI Line positions and intensities for the v(12) band of (CCH6)-C-13-C-12 SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE Ethane; (CCH6)-C-13-C-12; Line positions; Line intensities; Infrared fundamental; Planetary atmospheres ID INCLUDING TEMPERATURE DEPENDENCES; HALF-WIDTH COEFFICIENTS; INTERNAL-ROTATION; SPECTROSCOPIC DATABASE; INFRARED-SPECTRA; NU(9) BAND; MU-M; ETHANE; ATMOSPHERE; JUPITER AB High-resolution, high signal-to-noise spectra of a high-purity (99%) mono-substituted 13C-enriched ethane ((CCH6)-C-13-C-12) in the v12 fundamental band near 12.2 um region were recorded with a Bruker IFS 125HR Fourier transform spectrometer. The data were obtained for four sample pressures at three different temperatures (130-208 K) using a 20.38-cm long coolable absorption cell. The spectra were fitted simultaneously to retrieve individual line positions and absolute line intensities for 1660 absorption features. A multispectrum nonlinear least squares spectrum fitting technique was employed in the analysis. Constraints were used to fit each pair of doublet components arising from torsional Coriolis interaction of the excited v(12) = 1 state with the nearby excited torsional v6 = 3 state. Line positions and absolute line intensities were retrieved by simultaneously fitting the four experimental spectra recorded at three low sample temperatures (130 K, 178 K and 208 K). The measured positions and intensities were determined for the standard reference temperature of 296 K and compared with the predicted values listed in the HITRAN database. Calculated line intensities at each of the measured spectrum temperatures are also provided as supplemental data. Integrated intensities are also reported. (C) 2014 Elsevier Inc. All rights reserved. C1 [Devi, V. Malathy; Benner, D. Chris] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. [Sung, Keeyoon; Crawford, Timothy J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Mantz, Arlan W.] Connecticut Coll, Dept Phys Astron & Geophys, New London, CT 06320 USA. [Smith, Mary Ann H.] NASA, Sci Directorate, Langley Res Ctr, Hampton, VA 23681 USA. RP Devi, VM (reprint author), Coll William & Mary, Dept Phys, Box 8795, Williamsburg, VA 23187 USA. EM malathy.d.venkataraman@nasa.gov RI Sung, Keeyoon/I-6533-2015 FU NASA's Outer Planets Research Program FX NASA's Outer Planets Research Program supported the work performed at the College of William and Mary. Research at the Jet Propulsion Laboratory (JPL), California Institute of Technology, NASA Langley Research Center and Connecticut College was performed under contract with the National Aeronautics and Space Administration. NR 37 TC 1 Z9 1 U1 0 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 EI 1096-083X J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD JUL PY 2014 VL 301 BP 28 EP 38 DI 10.1016/j.jms.2014.05.005 PG 11 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA AL0NM UT WOS:000338823600007 ER PT J AU Zhu, WR Premaratne, M Gunapala, SD Agrawal, GP Stockman, MI AF Zhu, Weiren Premaratne, Malin Gunapala, Sarath D. Agrawal, Govind P. Stockman, Mark I. TI Quasi-static analysis of controllable optical cross-sections of a layered nanoparticle with a sandwiched gain layer SO JOURNAL OF OPTICS LA English DT Article DE nanoshell; gain; spaser ID SPASER; SCATTERING; AU; AG AB We theoretically study the optical performance of a layered nanoparticle with a sandwiched gain shell. Based on quasi-static analysis and full-wave numerical simulations, we show that it is possible to achieve a very high scattering cross-section (over 4 orders) accompanied with a negative absorption cross-section by changing the amount of gain in the sandwiched shell layer. This suggests that the proposed configuration can either be used for designing a spaser or as a switchable nano scatterer whose scattering cross-section can be manipulated from an ultra-high value to an ultra-low one. To provide more insight into the operation of this proposed configuration, we also study the near field, which again confirms a clear controllability of field enhancement through the sandwiched gain layer. C1 [Zhu, Weiren; Premaratne, Malin] Monash Univ, Dept Elect & Comp Syst Engn, Adv Comp & Simulat Lab AxL, Clayton, Vic 3800, Australia. [Gunapala, Sarath D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Agrawal, Govind P.] Univ Rochester, Inst Opt, Rochester, NY 14627 USA. [Stockman, Mark I.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. RP Zhu, WR (reprint author), Monash Univ, Dept Elect & Comp Syst Engn, Adv Comp & Simulat Lab AxL, Clayton, Vic 3800, Australia. EM weiren.zhu@monash.edu RI Zhu, Weiren/E-7749-2011; Agrawal, Govind/D-5380-2013; OI Agrawal, Govind/0000-0003-4486-8533; Premaratne, Malin/0000-0002-2419-4431; Zhu, Weiren/0000-0002-6568-738X FU Australian Research Council, through its Discovery Grant scheme [DP110100713, DP140100883] FX The work is supported by the Australian Research Council, through its Discovery Grant scheme under grants DP110100713 and DP140100883. NR 24 TC 7 Z9 7 U1 0 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2040-8978 EI 2040-8986 J9 J OPTICS-UK JI J. Opt. PD JUL PY 2014 VL 16 IS 7 AR 075003 DI 10.1088/2040-8978/16/7/075003 PG 6 WC Optics SC Optics GA AK9PO UT WOS:000338759200004 ER PT J AU Gelino, CR Smart, RL Marocco, F Kirkpatrick, JD Cushing, MC Mace, G Mendez, RA Tinney, CG Jones, HRA AF Gelino, Christopher R. Smart, R. L. Marocco, Federico Kirkpatrick, J. Davy Cushing, Michael C. Mace, Gregory Mendez, Rene A. Tinney, C. G. Jones, Hugh R. A. TI WISEP J061135.13-041024.0 AB: A J-BAND FLUX REVERSAL BINARY AT THE L/T TRANSITION SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: general; brown dwarfs; stars: fundamental parameters; stars: individual (WISEP J061135.13-041024.0); stars: low-mass ID STAR ADAPTIVE OPTICS; DWARF/T DWARF TRANSITION; T-DWARFS; SPECTROSCOPY; MULTIPLICITY; TEMPERATURE; ATMOSPHERES; PERFORMANCE; PARALLAXES; GRAVITY AB We present Keck II laser guide star adaptive optics observations of the brown dwarf WISEP J061135.13-041024.0 showing it is a binary with a component separation of 0 ''.4. This system is one of the six known resolved binaries in which the magnitude differences between the components show a reversal in sign between the Y/J band and the HI K bands. Deconvolution of the composite spectrum results in a best-fit binary solution with L9 and T1.5 components. We also present a preliminary parallax placing the system at a distance of 21.2 1.3 pc. Using the distance and resolved magnitudes we are able to place WISEP J061135.13-041024.0 AB on a color absolute magnitude diagram, showing that this system contributes to the well-known "J-band bump" and the components' properties appear similar to other late-type L and early-type T dwarfs. Fitting our data to a set of cloudy atmosphere models suggests the system has an age >1 Gyr with WISE 0611-0410 A having an effective temperature (T-eff) of 1275-1325 K and mass of 64-65 M-Jup, and WISE 0611-0410 B having T-eff = 1075-1115 K and mass 40-65 M-Jup. C1 [Gelino, Christopher R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Gelino, Christopher R.; Kirkpatrick, J. Davy] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Smart, R. L.] Osserv Astron Torino, Ist Nazl Astrofis, I-10025 Pino Torinese, Italy. [Marocco, Federico; Jones, Hugh R. A.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Cushing, Michael C.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Mace, Gregory] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Mendez, Rene A.] Univ Chile, Dept Astron, Santiago, Chile. [Tinney, C. G.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Tinney, C. G.] Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia. RP Gelino, CR (reprint author), CALTECH, NASA, Exoplanet Sci Inst, Mail Code 100-22,770 South Wilson Ave, Pasadena, CA 91125 USA. RI Mendez, Rene/J-6608-2016; Mendez, Rene/H-9496-2015; OI Smart, Richard/0000-0002-4424-4766; Tinney, Christopher/0000-0002-7595-0970 FU National Aeronautics and Space Administration (NASA); National Science Foundation; ARC [DP0774000, DP130102695] FX The authors acknowledge telescope operators Heather Hershley, Carolyn Jordan, Julie Renaud-Kim, and Cynthia Wilburn and instrument specialists Scott Dahm, Marc Kassis, and Luca Rizzi for their assistance during the Keck observations. We would also like to thank Chas Beichman for obtaining images of WISE 0611-0410 on 2012 November 29 and 2013 September 21, Mark Marley and Didier Saumon for providing the models, Mike Read for help in mining the UKIDSS database and useful discussions, and the anonymous referee for useful comments. Based partially on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile program 186.C-0756. R.L.S., H.R.A.J., and F.M. would like to acknowledge the Marie Curie 7th European Community Framework Programme grant no. 247593 Interpretation and Parameterization of Extremely Red COOL dwarfs (IPERCOOL) International Research Staff Exchange Scheme. R.A.M. acknowledges partial support from project P.F13-06 CATA and from project IC120009 "Millennium Institute of Astrophysics (MAS)" of the Iniciativa Cientifica Milenio del Ministerio de Economa, Fomento y Turismo de Chile. C.G.T. acknowledges the support of ARC grants DP0774000 and DP130102695. This publication makes use of data products from 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology (Caltech), funded by the National Aeronautics and Space Administration (NASA) and the National Science Foundation.; This publication makes use of data products from the Wide-field Infrared Survey Explorer (WISE), which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory (JPL)/Caltech, and NEOWISE, which is a project of JPL/Caltech. WISE and NEOWISE are funded by NASA. This work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Some of the data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to NASA through the agency's scientific partnership with the Caltech and the University of California. 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. NR 42 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUL PY 2014 VL 148 IS 1 AR 6 DI 10.1088/0004-6256/148/1/6 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK4PF UT WOS:000338405900006 ER PT J AU Harrison, TE Gelino, DM Buxton, M Fost, T AF Harrison, Thomas E. Gelino, Dawn M. Buxton, Michelle Fost, Tyler TI HERSCHEL OBSERVATIONS OF CIRCINUS X-1 DURING OUTBURST AND QUIESCENCE SO ASTRONOMICAL JOURNAL LA English DT Article DE stars: neutron ID X-RAY BINARIES; SPECTRAL ENERGY-DISTRIBUTION; SPITZER-SPACE-TELESCOPE; BLACK-HOLE; SCORPIUS X-1; NEUTRON-STAR; GRS 1915+105; INFRARED OBSERVATIONS; CYGNUS X-2; CATACLYSMIC VARIABLES AB We have used the Photodetector Array Camera and Spectrometer and Spectral and Photometric Imaging REceiver instruments on the Herschel Space Observatory to observe Cir X-1 both in and out of outburst. We detected Cir X-1 during outburst at 70 ism. Unfortunately, a cold background source dominates Cir X-1 at longer wavelengths. We have assembled optical and infrared (IR) data for Cir X-1 to model its spectral energy distribution (SED) in both quiescence and outburst and find that in both states it is consistent with a heavily reddened, 10,000 K blackbody. We believe this behavior is completely consistent with previous suggestions that these outbursts are due to accretion disk events, not unlike those of dwarf novae. To explore the behavior of other low-mass X-ray binaries with reported synchrotron jets, we have extracted and/or compiled optical and near- and mid-IR data sets for five such systems to construct their SEDs. The Z-source GX 349+2 and the black hole system GRS 1915+105 have strong and variable mid-IR excesses that suggest synchrotron emission. The other Z-sources have rather weak (or no) IR excesses that can be explained as reddened blackbody spectra with the addition of either synchrotron or bremsstrahlung components. C1 [Harrison, Thomas E.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Gelino, Dawn M.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Buxton, Michelle] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Fost, Tyler] John Jay High Sch, Cross River, NY 10518 USA. RP Harrison, TE (reprint author), New Mexico State Univ, Dept Astron, Box 30001,MSC 4500, Las Cruces, NM 88003 USA. EM tharriso@nmsu.edu; dawn@ipac.caltech.edu; michelle.buxton@yale.edu; tyler.fost@gmail.com FU National Aeronautics and Space Administration FX This work is based in part on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. 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 work is also based in part on observations made with the Spitzer Space Telescope, obtained from the NASA/IPAC Infrared Science Archive, both of which are operated by the Jet Propulsion NR 103 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUL PY 2014 VL 148 IS 1 AR 22 DI 10.1088/0004-6256/148/1/22 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK4PF UT WOS:000338405900022 ER PT J AU Littlejohns, OM Butler, NR Cucchiara, A Watson, AM Kutyrev, AS Lee, WH Richer, MG Klein, CR Fox, OD Prochaska, JX Bloom, JS Troja, E Ramirez-Ruiz, E de Dieg, JA Georgiev, L Gonzalez, J Roman-Zuniga, CG Gehrels, N Moseley, H AF Littlejohns, O. M. Butler, N. R. Cucchiara, A. Watson, A. M. Kutyrev, A. S. Lee, W. H. Richer, M. G. Klein, C. R. Fox, O. D. Prochaska, J. X. Bloom, J. S. Troja, E. Ramirez-Ruiz, E. de Dieg, J. A. Georgiev, L. Gonzalez, J. Roman-Zuniga, C. G. Gehrels, N. Moseley, H. TI IDENTIFYING HIGH-REDSHEFT GAMMA-RAY BURSTS WITH RATIR SO ASTRONOMICAL JOURNAL LA English DT Article DE Key gamma-ray burst: general; gamma-ray burst: individual (GRB 130606A); techniques: photometric ID ULTRAVIOLET EXTINCTION CURVES; WIDE-FIELD CAMERA; DUST EXTINCTION; PHOTOMETRIC REDSHIFTS; EARLY UNIVERSE; LIGHT CURVES; SKY SURVEY; MILKY-WAY; AFTERGLOWS; TELESCOPE AB We present a template-fitting algorithm for determining photometric redshifts, Z(phot), of candidate high-redshift gamma-ray bursts (GRBs).- Using afterglow photometry, obtained by the Reionization and Transients InfraRed (RATIR) camera, this algorithm accounts for the intrinsic GRB afterglow spectral energy distribution, host dust extinction, and the effect of neutral hydrogen (local and cosmological) along the line of sight. We present the results obtained by this algorithm and the RATIR photometry of GRB 130606A, finding a range of best-fit solutions, 5.6 < Z(phot) < 6.0, for models of several host dust extinction laws (none, the Milky Way, Large Magellanic Clouds, and Small Magellanic Clouds), consistent with spectroscopic measurements of the redshift of this GRB. Using simulated RATIR photometry, we find that our algorithm provides precise measures of z(phot) in the ranges of 4 < z(phot) < 8 and 9 < z(phot) < 10 and can robustly determine when z(phot) > 4. Further testing highlights the required caution in cases of highly dust-extincted host galaxies. These tests also show that our algorithm does not erroneously find z(phot) < 4 when z(stm) > 4, thereby minimizing false negatives and allowing us to rapidly identify all potential high-redshift events. C1 [Littlejohns, O. M.; Butler, N. R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Cucchiara, A.; Kutyrev, A. S.; Troja, E.; Gehrels, N.; Moseley, H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Watson, A. M.; Lee, W. H.; Richer, M. G.; de Dieg, J. A.; Georgiev, L.; Gonzalez, J.; Roman-Zuniga, C. G.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Klein, C. R.; Fox, O. D.; Bloom, J. S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Prochaska, J. X.; Ramirez-Ruiz, E.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. RP Littlejohns, OM (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. RI Gonzalez, Jose/L-6687-2014; Roman-Zuniga, Carlos/F-6602-2016; OI Gonzalez, Jose/0000-0002-3724-1583; Roman-Zuniga, Carlos/0000-0001-8600-4798; Jose A., de Diego/0000-0001-7040-069X FU NASA [NNX09AH71G, NNX09AT02G, NNX10AI27G, NNX12AE66G]; CONACyT [INFR-2009-01-122785, CB-2008-101958]; UNAM PAPIIT [IN113810]; UC MEXUS-CONACyT [CN 09-283] FX We thank Sandra Savaglio for a constructive referee report on this work. We thank the RATIR project team and the staff of the Observatorio Astronomico Nacional on Sierra San Pedro Martir. RATIR is a collaboration between the University of California, the Universidad Nacional Autonoma de Mexico, NASA Goddard Space Flight Center, and Arizona State University, benefiting from the loan of an H2RG detector and hardware and software support from Teledyne Scientific and Imaging RATIR, the automation of the Harold L. Johnson Telescope of the Observatorio Astronomico Nacional on Sierra San Pedro Martir, and the operation of both are funded through NASA grants NNX09AH71G, NNX09AT02G, NNX10AI27G, and NNX12AE66G, CONACyT grants INFR-2009-01-122785 and CB-2008-101958, UNAM PAPIIT grant IN113810, and UC MEXUS-CONACyT grant CN 09-283. NR 65 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUL PY 2014 VL 148 IS 1 AR 2 DI 10.1088/0004-6256/148/1/2 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK4PF UT WOS:000338405900002 ER PT J AU Masci, FJ Hoffman, DI Grillmair, CJ Cutri, RM AF Masci, Frank J. Hoffman, Douglas I. Grillmair, Carl J. Cutri, Roc M. TI AUTOMATED CLASSIFICATION OF PERIODIC VARIABLE STARS DETECTED BY THE WIDE-FIELD INFRARED SURVEY EXPLORER SO ASTRONOMICAL JOURNAL LA English DT Article DE methods: statistical; stars: variables: general ID SKY-VARIABILITY-SURVEY; PRELIMINARY DATA RELEASE; RR LYRAE STARS; SUPERVISED CLASSIFICATION; LUMINOSITY RELATIONS; LIGHT CURVES; METHODOLOGY; CANDIDATES; TRANSIENTS; DISCOVERY AB We describe a methodology to classify periodic variable stars identified using photometric time-series measurements constructed from the Wide-field Infrared Survey Explorer (WISE) full-mission single-exposure Source Databases. This will assist in the future construction of a WISE Variable Source Database that assigns variables to specific science classes as constrained by the WISE observing cadence with statistically meaningful classification probabilities. We have analyzed the WISE light curves of 8273 variable stars identified in previous optical variability surveys (MACHO, GCVS, and ASAS) and show that Fourier decomposition techniques can be extended into the mid-IR to assist with their classification. Combined with other periodic light-curve features, this sample is then used to train a machine-learned classifier based on the random forest (RF) method. Consistent with previous classification studies of variable stars in general, the RF machine-learned classifier is superior to other methods in terms of accuracy, robustness against outliers, and relative immunity to features that carry little or redundant class information. For the three most common classes identified by WISE: Algols, RR Lyrae, and W Ursae Majoris type variables, we obtain classification efficiencies of 80.7%, 82.7%, and 84.5% respectively using cross-validation analyses, with 95% confidence intervals of approximately +/- 2%. These accuracies are achieved at purity (or reliability) levels of 88.5%, 96.2%, and 87.8% respectively, similar to that achieved in previous automated classification studies of periodic variable stars. C1 [Masci, Frank J.; Grillmair, Carl J.; Cutri, Roc M.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Hoffman, Douglas I.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Masci, FJ (reprint author), CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. EM fmasci@ipac.caltech.edu FU NASA Astrophysics Data Analysis Program [NNX13AF37G]; NEOWISE; Planetary Science Division of the National Aeronautics and Space Administration FX This work was funded by NASA Astrophysics Data Analysis Program grant NNX13AF37G. We thank the anonymous referee for invaluable comments that helped improve the quality of this manuscript. We are grateful to Max Kuhn for reviewing some of the details of our analyses and descriptions of the algorithms implemented in the R caret package. 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. Long-term archiving and access to the WISE single-exposure database is funded by NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 54 TC 13 Z9 13 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 JUL PY 2014 VL 148 IS 1 AR 21 DI 10.1088/0004-6256/148/1/21 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK4PF UT WOS:000338405900021 ER PT J AU Rodney, SA Riess, AG Strolger, LG Dahlen, T Graur, O Casertano, S Dickinson, ME Ferguson, HC Garnavich, P Hayden, B Jha, SW Jones, DO Kirshner, RP Koekemoer, AM McCully, C Mobasher, B Patel, B Weiner, BJ Cenko, SB Clubb, KI Cooper, M Filippenko, AV Frederiksen, TF Hjorth, J Leibundgut, B Matheson, T Nayyeri, H Penner, K Trump, J Silverman, JM Vivian, U Bostroem, KA Challis, P Rajan, A Wolff, S Faber, SM Grogin, NA Kocevski, D AF Rodney, Steven A. Riess, Adam G. Strolger, Louis-Gregory Dahlen, Tomas Graur, Or Casertano, Stefano Dickinson, Mark E. Ferguson, Henry C. Garnavich, Peter Hayden, Brian Jha, Saurabh W. Jones, David O. Kirshner, Robert P. Koekemoer, Anton M. McCully, Curtis Mobasher, Bahram Patel, Brandon Weiner, Benjamin J. Cenko, S. Bradley Clubb, Kelsey I. Cooper, Michael Filippenko, Alexei V. Frederiksen, Teddy F. Hjorth, Jens Leibundgut, Bruno Matheson, Thomas Nayyeri, Hooshang Penner, Kyle Trump, Jonathan Silverman, Jeffrey M. Vivian, U. Bostroem, K. Azalee Challis, Peter Rajan, Abhijith Wolff, Schuyler Faber, S. M. Grogin, Norman A. Kocevski, Dale TI TYPE Ia SUPERNOVA RATE MEASUREMENTS TO REDSHIFT 2.5 FROM CANDELS: SEARCHING FOR PROMPT EXPLOSIONS IN THE EARLY UNIVERSE SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared: general; supernovae: general; surveys ID CORE-COLLAPSE SUPERNOVAE; DELAY-TIME DISTRIBUTION; ORIGINS DEEP SURVEY; DIGITAL SKY SURVEY; EXTRAGALACTIC LEGACY SURVEY; TELESCOPE ADVANCED CAMERA; GOODS-SOUTH FIELD; GAMMA-RAY BURSTS; II-P SUPERNOVAE; STAR-FORMATION AB dThe Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) was a multi-cycle treasury program on the Hubble Space Telescope (HST) that surveyed a total area of -0.25 deg2 with -900 HST orbits spread across five fields over three years. Within these survey images we discovered 65 supernovae (SNe) of all types, out to z 2.5. We classify -24 of these as Type Ia SNe (SNe Ia) based on host galaxy redshifts and SN photometry (supplemented by grism spectroscopy of six SNe). Here we present a measurement of the volumetric SN Ia rate as a function of redshift, reaching for the first time beyond z =- 2 and putting new constraints on SN Ia progenitor models. Our highest redshift bin includes detections of SNe that exploded when the universe was only -3 Gyr old and near the peak of the cosmic star formation history. This gives the CANDELS high redshift sample unique leverage for evaluating the fraction of SNe Ia that explode promptly after formation (<500 Myr). Combining the CANDELS rates with all available SN Ia rate measurements in the literature we find that this prompt SN Ia fraction is fp = 0.53st=sg.Zc6', consistent with a delay time distribution that follows a simple t-1 power law for all times t > 40 Myr. However, mild tension is apparent between ground-based low-z surveys and space-based high-z surveys. In both CANDELS and the sister HST program CLASH (Cluster Lensing And Supernova Survey with Hubble), we find a low rate of SNe Ia at z > 1. This could be a hint that prompt progenitors are in fact relatively rare, accounting for only 20% of all SN Ia explosions-though further analysis and larger samples will be needed to examine that suggestion. Key words: infrared: general - supernovae: C1 [Rodney, Steven A.; Riess, Adam G.; Graur, Or; Jones, David O.; Wolff, Schuyler] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Riess, Adam G.; Strolger, Louis-Gregory; Dahlen, Tomas; Casertano, Stefano; Ferguson, Henry C.; Koekemoer, Anton M.; Bostroem, K. Azalee; Grogin, Norman A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Graur, Or] Tel Aviv Univ, Dept Astrophys, IL-69978 Tel Aviv, Israel. [Graur, Or] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Dickinson, Mark E.; Matheson, Thomas] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Garnavich, Peter] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Hayden, Brian] EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Jha, Saurabh W.; McCully, Curtis; Patel, Brandon] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Kirshner, Robert P.; Challis, Peter] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mobasher, Bahram; Nayyeri, Hooshang; Vivian, U.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Weiner, Benjamin J.; Penner, Kyle] Univ Arizona, Dept Astron, Tucson, AZ 85721 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. [Clubb, Kelsey I.; Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Cooper, Michael] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Frederiksen, Teddy F.; Hjorth, Jens] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Leibundgut, Bruno] European So Observ, Garching, Germany. [Leibundgut, Bruno] Tech Univ Munich, D-80290 Munich, Germany. [Trump, Jonathan] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Silverman, Jeffrey M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Rajan, Abhijith] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Faber, S. M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 92064 USA. [Kocevski, Dale] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. RP Rodney, SA (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RI Hjorth, Jens/M-5787-2014; OI Hjorth, Jens/0000-0002-4571-2306; Graur, Or/0000-0002-4391-6137; Koekemoer, Anton/0000-0002-6610-2048 NR 117 TC 28 Z9 28 U1 0 U2 5 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 JUL PY 2014 VL 148 IS 1 AR 13 DI 10.1088/0004-6256/148/1/13 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK4PF UT WOS:000338405900013 ER PT J AU Mommert, M Farnocchia, D Hora, JL Chesley, SR Trilling, DE Chodas, PW Mueller, M Harris, AW Smith, HA Fazio, GG AF Mommert, M. Farnocchia, D. Hora, J. L. Chesley, S. R. Trilling, D. E. Chodas, P. W. Mueller, M. Harris, A. W. Smith, H. A. Fazio, G. G. TI PHYSICAL PROPERTIES OF NEAR-EARTH ASTEROID 2011 MD SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE infrared: planetary systems; minor planets, asteroids: individual (2011 MD) ID SPITZER-SPACE-TELESCOPE; RADIATION PRESSURE; YARKOVSKY; FRAGMENTS; NEOWISE AB We report on observations of near-Earth asteroid 2011 MD with the Spitzer Space Telescope. We have spent 19.9 hr of observing time with channel 2 (4.5 mu m) of the Infrared Array Camera and detected the target within the 2 sigma positional uncertainty ellipse. Using an asteroid thermophysical model and a model of nongravitational forces acting upon the object, we constrain the physical properties of 2011 MD, based on the measured flux density and available astrometry data. We estimate 2011 MD to be (6(-2)(+4) ) m in diameter with a geometric albedo of 0.3(-0.2)(+0.4) (uncertainties are 1 sigma). We find the asteroid's most probable bulk density to be (1.1(-0.5)(+0.7) ) g cm(-3), which implies a total mass of (50-350) t and a macroporosity of >= 65%, assuming a material bulk density typical of non-primitive meteorite materials. A high degree of macroporosity suggests that 2011 MD is a rubble-pile asteroid, the rotation of which is more likely to be retrograde than prograde. C1 [Mommert, M.; Trilling, D. E.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. [Farnocchia, D.; Chesley, S. R.; Chodas, P. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hora, J. L.; Smith, H. A.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mueller, M.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Harris, A. W.] DLR Inst Planetary Res, D-12489 Berlin, Germany. RP Mommert, M (reprint author), No Arizona Univ, Dept Phys & Astron, POB 6010, Flagstaff, AZ 86011 USA. OI Mueller, Michael/0000-0003-3217-5385; Chesley, Steven/0000-0003-3240-6497 FU Arizona's Technology and Research Initiative Fund; Jet Propulsion Laboratory RSA [1367413] FX Some of the computational analyses were run on Northern Arizona University's monsoon computing cluster, funded by Arizona's Technology and Research Initiative Fund. M. Mommert thanks P. Penteado for support on the computational aspects of this work. We thank J. Lee and T. J. Martin-Mur for providing information on the Spitzer ephemeris uncertainties. We thank an anonymous referee for useful suggestions that led to the improvement of this manuscript. The work of D. Farnocchia, S. Chesley, and P. W. Chodas was conducted at the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration. J. L. Hora and H. A. Smith acknowledge partial support from Jet Propulsion Laboratory RSA #1367413. 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. NR 23 TC 6 Z9 6 U1 1 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 JUL 1 PY 2014 VL 789 IS 1 AR L22 DI 10.1088/2041-8205/789/1/L22 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK6UR UT WOS:000338563300022 ER PT J AU Morley, CV Marley, MS Fortney, JJ Lupu, R AF Morley, Caroline V. Marley, Mark S. Fortney, Jonathan J. Lupu, Roxana TI SPECTRAL VARIABILITY FROM THE PATCHY ATMOSPHERES OF T AND Y DWARFS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE brown dwarfs; planets and satellites: atmospheres; stars: atmospheres ID EXTRASOLAR GIANT PLANETS; HR 8799 PLANETS; BROWN DWARF; THERMAL STRUCTURE; EVOLVING WEATHER; HOT JUPITERS; LIGHT CURVES; CLOUDS; TRANSITION; CHEMISTRY AB Brown dwarfs of a variety of spectral types have been observed to be photometrically variable. Previous studies have focused on objects at the L/T transition, where the iron and silicate clouds in L dwarfs break up or dissipate. However, objects outside of this transitional effective temperature regime also exhibit variability. Here, we present models for mid-late T dwarfs and Y dwarfs. We present models that include patchy salt and sulfide clouds as well as water clouds for the Y dwarfs. We find that for objects over 375 K, patchy cloud opacity would generate the largest amplitude variability within near-infrared spectral windows. For objects under 375 K, water clouds also become important and generate larger amplitude variability in the mid-infrared. We also present models in which we perturb the temperature structure at different pressure levels of the atmosphere to simulate hot spots. These models show the most variability in the absorption features between spectral windows. The variability is strongest at wavelengths that probe pressure levels at which the heating is the strongest. The most illustrative types of observations for understanding the physical processes underlying brown dwarf variability are simultaneous, multi-wavelength observations that probe both inside and outside of molecular absorption features. C1 [Morley, Caroline V.; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Marley, Mark S.; Lupu, Roxana] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Morley, CV (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. EM cmorley@ucolick.org RI Marley, Mark/I-4704-2013; Lupu, Roxana/P-9060-2014; OI Lupu, Roxana/0000-0003-3444-5908; Marley, Mark/0000-0002-5251-2943 FU NSF [AST-1312545]; NASA FX We acknowledge Didier Saumon for providing models and for helpful comments on this Letter. We acknowledge the Database of Ultracool Parallaxes maintained by Trent Dupuy. JJF acknowledges the support of NSF grant AST-1312545 and M. S. M. acknowledges the support of the NASA Astrophysics Theory and Origins Programs. NR 44 TC 11 Z9 11 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 1 PY 2014 VL 789 IS 1 AR L14 DI 10.1088/2041-8205/789/1/L14 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK6UR UT WOS:000338563300014 ER PT J AU Vahidinia, S Cuzzi, JN Marley, M Fortney, J AF Vahidinia, Sanaz Cuzzi, Jeffrey N. Marley, Mark Fortney, Jonathan TI CLOUD BASE SIGNATURE IN TRANSMISSION SPECTRA OF EXOPLANET ATMOSPHERES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE methods: analytical; planets and satellites: atmospheres; radiative transfer; scattering ID HUBBLE-SPACE-TELESCOPE; HD 189733B; HOT JUPITERS; PLANET; HAZE AB We present an analytical model for the transmission spectrum of a transiting exoplanet, showing that a cloud base can produce an observable inflection point in the spectrum. The wavelength and magnitude of the inflection can be used to break the degeneracy between the atmospheric pressure and the abundance of the main cloud material, however, the abundance still depends on cloud particle size. An observed inflection also provides a specific point on the atmospheric P-T profile, giving us a "thermometer" to directly validate or rule out postulated cloud species. We apply the model to the transit spectrum of HD 189733b. C1 [Vahidinia, Sanaz] NASA Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Cuzzi, Jeffrey N.; Marley, Mark] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Fortney, Jonathan] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA. RP Vahidinia, S (reprint author), NASA Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. EM sanaz.vahidinia@nasa.gov RI Marley, Mark/I-4704-2013; OI Marley, Mark/0000-0002-5251-2943 NR 11 TC 1 Z9 1 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 1 PY 2014 VL 789 IS 1 AR L11 DI 10.1088/2041-8205/789/1/L11 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK6UR UT WOS:000338563300011 ER PT J AU McAndrews, HJ Thomsen, MF Arridge, CS Jackman, CM Wilson, RJ Henderson, MG Tokar, RL Khurana, KK Sittler, EC Coates, AJ Dougherty, MK AF McAndrews, H. J. Thomsen, M. F. Arridge, C. S. Jackman, C. M. Wilson, R. J. Henderson, M. G. Tokar, R. L. Khurana, K. K. Sittler, E. C. Coates, A. J. Dougherty, M. K. TI Plasma in Saturn's nightside magnetosphere and the implications for global circulation (vol 57, pg 1714, 2009) SO PLANETARY AND SPACE SCIENCE LA English DT Correction C1 [Thomsen, M. F.; Tokar, R. L.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Arridge, C. S.; Coates, A. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Arridge, C. S.; Coates, A. J.] UCL Birkbeck, Ctr Planetary Sci, London WC1E 6BT, England. [Jackman, C. M.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. [Wilson, R. J.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA. [Henderson, M. G.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Khurana, K. K.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Sittler, E. C.] NASA, Heliophys Sci Div, Geospace Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dougherty, M. K.] Univ London Imperial Coll Sci Technol & Med, Space & Atmospher Phys Grp, London SW7 2BW, England. RP Thomsen, MF (reprint author), Planetary Sci Inst, Tucson, AZ 85719 USA. EM mthomsen@psi.edu RI Wilson, Rob/C-2689-2009; Arridge, Christopher/A-2894-2009; Coates, Andrew/C-2396-2008; Henderson, Michael/A-3948-2011 OI Wilson, Rob/0000-0001-9276-2368; Arridge, Christopher/0000-0002-0431-6526; Coates, Andrew/0000-0002-6185-3125; Henderson, Michael/0000-0003-4975-9029 NR 1 TC 4 Z9 4 U1 0 U2 3 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 JUL PY 2014 VL 97 BP 86 EP 87 DI 10.1016/j.pss.2014.05.011 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK7OS UT WOS:000338618200009 ER PT J AU Venkateswaran, K Vaishampayan, P Cisneros, J Pierson, DL Rogers, SO Perry, J AF Venkateswaran, Kasthuri Vaishampayan, Parag Cisneros, Jessica Pierson, Duane L. Rogers, Scott O. Perry, Jay TI International Space Station environmental microbiome - microbial inventories of ISS filter debris SO APPLIED MICROBIOLOGY AND BIOTECHNOLOGY LA English DT Article DE International Space Station; Vacuum cleaner debris; Pyrosequencing; Microbial diversity; Closed habitat; PMA; ATP; qPCR ID PROPIONIBACTERIUM-ACNES; CLEAN-ROOM; BACTERIAL COMMUNITIES; INDOOR AIR; DIVERSITY; SKIN; BIOAEROSOLS; POPULATIONS; GREENGENES; FACILITIES AB Despite an expanding array of molecular approaches for detecting microorganisms in a given sample, rapid and robust means of assessing the differential viability of the microbial cells, as a function of phylogenetic lineage, remain elusive. A propidium monoazide (PMA) treatment coupled with downstream quantitative polymerase chain reaction (qPCR) and pyrosequencing analyses was carried out to better understand the frequency, diversity, and distribution of viable microorganisms associated with debris collected from the crew quarters of the International Space Station (ISS). The cultured bacterial counts were more in the ISS samples than cultured fungal population. The rapid molecular analyses targeted to estimate viable population exhibited 5-fold increase in bacterial (qPCR-PMA assay) and 25-fold increase in microbial (adenosine triphosphate assay) burden than the cultured bacterial population. The ribosomal nucleic acid-based identification of cultivated strains revealed the presence of only four to eight bacterial species in the ISS samples, however, the viable bacterial diversity detected by the PMA-pyrosequencing method was far more diverse (12 to 23 bacterial taxa) with the majority consisting of members of actinobacterial genera (Propionibacterium, Corynebacterium) and Staphylococcus. Sample fractions not treated with PMA (inclusive of both live and dead cells) yielded a great abundance of highly diverse bacterial (94 to 118 taxa) and fungal lineages (41 taxa). Even though deep sequencing capability of the molecular analysis widened the understanding about the microbial diversity, the cultivation assay also proved to be essential since some of the spore-forming microorganisms were detected only by the culture-based method. Presented here are the findings of the first comprehensive effort to assess the viability of microbial cells associated with ISS surfaces, and correlate differential viability with phylogenetic affiliation. C1 [Venkateswaran, Kasthuri; Vaishampayan, Parag; Cisneros, Jessica] CALTECH, Biotechnol & Planetary Protect Grp, Jet Prop Lab, Pasadena, CA 91109 USA. [Pierson, Duane L.] Johnson Space Ctr, Houston, TX USA. [Rogers, Scott O.] Bowling Green State Univ, Dept Biol Sci, Bowling Green, OH 43403 USA. [Perry, Jay] Marshall Space Flight Ctr, Huntsville, AL USA. RP Venkateswaran, K (reprint author), CALTECH, Biotechnol & Planetary Protect Grp, Jet Prop Lab, M-S 89-2,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM kjvenkat@jpl.nasa.gov FU Space Biology [NNH12ZTT001N, 19-12829-26, NNN13D111T]; LSAMP-BD (Cohort X) program (National Science Foundation) [HRD-1246662] FX Part of the research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This research was funded by a 2012 Space Biology NNH12ZTT001N grant # 19-12829-26 under Task Order NNN13D111T award to K. Venkateswaran. J. Cisneros, a Louis Stokes Alliance for Minority Participation - Bridge to the Doctorate (LSAMP-BD) fellow, was supported by the LSAMP-BD (Cohort X) program (National Science Foundation grant # HRD-1246662). The authors gratefully acknowledge ISS Expedition 31 crew for sample collection and D. Eisenman, JPL for effective coordination of sample procurement. We would also like to thank JSC Microbiology Laboratory members in performing culture-based analysis and Y. Sun (Research and Testing Laboratory) for trouble shooting discussion on the pyrosequencing method. The authors are indebted to M. Jones and C. Guethe from JPL for critical review of this manuscript. (C) 2014 California Institute of Technology. Government sponsorship acknowledged. NR 57 TC 13 Z9 13 U1 6 U2 30 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0175-7598 EI 1432-0614 J9 APPL MICROBIOL BIOT JI Appl. Microbiol. Biotechnol. PD JUL PY 2014 VL 98 IS 14 BP 6453 EP 6466 DI 10.1007/s00253-014-5650-6 PG 14 WC Biotechnology & Applied Microbiology SC Biotechnology & Applied Microbiology GA AK2GP UT WOS:000338237400025 PM 24695826 ER PT J AU Crucian, B Simpson, RJ Mehta, S Stowe, R Chouker, A Hwang, SA Actor, JK Salam, AP Pierson, D Sams, C AF Crucian, Brian Simpson, Richard J. Mehta, Satish Stowe, Raymond Chouker, Alexander Hwang, Shen-An Actor, Jeffrey K. Salam, Alex P. Pierson, Duane Sams, Clarence TI Terrestrial stress analogs for spaceflight associated immune system dysregulation SO BRAIN BEHAVIOR AND IMMUNITY LA English DT Review DE Spaceflight; Immunity; Exercise; Stress; T cells; Cytokines ID EPSTEIN-BARR-VIRUS; HINDLIMB-UNLOADING MODEL; SIMULATED MICROGRAVITY ENVIRONMENT; LISTERIA-MONOCYTOGENES INFECTION; T-CELL-ACTIVATION; HEAD-DOWN TILT; BED REST; SPACE-FLIGHT; DURATION SPACEFLIGHT; HERPESVIRUS LATENCY AB Recent data indicates that dysregulation of the immune system occurs and persists during spaceflight. Impairment of immunity, especially in conjunction with elevated radiation exposure and limited clinical care, may increase certain health risks during exploration-class deep space missions (i.e. to an asteroid or Mars). Research must thoroughly characterize immune dysregulation in astronauts to enable development of a monitoring strategy and validate any necessary countermeasures. Although the International Space Station affords an excellent platform for on-orbit research, access may be constrained by technical, logistical vehicle or funding limitations. Therefore, terrestrial spaceflight analogs will continue to serve as lower cost, easier access platforms to enable basic human physiology studies. Analog work can triage potential in-flight experiments and thus result in more focused on-orbit studies, enhancing overall research efficiency. Terrestrial space analogs generally replicate some of the physiological or psychological stress responses associated with spaceflight. These include the use of human test subjects in a laboratory setting (i.e. exercise, bed rest, confinement, circadian misalignment) and human remote deployment analogs (Antarctica winterover, undersea, etc.) that incorporate confinement, isolation, extreme environment, physiological mission stress and disrupted circadian rhythms. While bed rest has been used to examine the effects of physical deconditioning, radiation and microgravity may only be simulated in animal or microgravity cell culture (clinorotation) analogs. This article will characterize the array of terrestrial analogs for spaceflight immune dysregulation, the current evidence base for each, and interpret the analog catalog in the context of acute and chronic stress. Published by Elsevier Inc. C1 [Crucian, Brian; Pierson, Duane] NASA, Lyndon B Johnson Space Ctr, Div Biomed & Environm Sci, Houston, TX 77058 USA. [Simpson, Richard J.] Univ Houston, Dept Hlth & Human Performance, Lab Integrated Physiol, Houston, TX USA. [Mehta, Satish] EASI Inc, Houston, TX USA. [Stowe, Raymond] Microgen Labs Inc, La Marque, TX USA. [Chouker, Alexander] Hosp Ludwig Maximilians Univ, Dept Anesthesiol, Munich, Germany. [Hwang, Shen-An; Actor, Jeffrey K.] Univ Texas Houston, Sch Med, Dept Pathol, Houston, TX 77030 USA. [Salam, Alex P.] Chelsea & Westminster Hosp, Dept HIV Infect, London, England. [Sams, Clarence] NASA, Lyndon B Johnson Space Ctr, Space & Clin Operat Div, Houston, TX 77058 USA. RP Crucian, B (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy,Mail Code SK4, Houston, TX 77058 USA. EM brian.crucian-1@nasa.gov OI Actor, Jeffrey/0000-0002-9265-7012 FU National Institutes of Health; National Center for Advancing Translational Sciences [1UL1RR029876-01]; NASA [NNX12AB48G, NNJ04HD75G]; European Space Agency (ESA); German National Space Program (DLR) [50WB0719, WB0919] FX Part of this work was supported by National Institutes of Health, National Center for Advancing Translational Sciences, grant 1UL1RR029876-01 and the NASA Flight Analogs Project (B. Crucian); by NASA grant NNX12AB48G to RJ Simpson and by NASA grant NNJ04HD75G to RP Stowe. A. Chouker was supported by the European Space Agency (ESA) ELIPS 3 and 4 programs and the German National Space Program (DLR, #50WB0719 and #WB0919). NR 82 TC 12 Z9 12 U1 4 U2 22 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0889-1591 EI 1090-2139 J9 BRAIN BEHAV IMMUN JI Brain Behav. Immun. PD JUL PY 2014 VL 39 SI SI BP 23 EP 32 DI 10.1016/j.bbi.2014.01.011 PG 10 WC Immunology; Neurosciences SC Immunology; Neurosciences & Neurology GA AK1MJ UT WOS:000338178900003 PM 24462949 ER PT J AU Bigley, AB Rezvani, K Chew, C Sekine, T Pistillo, M Crucian, B Bollard, CM Simpson, RJ AF Bigley, Austin B. Rezvani, Katayoun Chew, Claude Sekine, Takuya Pistillo, Mira Crucian, Brian Bollard, Catherine M. Simpson, Richard J. TI Acute exercise preferentially redeploys NK-cells with a highly-differentiated phenotype and augments cytotoxicity against lymphoma and multiple myeloma target cells SO BRAIN BEHAVIOR AND IMMUNITY LA English DT Article DE Exercise immunology; Acute stress; CD57; CD158; NKG2C; NKG2A; KLRG1; U266; 721.221; 221 AEH; RPMI-8226; K562 ID NATURAL-KILLER-CELL; LATENT CYTOMEGALOVIRUS-INFECTION; E SURFACE EXPRESSION; BLOOD T-CELLS; PERIPHERAL-BLOOD; CLASS-I; HLA-E; INHIBITORY RECEPTORS; INTENSITY EXERCISE; CANCER PREVENTION AB NK-cells undergo a "licensing" process as they develop into fully-functional cells capable of efficiently killing targets. NK-cell differentiation is accompanied by an increased surface expression of inhibitory killer immunoglobulin-like receptor (KIR) molecules, which is positively associated with cytotoxicity against the HLA-deficient K562 cell line. NK-cells are rapidly redeployed between the blood and tissues in response to acute exercise, but it is not known if exercise evokes a preferential trafficking of differentiated NK-cells or impacts NK-cell cytotoxic activity (NKCA) against HLA-expressing target cells. Sixteen healthy cyclists performed three 30-min bouts of cycling exercise at -5%, +5%, and +15% of lactate threshold. Blood samples obtained before, immediately after, and 1 h after exercise were used to enumerate NK-cells and their subsets, and determine NKCA and degranulating subsets (CD107+) against cell lines of multiple myeloma (U266 and RPMI-8226), lymphoma (721.221 and 221 AEH), and leukemia (K562) origin by 4 and 10-color flow cytometry, respectively. Exercise evoked a stepwise redeployment of NK-cell subsets in accordance with differentiation status [highly-differentiated (KIR+/NKG2A-) > medium-differentiated (KIR+/NKG2A+) > low-differentiated (KIR-/NKG2A+)] that was consistent across all exercise intensities. NKCA per cell increased similar to 6-fold against U266 and 221 AEH targets 1 h post-exercise and was associated with a decreased proportion of NK-cells expressing the inhibitory receptor CD158b and increased proportion of NK-cells expressing the activating receptor NKG2C, respectively. We conclude that exercise evokes a preferential redeployment of NK-cell subsets with a high differentiation phenotype and augments cytotoxicity against HLA-expressing target cells. Exercise may serve as a simple strategy to enrich the blood compartment of highly cytotoxic NK-cell subsets that can be harvested for clinical use. (C) 2013 Elsevier Inc. All rights reserved. C1 [Bigley, Austin B.; Pistillo, Mira; Simpson, Richard J.] Univ Houston, Dept Hlth & Human Performance, Lab Integrated Physiol, Houston, TX 77204 USA. [Rezvani, Katayoun; Chew, Claude; Sekine, Takuya] Univ Texas MD Anderson Canc Ctr, Div Canc Med, Dept Stem Cell Transplantat, Houston, TX 77030 USA. [Crucian, Brian] NASA, Biomed Res & Environm Sci Div, Johnson Space Ctr, Houston, TX 77058 USA. [Bollard, Catherine M.] Baylor Coll Med, Ctr Cell & Gene Therapy, Dept Pediat, Houston, TX 77030 USA. [Bollard, Catherine M.] Baylor Coll Med, Ctr Cell & Gene Therapy, Dept Med, Houston, TX 77030 USA. [Bollard, Catherine M.] Baylor Coll Med, Ctr Cell & Gene Therapy, Dept Pathol & Immunol, Houston, TX 77030 USA. RP Bigley, AB (reprint author), Univ Houston, Dept Hlth & Human Performance, Lab Integrated Physiol, 3855 Holman St, Houston, TX 77204 USA. EM abbigley@uh.edu FU NASA [NNX12AB48G] FX The authors thank Emily C. LaVoy, Justin Reed, Hawley Kunz, Teja Ograjsek, and Ana Bello for their assistance in the laboratory; Dr. Hanspeter Pircher for providing the Alexa488-conjugated anti-KLRG1 (clone 13F12F2) monoclonal antibody; and Dr. Dan Geraghty for providing the 721.221 and 221 AEH cells. This work was supported by NASA Grant NNX12AB48G to R.J. Simpson. NR 45 TC 18 Z9 19 U1 2 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0889-1591 EI 1090-2139 J9 BRAIN BEHAV IMMUN JI Brain Behav. Immun. PD JUL PY 2014 VL 39 SI SI BP 160 EP 171 DI 10.1016/j.bbi.2013.10.030 PG 12 WC Immunology; Neurosciences SC Immunology; Neurosciences & Neurology GA AK1MJ UT WOS:000338178900018 PM 24200514 ER PT J AU Dong, XQ Zib, BJ Xi, BK Stanfield, R Deng, Y Zhang, XD Lin, B Long, CN AF Dong, Xiquan Zib, Behnjamin J. Xi, Baike Stanfield, Ryan Deng, Yi Zhang, Xiangdong Lin, Bing Long, Charles N. TI Critical mechanisms for the formation of extreme arctic sea-ice extent in the summers of 2007 and 1996 SO CLIMATE DYNAMICS LA English DT Article DE Trigger and cause of Arctic sea ice retreat; Cloud-radiation-water vapor feedback to the sea-ice-concentration variation; Extreme Arctic sea-ice extent formation mechanisms; Triggered by atmospheric forcings; Enhanced clouds-radiation-PWV feedback ID RADIATION CHARACTERISTICS; CLOUD FRACTION; VARIABILITY; CIRCULATION; ENERGY; WATER; MERRA; SENSITIVITY; REANALYSES; ATMOSPHERE AB Along with significant changes in the Arctic climate system, the largest year-to-year variation in sea-ice extent (SIE) has occurred in the Laptev, East Siberian, and Chukchi seas (defined here as the area of focus, AOF), among which the two highly contrasting extreme events were observed in the summers of 2007 and 1996 during the period 1979-2012. Although most efforts have been devoted to understanding the 2007 low, a contrasting high September SIE in 1996 might share some related but opposing forcing mechanisms. In this study, we investigate the mechanisms for the formation of these two extremes and quantitatively estimate the cloud-radiation-water vapor feedback to the sea-ice-concentration (SIC) variation utilizing satellite-observed sea-ice products and the NASA MERRA reanalysis. The low SIE in 2007 was associated with a persistent anticyclone over the Beaufort Sea coupled with low pressure over Eurasia, which induced anomalous southerly winds. Ample warm and moist air from the North Pacific was transported to the AOF and resulted in positive anomalies of cloud fraction (CF), precipitable water vapor (PWV), surface LWnet (down-up), total surface energy and temperature. In contrast, the high SIE event in 1996 was associated with a persistent low pressure over the central Arctic coupled with high pressure along the Eastern Arctic coasts, which generated anomalous northerly winds and resulted in negative anomalies of above mentioned atmospheric parameters. In addition to their immediate impacts on sea ice reduction, CF, PWV and radiation can interplay to lead to a positive feedback loop among them, which plays a critical role in reinforcing sea ice to a great low value in 2007. During the summer of 2007, the minimum SIC is 31 % below the climatic mean, while the maximum CF, LWnet and PWV can be up to 15 %, 20 Wm(-2), and 4 kg m(-3) above. The high anti-correlations (-0.79, -0.61, -0.61) between the SIC and CF, PWV, and LWnet indicate that CF, PWV and LW radiation are indeed having significant impacts on the SIC variation. A new record low occurred in the summer of 2012 was mainly triggered by a super storm over the central Arctic Ocean in early August that caused substantial mechanical ice deformation on top of the long-term thinning of an Arctic ice pack that had become more dominated by seasonal ice. C1 [Dong, Xiquan] Beijing Normal Univ, GCESS, Beijing 100875, Peoples R China. [Dong, Xiquan; Zib, Behnjamin J.; Xi, Baike; Stanfield, Ryan] Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58202 USA. [Deng, Yi] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA. [Zhang, Xiangdong] Univ Alaska, Int Arctic Res Ctr, Dept Atmospher Sci, Fairbanks, AK 99701 USA. [Lin, Bing] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Long, Charles N.] DOE Pacific Northwest Natl Lab, Richland, WA USA. RP Dong, XQ (reprint author), Univ N Dakota, Dept Atmospher Sci, 4149 Univ Ave Stop 9006, Grand Forks, ND 58202 USA. EM dong@aero.und.edu RI Zhang, Xiangdong/A-9711-2009 OI Zhang, Xiangdong/0000-0001-5893-2888 FU National Basic Research Program of China (973 Program) at Beijing Normal University [2013CB955804]; NASA EPSCoR CAN at University of North Dakota [NNX11AM15A]; NASA NEWS [NNX09AJ36G]; NSF [ARC 1023592, 1107509]; Climate Change Research Division of the US Department of Energy as part of the Atmospheric System Research (ASR) Program FX This work is supported by the National Basic Research Program of China (973 Program, 2013CB955804) at Beijing Normal University. Researchers at University of North Dakota were supported by NASA EPSCoR CAN under Grant NNX11AM15A at University of North Dakota. The Georgia Tech co-author (Deng) was supported by the NASA NEWS under Grant NNX09AJ36G. X. Zhang was funded by the NSF through the Grant # ARC 1023592 and 1107509. Dr. Long acknowledges the support of the Climate Change Research Division of the US Department of Energy as part of the Atmospheric System Research (ASR) Program. NR 56 TC 5 Z9 5 U1 5 U2 25 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 JUL PY 2014 VL 43 IS 1-2 BP 53 EP 70 DI 10.1007/s00382-013-1920-8 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AK3PS UT WOS:000338337700004 ER PT J AU Kim, D Lee, MI Kim, D Schubert, SD Waliser, DE Tian, B AF Kim, Daehyun Lee, Myong-In Kim, Dongmin Schubert, Siegfried D. Waliser, Duane E. Tian, Baijun TI Representation of tropical subseasonal variability of precipitation in global reanalyses SO CLIMATE DYNAMICS LA English DT Article DE Reanalysis; Precipitation; Tropics; Subseasonal variability; Madden-Julian oscillation; Convectively-coupled equatorial waves ID MADDEN-JULIAN OSCILLATION; COUPLED EQUATORIAL WAVES; DATA ASSIMILATION SYSTEM; INTRASEASONAL VARIABILITY; CLIMATE MODELS; EL-NINO; PART I; PARAMETERIZATION; MODULATION; CONVECTION AB Tropical subseasonal variability of precipitation from five global reanalyses (RAs) is evaluated against Global Precipitation Climatology Project (GPCP) and Tropical Rainfall Measuring Mission (TRMM) observations. The RAs include the three generations of global RAs from the National Center for Environmental Prediction (NCEP), and two other RAs from the European Centre for Medium-Range Weather Forecasts (ECMWF) and the National Aeronautics and Space Administration/Goddard Space Flight Center (NASA/GSFC). The analysis includes comparisons of the seasonal means and subseasonal variances of precipitation, and probability densities of rain intensity in selected areas. In addition, the space-time power spectrum was computed to examine the tropical Madden-Julian Oscillation (MJO) and convectively coupled equatorial waves (CCEWs). The modern RAs show significant improvement in their representation of the mean state and subseasonal variability of precipitation when compared to the two older NCEP RAs: patterns of the seasonal mean state and the amplitude of subseasonal variability are more realistic in the modern RAs. However, the probability density of rain intensity in the modern RAs show discrepancies from observations that are similar to what the old RAs have. The modern RAs show higher coherence of CCEWs with observed variability and more realistic eastward propagation of the MJO precipitation. The modern RAs, however, exhibit common systematic deficiencies including: (1) variability of the CCEWs that tends to be either too weak or too strong, (2) limited coherence with observations for waves other than the MJO, and (3) a systematic phase lead or lag for the higher-frequency waves. C1 [Kim, Daehyun] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Lee, Myong-In; Kim, Dongmin] Ulsan Natl Inst Sci & Technol, Sch Urban & Environm Engn, Ulsan 689798, South Korea. [Schubert, Siegfried D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Waliser, Duane E.; Tian, Baijun] NASA, Jet Prop Lab, Pasadena, CA USA. RP Lee, MI (reprint author), Ulsan Natl Inst Sci & Technol, Sch Urban & Environm Engn, UNIST Gil 50, Ulsan 689798, South Korea. EM milee@unist.ac.kr RI Tian, Baijun/A-1141-2007; OI Tian, Baijun/0000-0001-9369-2373; Lee, Myong-In/0000-0001-8983-8624 FU Korea Meteorological Administration Research and Development Program [APCC 2013-3141]; NASA [NNX09AK34G]; NASA Modeling, Analysis, and Prediction (MAP) program; National Aeronautics and Space Administration (NASA) FX This work was supported by the Korea Meteorological Administration Research and Development Program under Grant APCC 2013-3141. Also, this work was supported by the NASA grant NNX09AK34G for DK, and the NASA Modeling, Analysis, and Prediction (MAP) program for SDS. DEW's and BT's contribution to this research was performed at Jet Propulsion Laboratory (JPL), California Institute of Technology (Caltech), under a contract with National Aeronautics and Space Administration (NASA). The authors are grateful for the computing resources provided by NASA and the Supercomputing Center at Korea Institute of Science and Technology Information (KSC-2013-C2-011). NR 54 TC 7 Z9 7 U1 2 U2 26 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 JUL PY 2014 VL 43 IS 1-2 BP 517 EP 534 DI 10.1007/s00382-013-1890-x PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AK3PS UT WOS:000338337700034 ER PT J AU Sokolovskiy, SV Schreiner, WS Zeng, Z Hunt, DC Kuo, YH Meehan, TK Stecheson, TW Mannucci, AJ Ao, CO AF Sokolovskiy, S. V. Schreiner, W. S. Zeng, Z. Hunt, D. C. Kuo, Y. -H. Meehan, T. K. Stecheson, T. W. Mannucci, A. J. Ao, C. O. TI Use of the L2C signal for inversions of GPS radio occultation data in the neutral atmosphere SO GPS SOLUTIONS LA English DT Article DE GPS radio occultation; Signal tracking; Inversion methods AB Results from processing FORMOSAT-3/COSMIC radio occultations (RO) with the new GPS L2C signal acquired both in phase locked loop (PLL) and open loop (OL) modes are presented. Analysis of L2P, L2C, and L1CA signals acquired in PLL mode shows that in the presence of strong ionospheric scintillation not only L2P tracking, but also L1CA tracking often fails, while L2C tracking is most stable. The use of L2C improves current RO processing in the neutral atmosphere mainly by increasing the number of processed occultations (due to significant reduction in the number of L2 tracking failures) and marginally by a reduction in noise in statistics. The latter is due to the combination of reduced L2C noise (compared to L2P) and increased L1CA noise in those occultations where L2P would have failed. This result suggests application of OL tracking for L1CA and L2C signals throughout an entire occultation to optimally acquire RO data. Two methods of concurrent processing of L1CA and L2C RO signals are considered. Based on testing of individual occultations, these methods allow: (1) reduction in uncertainty of bending angles retrieved by wave optics in the lower troposphere and (2) reduction in small-scale residual errors of the ionospheric correction in the stratosphere. C1 [Sokolovskiy, S. V.; Schreiner, W. S.; Zeng, Z.; Hunt, D. C.; Kuo, Y. -H.] Univ Corp Atmospher Res, Boulder, CO 80307 USA. [Meehan, T. K.; Stecheson, T. W.; Mannucci, A. J.; Ao, C. O.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RP Sokolovskiy, SV (reprint author), Univ Corp Atmospher Res, Boulder, CO 80307 USA. EM sergey@ucar.edu RI Zeng, Zhen/J-5183-2014 FU National Science Foundation [AGS-1033112] FX Research performed at the University Corporation for Atmospheric Research was supported by the National Science Foundation under the Cooperative Agreement AGS-1033112. Portions of this research were carried out at the Jet Propulsion Laboratory of the California Institute of technology, under a contract with the National Aeronautics and Space Administration. NR 22 TC 5 Z9 5 U1 0 U2 14 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1080-5370 EI 1521-1886 J9 GPS SOLUT JI GPS Solut. PD JUL PY 2014 VL 18 IS 3 BP 405 EP 416 DI 10.1007/s10291-013-0340-x PG 12 WC Remote Sensing SC Remote Sensing GA AK0YD UT WOS:000338141400009 ER PT J AU Strekalov, DV AF Strekalov, Dmitry V. TI A bundle of photons, please SO NATURE PHOTONICS LA English DT News Item ID QUANTUM-MECHANICS; CURRENT SITUATION C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Strekalov, DV (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM dmitry.v.strekalov@jpl.nasa.gov NR 12 TC 0 Z9 0 U1 1 U2 6 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1749-4885 EI 1749-4893 J9 NAT PHOTONICS JI Nat. Photonics PD JUL PY 2014 VL 8 IS 7 BP 500 EP 501 PG 2 WC Optics; Physics, Applied SC Optics; Physics GA AK1YT UT WOS:000338216000002 ER PT J AU Chakrabarty, RK Beres, ND Moosmuller, H China, S Mazzoleni, C Dubey, MK Liu, L Mishchenko, MI AF Chakrabarty, Rajan K. Beres, Nicholas D. Moosmueller, Hans China, Swarup Mazzoleni, Claudio Dubey, Manvendra K. Liu, Li Mishchenko, Michael I. TI Soot superaggregates from flaming wildfires and their direct radiative forcing SO SCIENTIFIC REPORTS LA English DT Article ID INDIVIDUAL AEROSOL-PARTICLES; BIOMASS BURNING PARTICLES; SOUTHERN AFRICA; CARBONACEOUS PARTICLES; FRACTAL DIMENSION; LIGHT-SCATTERING; BROWN CARBON; MEXICO-CITY; T-MATRIX; ABSORPTION AB Wildfires contribute significantly to global soot emissions, yet their aerosol formation mechanisms and resulting particle properties are poorly understood and parameterized in climate models. The conventional view holds that soot is formed via the cluster-dilute aggregation mechanism in wildfires and emitted as aggregates with fractal dimension D-f approximate to 1.8 mobility diameter D-m <= 1 mu m, and aerodynamic diameter D-a <= 300 nm. Here we report the ubiquitous presence of soot superaggregates (SAs) in the outflow from a major wildfire in India. SAs are porous, low-density aggregates of cluster-dilute aggregates with characteristic D-f approximate to 2.6, D-m > 1 mu m, and D-a <= 300 nm that form via the cluster-dense aggregation mechanism. We present additional observations of soot SAs in wildfire smoke-laden air masses over Northern California, New Mexico, and Mexico City. We estimate that SAs contribute, per unit optical depth, up to 35% less atmospheric warming than freshly-emitted (Df approximate to 1.8) aggregates, and approximate to 90% more warming than the volume-equivalent spherical soot particles simulated in climate models. C1 [Chakrabarty, Rajan K.] Washington Univ, Dept Energy Environm & Chem Engn, St Louis, MO 63130 USA. [Chakrabarty, Rajan K.; Beres, Nicholas D.; Moosmueller, Hans] Nevada Syst Higher Educ, Desert Res Inst, Reno, NV USA. [China, Swarup; Mazzoleni, Claudio] Michigan Technol Univ, Atmospher Sci Program, Houghton, MI 49931 USA. [Dubey, Manvendra K.] Los Alamos Natl Lab, Earth Syst Observat, Los Alamos, NM USA. [Liu, Li; Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Chakrabarty, RK (reprint author), Washington Univ, Dept Energy Environm & Chem Engn, St Louis, MO 63130 USA. EM rajan.chakrabarty@gmail.com RI Dubey, Manvendra/E-3949-2010; Mishchenko, Michael/D-4426-2012; OI Dubey, Manvendra/0000-0002-3492-790X; Moosmuller, Hans/0000-0002-1021-8877 FU NASA [NNX10AR89A, NNX11AB79G, NNX12AN97H]; U.S. Department of Energy Atmospheric System Research(PI-MKD) [DE-SC0010019, F265-LANL]; Desert Research Institute; U. S. National Science Foundation Division of Atmospheric and Geospace Sciences [ATM07-21142] FX This material is based upon work supported by NASA (NNX10AR89A, NNX11AB79G and NNX12AN97H), the U.S. Department of Energy Atmospheric System Research (DE-SC0010019 and F265-LANL(PI-MKD)), the U. S. National Science Foundation Division of Atmospheric and Geospace Sciences (ATM07-21142), and the Desert Research Institute. We thank V. Ramanathan for facilitating our participation in the field campaign at Maldives; K. Gorkowski for his help with sampling aerosols during CARES and the Las Conchas fire; O. Gustafsson for providing quartz fiber filter samples; B. Zielinska and her laboratory for performing mass spectrometry analyses of quartz fiber filters; M. Ahmadian for assisting with microscopy analysis; L. Wable for illustrations; R. Kreidberg for help with editing the manuscript; and C. M. Sorensen for insightful discussions. NR 56 TC 24 Z9 24 U1 3 U2 54 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2045-2322 J9 SCI REP-UK JI Sci Rep PD JUL 1 PY 2014 VL 4 AR 5508 DI 10.1038/srep05508 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AK4UR UT WOS:000338420100005 PM 24981204 ER PT J AU Sobron, P Bishop, JL Blake, DF Chen, B Rull, F AF Sobron, Pablo Bishop, Janice L. Blake, David F. Chen, Bin Rull, Fernando TI Natural Fe-bearing oxides and sulfates from the Rio Tinto Mars analog site: Critical assessment of VNIR reflectance spectroscopy, laser Raman spectroscopy, and XRD as mineral identification tools SO AMERICAN MINERALOGIST LA English DT Article DE Raman; VNIR reflectance; XRD; sulfates; iron; Mars; analog; Rio Tinto ID MERIDIANI-PLANUM; JAROSITE; HEMATITE; ROCKS; WATER; SPECTROMETER; DEPOSITS; SURFACE; GYPSUM; SOILS AB We have characterized complex iron- and sulfate-bearing samples from Rio Tinto (Spain) using X-ray diffraction (XRD), visible-near infrared reflectance (VNIR) spectroscopy, and laser Raman spectroscopy (LRS). Samples were collected for this study from the Pena de Hierro region of Rio Tinto because this site represents a natural acidic environment that is a potential analog for such environments on Mars. We report an evaluation of the capabilities of these three techniques in performing detailed mineralogical characterization of potential Mars-like samples from a natural acidic terrestrial environment. Sulfate minerals found in these samples include gypsum, jarosite, and copiapite, and iron hydroxide bearing minerals found include goethite and ferrihydrite. These sulfate and iron hydroxide/oxyhydroxide minerals were detected by XRD, VNIR, and LRS. Minor quartz was identified in some samples by XRD as well, but was not identified using VNIR spectroscopy. Coordinating the results from these three techniques provides a complete picture of the mineralogical composition of the samples. Field instruments were used for this study to mimic the kinds of analyses that could be performed in the field or on martian rovers. C1 [Sobron, Pablo; Bishop, Janice L.] SETI Inst, Mountain View, CA 94043 USA. [Sobron, Pablo] MalaUva Labs, St Louis, MO 63104 USA. [Bishop, Janice L.; Blake, David F.; Chen, Bin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rull, Fernando] UVA Ctr Astrobiol, Unidad Asociada, Boecillo 47151, Spain. RP Sobron, P (reprint author), SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA. EM psobron@seti.org FU Research Council of Spain (CSIC) [UAC2005-007]; NASA Astrobiology Institute FX This work was partially supported by the Research Council of Spain (CSIC) through grant no. UAC2005-007 and the NASA Astrobiology Institute through the Lewis and Clark Fund for Exploration and Field Research in Astrobiology. The authors thank Aurelio Sanz and Tayro Acosta for their valuable assistance in the collection and preservation of samples. NR 51 TC 4 Z9 4 U1 2 U2 26 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 JUL PY 2014 VL 99 IS 7 BP 1199 EP 1205 DI 10.2138/am.2014.4595 PG 7 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA AK0FR UT WOS:000338088800004 ER PT J AU Bell, AS Burger, PV Le, L Shearer, CK Papike, JJ Sutton, SR Newville, M Jones, J AF Bell, Aaron S. Burger, Paul V. Le, Loan Shearer, Charles K. Papike, James J. Sutton, Steve R. Newville, Matthew Jones, John TI XANES measurements of Cr valence in olivine and their applications to planetary basalts SO AMERICAN MINERALOGIST LA English DT Article DE XANES; Cr valence; redox equilibria; martian basalts ID PHYRIC MARTIAN BASALTS; OXIDATION-STATE; OXYGEN FUGACITY; REDOX STATES; UPPER-MANTLE; SIDEROPHILE ELEMENTS; SILICATE MELTS; CHROMIUM; MAGMAS; LIQUID AB In this work we present a series of experiments that examine the relationship between oxygen fugacity and Cr valence ratio in olivine grown from a basaltic liquid. These experiments are specifically targeted for an olivine-rich martian basalt composition that was modeled after the bulk chemistry of the meteorite Yamato 980459 (i.e., Y-98). The chromium valence ratio in the olivine crystals was measured with X-ray absorption near edge spectroscopy (XANES) at the Advanced Photon Source, Argonne National Laboratory. Results from the XANES measurements indicate that the ratio of divalent to trivalent Cr in the olivine is not only systematically correlated with f(O2), but is also reflective of the molar Cr3+/Cr2+ in the silicate liquid from which it grew. In this way, measurements of Cr valence in olivine phenocrysts can yield important information about the oxygen fugacity and molar Cr3+/Cr2+ of its parental liquid in the absence of a quenched melt phase. Although the results from the experiments presented in this work specifically apply to the Y-98 parental melt, the concepts and XANES analytical techniques discussed within the text present a novel, generalized methodology that may be applicable to any olivine-bearing basalt. Furthermore, the XANES-based measurements are made on a micrometer-scale, thus potential changes of the Cr3+/Cr2+ in the melt during crystallization could be examined with a great deal of spatial detail. C1 [Bell, Aaron S.; Burger, Paul V.; Shearer, Charles K.; Papike, James J.] Univ New Mexico, Dept Earth & Planetary Sci, Inst Meteorit, Albuquerque, NM 87131 USA. [Le, Loan; Jones, John] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Sutton, Steve R.; Newville, Matthew] Univ Chicago, Ctr Adv Radiat Sources, Chicago, IL 60637 USA. RP Bell, AS (reprint author), Univ New Mexico, Dept Earth & Planetary Sci, Inst Meteorit, Albuquerque, NM 87131 USA. EM asbell@unm.edu FU NASA Cosmochemistry grants; National Science Foundation-Earth Sciences [EAR-1128799]; Department Geosciences [DE-FG02-94ER14466]; U.S. Department of Energy. Office of Science. Office of Basic Energy Science [DE-AC02-06CH11357] FX This research was supported by NASA Cosmochemistry grants to C. Shearer and J. Jones. Francis McCubbin is also thanked an early, informal review of the manuscript. Steve Simon and Fred Davis are thanked for reviews that improved the content and the readability of the manuscript. We gratefully acknowledge the beamline award, as well as assistance of GSECARS beamline staff. GeoSoilEnviroCARS is supported by the National Science Foundation-Earth Sciences (EAR-1128799) and Department Geosciences (DE-FG02-94ER14466). Use of the Advanced Photon Source was supported by U.S. Department of Energy. Office of Science. Office of Basic Energy Science under Contract No. DE-AC02-06CH11357. NR 33 TC 9 Z9 9 U1 4 U2 28 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 JUL PY 2014 VL 99 IS 7 BP 1404 EP 1412 DI 10.2138/am.2014.4646 PG 9 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA AK0FR UT WOS:000338088800023 ER PT J AU Shen, ZZ Konishi, H Szlufarska, I Brown, PE Xu, HF AF Shen, Zhizhang Konishi, Hiromi Szlufarska, Izabela Brown, Philip E. Xu, Huifang TI Z-contrast imaging and ab initio study on "d" superstructure in sedimentary dolomite SO AMERICAN MINERALOGIST LA English DT Article DE Dolomite; d superstructure; Z-contrast imaging; density functional theory; molar tooth carbonate ID MOLAR-TOOTH STRUCTURES; MECHANICAL-PROPERTIES; CARBONATES; SERIES; INTERSTRATIFICATION; 1ST-PRINCIPLES; MICROSCOPY; CHINA; ROCK AB Nano-precipitates with tripled periodicity along the c-axis are observed in a Ca-rich dolomite sample from Proterozoic carbonate rocks with "molar tooth" structure. This observation is consistent with previous description of d reflections. High-angle annular dark-field STEM imaging (or Z-contrast imaging) that avoids dynamic diffraction as seen in electron diffraction and high-resolution TEM imaging modes, confirms that d reflections correspond to nanoscale precipitates aligned parallel to (001) of the host dolomite. The lamellae precipitates have a cation ordering sequence of Ca-Ca-Mg-Ca-Ca-Mg along the c direction resulting in a chemical composition of Ca0.67Mg0.33CO3. This superstructure is attributed to the extra or d reflections, thus is referred to as the d superstructure in this study. The structure can be simply described as interstratified calcite/dolomite. The crystal structure of the d superstructure calculated from density functional theory (DFT) has a space group of P31c and has a and c unit-cell parameters of 4.879 and 16.260 angstrom, respectively, values between those of dolomite and calcite. The detailed structural characteristics and parameters obtained from ab initio calculations are also reported in this paper. The method of combining Z-contrast imaging and ab initio calculations can be used for solving structures of other nano-precipitates and nano-phases. C1 [Shen, Zhizhang; Konishi, Hiromi; Brown, Philip E.; Xu, Huifang] Univ Wisconsin, NASA Astrobiol Inst, Dept Geosci, Madison, WI 53706 USA. [Szlufarska, Izabela] Univ Wisconsin, Dept Mat Sci & Engn, Madison, WI 53706 USA. RP Shen, ZZ (reprint author), Univ Wisconsin, NASA Astrobiol Inst, Dept Geosci, Madison, WI 53706 USA. EM hfxu@geology.wisc.edu FU NASA Astrobiology Institute [N07-5489]; NSF [EAR-095800] FX This work is supported by NASA Astrobiology Institute (N07-5489) and NSF (EAR-095800). Shen also thanks alumni of the Department of Geoscience of University of Wisconsin-Madison for supporting his field trips. NR 37 TC 2 Z9 2 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 JUL PY 2014 VL 99 IS 7 BP 1413 EP 1419 DI 10.2138/am.2014.4647 PG 7 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA AK0FR UT WOS:000338088800024 ER PT J AU Hunter, SD Bloser, PF Depaola, GO Dion, MP DeNolfo, GA Hanu, A Iparraguirre, M Legere, J Longo, F McConnell, ML Nowicki, SF Ryan, JM Son, S Stecker, FW AF Hunter, Stanley D. Bloser, Peter F. Depaola, Gerardo O. Dion, Michael P. DeNolfo, Georgia A. Hanu, Andrei Iparraguirre, Marcos Legere, Jason Longo, Francesco McConnell, Mark L. Nowicki, Suzanne F. Ryan, James M. Son, Seunghee Stecker, Floyd W. TI A pair production telescope for medium-energy gamma-ray polarimetry SO ASTROPARTICLE PHYSICS LA English DT Article DE Gamma rays; Pair production; Angular resolution; Polarimetry; Sensitivity; Time projection chamber ID DOUBLE RADIO-SOURCES; CARBON-DISULFIDE; LONGITUDINAL DIFFUSION; PROPORTIONAL-COUNTERS; MULTIPLE-SCATTERING; LINEAR-POLARIZATION; EGRET OBSERVATIONS; CRAB PULSAR; DETECTORS; EMISSION AB We describe the science motivation and development of a pair production telescope for medium-energy (similar to 5-200 MeV) gamma-ray polarimetry. Our instrument concept, the Advanced Energetic Pair Telescope (AdEPT), takes advantage of the Three-Dimensional Track Imager, a low-density gaseous time projection chamber, to achieve angular resolution within a factor of two of the pair production kinematics limit (similar to 0.6 degrees at 70 MeV), continuum sensitivity comparable with the Fermi-LAT front detector (<3 x 10(-6) MeV cm(-2) s(-1) 70 MeV), and minimum detectable polarization less than 10% for a 10 mCrab source in 10(6) s. Published by Elsevier B.V. C1 [Hunter, Stanley D.; DeNolfo, Georgia A.; Hanu, Andrei; Nowicki, Suzanne F.; Son, Seunghee; Stecker, Floyd W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bloser, Peter F.; Legere, Jason; McConnell, Mark L.; Ryan, James M.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Depaola, Gerardo O.; Iparraguirre, Marcos] Univ Cordoba, Fac Matemat Astron & Fis, RA-5008 Cordoba, Argentina. [Dion, Michael P.] Pacific NW Natl Lab, Richland, WA 99352 USA. [Longo, Francesco] Univ Trieste, Dipartimento Fis, Treste, Italy. [Nowicki, Suzanne F.; Son, Seunghee] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. RP Hunter, SD (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM stanley.d.hunter@nasa.gov OI Dion, Michael/0000-0002-3030-0050 NR 89 TC 12 Z9 12 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 EI 1873-2852 J9 ASTROPART PHYS JI Astropart Phys. PD JUL-AUG PY 2014 VL 59 BP 18 EP 28 DI 10.1016/j.astropartphys.2014.04.002 PG 11 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AJ7MT UT WOS:000337881500004 ER PT J AU Sturrock, PA Fischbach, E Javorsek, D Jenkins, JH Lee, RH Nistor, J Scargle, JD AF Sturrock, P. A. Fischbach, E. Javorsek, D., II Jenkins, J. H. Lee, R. H. Nistor, J. Scargle, J. D. TI Comparative study of beta-decay data for eight nuclides measured at the Physikalisch-Technische Bundesanstalt SO ASTROPARTICLE PHYSICS LA English DT Article DE Sun; Neutrinos; Nuclear decays ID R-MODE OSCILLATIONS; SOLAR; ROTATION; RATES AB We present the results of time-series analyses of data, kindly provided by the Physikalisch-Technische Bundesanstalt, concerning the beta-decays of Ag108, Ba133, Cs137, Eu152, Eu154, Kr85, Ra226, and Sr90. From measurements of the detector currents, we find evidence of annual oscillations (especially for Ra226), and for several solar r-mode oscillations. It is notable that the frequencies of these r-mode oscillations correspond to exactly the same sidereal rotation rate (12.08 year(-1)) that we have previously identified in r-mode oscillations detected in both Mt Wilson solar diameter data and Lomonosov Moscow State University Sr90 beta-decay data. Ba133 is found to be anomalous in that current measurements for this nuclide have a much larger variation (by 4 sigma) than those of the other nuclides. It is interesting that analysis of variability measurements in the PTB files yields strong evidence for an oscillation for Ba133 but only weak evidence for Ra226. (C) 2014 Elsevier B.V. All rights reserved. C1 [Sturrock, P. A.] Stanford Univ, Ctr Space Sci & Astrophys, Stanford, CA 94305 USA. [Fischbach, E.; Nistor, J.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Jenkins, J. H.] Texas A&M Univ, Dept Nucl Engn, College Stn, TX 77843 USA. [Lee, R. H.] US Air Force Acad, Dept Phys, Colorado Springs, CO 80920 USA. [Scargle, J. D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Sturrock, PA (reprint author), Stanford Univ, Ctr Space Sci & Astrophys, Stanford, CA 94305 USA. EM sturrock@stanford.edu OI Javorsek, Daniel/0000-0002-0329-4011 NR 18 TC 10 Z9 10 U1 2 U2 14 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 EI 1873-2852 J9 ASTROPART PHYS JI Astropart Phys. PD JUL-AUG PY 2014 VL 59 BP 47 EP 58 DI 10.1016/j.astropartphys.2014.04.006 PG 12 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AJ7MT UT WOS:000337881500007 ER PT J AU Ajello, M Albert, A Allafort, A Baldini, L Barbiellini, G Bastieri, D Bellazzini, R Bissaldi, E Bonamente, E Brandt, TJ Bregeon, J Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Cecchi, C Charles, E Chekhtman, A Chiang, J Chiaro, G Ciprini, S Claus, R Cohen-Tanugi, J Cominsky, LR Conrad, J Cutini, S D'Ammando, F de Palma, F Dermer, CD Desiante, R Digel, SW Silva, EDE Drell, PS Drlica-Wagner, A Favuzzi, C Focke, WB Franckowiak, A Fukazawa, Y Fusco, P Gargano, F Gasparrini, D Germani, S Giglietto, N Giommi, P Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grove, JE Guiriec, S Hadasch, D Hayashida, M Hays, E Horan, D Hou, X Hughes, RE Inoue, Y Jackson, MS Jogler, T Johannesson, G Johnson, AS Johnson, WN Kamae, T Knodlseder, J Kocevski, D Kuss, M Lande, J Larsson, S Latronico, L Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Mayer, M Mazziotta, MN McEnery, JE Michelson, PF Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Murphy, R Nakamori, T Nemmen, R Nuss, E Ohno, M Ohsugi, T Omodei, N Orienti, M Orlando, E Ormes, JF Paneque, D Panetta, JH Perkins, JS Pesce-Rollins, M Petrosian, V Piron, F Pivato, G Porter, TA Raino, S Rando, R Razzano, M Reimer, A Reimer, O Roth, M Schulz, A Sgro, C Siskind, EJ Spandre, G Spinelli, P Takahashi, H Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tinivella, M Tosti, G Troja, E Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Werner, M Winer, BL Wood, DL Wood, KS Yang, Z AF Ajello, M. Albert, A. Allafort, A. Baldini, L. Barbiellini, G. Bastieri, D. Bellazzini, R. Bissaldi, E. Bonamente, E. Brandt, T. J. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cecchi, C. Charles, E. Chekhtman, A. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. Cohen-Tanugi, J. Cominsky, L. R. Conrad, J. Cutini, S. D'Ammando, F. de Palma, F. Dermer, C. D. Desiante, R. Digel, S. W. do Couto e Silva, E. Drell, P. S. Drlica-Wagner, A. Favuzzi, C. Focke, W. B. Franckowiak, A. Fukazawa, Y. Fusco, P. Gargano, F. Gasparrini, D. Germani, S. Giglietto, N. Giommi, P. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guiriec, S. Hadasch, D. Hayashida, M. Hays, E. Horan, D. Hou, X. Hughes, R. E. Inoue, Y. Jackson, M. S. Jogler, T. Johannesson, G. Johnson, A. S. Johnson, W. N. Kamae, T. Knoedlseder, J. Kocevski, D. Kuss, M. Lande, J. Larsson, S. Latronico, L. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Mayer, M. Mazziotta, M. N. McEnery, J. E. Michelson, P. F. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Murphy, R. Nakamori, T. Nemmen, R. Nuss, E. Ohno, M. Ohsugi, T. Omodei, N. Orienti, M. Orlando, E. Ormes, J. F. Paneque, D. Panetta, J. H. Perkins, J. S. Pesce-Rollins, M. Petrosian, V. Piron, F. Pivato, G. Porter, T. A. Raino, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Roth, M. Schulz, A. Sgro, C. Siskind, E. J. Spandre, G. Spinelli, P. Takahashi, H. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tinivella, M. Tosti, G. Troja, E. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Werner, M. Winer, B. L. Wood, D. L. Wood, K. S. Yang, Z. TI IMPULSIVE AND LONG DURATION HIGH-ENERGY GAMMA-RAY EMISSION FROM THE VERY BRIGHT 2012 MARCH 7 SOLAR FLARES SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: flares; Sun: X-rays, gamma rays ID LARGE-AREA TELESCOPE; STOCHASTIC ACCELERATION; X-RAY; VELA PULSAR; ELECTRON ACCELERATION; EGRET; CALIBRATION; PARTICLES; COMPTON; DIRECTIVITY AB The Fermi Large Area Telescope (LAT) detected gamma-rays up to 4 GeV from two bright X-class solar flares on 2012 March 7, showing both an impulsive and temporally extended emission phases. The gamma-rays appear to originate from the same active region as the X-rays associated with these flares. The >100 MeV gamma-ray flux decreases monotonically during the first hour (impulsive phase) followed by a slower decrease for the next 20 hr. A power law with a high-energy exponential cutoff can adequately describe the photon spectrum. Assuming that the gamma rays result from the decay of pions produced by accelerated protons and ions with a power-law spectrum, we find that the index of that spectrum is similar to 3, with minor variations during the impulsive phase. During the extended phase the photon spectrum softens monotonically, requiring the proton index varying from similar to 4 to >5. The >30 MeV proton flux observed by the GOES satellites also shows a flux decrease and spectral softening, but with a harder spectrum (index similar to 2-3). Based on these observations, we explore the relative merits of prompt or continuous acceleration scenarios, hadronic or leptonic emission processes, and acceleration at the solar corona or by the fast coronal mass ejections. We conclude that the most likely scenario is continuous acceleration of protons in the solar corona that penetrate the lower solar atmosphere and produce pions that decay into gamma rays. However, acceleration in the downstream of the shock cannot be definitely ruled out. C1 [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Albert, A.; Allafort, A.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Inoue, Y.; Jogler, T.; Johnson, A. S.; Kamae, T.; Kocevski, D.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Petrosian, V.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Albert, A.; Allafort, A.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Inoue, Y.; Jogler, T.; Johnson, A. S.; Kamae, T.; Kocevski, D.; Lande, J.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Petrosian, V.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Baldini, L.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Barbiellini, G.; Bissaldi, E.; Desiante, R.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Chiaro, G.; Pivato, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bissaldi, E.] Univ Trieste, I-34127 Trieste, Italy. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brandt, T. J.; Guiriec, S.; Hays, E.; McEnery, J. E.; Moiseev, A. A.; Nemmen, R.; Perkins, J. S.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Horan, D.] Ecole Polytech, CNRS IN2P3, Lab Leprince Ringuet, Palaiseau, France. [Buehler, R.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Chekhtman, A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Ciprini, S.; Cutini, S.; Gasparrini, D.; Giommi, P.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Frascati, Roma, Italy. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Ist Nazl Astrofis Osservatorio Astron Roma, I-00040 Rome, Italy. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS IN2P3, Lab Univers & Particules Montpellier, Montpellier, France. [Cominsky, L. R.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA. [Conrad, J.; Larsson, S.; Yang, Z.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Conrad, J.; Jackson, M. S.; Larsson, S.; Yang, Z.] Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden. [D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Murphy, R.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Drlica-Wagner, A.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Fukazawa, Y.; Ohno, M.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Grenier, I. A.] CEA IRFU CNRS Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM, F-91191 Gif Sur Yvette, France. [Hadasch, D.; Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Hadasch, D.; Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Hayashida, M.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Hou, X.; Lott, B.] Univ Bordeaux 1, CNRS IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Jackson, M. S.] Royal Inst Technol KTH, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Knoedlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, UPS OMP, IRAP, GAHEC, Toulouse, France. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [McEnery, J. E.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.; Moiseev, A. A.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Moiseev, A. A.] CRESST, Greenbelt, MD 20771 USA. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Murgia, S.] Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Wood, D. L.] Praxis Inc, Alexandria, VA 22303 USA. RP Ajello, M (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. EM nicola.omodei@stanford.edu; melissa.pesce.rollins@pi.infn.it; vahep@stanford.edu RI Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Mazziotta, Mario /O-8867-2015; Orlando, E/R-5594-2016; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Sgro, Carmelo/K-3395-2016; Bissaldi, Elisabetta/K-7911-2016 OI Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726; giommi, paolo/0000-0002-2265-5003; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; Inoue, Yoshiyuki/0000-0002-7272-1136; Bastieri, Denis/0000-0002-6954-8862; Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; Reimer, Olaf/0000-0001-6953-1385; Morselli, Aldo/0000-0002-7704-9553; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Mazziotta, Mario /0000-0001-9325-4672; Giordano, Francesco/0000-0002-8651-2394; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; Bissaldi, Elisabetta/0000-0001-9935-8106 NR 56 TC 25 Z9 25 U1 1 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 JUL 1 PY 2014 VL 789 IS 1 AR 20 DI 10.1088/0004-637X/789/1/20 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400020 ER PT J AU Bulbul, E Markevitch, M Foster, A Smith, RK Loewenstein, M Randall, SW AF Bulbul, Esra Markevitch, Maxim Foster, Adam Smith, Randall K. Loewenstein, Michael Randall, Scott W. TI DETECTION OF AN UNIDENTIFIED EMISSION LINE IN THE STACKED X-RAY SPECTRUM OF GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; elementary particles; line: identification; neutrinos; X-rays: galaxies: clusters ID DWARF SPHEROIDAL GALAXY; XMM-NEWTON SPECTROSCOPY; DECAYING DARK-MATTER; STERILE NEUTRINOS; CHANDRA; SAMPLE; CONSTRAINTS; COSMOLOGY; MODEL; LIGHT AB We detect a weak unidentified emission line at E = (3.55-3.57) +/- 0.03 keV in a stacked XMM-Newton spectrum of 73 galaxy clusters spanning a redshift range 0.01-0.35. When the full sample is divided into three subsamples (Perseus, Centaurus+Ophiuchus+Coma, and all others), the line is seen at >3 sigma statistical significance in all three independent MOS spectra and the PN "all others" spectrum. It is also detected in the Chandra spectra of the Perseus Cluster. However, it is very weak and located within 50-110 eV of several known lines. The detection is at the limit of the current instrument capabilities. We argue that there should be no atomic transitions in thermal plasma at this energy. An intriguing possibility is the decay of sterile neutrino, a long-sought dark matter particle candidate. Assuming that all dark matter is in sterile neutrinos with m(s) = 2 E = 7.1 keV, our detection corresponds to a neutrino decay rate consistent with previous upper limits. However, based on the cluster masses and distances, the line in Perseus is much brighter than expected in this model, significantly deviating from other subsamples. This appears to be because of an anomalously bright line at E = 3.62 keV in Perseus, which could be an Ar XVII dielectronic recombination line, although its emissivity would have to be 30 times the expected value and physically difficult to understand. Another alternative is the above anomaly in the Ar line combined with the nearby 3.51 keV K line also exceeding expectation by a factor of 10-20. Confirmation with Astro-H will be critical to determine the nature of this new line. C1 [Bulbul, Esra; Foster, Adam; Smith, Randall K.; Randall, Scott W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bulbul, Esra; Loewenstein, Michael] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Bulbul, Esra; Loewenstein, Michael] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Markevitch, Maxim] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Loewenstein, Michael] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Bulbul, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ebulbul@cfa.harvard.edu OI Randall, Scott/0000-0002-3984-4337; Smith, Randall/0000-0003-4284-4167 FU Chandra grant [AR0-11020X, GO1-12104X]; NASA ADAP grant [NNX12AF44G]; Chandra X-ray Center through NASA [NAS8-03060]; Smithsonian Institution FX The authors thank Alexey Vikhlinin for extensive discussions, cross-checking the results, and spotting several errors; Douglas Finkbeiner and Serkan Cabi for useful discussions; Christine Jones, Signe Riemer-Sorensen, Alexander Kusenko, and the anonymous referee for useful comments on the draft; and Kevork Abazajian and Shunsaku Horiuchi for providing the limits from their M31 analysis. E.B. also thanks Adrian Batu Gerard for patiently waiting for the submission to be born. E.B. was supported in part by Chandra grant AR0-11020X and GO1-12104X. A.F. and R.S. were supported in part by NASA ADAP grant NNX12AF44G. S.W.R. was supported by the Chandra X-ray Center through NASA contract NAS8-03060 and the Smithsonian Institution. NR 69 TC 218 Z9 218 U1 2 U2 20 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2014 VL 789 IS 1 AR 13 DI 10.1088/0004-637X/789/1/13 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400013 ER PT J AU Donoso, E Yan, L Stern, D Assef, RJ AF Donoso, E. Yan, Lin Stern, D. Assef, R. J. TI THE ANGULAR CLUSTERING OF WISE-SELECTED ACTIVE GALACTIC NUCLEI: DIFFERENT HALOS FOR OBSCURED AND UNOBSCURED ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; infrared: galaxies; surveys ID DIGITAL-SKY-SURVEY; PHOTOMETRICALLY CLASSIFIED QUASARS; SUPERMASSIVE BLACK-HOLES; GALAXY REDSHIFT SURVEY; WIDE-FIELD SURVEY; RAY SELECTED AGN; X-RAY; COSMOS FIELD; MIDINFRARED SELECTION; BOOTES FIELD AB We calculate the angular correlation function for a sample of similar to 170,000 active galactic nuclei (AGNs) extracted from the Wide-field Infrared Survey Explorer (WISE) catalog, selected to have red mid-IR colors (W1 - W2 > 0.8) and 4.6 mu m flux densities brighter than 0.14 mJy). The sample is expected to be > 90% reliable at identifying AGNs and to have a mean redshift of < z > = 1.1. In total, the angular clustering of WISE AGNs is roughly similar to that of optical AGNs. We cross-match these objects with the photometric Sloan Digital Sky Survey catalog and distinguish obscured sources with r - W2 > 6 from bluer, unobscured AGNs. Obscured sources present a higher clustering signal than unobscured sources. Since the host galaxy morphologies of obscured AGNs are not typical red sequence elliptical galaxies and show disks in many cases, it is unlikely that the increased clustering strength of the obscured population is driven by a host galaxy segregation bias. By using relatively complete redshift distributions from the COSMOS survey, we find that obscured sources at < z > similar to 0.9 have a bias of b = 2.9 +/- 0.6 and are hosted in dark matter halos with a typical mass of log(M/M(circle dot)h(-1)) similar to 13.5. In contrast, unobscured AGNs at < z > similar to 1.1 have a bias of b = 1.6 +/- 0.6 and inhabit halos of log(M/M(circle dot)h(-1)) similar to 12.4. These findings suggest that obscured AGNs inhabit denser environments than unobscured AGNs, and they are difficult to reconcile with the simplest AGN unification models, where obscuration is driven solely by orientation. C1 [Donoso, E.] ICATE, RA-5400 San Juan, Argentina. [Donoso, E.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Yan, Lin] CALTECH, Infrared Proc & Anal Ctr, Dept Astron, Pasadena, CA 91125 USA. [Stern, D.; Assef, R. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Assef, R. J.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Santiago, Chile. RP Donoso, E (reprint author), ICATE, RA-5400 San Juan, Argentina. FU National Aeronautics and Space Administration; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; CONICET; Gemini grant [32120009]; NASA Astrophysics Data Analysis Program (ADAP) FX We thank A. Myers for useful replies to questions and extend our gratitude to the WISE extragalactic science team for its continuous support and interesting discussions over the years. We also gratefully acknowledge the anonymous referee and numerous colleagues, including G. Hasinger and R. Hickox, who provided insightful comments that have improved our discussion. 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. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS website is http://www.sdss.org/. R.J.A. was supported in part by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. This research was partially supported by CONICET. R.J.A. was also supported in part by Gemini grant number 32120009. We also thank the NASA Astrophysics Data Analysis Program (ADAP) for its support. NR 64 TC 23 Z9 23 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2014 VL 789 IS 1 AR 44 DI 10.1088/0004-637X/789/1/44 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400044 ER PT J AU Henning, WG Hurford, T AF Henning, Wade G. Hurford, Terry TI TIDAL HEATING IN MULTILAYERED TERRESTRIAL EXOPLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE celestial mechanics; planetary systems; planets and satellites: general ID EXTRASOLAR PLANETARY SYSTEMS; SPIN-ORBIT RESONANCES; EARTH-LIKE PLANETS; CLOSE-IN PLANETS; GIANT PLANETS; HOT JUPITERS; SUPER-EARTH; DYNAMICAL EVOLUTION; NONSYNCHRONOUS ROTATION; SHORT-PERIOD AB The internal pattern and overall magnitude of tidal heating for spin-synchronous terrestrial exoplanets from 1 to 2.5 R-E is investigated using a propagator matrix method for a variety of layer structures. Particular attention is paid to ice-silicate hybrid super-Earths, where a significant ice mantle is modeled to rest atop an iron-silicate core, and may or may not contain a liquid water ocean. We find multilayer modeling often increases tidal dissipation relative to a homogeneous model, across multiple orbital periods, due to the ability to include smaller volume low viscosity regions, and the added flexure allowed by liquid layers. Gradations in parameters with depth are explored, such as allowed by the Preliminary Earth Reference Model. For ice-silicate hybrid worlds, dramatically greater dissipation is possible beyond the case of a silicate mantle only, allowing non-negligible tidal activity to extend to greater orbital periods than previously predicted. Surface patterns of tidal heating are found to potentially be useful for distinguishing internal structure. The influence of ice mantle depth and water ocean size and position are shown for a range of forcing frequencies. Rates of orbital circularization are found to be 10-100 times faster than standard predictions for Earth-analog planets when interiors are moderately warmer than the modern Earth, as well as for a diverse range of ice-silicate hybrid super-Earths. Circularization rates are shown to be significantly longer for planets with layers equivalent to an ocean-free modern Earth, as well as for planets with high fractions of either ice or silicate melting. C1 [Henning, Wade G.; Hurford, Terry] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Henning, WG (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM wade.g.henning@nasa.gov RI Hurford, Terry/F-2625-2012 FU NASA Postdoctoral Program FX This work has been supported by the NASA Postdoctoral Program. We thank William Moore, Dimitar Sasselov, Richard O'Connell, Sarah Stewart, Lisa Kaltenegger, Alec Brenner, Marc Kuchner, Avi Mandell, Soko Matsumura, Robert Tyler, Valeri Makarov, and Christopher Hamilton for many useful discussions and comments. We especially thank Michael Efroimsky for a very thoughtful review which significantly helped to improve this manuscript. This work gratefully utilized the Tide-Lab suite of code developed and provided by William Moore for calculations of surface Love numbers on planets containing liquid oceans. NR 193 TC 11 Z9 11 U1 0 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2014 VL 789 IS 1 AR 30 DI 10.1088/0004-637X/789/1/30 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400030 ER PT J AU Hermes, JJ Charpinet, S Barclay, T Pakstiene, E Mullally, F Kawaler, SD Bloemen, S Castanheira, BG Winget, DE Montgomery, MH Van Grootel, V Huber, D Still, M Howell, SB Caldwell, DA Haas, MR Bryson, ST AF Hermes, J. J. Charpinet, S. Barclay, Thomas Pakstiene, E. Mullally, Fergal Kawaler, Steven D. Bloemen, S. Castanheira, Barbara G. Winget, D. E. Montgomery, M. H. Van Grootel, V. Huber, Daniel Still, Martin Howell, Steve B. Caldwell, Douglas A. Haas, Michael R. Bryson, Stephen T. TI PRECISION ASTEROSEISMOLOGY OF THE PULSATING WHITE DWARF GD 1212 USING A TWO-WHEEL-CONTROLLED KEPLER SPACECRAFT SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: evolution; stars: individual (GD 1212); stars: oscillations (including pulsations); stars: variables: general; white dwarfs ID WHOLE EARTH TELESCOPE; ZZ-CETI STARS; GRAVITY MODES; LIGHT-CURVE; G29-38; PG-1159-035; INSTABILITY; DISCOVERY; G226-29; PERIOD AB We present a preliminary analysis of the cool pulsating white dwarf (WD) GD 1212, enabled by more than 11.5 days of space-based photometry obtained during an engineering test of the two-reaction-wheel-controlled Kepler spacecraft. We detect at least 19 independent pulsation modes, ranging from 828.2-1220.8 s, and at least 17 nonlinear combination frequencies of those independent pulsations. Our longest uninterrupted light curve, 9.0 days in length, evidences coherent difference frequencies at periods inaccessible from the ground, up to 14.5 hr, the longest-period signals ever detected in a pulsating WD. These results mark some of the first science to come from a two-wheel-controlled Kepler spacecraft, proving the capability for unprecedented discoveries afforded by extending Kepler observations to the ecliptic. C1 [Hermes, J. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Charpinet, S.] Univ Toulouse, UPS OMP, IRAP, F-75205 Toulouse, France. [Charpinet, S.] CNRS, IRAP, F-31400 Toulouse, France. [Barclay, Thomas; Mullally, Fergal; Huber, Daniel; Still, Martin; Howell, Steve B.; Caldwell, Douglas A.; Haas, Michael R.; Bryson, Stephen T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Barclay, Thomas; Still, Martin] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Pakstiene, E.] Vilnius State Univ, Inst Theoret Phys & Astron, LT-01108 Vilnius, Lithuania. [Mullally, Fergal; Huber, Daniel; Caldwell, Douglas A.] SETI Inst, Mountain View, CA 94043 USA. [Kawaler, Steven D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Bloemen, S.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Castanheira, Barbara G.; Winget, D. E.; Montgomery, M. H.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Castanheira, Barbara G.; Winget, D. E.; Montgomery, M. H.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Van Grootel, V.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Van Grootel, V.] FNRS, B-1000 Brussels, Belgium. RP Hermes, JJ (reprint author), Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. RI Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Charpinet, Stephane/0000-0002-6018-6180 FU European Research Council under the European Union [320964]; NSF [AST-0909107, AST-1312678]; Norman Hackerman Advanced Research Program [003658-0252-2009]; NASA [NNX12AC96G, NNX13AC23G, NNX14AB92G]; Foundation for Fundamental Research on Matter (FOM), Netherlands Organisation for Scientific Research (NWO) FX We acknowledge Working Group 11 of the Kepler Asteroseismic Science Consortium for the eager discussion and analysis that led to this rapid result. We thank the referee, S.O. Kepler, for helpful comments that improved aspects of the discussion. J.J.H. acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement No. 320964 (WDTracer). M.H.M. and D.E.W. gratefully acknowledge the support of the NSF under grants AST-0909107 and AST-1312678 and the Norman Hackerman Advanced Research Program under grant 003658-0252-2009. M.H.M. acknowledges the support of NASA under grant NNX12AC96G, and D.E.W. acknowledges the support of NASA under grant NNX13AC23G. S.B. is supported by the Foundation for Fundamental Research on Matter (FOM), which is part of the Netherlands Organisation for Scientific Research (NWO). D.H. acknowledges support by NASA under grant NNX14AB92G issued through the Kepler Participating Scientist Program. NR 40 TC 17 Z9 17 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 JUL 1 PY 2014 VL 789 IS 1 AR 85 DI 10.1088/0004-637X/789/1/85 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400085 ER PT J AU Kelly, PL Filippenko, AV Modjaz, M Kocevski, D AF Kelly, Patrick L. Filippenko, Alexei V. Modjaz, Maryam Kocevski, Daniel TI THE HOST GALAXIES OF FAST-EJECTA CORE-COLLAPSE SUPERNOVAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: abundances; galaxies: star formation; gamma-ray burst: general; supernovae: general ID GAMMA-RAY BURSTS; DIGITAL SKY SURVEY; STAR-FORMING GALAXIES; MASSIVE STARS; OBSERVATIONAL CONSTRAINTS; LUMINOSITY FUNCTIONS; SURFACE BRIGHTNESS; OPTICAL AFTERGLOW; LINE SPECTRA; DARK BURSTS AB Spectra of broad-lined Type Ic supernovae (SNe Ic-BL), the only kind of SN observed at the locations of long-duration gamma-ray bursts (LGRBs), exhibit wide features indicative of high ejecta velocities (similar to 0.1c). We study the host galaxies of a sample of 245 low-redshift (z < 0.2) core-collapse SNe, including 17 SNe Ic-BL, discovered by galaxy-untargeted searches, and 15 optically luminous and dust-obscured z < 1.2 LGRBs. We show that, in comparison with Sloan Digital Sky Survey galaxies having similar stellar masses, the hosts of low-redshift SNe Ic-BL and z < 1.2 LGRBs have high stellar mass and star formation rate densities. Core-collapse SNe having typical ejecta velocities, in contrast, show no preference for such galaxies. Moreover, we find that the hosts of SNe Ic-BL, unlike those of SNe Ib/Ic and SNe II, exhibit high gas velocity dispersions for their stellar masses. The patterns likely reflect variations among star-forming environments and suggest that LGRBs can be used as probes of conditions in high-redshift galaxies. They may be caused by efficient formation of massive binary progenitor systems in densely star-forming regions, or, less probably, a higher fraction of stars created with the initial masses required for an SN Ic-BL or LGRB. Finally, we show that the preference of SNe Ic-BL and LGRBs for galaxies with high stellar mass and star formation rate densities cannot be attributed to a preference for low metal abundances but must reflect the influence of a separate environmental factor. C1 [Kelly, Patrick L.; Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Modjaz, Maryam] NYU, CCPP, New York, NY 10003 USA. [Kocevski, Daniel] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kelly, PL (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. FU Christopher R. Redlich Fund; TABASGO Foundation; NSF [AST-1211916]; NASA/HST grant from the Space Telescope Science Institute [AR-12850]; NASA [NAS5-26555]; NASA/Spitzer RSA Agreement [1287913] FX We thank Sandra Savaglio who, as referee, provided insightful comments and suggestions. We additionally acknowledge useful discussions about measurements and host galaxies with Jarle Brinchmann, Ori Fox, David Elbaz, John Graham, Matt Lehnert, Steven Stahler, Paul Crowther, and Josh Bloom. A.V.F.'s group at UC Berkeley has received generous financial assistance from the Christopher R. Redlich Fund, the TABASGO Foundation, Weldon Wood, and NSF grant AST-1211916, as well as from NASA/HST grant AR-12850 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under NASA contract NAS5-26555. This research has made use of the GHostS database (www.grbhosts.org), which is partly funded by NASA/Spitzer RSA Agreement No. 1287913. NR 70 TC 20 Z9 20 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 JUL 1 PY 2014 VL 789 IS 1 AR 23 DI 10.1088/0004-637X/789/1/23 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400023 ER PT J AU Lehmer, BD Berkeley, M Zezas, A Alexander, DM Basu-Zych, A Bauer, FE Brandt, WN Fragos, T Hornschemeier, AE Kalogera, V Ptak, A Sivakoff, GR Tzanavaris, P Yukita, M AF Lehmer, B. D. Berkeley, M. Zezas, A. Alexander, D. M. Basu-Zych, A. Bauer, F. E. Brandt, W. N. Fragos, T. Hornschemeier, A. E. Kalogera, V. Ptak, A. Sivakoff, G. R. Tzanavaris, P. Yukita, M. TI THE X-RAY LUMINOSITY FUNCTIONS OF FIELD LOW-MASS X-RAY BINARIES IN EARLY-TYPE GALAXIES: EVIDENCE FOR A STELLAR AGE DEPENDENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: evolution; Galaxy: stellar content; globular clusters: general; X-rays: binaries; X-rays: galaxies ID GLOBULAR-CLUSTERS; ELLIPTIC GALAXIES; STAR-FORMATION; HOT GAS; SAURON PROJECT; DEEP CHANDRA; POPULATIONS; LMXBS; CATALOG; ENVIRONMENTS AB We present direct constraints on how the formation of low-mass X-ray binary (LMXB) populations in galactic fields depends on stellar age. In this pilot study, we utilize Chandra and Hubble Space Telescope (HST) data to detect and characterize the X-ray point source populations of three nearby early-type galaxies: NGC 3115, 3379, and 3384. The luminosity-weighted stellar ages of our sample span approximate to 3-10 Gyr. X-ray binary population synthesis models predict that the field LMXBs associated with younger stellar populations should be more numerous and luminous per unit stellar mass than older populations due to the evolution of LMXB donor star masses. Crucially, the combination of deep Chandra and HST observations allows us to test directly this prediction by identifying and removing counterparts to X-ray point sources that are unrelated to the field LMXB populations, including LMXBs that are formed dynamically in globular clusters, Galactic stars, and background active galactic nuclei/galaxies. We find that the "young" early-type galaxy NGC 3384 (approximate to 2-5 Gyr) has an excess of luminous field LMXBs (L-X greater than or similar to (5-10) x 10(37) erg s(-1)) per unit K-band luminosity (L-K; a proxy for stellar mass) than the "old" early-type galaxies NGC 3115 and 3379 (approximate to 8-10 Gyr), which results in a factor of approximate to 2-3 excess of L-X/L-K for NGC 3384. This result is consistent with the X-ray binary population synthesis model predictions; however, our small galaxy sample size does not allow us to draw definitive conclusions on the evolution field LMXBs in general. We discuss how future surveys of larger galaxy samples that combine deep Chandra and HST data could provide a powerful new benchmark for calibrating X-ray binary population synthesis models. C1 [Lehmer, B. D.; Tzanavaris, P.; Yukita, M.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Lehmer, B. D.; Berkeley, M.; Basu-Zych, A.; Hornschemeier, A. E.; Ptak, A.; Tzanavaris, P.; Yukita, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Berkeley, M.] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Zezas, A.; Sivakoff, G. R.] Univ Crete, Dept Phys, Iraklion, Greece. [Zezas, A.; Fragos, T.] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece. [Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Basu-Zych, A.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Bauer, F. E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Kalogera, V.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Sivakoff, G. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. RP Lehmer, BD (reprint author), Johns Hopkins Univ, Homewood Campus, Baltimore, MD 21218 USA. RI Sivakoff, Gregory/G-9602-2011; Brandt, William/N-2844-2015; Zezas, Andreas/C-7543-2011; Fragos, Tassos/A-3581-2016 OI Sivakoff, Gregory/0000-0001-6682-916X; Brandt, William/0000-0002-0167-2453; Zezas, Andreas/0000-0001-8952-676X; Fragos, Tassos/0000-0003-1474-1523 FU Chandra X-ray Center grant [G02-13107A]; Space Telescope Science Institute [GO-12760]; NASA ADP [NNX13AI48G, NNX12AL39G]; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT 1101024, Gemini-CONICYT 32120003, Anillo ACT1101]; Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo [IC120009]; ADP [NNX10AC99G]; NSERC FX We thank the referee for providing thoughtful comments that have improved the quality of this paper. We thank Zhongli Zhang for providing data. We gratefully acknowledge financial support from Chandra X-ray Center grant G02-13107A, Space Telescope Science Institute grant GO-12760, and NASA ADP grant NNX13AI48G (B.D.L.). F.E.B. acknowledges support from Basal-CATA PFB-06/2007, CONICYT-Chile (grants FONDECYT 1101024, 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. W.N.B. acknowledges ADP grant NNX10AC99G. G.R.S. is supported by an NSERC Discovery Grant. V.K. acknowledges support for this work from NASA ADP grant NNX12AL39G (sub-contract to Northwestern University) NR 63 TC 11 Z9 11 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2014 VL 789 IS 1 AR 52 DI 10.1088/0004-637X/789/1/52 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400052 ER PT J AU Lyra, W AF Lyra, Wladimir TI CONVECTIVE OVERSTABILITY IN ACCRETION DISKS: THREE-DIMENSIONAL LINEAR ANALYSIS AND NONLINEAR SATURATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; instabilities; methods: analytical; methods: numerical; planets and satellites: formation; protoplanetary disks ID SPIRAL DENSITY WAVES; BAROCLINIC VORTICITY PRODUCTION; WEAKLY MAGNETIZED DISKS; PROTOPLANETARY DISKS; TURBULENT FLUCTUATIONS; NUMERICAL SIMULATIONS; CIRCUMSTELLAR DISKS; SHEAR INSTABILITY; DEAD ZONE; VORTEX AB Recently, Klahr & Hubbard claimed that a hydrodynamical linear overstability exists in protoplanetary disks, powered by buoyancy in the presence of thermal relaxation. We analyze this claim, confirming it through rigorous compressible linear analysis. We model the system numerically, reproducing the linear growth rate for all cases studied. We also study the saturated properties of the overstability in the shearing box, finding that the saturated state produces finite amplitude fluctuations strong enough to trigger the subcritical baroclinic instability (SBI). Saturation leads to a fast burst of enstrophy in the box, and a large-scale vortex develops in the course of the next approximate to 100 orbits. The amount of angular momentum transport achieved is of the order of alpha approximate to 10(-3), as in compressible SBI models. For the first time, a self-sustained three-dimensional vortex is produced from linear amplitude perturbation of a quiescent base state. C1 [Lyra, Wladimir] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lyra, Wladimir] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Lyra, W (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM wlyra@caltech.edu FU National Aeronautics and Space Administration (NASA) through the Sagan Fellowship Program FX This work was performed in part at the Jet Propulsion Laboratory, under contract with the California Institute of Technology funded by the National Aeronautics and Space Administration (NASA) through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. This paper started from a discussion between the author, Alexander Hubbard, Matthew Kunz, Hubert Klahr, Henrik Latter, Geoffroy Lesur, Min-Kai Lin, George Mamatsashvili, and Orkan Umurhan. It further profited from input from Anders Johansen, Mordecai-Mark Mac Low, Colin McNally, Neal Turner, and Andrew Youdin. NR 28 TC 17 Z9 18 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 JUL 1 PY 2014 VL 789 IS 1 AR 77 DI 10.1088/0004-637X/789/1/77 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400077 ER PT J AU Mason, JP Woods, TN Caspi, A Thompson, BJ Hock, RA AF Mason, James Paul Woods, T. N. Caspi, A. Thompson, B. J. Hock, R. A. TI MECHANISMS AND OBSERVATIONS OF CORONAL DIMMING FOR THE 2010 AUGUST 7 EVENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; Sun: activity; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: UV radiation ID SOHO EIT OBSERVATIONS; MASS EJECTION ONSET; SOLAR-FLARE; YOHKOH SXT; CMES; PROMINENCES; WAVES AB Coronal dimming of extreme ultraviolet (EUV) emission has the potential to be a useful forecaster of coronal mass ejections (CMEs). As emitting material leaves the corona, a temporary void is left behind which can be observed in spectral images and irradiance measurements. The velocity and mass of the CMEs should impact the character of those observations. However, other physical processes can confuse the observations. We describe these processes and the expected observational signature, with special emphasis placed on the differences. We then apply this understanding to a coronal dimming event with an associated CME that occurred on 2010 August 7. Data from the Solar Dynamics Observatory's Atmospheric Imaging Assembly and EUV Variability Experiment (EVE) are used for observations of the dimming, while the Solar and Heliospheric Observatory's Large Angle and Spectrometric Coronagraph and the Solar Terrestrial Relations Observatory's COR1 and COR2 are used to obtain velocity and mass estimates for the associated CME. We develop a technique for mitigating temperature effects in coronal dimming from full-disk irradiance measurements taken by EVE. We find that for this event, nearly 100% of the dimming is due to mass loss in the corona. C1 [Mason, James Paul; Woods, T. N.; Caspi, A.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA. [Thompson, B. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hock, R. A.] US Air Force Res Lab, Space Vehicles Directorate, Kirtland AFB, NM USA. RP Mason, JP (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA. EM james.mason@lasp.colorado.edu RI Thompson, Barbara/C-9429-2012; OI Caspi, Amir/0000-0001-8702-8273 FU NASA SDO project, NASA [NAS5-02140] FX The authors would like to thank Angelos Vourlidas for providing computations of mass and true velocity for the event discussed in this paper. Additionally, the CDAW CME catalog is generated and maintained at the CDAW Data Center by NASA and The Catholic University of America in cooperation with the Naval Research Laboratory. SOHO is a project of international cooperation between ESA and NASA. This research is supported by the NASA SDO project, NASA grant NAS5-02140. NR 43 TC 7 Z9 7 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 JUL 1 PY 2014 VL 789 IS 1 AR 61 DI 10.1088/0004-637X/789/1/61 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400061 ER PT J AU Neill, JL Bergin, EA Lis, DC Schilke, P Crockett, NR Favre, C Emprechtinger, M Comito, C Qin, SL Anderson, DE Burkhardt, AM Chen, JH Harris, BJ Lord, SD McGuire, BA McNeill, TD Monje, RR Phillips, TG Steber, AL Vasyunina, T Yu, SS AF Neill, Justin L. Bergin, Edwin A. Lis, Dariusz C. Schilke, Peter Crockett, Nathan R. Favre, Cecile Emprechtinger, Martin Comito, Claudia Qin, Sheng-Li Anderson, Dana E. Burkhardt, Andrew M. Chen, Jo-Hsin Harris, Brent J. Lord, Steven D. McGuire, Brett A. McNeill, Trevor D. Monje, Raquel R. Phillips, Thomas G. Steber, Amanda L. Vasyunina, Tatiana Yu, Shanshan TI HERSCHEL OBSERVATIONS OF EXTRAORDINARY SOURCES: ANALYSIS OF THE FULL HERSCHEL/HIFI MOLECULAR LINE SURVEY OF SAGITTARIUS B2(N) SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: clouds; ISM: individual objects (Sagittarius B2(N)); ISM: molecules ID STAR-FORMING REGIONS; INTER-STELLAR CLOUDS; GAS-PHASE CHEMISTRY; SPIRAL ARM CLOUDS; GALACTIC-CENTER; CONTINUUM OBSERVATIONS; SPECTRAL-LINE; ORION-KL; SGR B2; INTERSTELLAR CLOUDS AB A sensitive broadband molecular line survey of the Sagittarius B2(N) star-forming region has been obtained with the Heterodyne Instrument for the Far-Infrared (HIFI) instrument on the Herschel Space Observatory, offering the first high spectral resolution look at this well-studied source in a wavelength region largely inaccessible from the ground (625-157 mu m). From the roughly 8000 spectral features in the survey, a total of 72 isotopologues arising from 44 different molecules have been identified, ranging from light hydrides to complex organics, and arising from a variety of environments from cold and diffuse to hot and dense gas. We present a local thermodynamic equilibrium (LTE) model to the spectral signatures of each molecule, constraining the source sizes for hot core species with complementary Submillimeter Array interferometric observations and assuming that molecules with related functional group composition are cospatial. For each molecule, a single model is given to fit all of the emission and absorption features of that species across the entire 480-1910 GHz spectral range, accounting for multiple temperature and velocity components when needed to describe the spectrum. As with other HIFI surveys toward massive star-forming regions, methanol is found to contribute more integrated line intensity to the spectrum than any other species. We discuss the molecular abundances derived for the hot core where the LTE approximation is generally found to describe the spectrum well, in comparison to abundances derived for the same molecules in the Orion KL region from a similar HIFI survey. Notably, we find significantly higher abundances of amine- and amide-bearing molecules (CH3NH2, CH2NH, and NH2CHO) toward Sgr B2(N) than Orion KL and lower abundances of some complex oxygen-bearing molecules (CH3OCHO in particular). In addition to information on the chemical composition of the hot core, the strong far-infrared dust continuum allows a number of molecules to be detected in absorption in the Sgr B2(N) envelope for the first time at high spectral resolution, and we discuss the possible physical origin of the kinematic components observed in absorption. Additionally, from the detection of new HOCO+ transitions in absorption compared to published HCO+ isotopic observations, we discuss constraints on the gas-phase CO2 abundance and compare this to observations of the ice composition in the Galactic center region, and to CO2 abundance estimates toward other high-mass star-forming regions. The reduced HIFI spectral scan and LTE model are made available to the public as a resource for future investigations of star-forming regions in the submillimeter and far-infrared. C1 [Neill, Justin L.; Bergin, Edwin A.; Crockett, Nathan R.; Favre, Cecile; Anderson, Dana E.; Burkhardt, Andrew M.; McNeill, Trevor D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Lis, Dariusz C.; Emprechtinger, Martin; Monje, Raquel R.; Phillips, Thomas G.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Schilke, Peter; Comito, Claudia; Qin, Sheng-Li] Univ Cologne, Inst Phys, D-50937 Cologne, Germany. [Chen, Jo-Hsin; Yu, Shanshan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Harris, Brent J.; Steber, Amanda L.; Vasyunina, Tatiana] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Lord, Steven D.] CALTECH, Natl Herschel Sci Ctr, Pasadena, CA 91125 USA. [McGuire, Brett A.] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. RP Neill, JL (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM jneill@umich.edu; ebergin@umich.edu RI Yu, Shanshan/D-8733-2016; OI McGuire, Brett/0000-0003-1254-4817; Steber, Amanda/0000-0002-8203-2174 FU NASA through JPL/Caltech FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada, and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France, and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland: NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; 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 Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 133 TC 21 Z9 21 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 JUL 1 PY 2014 VL 789 IS 1 AR 8 DI 10.1088/0004-637X/789/1/8 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400008 ER PT J AU Nynka, M Hailey, CJ Reynolds, SP An, HJ Baganoff, FK Boggs, SE Christensen, FE Craig, WW Gotthelf, EV Grefenstette, BW Harrison, FA Krivonos, R Madsen, KK Mori, K Perez, K Stern, D Wik, DR Zhang, WW Zoglauer, A AF Nynka, Melania Hailey, Charles J. Reynolds, Stephen P. An, Hongjun Baganoff, Frederick K. Boggs, Steven E. Christensen, Finn E. Craig, William W. Gotthelf, Eric V. Grefenstette, Brian W. Harrison, Fiona A. Krivonos, Roman Madsen, Kristin K. Mori, Kaya Perez, Kerstin Stern, Daniel Wik, Daniel R. Zhang, William W. Zoglauer, Andreas TI NuSTAR STUDY OF HARD X-RAY MORPHOLOGY AND SPECTROSCOPY OF PWN G21.5-0.9 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (G21.5-0.9); ISM: supernova remnants; radiation mechanisms: general; stars: neutron; X-rays: ISM ID SUPERNOVA REMNANT G21.5-0.9; PULSAR-WIND NEBULAE; XMM-NEWTON; CRAB-NEBULA; RELATIVISTIC ELECTRONS; INTERSTELLAR-MEDIUM; DUST SCATTERING; PSR J1833-1034; YOUNG PULSAR; HALO AB We present NuSTAR high-energy X-ray observations of the pulsar wind nebula (PWN)/supernova remnant G21.5-0.9. We detect integrated emission from the nebula up to similar to 40 keV, and resolve individual spatial features over a broad X-ray band for the first time. The morphology seen by NuSTAR agrees well with that seen by XMM-Newton and Chandra below 10 keV. At high energies, NuSTAR clearly detects non-thermal emission up to similar to 20 keV that extends along the eastern and northern rim of the supernova shell. The broadband images clearly demonstrate that X-ray emission from the North Spur and Eastern Limb results predominantly from non-thermal processes. We detect a break in the spatially integrated X-ray spectrum at similar to 9 keV that cannot be reproduced by current spectral energy distribution models, implying either a more complex electron injection spectrum or an additional process such as diffusion compared to what has been considered in previous work. We use spatially resolved maps to derive an energy-dependent cooling length scale, L(E) proportional to E-m with m = -0.21 +/- 0.01. We find this to be inconsistent with the model for the morphological evolution with energy described by Kennel & Coroniti. This value, along with the observed steepening in power-law index between radio and X-ray, can be quantitatively explained as an energy-loss spectral break in the simple scaling model of Reynolds, assuming particle advection dominates over diffusion. This interpretation requires a substantial departure from spherical magnetohydrodynamic, magnetic-flux-conserving outflow, most plausibly in the form of turbulent magnetic-field amplification. C1 [Nynka, Melania; Hailey, Charles J.; Gotthelf, Eric V.; Mori, Kaya; Perez, Kerstin] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Reynolds, Stephen P.] NC State Univ, Dept Phys, Raleigh, NC 27695 USA. [An, Hongjun] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Baganoff, Frederick K.] MIT, Ctr Space Res, Cambridge, MA 02139 USA. [Boggs, Steven E.; Craig, William W.; Krivonos, Roman; Zoglauer, Andreas] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Grefenstette, Brian W.; Harrison, Fiona A.; Madsen, Kristin K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wik, Daniel R.; Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Nynka, M (reprint author), Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA. RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; An, Hongjun/0000-0002-6389-9012; Madsen, Kristin/0000-0003-1252-4891 FU NASA [NNG08FD60C] FX This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTAR-DAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). NR 52 TC 10 Z9 10 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2014 VL 789 IS 1 AR 72 DI 10.1088/0004-637X/789/1/72 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400072 ER PT J AU Seifina, E Titarchuk, L Shaposhnikov, N AF Seifina, Elena Titarchuk, Lev Shaposhnikov, Nikolai TI BLACK HOLE MASS DETERMINATION IN THE X-RAY BINARY 4U 1630-47: SCALING OF SPECTRAL AND VARIABILITY CHARACTERISTICS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; radiation mechanisms: non-thermal; stars: individual (4U 1630-47) ID QUASI-PERIODIC OSCILLATIONS; MONTE-CARLO SIMULATIONS; ABSORPTION-LINE FEATURES; MICROQUASAR GRO J1655-40; CANDIDATE XTE J1550-564; 1998 OUTBURST; NEUTRON-STAR; GX 339-4; TRANSIENT 4U-1630-47; INTRINSIC SIGNATURE AB We present the results of a comprehensive investigation on the evolution of spectral and timing properties of the Galactic black hole candidate 4U 1630-47 during its spectral transitions. In particular, we show how a scaling of the correlation of the photon index of the Comptonized spectral component G with low-frequency quasi-periodic oscillations (QPOs), nu(L), and mass accretion rate, (M) over dot, can be applied to the black hole mass and the inclination angle estimates. We analyze the transition episodes observed with the Rossi X-Ray Timing Explorer and BeppoSAX satellites. We find that the broadband X-ray energy spectra of 4U 1630-47 during all spectral states can be modeled by a combination of a thermal component, a Comptonized component, and a red-skewed iron-line component. We also establish that Gamma monotonically increases during transition from the low-hard state to the high-soft state and then saturates for high mass accretion rates. The index saturation levels vary for different transition episodes. Correlations of Gamma versus nu(L) also show saturation at Gamma similar to 3. Gamma-(M) over dot and Gamma-nu(L) correlations with their index saturation revealed in 4U 1630-47 are similar to those established in a number of other black hole candidates and can be considered as an observational evidence for the presence of a black hole in these sources. The scaling technique, which relies on XTE J1550-564, GRO 1655-40, and H1743-322 as reference sources, allows us to evaluate a black hole mass in 4U 1630-47 yielding M-BH similar to 10 +/- 0.1 solar masses and to constrain the inclination angle of i less than or similar to 70 degrees. C1 [Seifina, Elena] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. [Titarchuk, Lev] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy. [Titarchuk, Lev] George Mason Univ, Fairfax, VA 22030 USA. [Titarchuk, Lev; Shaposhnikov, Nikolai] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Shaposhnikov, Nikolai] Univ Maryland, Dept Astron, CRESST, College Pk, MD 20742 USA. RP Seifina, E (reprint author), Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Prospect 13, Moscow 119992, Russia. EM seif@sai.msu.ru; titarchuk@fe.infn.it; lev@milkyway.gsfc.nasa.gov NR 103 TC 7 Z9 7 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2014 VL 789 IS 1 AR 57 DI 10.1088/0004-637X/789/1/57 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400057 ER PT J AU Stark, CC Schneider, G Weinberger, AJ Debes, JH Grady, CA Jang-Condell, H Kuchner, MJ AF Stark, Christopher C. Schneider, Glenn Weinberger, Alycia J. Debes, John H. Grady, Carol A. Jang-Condell, Hannah Kuchner, Marc J. TI REVEALING ASYMMETRIES IN THE HD181327 DEBRIS DISK: A RECENT MASSIVE COLLISION OR INTERSTELLAR MEDIUM WARPING SO ASTROPHYSICAL JOURNAL LA English DT Article DE telescopes; methods: numerical; planetary systems ID MAIN-SEQUENCE STARS; ICY KUIPER-BELT; BETA-PICTORIS; CIRCUMSTELLAR DISK; PLANETARY SYSTEM; AU MICROSCOPII; FOMALHAUT B; HD 181327; HR 4796A; DUST AB New multi-roll coronagraphic images of the HD181327 debris disk obtained using the Space Telescope Imaging Spectrograph on board the Hubble Space Telescope reveal the debris ring in its entirety at high signal-to-noise ratio and unprecedented spatial resolution. We present and apply a new multi-roll image processing routine to identify and further remove quasi-static point-spread function-subtraction residuals and quantify systematic uncertainties. We also use a new iterative image deprojection technique to constrain the true disk geometry and aggressively remove any surface brightness asymmetries that can be explained without invoking dust density enhancements/deficits. The measured empirical scattering phase function for the disk is more forward scattering than previously thought and is not well-fit by a Henyey-Greenstein function. The empirical scattering phase function varies with stellocentric distance, consistent with the expected radiation pressured-induced size segregation exterior to the belt. Within the belt, the empirical scattering phase function contradicts unperturbed debris ring models, suggesting the presence of an unseen planet. The radial profile of the flux density is degenerate with a radially varying scattering phase function; therefore estimates of the ring's true width and edge slope may be highly uncertain. We detect large scale asymmetries in the disk, consistent with either the recent catastrophic disruption of a body with mass >1% the mass of Pluto, or disk warping due to strong interactions with the interstellar medium. C1 [Stark, Christopher C.; Kuchner, Marc J.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Schneider, Glenn] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Weinberger, Alycia J.] Carnegie Inst Washington Observ, Dept Terr Magnetism, Washington, DC 20015 USA. [Debes, John H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Grady, Carol A.] Eureka Sci, Oakland, CA 96002 USA. [Jang-Condell, Hannah] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. RP Stark, CC (reprint author), NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA. EM christopher.c.stark@nasa.gov OI Jang-Condell, Hannah/0000-0002-7639-1322 FU NASA through Space Telescope Science Institute [12228]; NASA/ESA Hubble Space Telescope [12228]; NASA [NAS 5-26555, NNA09DA81A] FX Based on observations made with the NASA/ESA Hubble Space Telescope, from program #12228. Support for program #12228 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. C.C.S. acknowledges the support of a Carnegie Fellowship and an appointment to the NASA Postdoctoral Program at NASA Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. This work was also supported by NASA Astrobiology Institute grant NNA09DA81A. NR 45 TC 22 Z9 22 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 JUL 1 PY 2014 VL 789 IS 1 AR 58 DI 10.1088/0004-637X/789/1/58 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400058 ER PT J AU Vogel, JK Hascoet, R Kaspi, VM An, HJ Archibald, R Beloborodov, AM Boggs, SE Christensen, FE Craig, WW Gotthelf, EV Grefenstette, BW Hailey, CJ Harrison, FA Kennea, JA Madsen, KK Pivovaroff, MJ Stern, D Zhang, WW AF Vogel, Julia K. Hascoet, Romain Kaspi, Victoria M. An, Hongjun Archibald, Robert Beloborodov, Andrei M. Boggs, Steven E. Christensen, Finn E. Craig, William W. Gotthelf, Eric V. Grefenstette, Brian W. Hailey, Charles J. Harrison, Fiona A. Kennea, Jamie A. Madsen, Kristin K. Pivovaroff, Michael J. Stern, Daniel Zhang, William W. TI NuSTAR OBSERVATIONS OF THE MAGNETAR 1E 2259+586 SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: individual (1E 2259+586); stars: magnetars; stars: neutron; X-rays: bursts ID X-RAY PULSAR; SOFT GAMMA REPEATERS; NEUTRON-STARS; 2002 OUTBURST; 4U 0142+61; EMISSION; SPECTRA; RXTE; ABSORPTION; G109.1-1.0 AB We report on new broad band spectral and temporal observations of the magnetar 1E 2259+586, which is located in the supernova remnant CTB 109. Our data were obtained simultaneously with the Nuclear Spectroscopic Telescope Array (NuSTAR) and Swift, and cover the energy range from 0.5-79 keV. We present pulse profiles in various energy bands and compare them to previous RXTE results. The NuSTAR data show pulsations above 20 keV for the first time and we report evidence that one of the pulses in the double-peaked pulse profile shifts position with energy. The pulsed fraction of the magnetar is shown to increase strongly with energy. Our spectral analysis reveals that the soft X-ray spectrum is well characterized by an absorbed double blackbody or blackbody plus power-law model in agreement with previous reports. Our new hard X-ray data, however, suggest that an additional component, such as a power law, is needed to describe the NuSTAR and Swift spectrum. We also fit the data with the recently developed coronal outflow model by Beloborodov for hard X-ray emission from magnetars. The outflow from a ring on the magnetar surface is statistically preferred over outflow from a polar cap. C1 [Vogel, Julia K.; Craig, William W.; Pivovaroff, Michael J.] Lawrence Livermore Natl Lab, Div Phys, Phys & Life Sci Directorate, Livermore, CA 94550 USA. [Hascoet, Romain; Beloborodov, Andrei M.; Gotthelf, Eric V.; Hailey, Charles J.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Hascoet, Romain; Beloborodov, Andrei M.; Gotthelf, Eric V.; Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Kaspi, Victoria M.; An, Hongjun; Archibald, Robert] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Grefenstette, Brian W.; Harrison, Fiona A.; Madsen, Kristin K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Kennea, Jamie A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Vogel, JK (reprint author), Lawrence Livermore Natl Lab, Div Phys, Phys & Life Sci Directorate, Livermore, CA 94550 USA. RI Pivovaroff, Michael/M-7998-2014; Boggs, Steven/E-4170-2015; OI Pivovaroff, Michael/0000-0001-6780-6816; Boggs, Steven/0000-0001-9567-4224; An, Hongjun/0000-0002-6389-9012; Madsen, Kristin/0000-0003-1252-4891 FU U.S. Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; LDRD program [13-ERD-033]; NASA [NNG08FD60C]; National Aeronautics and Space Administration; NSERC; Centre de Recherche en Astrophysique du Quebec; Canadian Institute for Advanced Study; Canada Research Chairs Program; Lorne Trottier Chair in Astrophysics and Cosmology; NASA ATP [NNX 13AI34G] FX Part of this work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344 with support from the LDRD program through grant 13-ERD-033. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). V. M. K. receives support from an NSERC Discovery Grant and Accelerator Supplement, from the Centre de Recherche en Astrophysique du Quebec, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Study, the Canada Research Chairs Program, and the Lorne Trottier Chair in Astrophysics and Cosmology. A. M. B. is supported by the NASA ATP grant NNX 13AI34G. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. We also thank Dr. A. M. Archibald for helpful discussions. NR 38 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 JUL 1 PY 2014 VL 789 IS 1 AR 75 DI 10.1088/0004-637X/789/1/75 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400075 ER PT J AU Zoghbi, A Cackett, EM Reynolds, C Kara, E Harrison, FA Fabian, AC Lohfink, A Matt, G Balokovic, M Boggs, SE Christensen, FE Craig, W Hailey, CJ Stern, D Zhang, WW AF Zoghbi, A. Cackett, E. M. Reynolds, C. Kara, E. Harrison, F. A. Fabian, A. C. Lohfink, A. Matt, G. Balokovic, M. Boggs, S. E. Christensen, F. E. Craig, W. Hailey, C. J. Stern, D. Zhang, W. W. TI OBSERVATIONS OF MCG-5-23-16 WITH SUZAKU, XMM-NEWTON AND NUSTAR: DISK TOMOGRAPHY AND COMPTON HUMP REVERBERATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; X-rays: galaxies; X-rays: individual (MCG-5-23-16) ID X-RAY REVERBERATION; ACTIVE GALACTIC NUCLEI; HOLE ACCRETION DISKS; BLACK-HOLE; IRON K; TIME-LAGS; SPECTRAL VARIABILITY; TIMING PROPERTIES; IRAS 13224-3809; CYGNUS X-1 AB MCG-5-23-16 is one of the first active galactic nuclei (AGNs) where relativistic reverberation in the iron K line originating in the vicinity of the supermassive black hole was found, based on a short XMM-Newton observation. In this work, we present the results from long X-ray observations using Suzaku, XMM-Newton, and NuSTAR designed to map the emission region using X-ray reverberation. A relativistic iron line is detected in the lag spectra on three different timescales, allowing the emission from different regions around the black hole to be separated. Using NuSTAR coverage of energies above 10 keV reveals a lag between these energies and the primary continuum, which is detected for the first time in an AGN. This lag is a result of the Compton reflection hump responding to changes in the primary source in a manner similar to the response of the relativistic iron K line. C1 [Zoghbi, A.; Reynolds, C.; Lohfink, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Zoghbi, A.; Reynolds, C.] Joint Space Sci Inst JSI, College Pk, MD 20742 USA. [Cackett, E. M.] Wayne State Univ, Dept Phys & Astron, Detroit, MI 48201 USA. [Kara, E.; Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Harrison, F. A.; Balokovic, M.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Matt, G.] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Boggs, S. E.; Craig, W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Zoghbi, A (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM azoghbi@astro.umd.edu RI Boggs, Steven/E-4170-2015; XRAY, SUZAKU/A-1808-2009; Zoghbi, Abderahmen/A-8445-2017 OI Boggs, Steven/0000-0001-9567-4224; Zoghbi, Abderahmen/0000-0002-0572-9613 FU NASA [NNX14AF89G]; National Aeronautics and Space Administration; ESA Member States FX This work has been partly supported by NASA grant NNX14AF89G. The research in this article has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). We 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. Part of this work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. NR 50 TC 22 Z9 22 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2014 VL 789 IS 1 AR 56 DI 10.1088/0004-637X/789/1/56 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK0LD UT WOS:000338103400056 ER PT J AU Itterly, KF Taylor, PC AF Itterly, Kyle F. Taylor, Patrick C. TI Evaluation of the Tropical TOA Flux Diurnal Cycle in MERRA and ERA-Interim Retrospective Analyses SO JOURNAL OF CLIMATE LA English DT Article ID OUTGOING LONGWAVE RADIATION; ENERGY BUDGET; CLOUD; PRECIPITATION; VARIABILITY; CONVECTION; SATELLITE; MODEL; CERES; TEMPERATURE AB Reanalysis model output is extensively used in atmospheric research and must be rigorously and continuously evaluated to understand the strengths and weaknesses. This paper evaluates the tropical top-of-atmosphere (TOA) flux diurnal cycle in NASA's Modern-Era Retrospective Analysis for Research and Applications (MERRA) and the ECMWF Interim Re-Analysis (ERA-Interim) against Clouds and the Earth's Radiant Energy System (CERES) synoptic edition 3A (SYN Ed3A) TOA flux data. MERRA and ERA-Interim are able to reproduce large-scale features of the diurnal cycle, including land-ocean contrast. MERRA and ERA-Interim, however, fail to reproduce many regional features of the climatological annual diurnal cycle. The TOA flux diurnal cycle errors in regions dominated by convective diurnal cycles are 5-10 times larger than in nonconvective regions. These errors in the TOA radiative flux diurnal cycle are primarily attributed to errors in the cloud diurnal evolution and specifically the failure to reproduce diurnally forced propagating convection. The largest diurnal cycle errors are found in ocean convective regions (e.g., Indian and equatorial Pacific Oceans); the observed longwave cloud forcing (LWCF) diurnal evolution in several oceanic convective regions shows two peaks: an afternoon and a near midnight peak; however, the reanalysis models produce a single midnight peak. The outgoing longwave radiation (OLR) diurnal cycle over tropical land is 20%-30% too weak in both reanalyses. The small diurnal cycle errors in marine stratocumulus regions are a result of two common misrepresentations in MERRA and ERA-Interim: 1) the dissipation of marine stratocumulus clouds from morning to afternoon is too slow and 2) the cloud diurnal cycle is too weak. Overall, the intermodel differences in the representation of the TOA flux diurnal cycle are smaller than the differences between reanalysis models and observations. C1 NASA, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA. SSAI, Hampton, VA USA. RP Taylor, PC (reprint author), NASA, Langley Res Ctr, 21 Langley Blvd,Mail Stop 420, Hampton, VA 23681 USA. EM patrick.c.taylor@nasa.gov RI Taylor, Patrick/D-8696-2015 OI Taylor, Patrick/0000-0002-8098-8447 FU The NASA Energy and Water Cycle Studies (NEWS) Program [NNH10ZDA001N-NEWS] FX The authors thank two anonymous reviewers for insightful comments on this manuscript. This work was supported by The NASA Energy and Water Cycle Studies (NEWS) Program (NNH10ZDA001N-NEWS). CERES data were obtained from the NASA Langley Research Center Atmospheric Sciences Data Center. ERA-Interim data used in this study have been obtained from the ECMWF Data Server (http://data-portal.ecmwf.int/data/d/interim_mnth/). MERRA data used in this study have been provided by the Global Modeling and Assimilation Office (GMAO) at NASA Goddard Space Flight Center through the NASA GES DISC online archive (ftp://goldsmr2.sci.gsfc.nasa.gov/data/). NR 38 TC 5 Z9 5 U1 0 U2 15 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 JUL 1 PY 2014 VL 27 IS 13 BP 4781 EP 4796 DI 10.1175/JCLI-D-13-00737.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ8WG UT WOS:000337988200001 ER PT J AU Cullather, RI Nowicki, SMJ Zhao, B Suarez, MJ AF Cullather, Richard I. Nowicki, Sophie M. J. Zhao, Bin Suarez, Max J. TI Evaluation of the Surface Representation of the Greenland Ice Sheet in a General Circulation Model SO JOURNAL OF CLIMATE LA English DT Article ID REGIONAL CLIMATE MODEL; MASS-BALANCE MODEL; ENERGY-BALANCE; SNOW PARAMETERIZATION; SPATIAL-RESOLUTION; ATMOSPHERIC MODEL; DATA ASSIMILATION; SEA-LEVEL; GCM; ACCUMULATION AB Simulated surface conditions of the Goddard Earth Observing System model, version 5 (GEOS-5), atmospheric general circulation model (AGCM) are examined for the contemporary Greenland Ice Sheet (GrIS). A surface parameterization that explicitly models surface processes including snow compaction, meltwater percolation and refreezing, and surface albedo is found to remedy an erroneous deficit in the annual net surface energy flux and provide an adequate representation of surface mass balance (SMB) in an evaluation using simulations at two spatial resolutions. The simulated 1980-2008 GrIS SMB average is 24.7 +/- 4.5 cm yr(-1) water-equivalent (w.e.) at 1/2 degrees model grid spacing, and 18.2 +/- 3.3 cm yr(-1) w.e. for 2 degrees grid spacing. The spatial variability and seasonal cycle of the 1/2 degrees simulation compare favorably to recent studies using regional climate models, while results from 2 degrees integrations reproduce the primary features of the SMB field. In comparison to historical glaciological observations, the coarser-resolution model overestimates accumulation in the southern areas of the GrIS, while the overall SMB is underestimated. These changes relate to the sensitivity of accumulation and melt to the resolution of topography. The GEOS-5 SMB fields contrast with available corresponding atmospheric models simulations from phase 5 of the Coupled Model Intercomparison Project (CMIP5). It is found that only a few of the CMIP5 AGCMs examined provide significant summertime runoff, a dominant feature of the GrIS seasonal cycle. This is a condition that will need to be remedied if potential contributions to future eustatic change from polar ice sheets are to be examined with GCMs. C1 [Cullather, Richard I.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Nowicki, Sophie M. J.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. [Zhao, Bin] Sci Applicat Int Corp, Greenbelt, MD USA. [Suarez, Max J.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Cullather, RI (reprint author), NASA, Goddard Space Flight Ctr, Code 610-1,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM richard.cullather@nasa.gov FU NASA Modeling Analysis and Prediction Program (MAP) FX GC-Net AWS data were obtained from the Cooperative Institute for Research in Environmental Sciences at the University of Colorado at Boulder. DMI AWS data were obtained from the Danish Meteorological Institute. ERA-I fields were obtained from the online ordering system of the European Centre for Medium-Range Weather Forecasts. CMIP5 model output was obtained from the Program for Climate Model Diagnosis and Intercomparison (PCMDI). RACMO2 fields were obtained from the Sea-level Response to Ice Sheet Evolution project (SeaRISE). The authors thank D.K. Hall for access to and assistance in using the MODIS surface temperature dataset. The authors thank C.A. Shuman for constructive suggestions for the revision of the manuscript. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Center for Climate Simulation (NCCS) at Goddard Space Flight Center. This study was funded by a grant from the NASA Modeling Analysis and Prediction Program (MAP) to the second author. NR 85 TC 13 Z9 13 U1 0 U2 14 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD JUL 1 PY 2014 VL 27 IS 13 BP 4835 EP 4856 DI 10.1175/JCLI-D-13-00635.1 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ8WG UT WOS:000337988200004 ER PT J AU Wang, HL Schubert, S AF Wang, Hailan Schubert, Siegfried TI The Precipitation Response over the Continental United States to Cold Tropical Pacific Sea Surface Temperatures SO JOURNAL OF CLIMATE LA English DT Article ID ATMOSPHERIC MOISTURE TRANSPORT; REANALYSIS PROJECT; STATIONARY WAVES; NORTH-AMERICA; BOREAL SUMMER; VARIABILITY; DROUGHT; TELECONNECTIONS; NCEP/NCAR; MODELS AB The dominant pattern of SST variability in the Pacific during its cold phase produces pronounced precipitation deficits over the continental United States throughout the annual cycle. This study investigates the observed physical and dynamical processes through which the cold Pacific pattern affects U.S. precipitation, particularly the causes for the peak dry impacts in fall, as well as the nature of the differences between the summer and fall responses. Results show that the peak precipitation deficit over the United States during fall is primarily due to reduced atmospheric moisture transport from the Gulf of Mexico into the central and eastern United States and secondarily a reduction in local evaporation from land atmosphere feedback. The former is associated with a strong and systematic low-level northeasterly flow anomaly over the southeastern United States that counteracts the northwest branch of the climatological North Atlantic subtropical high. The above northeasterly anomaly is maintained by both diabatic heating anomalies in the nearby intra-American seas and diabatic cooling anomalies in the tropical Pacific. In contrast, the modest summertime precipitation deficit over the central United States is mainly an intensification of the local dry anomaly in the preceding spring from local land atmosphere feedback; the rather weak and disorganized atmospheric circulation anomalies over and to the south of the United States make little contribution. An evaluation of the NASA Seasonal-to-Interannual Prediction Project (NSIPP-1) AGCM simulations shows it lobe deficient in simulating the warm season tropical convection responses over the intra-American seas to the cold Pacific pattern and thereby the precipitation responses over the United States, a problem that appears to be common to many AGCMs. C1 [Wang, Hailan; Schubert, Siegfried] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Wang, HL (reprint author), Sci Syst & Applicat Inc, 1 Enterprise Pkwy,Suite 200, Hampton, VA 23666 USA. EM hailan.wang@nasa.gov FU NASA Modeling, Analysis and Prediction (MAP) program FX This study is supported by the NASA Modeling, Analysis and Prediction (MAP) program. We thank three anonymous reviewers whose comments and suggestions have significantly improved this paper. NR 33 TC 6 Z9 6 U1 1 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 JUL 1 PY 2014 VL 27 IS 13 BP 5036 EP 5055 DI 10.1175/JCLI-D-13-00453.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ8WG UT WOS:000337988200016 ER PT J AU Eriksson, D MacMillan, DS AF Eriksson, David MacMillan, D. S. TI Continental hydrology loading observed by VLBI measurements SO JOURNAL OF GEODESY LA English DT Article DE Hydrology; Loading; VLBI; GLDAS; GRACE ID BASE-LINE INTERFEROMETRY; SYSTEM; WATER; MODEL AB Variations in continental water storage lead to loading deformation of the crust with typical peak-to-peak variations at very long baseline interferometry (VLBI) sites of 3-15 mm in the vertical component and 1-2 mm in the horizontal component. The hydrology signal at VLBI sites has annual and semi-annual components and clear interannual variations. We have calculated the hydrology loading series using mass loading distributions derived from the global land data assimilation system (GLDAS) hydrology model and alternatively from a global grid of equal-area gravity recovery and climate experiment (GRACE) mascons. In the analysis of the two weekly VLBI 24-h R1 and R4 network sessions from 2003 to 2010 the baseline length repeatabilities are reduced in 79 % (80 %) of baselines when GLDAS (GRACE) loading corrections are applied. Site vertical coordinate repeatabilities are reduced in about 80 % of the sites when either GLDAS or GRACE loading is used. In the horizontal components, reduction occurs in 70-80 % of the sites. Estimates of the annual site vertical amplitudes were reduced for 16 out of 18 sites if either loading series was applied. We estimated loading admittance factors for each site and found that the average admittances were 1.01 0.05 for GRACE and 1.39 0.07 for GLDAS. The standard deviations of the GRACE admittances and GLDAS admittances were 0.31 and 0.68, respectively. For sites that have been observed in a set of sufficiently temporally dense daily sessions, the average correlation between VLBI vertical monthly averaged series and GLDAS or GRACE loading series was 0.47 and 0.43, respectively. C1 [Eriksson, David] Chalmers, S-41296 Gothenburg, Sweden. [MacMillan, D. S.] NVI Inc, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. RP MacMillan, DS (reprint author), NVI Inc, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. EM david.eriksson89@gmail.com; daniel.s.macmillan@nasa.gov OI Eriksson, David/0000-0002-3143-0922 NR 25 TC 4 Z9 4 U1 1 U2 8 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0949-7714 EI 1432-1394 J9 J GEODESY JI J. Geodesy PD JUL PY 2014 VL 88 IS 7 BP 675 EP 690 DI 10.1007/s00190-014-0713-0 PG 16 WC Geochemistry & Geophysics; Remote Sensing SC Geochemistry & Geophysics; Remote Sensing GA AJ9KE UT WOS:000338028000004 ER PT J AU Bloem, M Drew, M Lai, CF Bilimoria, KD AF Bloem, Michael Drew, Michael Lai, Chok Fung Bilimoria, Karl D. TI Advisory Algorithm for Scheduling Open Sectors, Operating Positions, and Workstations SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article AB Air traffic controller supervisors configure available sector, operating position, and workstation resources to safely and efficiently control air traffic in a region of airspace. In this paper, an algorithm for assisting supervisors with this task is described and demonstrated on two example problem instances. The algorithm produces configuration-schedule advisories that minimize a cost. The cost is a weighted sum of two competing costs: one penalizing mismatches between configurations and predicted air traffic and another penalizing the effort associated with changing configurations. The problem considered by the algorithm is a shortest-path problem. The parameter determining the relative importance of the two competing costs is tuned by comparing historical configurations with corresponding algorithm advisories. Furthermore, some operationally-meaningful metrics are computed with the results of simulations of the algorithm for various values of this parameter. Two example problem instances for which appropriate configuration advisories are obvious were designed to illustrate characteristics of the algorithm. The results demonstrate how the algorithm suggests advisories that appropriately use changes in airspace configurations and changes in the number of operating positions allocated to each open sector. The results also demonstrate how the advisories suggest appropriate times for configuration changes. C1 [Bloem, Michael] NASA, Ames Res Ctr, Syst Modeling & Optimizat Branch, Moffett Field, CA 94035 USA. [Drew, Michael; Lai, Chok Fung] Univ Calif Santa Cruz, Syst Modeling & Optimizat Branch, Moffett Field, CA 94035 USA. [Bilimoria, Karl D.] NASA, Ames Res Ctr, Flight Trajectory Dynam & Controls Branch, Moffett Field, CA 94035 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; michael.c.drew@nasa.gov; chok.f.lai@nasa.gov; karl.bilimoria@nasa.gov NR 24 TC 1 Z9 1 U1 0 U2 1 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD JUL-AUG PY 2014 VL 37 IS 4 BP 1158 EP 1169 DI 10.2514/1.62292 PG 12 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA AJ9GS UT WOS:000338016500010 ER PT J AU Campagnola, S Boutonnet, A Schoenmaekers, J Grebow, DJ Petropoulos, AE Russell, RP AF Campagnola, Stefano Boutonnet, Arnaud Schoenmaekers, Johannes Grebow, Daniel J. Petropoulos, Anastassios E. Russell, Ryan P. TI Tisserand-Leveraging Transfers SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article ID TRAJECTORY DESIGN; GRAVITY ASSISTS; 3-BODY PROBLEM; ORBITER; JUPITER; CAPTURE; MISSION; MERCURY; VENUS; GRAPH AB Tisserand-leveraging transfers (TILTs) are introduced as a new method for computing low-Delta v orbit transfers with the help of third-body perturbations. The TILTs can mitigate the costs and risk of planetary missions by reducing the orbit insertion maneuver requirements while maintaining short flight times. TILTs connect two flybys at the minor body with an impulsive maneuver at an apse. Using the circular, restricted three-body problem, TILTs extend the concept of v-infinity leveraging beyond the patched-conics domain. In this paper, a new method is presented to compute TILTs and to patch them together to design low-energy transfers. The presented solutions have transfer times similar to the high-energy solutions, yet the Delta v cost is significantly reduced. For this reason, TILTs are used in the reference endgame of ESA's new mission option to Ganymede, JUICE, which is also presented here. JUICE's low-energy endgame halves the cost of similar high-energy endgames, which makes TILTs a mission-enabling technology for JUICE. The "lunar resonances" of SMART-1 are also explained in terms of low-thrust TILTs, suggesting future application of TILTs and low-thrust TILTs to design missions to the Moon and to other small-body destinations. C1 [Campagnola, Stefano] Japan Aerosp Explorat Agcy, Dept Space Flight Syst, Sagamihara, Kanagawa 2525210, Japan. [Boutonnet, Arnaud; Schoenmaekers, Johannes] ESA, European Space Operat Ctr, Miss Anal Sect, D-64293 Darmstadt, Germany. [Grebow, Daniel J.; Petropoulos, Anastassios E.] CALTECH, Jet Prop Lab, Outer Planet Miss Anal Grp, Pasadena, CA 91109 USA. [Russell, Ryan P.] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA. RP Campagnola, S (reprint author), Japan Aerosp Explorat Agcy, Dept Space Flight Syst, Yoshinodai 3-1-1, Sagamihara, Kanagawa 2525210, Japan. EM stefano.campagnola@jaxa.jp; arnaud.boutonnet@esa.int; johannes.schoenmaekers@esa.int; daniel.grebow@jpl.nasa.gov; anastassios.e.petropoulos@jpl.nasa.gov; ryan.russell@austin.utexas.edu NR 42 TC 3 Z9 3 U1 2 U2 5 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD JUL-AUG PY 2014 VL 37 IS 4 BP 1202 EP 1210 DI 10.2514/1.62369 PG 9 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA AJ9GS UT WOS:000338016500014 ER PT J AU Yildiz, Y Agogino, A Brat, G AF Yildiz, Yildiray Agogino, Adrian Brat, Guillaume TI Predicting Pilot Behavior in Medium-Scale Scenarios Using Game Theory and Reinforcement Learning SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS LA English DT Article C1 [Yildiz, Yildiray; Agogino, Adrian] Univ Calif Santa Cruz, Univ Affiliated Res Ctr, NASA, Ames Res Ctr, Moffett Field, CA 95035 USA. [Brat, Guillaume] Carnegie Mellon Univ, NASA, Ames Res Ctr, Moffett Field, CA 95035 USA. RP Yildiz, Y (reprint author), Bilkent Univ, Dept Mech Engn, Room EA 104, TR-06800 Ankara, Turkey. NR 12 TC 2 Z9 2 U1 0 U2 5 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0731-5090 EI 1533-3884 J9 J GUID CONTROL DYNAM JI J. Guid. Control Dyn. PD JUL-AUG PY 2014 VL 37 IS 4 BP 1335 EP 1342 DI 10.2514/1.G000176 PG 8 WC Engineering, Aerospace; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA AJ9GS UT WOS:000338016500028 ER PT J AU Zeri, C Besiktepe, S Giannakourou, A Krasakopoulou, E Tzortziou, M Tsoliakos, D Pavlidou, A Mousdis, G Pitta, E Scoullos, M Papathanassiou, E AF Zeri, C. Besiktepe, S. Giannakourou, A. Krasakopoulou, E. Tzortziou, M. Tsoliakos, D. Pavlidou, A. Mousdis, G. Pitta, E. Scoullos, M. Papathanassiou, E. TI Chemical properties and fluorescence of DOM in relation to biodegradation in the interconnected Marmara-North Aegean Seas during August 2008 SO JOURNAL OF MARINE SYSTEMS LA English DT Article DE Dissolved organic carbon; Dissolved organic nitrogen; Bacterial Production; CDOM Fluorescence; PARAFAC modelling; Mediterranean Sea ID DISSOLVED ORGANIC-MATTER; EASTERN MEDITERRANEAN SEA; PARALLEL FACTOR-ANALYSIS; WESTERN BLACK-SEA; OPTICAL-PROPERTIES; CHESAPEAKE BAY; WET-OXIDATION; PACIFIC-OCEAN; WATER COLUMN; SARGASSO SEA AB The dynamics of dissolved organic matter (DOM) in the Marmara Sea-Dardanelles Straits-North Aegean Sea were investigated using measurements of dissolved organic carbon and nitrogen (DOC, DON), PARAFAC modeling of 3-D excitation-emission fluorescence spectra and bacterial production (BP) and respiration (BR) rates. In the surface brackish waters, chemical parameters showed an increase from the Aegean to the Marmara (DOC: 65-217 mu mol L-1; DON: 3.08-934 mu mol L-1; Dissolved Inorganic Nitrogen (DIN): 0.044-1.38), followed by an increase in BP rates (7.2-195 nmol L-1 d(-1)). In the subsurface waters, DIN also showed an increase in the Marmara basin (0.085-9.79 mu mol L-1) followed by an increase in BP rates (3.3-17.4 nmol L-1 d(-1)). PARAFAC modeling revealed three fluorescent components: lambda(ex)/lambda(em): <260(330)1464 nm, humic-like; lambda(ex)/lambda(em): <(260) 285/364 nm, quinone-like; lambda(ex)/lambda(em): 270/308 nm, tyrosine-like. DOC:DON ratios were found similar for the Marmara (21 +/- 3) and the N. Aegean Sea (19 +/- 2). The slopes Delta DOC:Delta DON suggested that in the Marmara Sea mineralization processes require more carbon relative to nitrogen (223), whereas in the N. Aegean there is preferential removal of nitrogen over carbon (5.66). The lack of significant correlation between DOC and AOU (apparent oxygen utilization) in the deep Marmara waters indicates that particulate organic matter is important in deep mineralization processes. (C) 2013 Elsevier B.V. All rights reserved. C1 [Zeri, C.; Giannakourou, A.; Krasakopoulou, E.; Tsoliakos, D.; Pavlidou, A.; Pitta, E.; Papathanassiou, E.] Hellen Ctr Marine Res, Inst Oceanog, Anavyssos 19013, Greece. [Besiktepe, S.] NATO Undersea Res Ctr, I-19126 La Spezia, Italy. [Tzortziou, M.] Univ Maryland, ESSIC, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mousdis, G.] Natl Hellen Res Fdn, Inst Theoret & Phys Chem, GR-11635 Athens, Greece. [Tsoliakos, D.; Pitta, E.; Scoullos, M.] Univ Athens, Dept Chem, Environm Chem Lab, Panepistimiopolis 15701, Zografou, Greece. RP Zeri, C (reprint author), Hellen Ctr Marine Res, Inst Oceanog, Anavyssos 19013, Greece. EM chris@hcmr.gr RI Besiktepe, Sukru/L-2272-2013; Pavlidou, Alexandra/B-3265-2017; Mousdis, George/G-5573-2011 OI Besiktepe, Sukru/0000-0002-9615-4746; Pavlidou, Alexandra/0000-0002-0031-4726; Mousdis, George/0000-0002-0560-4829 FU European IP [GOCE-036949] FX The present study was conducted within the framework of the European IP Project FP6-Sesame EC Contract No. GOCE-036949. The collection of data during the NRV Alliance cruise to the area was made possible by the TSS Protocol, including as Participants the NATO Undersea Research Centre (NURC), Turkish Navy Office of Navigation, Hydrography and Oceanography. V. Avgoustidi is thanked for her valuable assistance during sampling. NR 84 TC 7 Z9 8 U1 1 U2 27 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0924-7963 EI 1879-1573 J9 J MARINE SYST JI J. Mar. Syst. PD JUL PY 2014 VL 135 SI SI BP 124 EP 136 DI 10.1016/j.jmarsys.2013.11.019 PG 13 WC Geosciences, Multidisciplinary; Marine & Freshwater Biology; Oceanography SC Geology; Marine & Freshwater Biology; Oceanography GA AJ7GO UT WOS:000337865400011 ER PT J AU Ruzmaikin, A Aumann, HH Manning, EM AF Ruzmaikin, Alexander Aumann, Hartmut H. Manning, Evan M. TI Relative Humidity in the Troposphere with AIRS SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID SEA-SURFACE TEMPERATURE; WATER-VAPOR FEEDBACK; OUTGOING LONGWAVE RADIATION; TROPICAL DEEP CONVECTION; CLIMATE; ATMOSPHERE; CLOUD; SENSITIVITY; DEPENDENCE; OCEANS AB New global satellite data from the Atmospheric Infrared Sounder (AIRS) are applied to study the tropospheric relative humidity (RH) distribution and its influence on outgoing longwave radiation (OLR) for January and July in 2003, 2007, and 2011. RH has the largest maxima over 90% in the equatorial tropopause layer in January. Maxima in July do not arise above 60%. Seasonal variations of about 20% in zonally averaged RH are observed in the equatorial region of the low troposphere, in the equatorial tropopause layer, and in the polar regions. The seasonal variability in the recent decade has increased by about 5% relative to that in 1973-88, indicating a positive trend. The observed RH profiles indicate a moist bias in the tropical and subtropical regions typically produced by the general circulation models. The new data and method of evaluating the statistical significance of bimodality confirm bimodal probability distributions of RH at large tropospheric scales, notably in the ascending branch of the Hadley circulation. Bimodality is also seen at 500300 hPa in mid-and high latitudes. Since the drying time of the air is short compared with the mixing time of moist and dry air, the bimodality reflects the large-scale distribution of sources of moisture and the atmospheric circulation. Analysis of OLR dependence on surface temperature shows a 0.2 W m(-2) K-1 difference in sensitivities between clear-sky and all-sky OLR, indicating a positive longwave cloud radiative forcing. Diagrams of the clear-sky OLR as functions of percentiles of surface temperature and relative humidity in the tropics are designed to provide a new measure of the supergreenhouse effect. C1 [Ruzmaikin, Alexander; Aumann, Hartmut H.; Manning, Evan M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Ruzmaikin, A (reprint author), CALTECH, Jet Prop Lab, MS 169-506,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM alexander.ruzmaikin@jpl.nasa.gov FU Jet Propulsion Laboratory of the California Institute of Technology; National Aeronautics and Space Administration FX We thank Joan Feynman, Eric Fetzer, Brian Kahn, and Hui Su for expert advice. We are grateful to two reviewers for helpful critical comments. This work was supported in part by the Jet Propulsion Laboratory of the California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 38 TC 5 Z9 5 U1 1 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 JUL PY 2014 VL 71 IS 7 BP 2516 EP 2533 DI 10.1175/JAS-D-13-0363.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ7ZF UT WOS:000337920200014 ER PT J AU Tyler, RH Kuang, WJ AF Tyler, Robert H. Kuang, Weijia TI Resonant tidal excitation of internal waves in the Earth's fluid core SO PHYSICS OF THE EARTH AND PLANETARY INTERIORS LA English DT Article DE Earth's core; Tidal dissipation; Geodynamo; Geophysical fluid dynamics ID STRATIFIED LAYER; OCEAN AB It has long been speculated that there is a stably stratified layer below the core-mantle boundary, and two recent studies have improved the constraints on the parameters describing this stratification. Here we consider the dynamical implications of this layer using a simplified model. We first show that the stratification in this surface layer has sensitive control over the rate at which tidal energy is transferred to the core. We then show that when the stratification parameters from the recent studies are used in this model, a resonant configuration arrives whereby tidal forces perform elevated rates of work in exciting core flow. Specifically, the internal wave speed derived from the two independent studies (150 and 155 m/s) are in remarkable agreement with the speed (152 m/s) required for excitation of the primary normal mode of oscillation as calculated from full solutions of the Laplace Tidal Equations applied to a reduced-gravity idealized model representing the stratified layer. In evaluating this agreement it is noteworthy that the idealized model assumed may be regarded as the most reduced representation of the stratified dynamics of the layer, in that there are no non-essential dynamical terms in the governing equations assumed. While it is certainly possible that a more realistic treatment may require additional dynamical terms or coupling, it is also clear that this reduced representation includes no freedom for coercing the correlation described. This suggests that one must accept either (1) that tidal forces resonantly excite core flow and this is predicted by a simple model or (2) that either the independent estimates or the dynamical model does not accurately portray the core surface layer and there has simply been an unlikely coincidence between three estimates of a stratification parameter which would otherwise have a broad plausible range. (C) 2014 Elsevier B.V. All rights reserved. C1 [Tyler, Robert H.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Tyler, Robert H.; Kuang, Weijia] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. RP Tyler, RH (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Code 698, Greenbelt, MD 20771 USA. EM robert.h.tyler@nasa.gov RI Kuang, Weijia/K-5141-2012 OI Kuang, Weijia/0000-0001-7786-6425 FU NASA Earth Surface and Interiors Program; NASA Outer Planets Program FX The authors wish to thank Yves Rogister, Nick Schmerr, and two anonymous reviewers for their discussion and reviews of this manuscript. For support, both authors thank the NASA Earth Surface and Interiors Program, and RI thanks the NASA Outer Planets Program. NR 25 TC 0 Z9 0 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-9201 EI 1872-7395 J9 PHYS EARTH PLANET IN JI Phys. Earth Planet. Inter. PD JUL PY 2014 VL 232 BP 15 EP 25 DI 10.1016/j.pepi.2014.03.006 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AJ7EG UT WOS:000337859400002 ER PT J AU Balla, RJ Rhode, MN Everhart, JL AF Balla, R. Jeffrey Rhode, Matthew N. Everhart, Joel L. TI Supersaturation Total Temperature, Pitot Pressure, and Rayleigh Scattering Measurements at Mach 10 SO AIAA JOURNAL LA English DT Article ID HYPERSONIC WIND-TUNNEL; HOMOGENEOUS NUCLEATION; VIBRATIONAL-RELAXATION; NITROGEN; AIR; CONDENSATION; FLOW AB A fundamental research study of the supersaturation region is presented. This region is mapped in the NASA Langley 31-Inch Mach 10 Air Wind Tunnel freestream flow using physical probes (total temperature and pitot) and a nonintrusive offbody diagnostic (laser Rayleigh scattering). Data from all three methods are acquired simultaneously. Facility stagnation pressures spanned 1.0-10.0 MPa (150-1450 psi), and stagnation temperatures spanned 357-1000 K (184-1350 degrees F). Each instrument has its own unique supersaturation region over which quantitative measurements can be obtained. The extent of each supersaturation region is a unique function of the sensitivity of the instrument selected to flowfield clustering. Laser-Rayleigh-scattering-measured density results agree to better than 15% with the freestream density computed using the GASPROPS code over a significant fraction of the supersaturation region. Evidence is presented showing that the "frozen" vibrational nonequilibrium Boltzmann population of O-2 and N-2 molecules inhibit clustering and condensation. This is the physical mechanism responsible for creating the supersaturation region. In direct conflict with the assumption in all hypersonic literature from the past 50 years, evidence is presented indicating that no hypersonic or hypervelocity freestream in which nucleation is occurring contains a frozen vibrational nonequilibrium population. This population is effectively eliminated by interacting with clusters. C1 [Balla, R. Jeffrey] NASA, Langley Res Ctr, Adv Sensing & Opt Measurement Branch, Hampton, VA 23681 USA. [Rhode, Matthew N.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. [Everhart, Joel L.] NASA, Langley Res Ctr, Res Directorate MS 225, Hampton, VA 23681 USA. RP Balla, RJ (reprint author), Old Dominion Univ, Dept Phys, Norfolk, VA 23529 USA. EM Robert.j.balla@nasa.gov NR 28 TC 3 Z9 3 U1 2 U2 4 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 JUL PY 2014 VL 52 IS 7 BP 1452 EP 1465 DI 10.2514/1.J052608 PG 14 WC Engineering, Aerospace SC Engineering GA AJ5SK UT WOS:000337747800010 ER PT J AU Donald, BW Baars, WJ Tinney, CE Ruf, JH AF Donald, Brian W. Baars, Woutijn J. Tinney, Charles E. Ruf, Joseph H. TI Sound Produced by Large Area-Ratio Nozzles During Fixed and Transient Operations SO AIAA JOURNAL LA English DT Article ID SHOCK-ASSOCIATED NOISE; CONVERGENT-DIVERGENT NOZZLES; LAUNCH VEHICLE ACOUSTICS; SUPERSONIC JETS; ROCKET NOZZLES; TURBULENCE; UNSTEADINESS; SEPARATION; SCREECH; CONTOUR AB Analysis of the acoustic signature produced by truncated ideal contour and thrust-optimized parabolic nozzles is conducted during both fixed and transient (startup) operations. The truncated ideal contour nozzle experiences free-shock separation flow, whereas the thrust-optimized parabolic nozzle experiences both free-shock separation and restricted-shock separation flow states during startup. This study provides a direct comparison of the acoustic signature produced during free-shock separation and restricted-shock separation flow states while operating under identical nozzle pressure ratios. During a transient episode, the continuous wavelet transform is used to compare the acoustic signatures produced by the nozzles. The truncated ideal contour nozzle demonstrates a gradual increase in broadband frequency energy with increasing nozzle pressure ratio and with broadband shock noise appearing at higher nozzle pressure ratios. The thrust-optimized parabolic nozzle, however, displays a much larger sensitivity to the nozzle pressure ratio. In particular, the free-shock separation to restricted-shock separation transition, which occurs around nozzle pressure ratio 24.4, is weakly revealed in the acoustic signature along sideline angles to the nozzle. At nozzle pressure ratio 13, the acoustic signal observed at shallow angles to the nozzle decreases abruptly across a broad range of frequencies. The latter phenomenon is attributed to the formation of an open-ended subsonic core surrounded by a supersonic annular flow in the thrust-optimized parabolic nozzle during free-shock separation operations of the nozzle, which does not occur in the truncated ideal contour nozzle. C1 [Donald, Brian W.; Baars, Woutijn J.; Tinney, Charles E.] Univ Texas Austin, Austin, TX 78712 USA. [Ruf, Joseph H.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Donald, BW (reprint author), Univ Texas Austin, Austin, TX 78712 USA. RI Baars, Woutijn/F-6600-2016 OI Baars, Woutijn/0000-0003-1526-3084 FU Space Shuttle Main Engine Project, NASA Engineering and Safety Center; Space Shuttle Loads Panel and Air Force Office of Scientific Research FX Funding for this study was provided graciously by the Space Shuttle Main Engine Project, NASA Engineering and Safety Center, the Space Shuttle Loads Panel (Edward Burns as Technical Monitor) and Air Force Office of Scientific Research (John Schmissuer as Technical Monitor). The authors would like to acknowledge the Nozzle Test Facility team members at NASA Marshall Space Flight Center and the collaborators at NASA Johnson Space Center in their contribution to this effort. The authors also wish to acknowledge Alexis Avram and Lauren Cooper for their assistance with this effort. NR 46 TC 6 Z9 6 U1 1 U2 9 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD JUL PY 2014 VL 52 IS 7 BP 1474 EP 1485 DI 10.2514/1.J052588 PG 12 WC Engineering, Aerospace SC Engineering GA AJ5SK UT WOS:000337747800012 ER PT J AU Bassu, S Brisson, N Durand, JL Boote, K Lizaso, J Jones, JW Rosenzweig, C Ruane, AC Adam, M Baron, C Basso, B Biernath, C Boogaard, H Conijn, S Corbeels, M Deryng, D De Sanctis, G Gayler, S Grassini, P Hatfield, J Hoek, S Izaurralde, C Jongschaap, R Kemanian, AR Kersebaum, KC Kim, SH Kumar, NS Makowski, D Muller, C Nendel, C Priesack, E Pravia, MV Sau, F Shcherbak, I Tao, F Teixeira, E Timlin, D Waha, K AF Bassu, Simona Brisson, Nadine Durand, Jean-Louis Boote, Kenneth Lizaso, Jon Jones, James W. Rosenzweig, Cynthia Ruane, Alex C. Adam, Myriam Baron, Christian Basso, Bruno Biernath, Christian Boogaard, Hendrik Conijn, Sjaak Corbeels, Marc Deryng, Delphine De Sanctis, Giacomo Gayler, Sebastian Grassini, Patricio Hatfield, Jerry Hoek, Steven Izaurralde, Cesar Jongschaap, Raymond Kemanian, Armen R. Kersebaum, K. Christian Kim, Soo-Hyung Kumar, Naresh S. Makowski, David Mueller, Christoph Nendel, Claas Priesack, Eckart Pravia, Maria Virginia Sau, Federico Shcherbak, Iurii Tao, Fulu Teixeira, Edmar Timlin, Dennis Waha, Katharina TI How do various maize crop models vary in their responses to climate change factors? SO GLOBAL CHANGE BIOLOGY LA English DT Article DE [CO2]; AgMIP; climate; maize; model intercomparison; simulation; temperature; uncertainty ID WATER-USE EFFICIENCY; AIR CO2 ENRICHMENT; SIMULATION-MODEL; ELEVATED CO2; SYSTEMS SIMULATION; NITROGEN DYNAMICS; CARBON-DIOXIDE; YIELD; WHEAT; AGRICULTURE AB Potential consequences of climate change on crop production can be studied using mechanistic crop simulation models. While a broad variety of maize simulation models exist, it is not known whether different models diverge on grain yield responses to changes in climatic factors, or whether they agree in their general trends related to phenology, growth, and yield. With the goal of analyzing the sensitivity of simulated yields to changes in temperature and atmospheric carbon dioxide concentrations [CO2], we present the largest maize crop model intercomparison to date, including 23 different models. These models were evaluated for four locations representing a wide range of maize production conditions in the world: Lusignan (France), Ames (USA), Rio Verde (Brazil) and Morogoro (Tanzania). While individual models differed considerably in absolute yield simulation at the four sites, an ensemble of a minimum number of models was able to simulate absolute yields accurately at the four sites even with low data for calibration, thus suggesting that using an ensemble of models has merit. Temperature increase had strong negative influence on modeled yield response of roughly -0.5 Mg ha(-1) per degrees C. Doubling [CO2] from 360 to 720 mu mol mol(-1) increased grain yield by 7.5% on average across models and the sites. That would therefore make temperature the main factor altering maize yields at the end of this century. Furthermore, there was a large uncertainty in the yield response to [CO2] among models. Model responses to temperature and [CO2] did not differ whether models were simulated with low calibration information or, simulated with high level of calibration information. C1 [Bassu, Simona; Brisson, Nadine; Makowski, David] INRA AgroParisTech, Unite Agron, F-78850 Thiverval Grignon, France. [Durand, Jean-Louis] INRA, Unite Rech Pluridisciplinaire Prairie & Plantes F, F-86600 Lusignan, France. [Boote, Kenneth] Univ Florida, Dept Agron, Gainesville, FL 32611 USA. [Lizaso, Jon; Sau, Federico] Univ Politecn Madrid, Dept Prod Vegetal, E-28040 Madrid, Spain. [Jones, James W.] Univ Florida, Dept Agr & Biol Engn, Gainesville, FL 32611 USA. [Rosenzweig, Cynthia; Ruane, Alex C.] NASA, Goddard Inst Space Studies, Climate Impacts Grp, New York, NY 10025 USA. [Adam, Myriam] CIRAD, UMR AGAP PAM, Montpellier, France. [Baron, Christian] CIRAD, UMR TETIS, F-34093 Montpellier, France. [Basso, Bruno; Shcherbak, Iurii] Michigan State Univ, Dept Geol Sci, E Lansing, MI 48824 USA. [Basso, Bruno; Shcherbak, Iurii] Univ Basilicata, Dept Crop Syst Forestry & Environm Sci, I-85100 Potenza, Italy. [Biernath, Christian; Priesack, Eckart] Helmholtz Zentrum Munchen, Inst Bodenokol, D-85764 Neuherberg, Germany. [Boogaard, Hendrik; Hoek, Steven] Alterra, Ctr Geoinformat, NL-6700 AA Wageningen, Netherlands. [Conijn, Sjaak; Jongschaap, Raymond] Univ Wageningen & Res Ctr, WUR Plant Res Int, NL-6700 AA Wageningen, Netherlands. [Corbeels, Marc] CIRAD Annual Cropping Syst, BR-73310970 Planaltina, DF, Brazil. [Deryng, Delphine] Univ E Anglia, Tyndall Ctr Climate Change Res, Norwich NR4 7TJ, Norfolk, England. [Deryng, Delphine] Univ E Anglia, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England. [De Sanctis, Giacomo] INRA, Unite AGROCLIM, F-84914 Avignon 9, France. [Gayler, Sebastian] Univ Tubingen, Water & Earth Syst Sci WESS Competence Cluster, D-72074 Tubingen, Germany. [Grassini, Patricio] Univ Nebraska, Dept Agron & Hort, Lincoln, NE 68503 USA. [Hatfield, Jerry] USDA ARS, Natl Soil Tilth Lab Agr & Environm, Ames, IA 50011 USA. [Izaurralde, Cesar] Pacific NW Natl Lab, College Pk, MD 20740 USA. [Izaurralde, Cesar] Univ Maryland, College Pk, MD 20740 USA. [Kemanian, Armen R.; Pravia, Maria Virginia] Penn State Univ, Dept Plant Sci, University Pk, PA 16802 USA. [Kersebaum, K. Christian; Nendel, Claas] Leibniz Ctr Agr Landscape Res, ZALF, Inst Landscape Syst Anal, D-15374 Muencheberg, Germany. [Kim, Soo-Hyung] Univ Washington, Sch Environm & Forest Sci, Seattle, WA 98195 USA. [Kumar, Naresh S.; Waha, Katharina] Indian Agr Res Inst, Ctr Environm Sci & Climate Resilient Agr, New Delhi 110012, India. [Mueller, Christoph] Potsdam Inst Climate Impact Res, D-14412 Potsdam, Germany. [Tao, Fulu] Chinese Acad Sci, Inst Geog Sci & Nat Resources Res, Beijing 100101, Peoples R China. [Teixeira, Edmar] New Zealand Inst Plant & Food Res Ltd, Sustainable Prod, Canterbury, New Zealand. [Timlin, Dennis] USDA ARS, Crop Syst & Global Change Lab, Beltsville, MD 20705 USA. RP Durand, JL (reprint author), INRA, Unite Rech Pluridisciplinaire Prairie & Plantes F, BP 80006, F-86600 Lusignan, France. EM jean-louis.durand@lusignan.inra.fr RI Kim, Soo-Hyung/A-3012-2009; Priesack, Eckart/M-7341-2014; Deryng, Delphine/F-7417-2010; Nendel, Claas/C-8844-2013; Basso, Bruno/A-3128-2012; Teixeira, Edmar/K-1238-2016; Mueller, Christoph/E-4812-2016; De Sanctis, Giacomo/F-3498-2017; OI Priesack, Eckart/0000-0002-5088-9528; Kim, Soo-Hyung/0000-0003-3879-4080; Deryng, Delphine/0000-0001-6214-7241; Nendel, Claas/0000-0001-7608-9097; Basso, Bruno/0000-0003-2090-4616; Teixeira, Edmar/0000-0002-4835-0590; Mueller, Christoph/0000-0002-9491-3550; De Sanctis, Giacomo/0000-0002-3527-8091; Shcherbak@qut.edu.au, Iurii/0000-0003-4153-3770; Boote, Kenneth/0000-0002-1358-5496; Kersebaum, Kurt Christian/0000-0002-3679-8427 NR 72 TC 96 Z9 97 U1 16 U2 174 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 JUL PY 2014 VL 20 IS 7 BP 2301 EP 2320 DI 10.1111/gcb.12520 PG 20 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AJ4WU UT WOS:000337680700025 PM 24395589 ER PT J AU Smith, HD Baque, M Duncan, AG Lloyd, CR McKay, CP Billi, D AF Smith, Heather D. Baque, Mickael Duncan, Andrew G. Lloyd, Christopher R. McKay, Christopher P. Billi, Daniela TI Comparative analysis of cyanobacteria inhabiting rocks with different light transmittance in the Mojave Desert: a Mars terrestrial analogue SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY LA English DT Article DE astrobiology; Chroococcidiopsis; hypoliths; light transmission; Mars analogue; Mojave Desert; phototrophs ID ATACAMA DESERT; MICROBIAL COMMUNITY; UVC RADIATION; NAMIB DESERT; CHROOCOCCIDIOPSIS; PHOTOSYNTHESIS; LIFE; CHLOROPHYLL; ENDURANCE; BIOMEX AB The Mojave Desert has been long considered a suitable terrestrial analogue to Mars in many geological and astrobiological aspects. The Silver Lake region in the Mojave Desert hosts several different rock types (talc, marble, quartz, white carbonate and red-coated carbonate) colonized by hypoliths within a few kilometres. This provides an opportunity to investigate the effect of rock type on hypolithic colonization in a given environment. Transmission measurements from 300 to 800 nm showed that the transmission of blue and UVA varied between rock types. The wavelength at which the transmission fell to 1% of the transmission at 600 nm was 475 nm for white carbonate and quartz, 425 nm for red- coated carbonate and talc and 380 nm for marble. The comparative analysis of the cyanobacterial component of hypoliths under different rocks, as revealed by sequencing 16S rRNA gene clone libraries, showed no significant variation with rock type; hypoliths were dominated by phylotypes of the genus Chroococcidiopsis, although less abundant phylotypes of the genus Loriellopsis, Leptolyngbya and Scytonema occurred. The comparison of the confocal laser scanning microscopy-lambda (CLSM-lambda) scan analysis of the spectral emission of the photosynthetic pigments of Chroococcidiopsis in different rocks with the spectrum of isolated Chroococcidiopsis sp. 029, revealed a 10 nm red shift in the emission fingerprinting for quartz and carbonate and a 5 nm red shift for talc samples. This result reflects the versatility of Chroococcidiopsis in inhabiting dry niches with different light availability for photosynthesis. C1 [Smith, Heather D.] Utah State Univ, Biol Engn Dept, Logan, UT 84322 USA. [Smith, Heather D.; McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Baque, Mickael; Billi, Daniela] Univ Roma Tor Vergata, Dept Biol, I-00133 Rome, Italy. [Duncan, Andrew G.; Lloyd, Christopher R.] Micro Bio Syst Utah, Logan, UT 84341 USA. RP Smith, HD (reprint author), Utah State Univ, Biol Engn Dept, UMC 4105, Logan, UT 84322 USA. EM billi@uniroma2.it FU Italian Ministry of Foreign Affairs; Direzione Generale per la Promozione del Sistema Paese; NASA's Astrobiology Science and Technology for Exploring Planets (ASTEP); NASA Graduate Student Research Programme FX This research was funded by the Italian Ministry of Foreign Affairs, Direzione Generale per la Promozione del Sistema Paese and NASA's Astrobiology Science and Technology for Exploring Planets (ASTEP) and the NASA Graduate Student Research Programme. The authors thank Dr Elena Romano, Centre of Advanced Microscopy of 'Tor Vergata' University, for skilful assistance in using the facility. NR 32 TC 5 Z9 5 U1 7 U2 35 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1473-5504 EI 1475-3006 J9 INT J ASTROBIOL JI Int. J. Astrobiol. PD JUL PY 2014 VL 13 IS 3 BP 271 EP 277 DI 10.1017/S1473550414000056 PG 7 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AJ5WG UT WOS:000337760300007 ER PT J AU Whalley, MS Takahashi, MD Fletcher, JW Moralez, E Ott, CR Olmstead, MG Savage, JC Goerzen, CL Schulein, GJ Burns, HN Conrad, B AF Whalley, Matthew S. Takahashi, Marc D. Fletcher, Jay W. Moralez, Ernesto, III Ott, Carl R. Olmstead, Michael G. Savage, James C. Goerzen, Chad L. Schulein, Gregory J. Burns, Hoyt N. Conrad, Bill TI Autonomous Black Hawk in Flight: Obstacle Field Navigation and Landing-site Selection on the RASCAL JUH-60A SO JOURNAL OF FIELD ROBOTICS LA English DT Article AB This paper describes the development and flight test of autonomous obstacle field navigation and safe landing area selection on the U. S. Army Aeroflightdynamics Directorate RASCAL JUH-60A research helicopter. Using laser detection and ranging (LADAR) as the primary terrain sensor, the autonomous flight system is able to avoid obstacles, including wires, and select safe landing sites. An autonomous integrated landing zone approach profile was developed and validated that integrates cruise flight, low-level terrain flight, and approach to a safe landing spot determined on the fly. Results are presented for a range of sites and conditions. Approximately 750 km of autonomous flight was performed, 230 km of which was at low altitude in mountainous terrain using the obstacle field navigation system. This is the first time a full-scale helicopter has been flown fully autonomously a significant distance in low-level flight over complex terrain, basing its planning solely on sensor data gathered from an onboard sensor. These flights demonstrate tight integration between terrain avoidance, control, and autonomous landing. (C) 2014 Wiley Periodicals, Inc. C1 [Whalley, Matthew S.; Takahashi, Marc D.; Fletcher, Jay W.; Moralez, Ernesto, III; Ott, Carl R.; Olmstead, Michael G.] US Army, Aviat Dev Directorate AFDD Aviat & Missile Res De, Dev & Engn Command, Moffett Field, CA 94035 USA. [Savage, James C.] US Air Force, Res Lab, Weap Seeker Sci Branch AFRL RWWS, Eglin AFB, FL 32542 USA. [Goerzen, Chad L.; Schulein, Gregory J.] San Jose State Univ, Ames Res Ctr, Moffett Field, CA 94035 USA. [Burns, Hoyt N.; Conrad, Bill] HN Burns Engn Corp, Orlando, FL 32826 USA. RP Goerzen, CL (reprint author), San Jose State Univ, Ames Res Ctr, Moffett Field, CA 94035 USA. EM chad.l.goerzen.ctr@mail.mil NR 31 TC 3 Z9 3 U1 3 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1556-4959 EI 1556-4967 J9 J FIELD ROBOT JI J. Field Robot. PD JUL-AUG PY 2014 VL 31 IS 4 SI SI BP 591 EP 616 DI 10.1002/rob.21511 PG 26 WC Robotics SC Robotics GA AJ4WI UT WOS:000337679200007 ER PT J AU Achtelik, MW Lynen, S Weiss, S Chli, M Siegwart, R AF Achtelik, Markus W. Lynen, Simon Weiss, Stephan Chli, Margarita Siegwart, Roland TI Motion- and Uncertainty-aware Path Planning for Micro Aerial Vehicles SO JOURNAL OF FIELD ROBOTICS LA English DT Article ID CALIBRATION AB Localization and state estimation are reaching a certain maturity in mobile robotics, often providing both a precise robot pose estimate at a point in time and the corresponding uncertainty. In the bid to increase the robots' autonomy, the community now turns to more advanced tasks, such as navigation and path planning. For a realistic path to be computed, neither the uncertainty of the robot's perception nor the vehicle's dynamics can be ignored. In this work, we propose to specifically exploit the information on uncertainty, while also accounting for the physical laws governing the motion of the vehicle. Making use of rapidly exploring random belief trees, here we evaluate offline multiple path hypotheses in a known map to select a path exhibiting the motion required to estimate the robot's state accurately and, inherently, to avoid motion in modes, where otherwise observable states are not excited. We demonstrate the proposed approach on a micro aerial vehicle performing visual-inertial navigation. Such a system is known to require sufficient excitation to reach full observability. As a result, the proposed methodology plans safe avoidance not only of obstacles, but also areas where localization might fail during real flights compensating for the limitations of the localization methodology available. We show that our planner actively improves the precision of the state estimation by selecting paths that minimize the uncertainty in the estimated states. Furthermore, our experiments illustrate by comparison that a naive planner would fail to reach the goal within bounded uncertainty in most cases. (C) 2014 Wiley Periodicals, Inc. C1 [Achtelik, Markus W.; Lynen, Simon] ETH, Autonomous Syst Lab, CH-8092 Zurich, Switzerland. [Weiss, Stephan] CALTECH, Jet Prop Lab, Comp Vis Grp, NASA, Pasadena, CA 91109 USA. [Chli, Margarita] Univ Edinburgh, Vis Robot Lab, Sch Informat, Edinburgh EH8 9AB, Midlothian, Scotland. [Siegwart, Roland] ETH, CH-8092 Zurich, Switzerland. RP Achtelik, MW (reprint author), ETH, Autonomous Syst Lab, CH-8092 Zurich, Switzerland. EM markus.achtelik@mavt.ethz.ch; simon.lynen@mavt.ethz.ch; stephan.weiss@ieee.org; mchli@inf.ed.ac.uk; r.siegwart@ieee.org FU European Community [266470, 600958] FX The research leading to these results has received funding from the European Community's Seventh Framework Programme (FP7) under grant agreements n. 266470 (myCopter) and n. 600958 (SHERPA). NR 39 TC 8 Z9 8 U1 2 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1556-4959 EI 1556-4967 J9 J FIELD ROBOT JI J. Field Robot. PD JUL-AUG PY 2014 VL 31 IS 4 SI SI BP 676 EP 698 DI 10.1002/rob.21522 PG 23 WC Robotics SC Robotics GA AJ4WI UT WOS:000337679200011 ER PT J AU Hale, MC Colletti, JA Gahr, SA Scardina, J Thrower, FP Harmon, M Carter, M Phillips, RB Thorgaard, GH Rexroad, CE Nichols, KM AF Hale, Matthew C. Colletti, John A. Gahr, Scott A. Scardina, Julie Thrower, Frank P. Harmon, Matthew Carter, Megan Phillips, Ruth B. Thorgaard, Gary H. Rexroad, Caird E., III Nichols, Krista M. TI Mapping and Expression of Candidate Genes for Development Rate in Rainbow Trout (Oncorhynchus mykiss) SO JOURNAL OF HEREDITY LA English DT Article DE qPCR; quantitative genetics; quantitative trait loci; salmonid ID QUANTITATIVE TRAIT LOCI; MICROSATELLITE LINKAGE MAP; ATLANTIC SALMON; STEELHEAD TROUT; MEIOTIC MAPS; ARCTIC CHARR; BODY-WEIGHT; ARCHITECTURE; POPULATIONS; FISH AB Development rate has important implications for individual fitness and physiology. In salmonid fishes, development rate correlates with many traits later in life, including life-history diversity, growth, and age and size at sexual maturation. In rainbow trout (Oncorhynchus mykiss), a quantitative trait locus for embryonic development rate has been detected on chromosome 5 across populations. However, few candidate genes have been identified within this region. In this study, we use gene mapping, gene expression, and quantitative genetic methods to further identify the genetic basis of embryonic developmental rate in O. mykiss. Among the genes located in the region of the major development rate quantitative trait locus (GHR1, Clock1a, Myd118-1, and their paralogs), all were expressed early in embryonic development (fertilization through hatch), but none were differentially expressed between individuals with the fast-or slow-developing alleles for a major embryonic development rate quantitative trait locus. In a follow-up study of migratory and resident rainbow trout from natural populations in Alaska, we found significant additive variation in development rate and, moreover, found associations between development rate and allelic variation in all 3 candidate genes within the quantitative trait locus for embryonic development. The mapping of these genes to this region and associations in multiple populations provide positional candidates for further study of their roles in growth, development, and life-history diversity in this model salmonid. C1 [Hale, Matthew C.; Colletti, John A.; Scardina, Julie; Harmon, Matthew; Carter, Megan; Nichols, Krista M.] Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA. [Gahr, Scott A.] St Vincent Coll, Dept Biol, Latrobe, PA USA. [Thrower, Frank P.] NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK USA. [Phillips, Ruth B.] Washington State Univ, Dept Biol Sci, Vancouver, WA USA. [Thorgaard, Gary H.] Washington State Univ, Dept Biol Sci, Pullman, WA 99164 USA. [Thorgaard, Gary H.] Washington State Univ, Ctr Reprod Biol, Pullman, WA 99164 USA. [Rexroad, Caird E., III] ARS, USDA, Natl Ctr Cool & Coldwater Aquaculture, Leetown, WV USA. [Nichols, Krista M.] Purdue Univ, Dept Forestry & Nat Resources, W Lafayette, IN 47907 USA. [Nichols, Krista M.] NOAA, Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Conservat Biol Div, Seattle, WA 98112 USA. RP Nichols, KM (reprint author), Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA. EM krista.nichols@noaa.gov FU National Research Council, US Department of Agriculture - National Research Initiative [2007-35205-17881]; National Science Foundation [NSF-DEB-0845265]; Howard Hughes Medical Institute FX National Research Council, US Department of Agriculture - National Research Initiative grant (2007-35205-17881), National Science Foundation Career Award (NSF-DEB-0845265) (to K.M.N.); Howard Hughes Medical Institute undergraduate fellowships (to J.A.C. and M.H.). NR 58 TC 2 Z9 2 U1 2 U2 23 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0022-1503 EI 1465-7333 J9 J HERED JI J. Hered. PD JUL-AUG PY 2014 VL 105 IS 4 BP 506 EP 520 DI 10.1093/jhered/esu018 PG 15 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA AJ6KJ UT WOS:000337802400007 PM 24744432 ER PT J AU Lecoutre, C Garrabos, Y Beysens, D Nikolayev, V Hahn, I AF Lecoutre, Carole Garrabos, Yves Beysens, Daniel Nikolayev, Vadim Hahn, Inseob TI Boiling phenomena in near-critical SF6 observed in weightlessness SO ACTA ASTRONAUTICA LA English DT Article DE Boiling phenomena; Boiling crisis; Critical heat flux; Liquid-gas critical point; Sulphur hexafluoride; Microgravity experiment ID CRITICAL HEAT-FLUX; MICROGRAVITY; DYNAMICS; CRISIS AB Boiling phenomena in the two-phase region of SF6 close to its critical point have been observed using the high-quality thermal and optical environment of the CNES dedicated facility ALI-DECLIC on board the International Space Station (ISS). The weightlessness environment of the fluid, which cancels buoyancy forces and favorites the three-dimensional spherical shape of the gas bubble, is proven to be an irreplaceable powerful tool for boiling studies. To identify each key mechanism of the boiling phenomena, the ALI-DECLIC experiments have benefited from (i) the well-adapted design of the test cells, (ii) the high-fidelity of the ALI insert teleoperation when long-duration experiment in stable thermal and microgravity environment are required and (iii) the high repeatability of the controlled thermal disturbances. These key mechanisms were observed by light transmission and interferometry technique independently with two sample cells filled with pure SF6 at a near-critical density. The fluid samples are driven away from thermal equilibrium by using a heater directly implemented in the fluid, or a surface heater on a sapphire optical window. In the interferometry cell, the bulk massive heater distinguishes two symmetrical two-phase domains. The modification of the gas bubble shape is observed during heating. In the direct observation cell, the gas bubble is separated by a liquid film from the thin layered transparent heater deposited on the sapphire window. The liquid film drying and the triple contact line motion during heating are observed using light transmission. The experiments have been performed in a temperature range of 10 K below the critical temperature 71, with special attention to the range 0.1 mK <= T-c-T <= 3 mK very close to the critical temperature. The unique advantage of this investigation is to provide opportunities to observe the boiling phenomena at very low heat fluxes, thanks to the fine adjustment of the liquid-vapor properties, (e.g. surface tension), by precise control of the distance to the critical point. We present the new observations of the gas bubble spreading over the heating surface which characterizes the regime where vapor bubbles nucleate separately and grow, as well as liquid drying, vapor film formation, triple contact line motion, which are the key mechanisms at the origin of the boiling crisis when the formed vapor film reduces the heat transfer drastically at the heater wall. (c) 2014 IAA. Published by Elsevier Ltd. All rights reserved. C1 [Lecoutre, Carole; Garrabos, Yves] Univ Bordeaux, CNRS, ICMCB ESEME, UPR 9048, F-33600 Pessac, France. [Beysens, Daniel; Nikolayev, Vadim] UMR E CEA UJF Grenoble 1, INAC, Serv Basses Temp, Grenoble, France. [Beysens, Daniel; Nikolayev, Vadim] PMMH ESPCI, ESEME, F-75231 Paris 5, France. [Hahn, Inseob] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lecoutre, C (reprint author), ICMCB CNRS, 87 Ave Dr Albert Schweitzer, F-33608 Pessac, France. EM lecoutre@icmcb-bordeaux.cnrs.fr; garrabos@icmcb-bordeaux.cnrs.fr; daniel.beysens@espci.fr; vadim.nikolayev@espci.fr; inseob.hahn@jpl.nasa.gov RI Lecoutre, Carole/H-3367-2013; Garrabos, Yves/H-5404-2013 FU CNES (Centre National d'Etudes Spatiales); CADMOS-CNES FX The authors acknowledge the financial support from CNES (Centre National d'Etudes Spatiales), and teleoperation capabilities from the CADMOS-CNES user center in Toulouse, in collaboration with NASA support operating centers. They gratefully thank the CNES-DECLIC project team, especially project managers Gerard Cambon, Sebastien Barde and Gabriel Pont, and the associated DECLIC industrial teams (ASTRIUM-ST, COMAT, EREMS, IDEAS, SODERN, SEIV-Aquitaine, ARCOFLUID, AXS) for their help during the accomplishment of this work. VN also thanks the LMS team (Ecole Polytechnique) for the collaboration in the frame of the ALICE ANR-08-BLAN-0212-03 project. NR 23 TC 1 Z9 1 U1 1 U2 13 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 JUL-AUG PY 2014 VL 100 BP 22 EP 29 DI 10.1016/j.actaastro.2014.03.012 PG 8 WC Engineering, Aerospace SC Engineering GA AI8VG UT WOS:000337204500003 ER PT J AU Campagnola, S Buffington, BB Petropoulos, AE AF Campagnola, Stefano Buffington, Brent B. Petropoulos, Anastassios E. TI Jovian tour design for orbiter and lander missions to Europa SO ACTA ASTRONAUTICA LA English DT Article DE Europa Mission; Multiple flyby trajectory; Moon tour; Multi-body dynamics; Tisserand-Poincare graph ID TRAJECTORY DESIGN; PLANAR; FLYBYS; GRAPH AB Europa is one of the most interesting targets for solar system exploration, as its ocean of liquid water could harbor life. Following the recommendation of the Planetary Decadal Survey, NASA commissioned a study for a multiple flyby only mission, an orbiter mission, and a lander mission. This paper presents the moon tours for the lander and orbiter concepts. The total Delta v and radiation dose would be reduced when compared to previous designs by exploiting multi-body dynamics and avoiding multi-revolution transfers in the Ganymede-to-Europa transfer. Tours 11-03, 1241 and 12-L4 and their performances compared to other tours from previous Europa mission studies are presented in detail. (c) 2014 IAA. Published by Elsevier Ltd. All rights reserved. C1 [Campagnola, Stefano] JAXA, ISAS, Sagamihara, Kanagawa 1550031, Japan. [Buffington, Brent B.; Petropoulos, Anastassios E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Campagnola, S (reprint author), JAXA, ISAS, Yoshinoday 3-1-1, Sagamihara, Kanagawa 1550031, Japan. EM stefano.campagnola@jax.jp FU National Aeronautics and Space Administration FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 43 TC 10 Z9 10 U1 3 U2 13 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 JUL-AUG PY 2014 VL 100 BP 68 EP 81 DI 10.1016/j.actaastro.2014.02.005 PG 14 WC Engineering, Aerospace SC Engineering GA AI8VG UT WOS:000337204500008 ER PT J AU Smirnova, OA Hu, SW Cucinotta, FA AF Smirnova, Olga A. Hu, Shaowen Cucinotta, Francis A. TI DYNAMICS OF ACUTELY IRRADIATED SKIN EPIDERMAL EPITHELIUM IN SWINE: MODELING STUDIES SO HEALTH PHYSICS LA English DT Article DE exposure, radiation; health effects; radiation effects; tissue, body ID ACUTE SINGLE EXPOSURES; X-RAYS; IONIZING-RADIATION; MOUSE SKIN; STEM-CELLS; PIG SKIN; QUANTIFICATION; MICROVASCULATURE; CHALONES; MINIPIG AB A mathematical model, which describes the dynamics of acutely irradiated skin epidermal epithelium in swine, is developed. This model embodies the key mechanisms of regulation of skin epidermal epithelium and the principal stages of development of its cells (basal, prickle, and corneal). The model is implemented as a system of nonlinear ordinary differential equations, whose variables and parameters have clear biological meaning. The modeling results for the dose-and time-dependent changes in basal and prickle cell populations are in a good agreement with relevant experimental data. The correlation between the experimental data on the dynamics of moist reaction in acutely irradiated swine skin epidermal epithelium and the corresponding modeling results on the dynamics of corneal cells is revealed. Proceeding from this, the threshold level of corneal cells, which indicates the appearance of the moist reaction, is found. All this bears witness to the validity of employment of the developed model, after appropriate identification, in the investigation and prediction of radiation effects on skin epidermal epithelium in humans. C1 [Smirnova, Olga A.] Fed State Unitary Enterprise Res & Tech Ctr Radia, Moscow 123182, Russia. [Hu, Shaowen] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA. [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Cucinotta, Francis A.] Univ Nevada, Las Vegas, NV 89154 USA. RP Cucinotta, FA (reprint author), Univ Nevada, Dept Hlth Phys & Diagnost Sci, Las Vegas, NV 89154 USA. EM Francis.Cucinotta@unlv.edu NR 50 TC 4 Z9 4 U1 0 U2 4 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3621 USA SN 0017-9078 EI 1538-5159 J9 HEALTH PHYS JI Health Phys. PD JUL PY 2014 VL 107 IS 1 BP 47 EP 59 DI 10.1097/HP.0000000000000058 PG 13 WC Environmental Sciences; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging GA AI8HY UT WOS:000337154200005 PM 24849903 ER PT J AU Yoo, JM Lee, YR Kim, D Jeong, MJ Stockwell, WR Kundu, PK Oh, SM Shin, DB Lee, SJ AF Yoo, Jung-Moon Lee, Yu-Ri Kim, Dongchul Jeong, Myeong-Jae Stockwell, William R. Kundu, Prasun K. Oh, Soo-Min Shin, Dong-Bin Lee, Suk-Jo TI New indices for wet scavenging of air pollutants (O-3, CO, NO2, SO2, and PM10) by summertime rain (vol 82, pg 226, 2014) SO ATMOSPHERIC ENVIRONMENT LA English DT Correction C1 [Yoo, Jung-Moon; Oh, Soo-Min] Ewha Womans Univ, Dept Sci Educ, Seoul, South Korea. [Lee, Yu-Ri; Shin, Dong-Bin] Yonsei Univ, Dept Atmospher Sci, Seoul 120749, South Korea. [Kim, Dongchul] Univ Space Res Assoc, Columbia, MD USA. [Jeong, Myeong-Jae] Gangneung Wonju Natl Univ, Dept Atmospher & Environm Sci, Kangnung, South Korea. [Stockwell, William R.] Howard Univ, Dept Chem, Washington, DC 20059 USA. [Kundu, Prasun K.] Univ Maryland Baltimore Cty, JCET, Baltimore, MD 21228 USA. [Kim, Dongchul; Kundu, Prasun K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lee, Suk-Jo] Natl Inst Environm Res, Inchon, South Korea. RP Kim, D (reprint author), Univ Space Res Assoc, Columbia, MD USA. EM Dongchul.kim@nasa.gov NR 1 TC 0 Z9 0 U1 1 U2 8 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 JUL PY 2014 VL 91 BP 178 EP 178 DI 10.1016/j.atmosenv.2014.03.037 PG 1 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AI6AP UT WOS:000336952500021 ER PT J AU Cook, SB Kanaley, JA Ploutz-Snyder, LL AF Cook, Summer B. Kanaley, Jill A. Ploutz-Snyder, Lori L. TI Neuromuscular function following muscular unloading and blood flow restricted exercise SO EUROPEAN JOURNAL OF APPLIED PHYSIOLOGY LA English DT Article DE Disuse; Weight lifting; Voluntary activation; Strength ID SKELETAL-MUSCLE FUNCTION; LOWER-LIMB SUSPENSION; RESISTANCE EXERCISE; VASCULAR OCCLUSION; BED REST; ADAPTATIONS; ACTIVATION; HUMANS; LOAD; EFFICACY AB The aim of the study is to evaluate central and peripheral neuromuscular function in the knee extensors (KE) and plantar flexors (PF) after 30 days of unilateral lower limb suspension (ULLS) and to examine the effects of low-load blood flow restricted (BFR) resistance training on the KE during ULLS. Strength, cross-sectional area (CSA), central activation, evoked force, and rates of force development and relaxation were assessed in the KE and PF before and after ULLS in sixteen subjects (9 M, 7F; 18-49 years). Eight of those subjects participated in BFR on the KE three times per week during ULLS (ULLS + Exercise). The ULLS group had decrements in strength and CSA of the KE (16 and 7 %, respectively) and PF (27 and 8 %, respectively) and the ULLS + Exercise maintained strength and CSA of the KE (P > 0.05), but significantly lost strength and CSA in the PF (21 and 5 %; P > 0.05). KE central activation declined 6 % in the ULLS group and was maintained in the ULLS + Exercise group, but a time x group interaction was not evident (P = 0.31). PF central activation was reduced in both groups (ULLS: -7.6 +/- A 9.9 and -7.9 +/- 11.6 %; time main effect P = 0.01). A time x group interaction for KE-evoked twitch force (P = 0.04) demonstrated a 9 % decline in the ULLS + Exercise group following the intervention. Evoked PF doublet torque decreased 12 % in both groups (P = 0.002). Central and peripheral neuromuscular function is compromised during unloading. While BFR resistance training on the KE during unloading can maintain muscle mass and strength, it may only partially attenuate neuromuscular dysfunction. C1 [Cook, Summer B.] Univ New Hampshire, Dept Kinesiol, Durham, NH 03824 USA. [Kanaley, Jill A.] Univ Missouri, Dept Nutr & Exercise Physiol, Columbia, MO 65211 USA. [Ploutz-Snyder, Lori L.] NASA, Lyndon B Johnson Space Ctr, Univ Space Res Assoc, Houston, TX 77058 USA. RP Cook, SB (reprint author), Univ New Hampshire, Dept Kinesiol, 124 Main St, Durham, NH 03824 USA. EM summer.cook@unh.edu; kanaleyj@missouri.edu; lori.ploutz-snyder-1@nasa.gov FU National Aeronautics and Space Administration (NASA) [NNX06AG26H, NNX079AP79H, NNX079AP79H2]; NASA Space Physiology Research Grant through the American College of Sports Medicine (ACSM) Foundation; Syracuse University Creative Writing Grant FX The authors would like to thank the subjects who graciously gave their time and energy to this research and to the numerous undergraduate and graduate students who assisted with data collection in this study. This work was supported by grants from the following: National Aeronautics and Space Administration (NASA) (NNX06AG26H, NNX079AP79H, and NNX079AP79H2), the 2006 and 2008 NASA Space Physiology Research Grant through the American College of Sports Medicine (ACSM) Foundation and the Syracuse University Creative Writing Grant 2006 and 2008. NR 35 TC 7 Z9 7 U1 0 U2 12 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1439-6319 EI 1439-6327 J9 EUR J APPL PHYSIOL JI Eur. J. Appl. Physiol. PD JUL PY 2014 VL 114 IS 7 BP 1357 EP 1365 DI 10.1007/s00421-014-2864-3 PG 9 WC Physiology; Sport Sciences SC Physiology; Sport Sciences GA AI7GD UT WOS:000337052300002 PM 24643427 ER PT J AU Sadovsky, AV Davis, D Isaacson, DR AF Sadovsky, Alexander V. Davis, Damek Isaacson, Douglas R. TI Efficient Computation of Separation-Compliant Speed Advisories for Air Traffic Arriving in Terminal Airspace SO JOURNAL OF DYNAMIC SYSTEMS MEASUREMENT AND CONTROL-TRANSACTIONS OF THE ASME LA English DT Article ID HYBRID SYSTEMS AB A class of problems in air traffic management (ATM) asks for a scheduling algorithm that supplies the air traffic services authority not only with a schedule of arrivals and departures but also with speed advisories. Since advisories must be finite, a scheduling algorithm must ultimately produce a finite data set, hence must either start with a purely discrete model or involve a discretization of a continuous one. The former choice, often preferred for intuitive clarity, naturally leads to mixed-integer programs (MIPs), hindering proofs of correctness and computational cost bounds (crucial for real-time operations). In this paper, a hybrid control system is used to model air traffic scheduling, capturing both the discrete and continuous aspects. This framework is applied to a class of problems, called the fully routed nominal problem. We prove a number of geometric results on feasible schedules and use these results to formulate an algorithm that attempts to compute a collective speed advisory, effectively piecewise linear with finitely many vertices, and has computational cost polynomial in the number of aircraft. This work is a first step toward optimization and models refined with more realistic detail. C1 [Sadovsky, Alexander V.; Isaacson, Douglas R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Davis, Damek] Univ Calif Los Angeles, Dept Math, Los Angeles, CA 90095 USA. RP Sadovsky, AV (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM alexander.v.sadovsky@nasa.gov FU NSF [DGE-0707424] FX D. Davis's research was supported by NSF Grant DGE-0707424. The authors thank D. Denery (NASA ARC) for suggesting the use of hybrid systems for ATM, W. Haskell (USC) for editing early drafts of the paper, and H. Swenson (NASA ARC) and J. Mitchell (SUNY Stony Brook) for helpful suggestions. NR 36 TC 1 Z9 1 U1 0 U2 5 PU ASME PI NEW YORK PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA SN 0022-0434 EI 1528-9028 J9 J DYN SYST-T ASME JI J. Dyn. Syst. Meas. Control-Trans. ASME PD JUL PY 2014 VL 136 IS 4 AR 041027 DI 10.1115/1.4026957 PG 10 WC Automation & Control Systems; Instruments & Instrumentation SC Automation & Control Systems; Instruments & Instrumentation GA AI5OB UT WOS:000336917200027 ER PT J AU Jackman, CH Fleming, EL AF Jackman, Charles H. Fleming, Eric L. TI Stratospheric ozone response to a solar irradiance reduction in a quadrupled CO2 environment SO EARTHS FUTURE LA English DT Article DE geoengineering; stratosphere; ozone; CO2; solar flux ID 2-DIMENSIONAL MODEL; MIDDLE ATMOSPHERE; GREENHOUSE GASES; DEPLETION; RECOVERY; IMPACT; ALBEDO AB We used the Goddard Space Flight Center (GSFC) global two-dimensional (2D) atmospheric model to investigate the stratospheric ozone response to a proposed geoengineering activity wherein a reduced top-of-atmosphere (TOA) solar irradiance is imposed to help counteract a quadrupled CO2 atmosphere. This study is similar to the Geoengineering Model Intercomparison Project (GeoMIP) Experiment G1. Three primary simulations were completed with the GSFC 2D model to examine this possibility: (A) a pre-industrial atmosphere with a boundary condition of 285 ppmv CO2 (piControl); (B) a base future atmosphere with 1140 ppmv CO2 (abrupt4xCO2); and (C) a perturbed future atmosphere with 1140 ppmv CO2 and a 4% reduction in the TOA total solar irradiance (G1). We found huge ozone enhancements throughout most of the stratosphere (up to 40%) as a result of a large computed temperature decrease (up to 18 K) when CO2 was quadrupled (compare simulation abrupt4xCO2 to piControl). Further, we found that ozone will additionally increase (up to 5%) throughout most of the stratosphere with total ozone increases of 1-2.5% as a result of a reduction in TOA total solar irradiance (compare simulation G1 to abrupt4xCO2). Decreases of atomic oxygen and temperature are the main drivers of this computed ozone enhancement from a reduction in TOA total solar irradiance. C1 [Jackman, Charles H.; Fleming, Eric L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fleming, Eric L.] Sci Syst & Applicat Inc, Lanham, MD USA. RP Jackman, CH (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM Charles.H.Jackman@nasa.gov RI Jackman, Charles/D-4699-2012 FU NASA Headquarters Atmospheric Composition Modeling and Analysis Program FX We thank the NASA Headquarters Atmospheric Composition Modeling and Analysis Program for support during the time that this manuscript was written. We thank Valentina Aquila and Paul Newman for valuable comments on an earlier version of this paper. The GSFC 2D Model output used in this manuscript will be provided to interested individuals upon request to author C. Jackman (Charles.H.Jackman@nasa.gov). NR 42 TC 1 Z9 1 U1 1 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2328-4277 J9 EARTHS FUTURE JI Earth Future PD JUL PY 2014 VL 2 IS 7 BP 331 EP 340 DI 10.1002/2014EF000244 PG 10 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA CN0WF UT WOS:000358134000001 ER PT J AU Cinquini, L Crichton, D Mattmann, C Harney, J Shipman, G Wang, FY Ananthakrishnan, R Miller, N Denvil, S Morgan, M Pobre, Z Bell, GM Doutriaux, C Drach, R Williams, D Kershaw, P Pascoe, S Gonzalez, E Fiore, S Schweitzer, R AF Cinquini, Luca Crichton, Daniel Mattmann, Chris Harney, John Shipman, Galen Wang, Feiyi Ananthakrishnan, Rachana Miller, Neill Denvil, Sebastian Morgan, Mark Pobre, Zed Bell, Gavin M. Doutriaux, Charles Drach, Robert Williams, Dean Kershaw, Philip Pascoe, Stephen Gonzalez, Estanislao Fiore, Sandro Schweitzer, Roland TI The Earth System Grid Federation: An open infrastructure for access to distributed geospatial data SO FUTURE GENERATION COMPUTER SYSTEMS-THE INTERNATIONAL JOURNAL OF GRID COMPUTING AND ESCIENCE LA English DT Article DE Climate science; Federation; Search; Discovery; Peer-to-peer; CMIP5 AB The Earth System Grid Federation (ESGF) is a multi-agency, international collaboration that aims at developing the software infrastructure needed to facilitate and empower the study of climate change on a global scale. The ESGF's architecture employs a system of geographically distributed peer nodes, which are independently administered yet united by the adoption of common federation protocols and application programming interfaces (APIs). The cornerstones of its interoperability are the peer-to-peer messaging that is continuously exchanged among all nodes in the federation; a shared architecture and API for search and discovery; and a security infrastructure based on industry standards (OpenID, SSL, GSI and SAML). The ESGF software stack integrates custom components (for data publishing, searching, user interface, security and messaging), developed collaboratively by the team, with popular application engines (Tomcat, Solr) available from the open source community. The full ESGF infrastructure has now been adopted by multiple Earth science projects and allows access to petabytes of geophysical data, including the entire Fifth Coupled Model Intercomparison Project (CMIP5) output used by the Intergovernmental Panel on Climate Change (IPCC) Fifth Assessment Report (AR5) and a suite of satellite observations (obs4MIPs) and reanalysis data sets (ANA4MIPs). This paper presents ESGF as a successful example of integration of disparate open source technologies into a cohesive, wide functional system, and describes our experience in building and operating a distributed and federated infrastructure to serve the needs of the global climate science community. (C) 2013 Elsevier B.V. All rights reserved. C1 [Cinquini, Luca; Crichton, Daniel; Mattmann, Chris] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cinquini, Luca; Crichton, Daniel; Mattmann, Chris] CALTECH, Pasadena, CA 91106 USA. [Harney, John; Wang, Feiyi] Oak Ridge Natl Lab, Oak Ridge, TN USA. [Shipman, Galen] Oak Ridge Natl Lab, Comp & Computat Sci Directorate, Oak Ridge, TN USA. [Ananthakrishnan, Rachana] Univ Chicago, Computat Inst, Chicago, IL 60637 USA. [Miller, Neill] Univ Chicago, Chicago, IL 60637 USA. [Ananthakrishnan, Rachana; Miller, Neill] Argonne Natl Lab, Argonne, IL 60439 USA. [Denvil, Sebastian] Inst Pierre Simon Laplace, Climate Modeling Grp, Paris, France. [Morgan, Mark] Inst Pierre Simon Laplace, Earth Syst Modeling Platform, Paris, France. [Pobre, Zed] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bell, Gavin M.; Doutriaux, Charles; Drach, Robert; Williams, Dean] Lawrence Livermore Natl Lab, Livermore, CA USA. [Kershaw, Philip] STEC Rutherford Appleton Lab, RAL Space, Ctr Environm Data Archival, Didcot, Oxon, England. [Pascoe, Stephen] STEC Rutherford Appleton Lab, Didcot, Oxon, England. [Kershaw, Philip; Pascoe, Stephen] NCAS BADC, Didcot, Oxon, England. [Gonzalez, Estanislao] German Climate Comp Ctr DKRZ, Hamburg, Germany. [Fiore, Sandro] Euromediterranean Ctr Climate Change CMCC, Lecce, Italy. [Schweitzer, Roland] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA. RP Cinquini, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM luca.cinquini@jpl.nasa.gov; daniel.j.crichton@jpl.nasa.gov; chris.a.mattmann@jpl.nasa.gov; harneyjf@ornl.gov; gshipman@ornl.gov; fwang2@ornl.gov; ranantha@mcs.anl.gov; neillm@mcs.anl.gov; sebastien.denvil@ipsl.jussieu.fr; momipsl@ipsl.jussieu.fr; zed.pobre@nasa.gov; gavin@llnl.gov; doutriaux1@llnl.gov; drach1@llnl.gov; williams13@llnl.gov; philip.kershaw@stfc.ac.uk; stephen.pascoe@stfc.ac.uk; estanislao.gonzalez@met.fu-berlin.de; sandro.fiore@unisalento.it; Roland.Schweitzer@noaa.gov OI Kershaw, Philip/0000-0002-7646-291X FU U.S. Department of Energy; National Atmospheric and Space Administration (NASA); European Infrastructure for the European Network for Earth System Modeling (IS-ENES) FX The development and operation of ESGF is supported by the efforts of principal investigators, software engineers, data managers and system administrators from many agencies and institutions worldwide. Primary contributors include ANL, ANU, BADC, CMCC, DKRZ, ESRL, GFDL, GSFC, JPL, IPSL, NCAR, ORNL, LBNL, LLNL (leading institution), PMEL, PNNL and SNL. Major funding provided by the U.S. Department of Energy, the National Atmospheric and Space Administration (NASA), and the European Infrastructure for the European Network for Earth System Modeling (IS-ENES). NR 18 TC 16 Z9 16 U1 2 U2 19 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0167-739X EI 1872-7115 J9 FUTURE GENER COMP SY JI Futur. Gener. Comp. Syst. PD JUL PY 2014 VL 36 BP 400 EP 417 DI 10.1016/j.future.2013.07.002 PG 18 WC Computer Science, Theory & Methods SC Computer Science GA AI3OB UT WOS:000336770700035 ER PT J AU Savas, AJ Hartwig, JW Moder, JP AF Savas, Anthony J. Hartwig, Jason W. Moder, Jeffrey P. TI Thermal analysis of a cryogenic liquid acquisition device under autogenous and non-condensable pressurization schemes SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER LA English DT Article DE Cryogenic; Liquid acquisition device; Autogenous pressurization; Interfacial temperature; Condensation rate; Evaporation rate; Subcooled liquid ID INTERFACIAL-TENSION; PRESSURE-DEPENDENCE; FLUID PHASES; SCREEN; FLOW; GAS AB This paper presents thermal analysis of a 325 x 2300 mesh LAD sample that was tested over a wide range of liquid methane temperatures (106-160 K) and pressures (0.0618-1.78 MPa) for a LAD using both autogenous (gaseous methane) and noncondensible (gaseous helium or nitrogen) pressurization schemes. To compare between schemes, screen interfacial temperatures, screen Reynolds numbers, condensation and/or evaporation mass flow rates at breakdown, and heat fluxes produced at the screen are computed as a function of liquid temperature and pressure. Condensation and evaporation rates are also computed using kinetic theory to allow comparison. Each parameter has a profound impact on surface tension and thus the performance of the LAD screen. The understanding gained here will be used to determine optimal propellant pressure and temperature operating regimes and will help mission designers determine whether autogenous pressurization is feasible for future space missions. Published by Elsevier Ltd. C1 [Savas, Anthony J.] Aerosp Corp, Chantilly, VA 20151 USA. [Hartwig, Jason W.] NASA, Glenn Res Ctr, Propellants & Prop Branch, Cleveland, OH 44135 USA. [Moder, Jeffrey P.] NASA, Glenn Res Ctr, Combust Branch, Cleveland, OH 44135 USA. RP Hartwig, JW (reprint author), NASA, Glenn Res Ctr, Propellants & Prop Branch, 21000 Brookpk Rd,MS 301-3, Cleveland, OH 44135 USA. EM ajs432@cornell.edu; jason.w.hartwig@nasa.gov; jeffrey.p.moder@nasa.gov FU Cryogenic Fluid Management Project at NASA Glenn Research Center under Exploration Systems Mission Directorate at NASA Headquarters FX This work was funded by the Cryogenic Fluid Management Project at NASA Glenn Research Center under the auspices of the Exploration Systems Mission Directorate at NASA Headquarters. The authors would like to thank the Ohio Aerospace Institute and Lewis' Educational and Research Collaborative Internship Project for providing a setting under which this research could be accomplished. In addition, the authors would like to thank the operations team and research support staff at CCL-7 for their assistance during the planning and testing phases. NR 33 TC 5 Z9 5 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0017-9310 EI 1879-2189 J9 INT J HEAT MASS TRAN JI Int. J. Heat Mass Transf. PD JUL PY 2014 VL 74 BP 403 EP 413 DI 10.1016/j.ijheatmasstransfer.2014.03.036 PG 11 WC Thermodynamics; Engineering, Mechanical; Mechanics SC Thermodynamics; Engineering; Mechanics GA AI2NV UT WOS:000336696100039 ER PT J AU Fixsen, DJ Moseley, SH Gerrits, T Lita, AE Nam, SW AF Fixsen, D. J. Moseley, S. H. Gerrits, T. Lita, A. E. Nam, S. W. TI Optimal Energy Measurement in Nonlinear Systems: An Application of Differential Geometry SO JOURNAL OF LOW TEMPERATURE PHYSICS LA English DT Article DE TES; X-ray; Microcalorimeter; Optimal filter; Nonlinear response; Non-stationary noise; Differential geometry ID EFFICIENCY; DETECTORS; NOISE AB Design of TES microcalorimeters requires a tradeoff between resolution and dynamic range. Often, experimenters will require linearity for the highest energy signals, which requires additional heat capacity be added to the detector. This results in a reduction of low energy resolution in the detector. We derive and demonstrate an algorithm that allows operation far into the nonlinear regime with little loss in spectral resolution. We use a least squares optimal filter that varies with photon energy to accommodate the nonlinearity of the detector and the non-stationarity of the noise. The fitting process we use can be seen as an application of differential geometry. This recognition provides a set of well-developed tools to extend our work to more complex situations. The proper calibration of a nonlinear microcalorimeter requires a source with densely spaced narrow lines. A pulsed laser multi-photon source is used here, and is seen to be a powerful tool for allowing us to develop practical systems with significant detector nonlinearity. The combination of our analysis techniques and the multi-photon laser source create a powerful tool for increasing the performance of future TES microcalorimeters. C1 [Fixsen, D. J.; Moseley, S. H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fixsen, D. J.] Univ Maryland, College Pk, MD 20742 USA. [Gerrits, T.; Lita, A. E.; Nam, S. W.] NIST, Boulder, CO USA. RP Moseley, SH (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM dale.j.fixsen@nasa.gov; harvey.moseley@nasa.gov NR 7 TC 8 Z9 8 U1 1 U2 6 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0022-2291 EI 1573-7357 J9 J LOW TEMP PHYS JI J. Low Temp. Phys. PD JUL PY 2014 VL 176 IS 1-2 BP 16 EP 26 DI 10.1007/s10909-014-1149-x PG 11 WC Physics, Applied; Physics, Condensed Matter SC Physics GA AI1HU UT WOS:000336602200002 ER PT J AU Thibault, F Martinez, RZ Bermejo, D Ivanov, SV Buzykin, OG Ma, QC AF Thibault, Franck Martinez, Raul Z. Bermejo, Dionisio Ivanov, Sergey V. Buzykin, Oleg G. Ma, Qiancheng TI An experimental and theoretical study of nitrogen-broadened acetylene lines SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Ethyne; Acetylene; Nitrogen; Pressure broadening coefficients; Stimulated Raman spectroscopy; Dynamical methods ID CLASSICAL METHODS; CROSS-SECTIONS; COUPLED-STATES; SPECTRAL LINES; NU(5) BAND; Q BRANCHES; C2H2; COEFFICIENTS; RAMAN; LINEWIDTHS AB We present experimental nitrogen-broadening coefficients derived from Voigt profiles of isotropic Raman Q-lines measured in the v(2) band of acetylene (C2H2) at 150 K and 298 K, and compare them to theoretical values obtained through calculations that were carried out specifically for this work. Namely, full classical calculations based on Gordon's approach, two kinds of semi-classical calculations based on Robert-Bonamy method as well as full quantum dynamical calculations were performed. All the computations employed exactly the same ab initio potential energy surface for the C2H2-N-2 system which is, to our knowledge, the most realistic, accurate and up-to-date one. The resulting calculated collisional half-widths are in good agreement with the experimental ones only for the full classical and quantum dynamical methods. In addition, we have performed similar calculations for IR absorption lines and compared the results to bibliographic values. Results obtained with the full classical method are again in good agreement with the available room temperature experimental data. The quantum dynamical close-coupling calculations are too time consuming to provide a complete set of values and therefore have been performed only for the R(0) line of C2H2. The broadening coefficient obtained for this line at 173 K and 297 K also compares quite well with the available experimental data. The traditional Robert-Bonamy semi-classical formalism, however, strongly overestimates the values of half-width for both Q- and R-lines. The refined semi-classical Robert-Bonamy method, first proposed for the calculations of pressure broadening coefficients of isotropic Raman lines, is also used for IR lines. By using this improved model that takes into account effects from line coupling, the calculated semi-classical widths are significantly reduced and closer to the measured ones. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Thibault, Franck] Univ Rennes 1, CNRS, UMR 6251, Inst Phys Rennes, F-35042 Rennes, France. [Martinez, Raul Z.; Bermejo, Dionisio] CSIC, Inst Estruct Mat, E-28006 Madrid, Spain. [Ivanov, Sergey V.] Russian Acad Sci, Inst Laser & Informat Technol, Troitsk 142190, Russia. [Buzykin, Oleg G.] Cent Aerohydrodynam Inst TsAGI, Zhukovskii 140160, Moscow Region, Russia. [Ma, Qiancheng] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Ma, Qiancheng] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA. RP Thibault, F (reprint author), Univ Rennes 1, CNRS, UMR 6251, Inst Phys Rennes, Campus Beaulieu,Bat 11B, F-35042 Rennes, France. EM Franck.Thibault@univ-rennes1.fr FU Ministry of Economy and Competitiveness through Research [FIS2012-38175]; NSF [1228861]; European GDRI HiRESMIR FX D.B. and R.Z.M. acknowledge the financial support of the Ministry of Economy and Competitiveness through Research Grant FIS2012-38175. QM. acknowledges the financial support from NSF under Grant 1228861. D.B., R.Z.M and F.T. acknowledge financial support from the European GDRI HiRESMIR (high resolution microwave, infrared and Raman molecular spectroscopy). NR 49 TC 3 Z9 3 U1 0 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD JUL PY 2014 VL 142 BP 17 EP 24 DI 10.1016/j.jqsrt.2014.03.009 PG 8 WC Optics; Spectroscopy SC Optics; Spectroscopy GA AI2RR UT WOS:000336706300003 ER PT J AU Tennyson, J Bernath, PF Brown, LR Campargue, A Csaszar, AG Daumont, L Gamache, RR Hodges, JT Naumenko, OV Polyansky, OL Rothman, LS Vandaele, AC Zobov, NF Denes, N Fazliev, AZ Furtenbacher, T Gordon, IE Hu, SM Szidarovszky, T Vasilenko, IA AF Tennyson, Jonathan Bernath, Peter F. Brown, Linda R. Campargue, Alain Csaszar, Attila G. Daumont, Ludovic Gamache, Robert R. Hodges, Joseph T. Naumenko, Olga V. Polyansky, Oleg L. Rothman, Laurence S. Vandaele, Ann Carine Zobov, Nikolai F. Denes, Nora Fazliev, Alexander Z. Furtenbacher, Tibor Gordon, Iouli E. Hu, Shui-Ming Szidarovszky, Tamas Vasilenko, Irina A. TI IUPAC critical evaluation of the rotational-vibrational spectra of water vapor. Part IV. Energy levels and transition wavenumbers for (D2O)-O-16, (D2O)-O-17, and (D2O)-O-18 SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Water vapor; Transition wavenumbers; Atmospheric physics; Energy levels; Spectroscopic information system ID LASER-ABSORPTION SPECTROSCOPY; HETERODYNE FREQUENCY MEASUREMENTS; LORENTZ-BROADENING COEFFICIENTS; FOURIER-TRANSFORM SPECTRUM; TRIPLY DEUTERATED AMMONIA; INTERSTELLAR HEAVY-WATER; LINE-SHIFT COEFFICIENTS; HOT EMISSION-SPECTRA; LONG PATH SPECTRA; D2O LOW-PRESSURE AB This paper is the fourth of a series of papers reporting critically evaluated rotational-vibrational line positions, transition intensities, pressure dependences, and energy levels, with associated critically reviewed assignments and uncertainties, for all the main isotopologues of water. This paper presents energy level and transition data for the following doubly and triply substituted isotopologues of water: (D2O)-O-16, (D2O)-O-17, and (D2O)-O-18. The MARVEL (Measured Active Rotational-Vibrational Energy Levels) procedure is used to determine the levels, the lines, and their self-consistent uncertainties for the spectral regions 0-14 016, 0-7969, and 0-9108 cm(-1) for (D2O)-O-16, (D2O)-O-17, and (D2O)-O-18, respectively. For (D2O)-O-16, (D2O)-O-17, and (D2O)-O-18, 53 534, 600, and 12 167 lines are considered, respectively, from spectra recorded in absorption at room temperature and in emission at elevated temperatures. The number of validated energy levels is 12 269, 338, and 3351 for (D2O)-O-16, (D2O)-O-17, and (D2O)-O-18, respectively. The energy levels have been checked against the ones determined, with an average accuracy of about 0.03 cm(-1), from variational rovibrational computations employing exact kinetic energy operators and an accurate potential energy surface. Furthermore, the rovibrational labels of the energy levels have been validated by an analysis of the computed wavefunctions using the rigid-rotor decomposition (RRD) scheme. The extensive list of MARVEL lines and levels obtained is deposited in the Supplementary Material of this paper, in a distributed information system applied to water, W@DIS, and on the official MARVEL website, where they can easily be retrieved. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Tennyson, Jonathan; Polyansky, Oleg L.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Bernath, Peter F.] Old Dominion Univ, Norfolk, VA USA. [Brown, Linda R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Campargue, Alain] Univ Grenoble Alpes, CNRS, Grenoble, France. [Csaszar, Attila G.; Denes, Nora; Furtenbacher, Tibor; Szidarovszky, Tamas] Eotvos Lorand Univ, Inst Chem, MTA ELTE Res Grp Complex Chem Syst, Budapest, Hungary. [Daumont, Ludovic] Univ Reims, Reims, France. [Gamache, Robert R.] Univ Massachusetts, Lowell, MA USA. [Hodges, Joseph T.] NIST, Gaithersburg, MD 20899 USA. [Naumenko, Olga V.; Polyansky, Oleg L.; Fazliev, Alexander Z.; Vasilenko, Irina A.] Russian Acad Sci, Inst Atmospher Opt, Tomsk, Russia. [Rothman, Laurence S.; Gordon, Iouli E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vandaele, Ann Carine] Inst Aeron Spatiale Belgique, B-1180 Brussels, Belgium. [Zobov, Nikolai F.] Russian Acad Sci, Inst Appl Phys, Nizhnii Novgorod 603600, Russia. [Hu, Shui-Ming] Univ Sci & Technol China, Hefei 230026, Peoples R China. RP Tennyson, J (reprint author), UCL, Dept Phys & Astron, Mortimer St, London WC1E 6BT, England. EM j.tennyson@ucl.ac.uk RI Tennyson, Jonathan/I-2222-2012; Csaszar, Attila/A-5241-2009; Bernath, Peter/B-6567-2012; Hu, Shuiming/C-4287-2008; Szidarovszky, Tamas/E-4376-2015; OI Tennyson, Jonathan/0000-0002-4994-5238; Bernath, Peter/0000-0002-1255-396X; Hu, Shuiming/0000-0002-1565-8468; Gordon, Iouli/0000-0003-4763-2841; Rothman, Laurence/0000-0002-3837-4847 FU International Union of Pure and Applied Chemistry [2004-035-1-100]; UK Natural Environment Research Council; ERC Advanced Investigator [267219]; Royal Society; Scientific Research Fund of Hungary [OTKA NK83583]; Russian Foundation for Basic Research; Belgian Federal Science Policy Office [EV/35/3A, SD/AT/01A, PRODEX 1514901NLSFe(IC)]; Belgian National Fund for Scientific Research (FRFC contracts); Communaute de Belgique (Action de Recherche Concertees); COST Action CoDECS [CM1002]; NASA AURA mission [NNX11AF91G] FX We all thank the International Union of Pure and Applied Chemistry for funding under project 2004-035-1-100 (A database of water transitions from experiment and theory). In addition, this work has received partial support from the UK Natural Environment Research Council, ERC Advanced Investigator Project 267219, the Royal Society, the Scientific Research Fund of Hungary (Grant OTKA NK83583), the Russian Foundation for Basic Research, the Belgian Federal Science Policy Office (contracts EV/35/3A, SD/AT/01A, PRODEX 1514901NLSFe(IC)), the Belgian National Fund for Scientific Research (FRFC contracts), the Communaute de Belgique (Action de Recherche Concertees), the COST Action CoDECS (CM1002), and the NASA AURA mission, under the grant NNX11AF91G. Part of the research described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contracts and grants with NASA. Alain Campargue and Ludovic Daumont are grateful for the financial support provided by the Programme National LEFE (CHAT) of CNRS (INSU). Semen Mikhailenko is thanked for providing part of the D216O dataset used during this study. We thank Christina Puzzarini for help deperturbing the published frequencies given in 13CaPu. NR 161 TC 28 Z9 33 U1 11 U2 66 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 JUL PY 2014 VL 142 BP 93 EP 108 DI 10.1016/j.jqsrt.2014.03.019 PG 16 WC Optics; Spectroscopy SC Optics; Spectroscopy GA AI2RR UT WOS:000336706300010 ER PT J AU Baker, R Fujiwara, M Minello, TJ AF Baker, Ronald Fujiwara, Masami Minello, Thomas J. TI Juvenile growth and mortality effects on white shrimp Litopenaeus setiferus population dynamics in the northern Gulf of Mexico SO FISHERIES RESEARCH LA English DT Article DE Nursery; Salt marsh; Stock assessment; Life table; Sustainable fisheries ID NATURAL MORTALITY; BROWN SHRIMP; SALT MARSHES; GALVESTON BAY; ESTUARINE NURSERIES; SPATIAL PATCHINESS; MARINE NURSERIES; PENAEUS-AZTECUS; TIME-DIVISION; WETLAND LOSS AB Processes regulating juvenile growth and mortality of white shrimp Litopenaeus setiferus in coastal nurseries may be particularly important in regulating offshore adult population size and sustainability. To advance the integration of these processes into fishery stock assessments, and to provide a better understanding of the functional role of coastal nurseries for fishery species, we explored the potential effects of variable juvenile growth and survival on white shrimp population growth rate. We developed a population model that incorporates available information on vital rates (growth, mortality, fecundity) for each shrimp life stage. We used the model to explore the potential impacts of variability in juvenile growth and mortality rates on the overall population growth rate. Modest changes in juvenile growth and mortality rates were projected to have a greater impact on stock size than the full range in fishing mortality over the past few decades. These results suggest that variability in juvenile survival may be a strong driver of adult stock size and that the processes that regulate juvenile growth and mortality need to be properly understood for the effective management of coastal nurseries and shrimp stocks. (C) 2014 Elsevier B.V. All rights reserved. C1 [Baker, Ronald; Minello, Thomas J.] NOAA, Natl Marine Fisheries Serv, SE Fisheries Sci Ctr, Galveston Lab, Galveston, TX 77551 USA. [Baker, Ronald] James Cook Univ, Sch Marine & Trop Biol, Ctr Trop Water & Aquat Ecosyst Res, Townsville, Qld 4811, Australia. [Baker, Ronald] CSIRO Land & Water, Townsville, Qld 4811, Australia. [Fujiwara, Masami] Texas A&M Univ, Dept Wildlife & Fisheries Sci, College Stn, TX 77843 USA. RP Baker, R (reprint author), James Cook Univ, Sch Marine & Trop Biol, Ctr Trop Water & Aquat Ecosyst Res, Townsville, Qld 4811, Australia. EM ronald.baker@jcu.edu.au RI Baker, Ronald/J-9060-2014; TropWATER, Research ID/P-1401-2014; Fujiwara, Masami/C-3115-2012 OI Baker, Ronald/0000-0001-8408-0324; Fujiwara, Masami/0000-0002-9255-6043 FU National Research Council; NOAA Fisheries in Galveston, TX, USA; Texas Sea Grant [02-S120031]; Commonwealth Scientific and Industrial Research Organisation; James Cook University in Townsville, Queensland FX This research was initiated while RB held a post-doctoral associateship from the National Research Council with NOAA Fisheries in Galveston, TX, USA and completed during a post-doctoral fellowship from the Tropical Landscapes Joint Venture between the Commonwealth Scientific and Industrial Research Organisation and James Cook University in Townsville, Queensland. MF was funded by Texas Sea Grant (Grant #02-S120031). We thank Phil Levin, Lawrence Rozas, and Rick Hart (NOAA) for discussions on modeling and information on white shrimp vital rates and stock assessments. The findings and conclusions in this paper are those of the authors and do not necessarily represent the views of the National Marine Fisheries Service. NR 70 TC 5 Z9 5 U1 3 U2 22 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-7836 EI 1872-6763 J9 FISH RES JI Fish Res. PD JUL PY 2014 VL 155 BP 74 EP 82 DI 10.1016/j.fishres.2014.02.026 PG 9 WC Fisheries SC Fisheries GA AH7XJ UT WOS:000336348400008 ER PT J AU Smith, KE Callahan, MP Gerakines, PA Dworkin, JP House, CH AF Smith, Karen E. Callahan, Michael P. Gerakines, Perry A. Dworkin, Jason P. House, Christopher H. TI Investigation of pyridine carboxylic acids in CM2 carbonaceous chondrites: Potential precursor molecules for ancient coenzymes SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID NITROGEN-HETEROCYCLIC COMPOUNDS; TAGISH LAKE METEORITE; MURCHISON METEORITE; AMINO-ACIDS; DIPHOSPHOPYRIDINE NUCLEOTIDE; NICOTINIC-ACID; ICE ANALOGS; ULTRAVIOLET PHOTOIRRADIATION; EXTRATERRESTRIAL NUCLEOBASES; DEUTERIUM ENRICHMENT AB The distribution and abundances of pyridine carboxylic acids (including nicotinic acid) in eight CM2 carbonaceous chondrites (ALH 85013, DOM 03183, DOM 08003, EET 96016, LAP 02333, LAP 02336, LEW 85311, and WIS 91600) were investigated by liquid chromatography coupled to UV detection and high resolution Orbitrap mass spectrometry. We find that pyridine monocarboxylic acids are prevalent in CM2-type chondrites and their abundance negatively correlates with the degree of pre-terrestrial aqueous alteration that the meteorite parent body experienced. We also report the first detection of pyridine dicarboxylic acids in carbonaceous chondrites. Additionally, we carried out laboratory studies of proton-irradiated pyridine in carbon dioxide-rich ices (a 1: 1 mixture) to serve as a model of the interstellar ice chemistry that may have led to the synthesis of pyridine carboxylic acids. Analysis of the irradiated ice residue shows that a comparable suite of pyridine mono-and dicarboxylic acids was produced, although aqueous alteration may still play a role in the synthesis (and ultimate yield) of these compounds in carbonaceous meteorites. Nicotinic acid is a precursor to nicotinamide adenine dinucleotide, a likely ancient molecule used in cellular metabolism in all of life, and its common occurrence in CM2 chondrites may indicate that meteorites may have been a source of molecules for the emergence of more complex coenzymes on the early Earth. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Smith, Karen E.; House, Christopher H.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Smith, Karen E.; House, Christopher H.] Penn State Univ, Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA. [Callahan, Michael P.; Gerakines, Perry A.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Callahan, Michael P.; Gerakines, Perry A.; Dworkin, Jason P.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. RP Smith, KE (reprint author), Penn State Univ, Dept Geosci, 220 Deike Bldg, University Pk, PA 16802 USA. EM karen.e.smith@nasa.gov RI Gerakines, Perry/D-2226-2012 OI Gerakines, Perry/0000-0002-9667-5904 FU NASA Astrobiology Institute via the Penn State Astrobiology Research Center [NNA09DA76A]; NASA Cosmochemistry Program; NASA Astrobiology Institute via the Goddard Center for Astrobiology; Goddard Center for Astrobiology; NASA Pennsylvania Space Grant Consortium FX The authors thank Kevin Righter and Cecilia Satterwhite (NASA Johnson Space Center, Houston, TX), and the Meteorite Working Group for providing the Antarctic meteorites. We thank Conel Alexander (Carnegie Institution for Science, Washington, DC) for helpful discussions regarding determination of aqueous alteration in meteorites. We thank Aaron Burton (NASA Johnson Space Center, Houston, TX) for his help with meteorite sample preparation. We also thank Steve Brown, Tom Ward, and Eugene Gerashchenko (Radiation Effects Facility, NASA Goddard Space Flight Center, Greenbelt, MD) for operation of the proton accelerator. K. E. S. acknowledges support from the NASA Pennsylvania Space Grant Consortium. K.E.S. and C.H.H. acknowledge support from the NASA Astrobiology Institute via the Penn State Astrobiology Research Center (cooperative agreement #NNA09DA76A). M.P.C. and J.P.D. acknowledge support from the NASA Cosmochemistry Program and the NASA Astrobiology Institute via the Goddard Center for Astrobiology. P.A.G acknowledges support from the Goddard Center for Astrobiology. NR 52 TC 7 Z9 7 U1 2 U2 26 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 JUL 1 PY 2014 VL 136 BP 1 EP 12 DI 10.1016/j.gca.2014.04.001 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AH9SG UT WOS:000336481800001 ER PT J AU Sebree, JA Trainer, MG Loeffler, MJ Anderson, CM AF Sebree, Joshua A. Trainer, Melissa G. Loeffler, Mark J. Anderson, Carrie M. TI Titan aerosol analog absorption features produced from aromatics in the far infrared SO ICARUS LA English DT Article DE Titan, atmosphere; Spectroscopy; Atmospheres, chemistry ID UPPER-ATMOSPHERE; OPTICAL-CONSTANTS; THOLINS; HAZE; SPECTROSCOPY; SPECTRA AB We present results on the formation of Titan aerosol analogs produced via far-UV irradiation of five aromatic precursors: benzene, naphthalene, pyridine, quinoline and isoquinoline. This is the first reported evidence of far-IR emission features observed below 200 cm(-1) in laboratory-created Titan aerosols. These laboratory studies were motivated by recent analyses of Cassini Composite Infrared Spectrometer (CIRS) spectra that show a broad aerosol emission feature in the far-IR spectral region centered near 140 cm(-1), which is unique to Titan's photochemically-produced aerosol (Anderson, C.M., Samuelson, R.E. [2011]. Icarus 212, 762-778). We find that all three of the aerosol analogs formed from nitrogen-containing aromatics have similar broad emission features near that of the observed CIRS far-IR aerosol spectral feature. In addition, the inclusion of 1.5% methane to that of trace amounts of benzene also gives rise to an aerosol with a weak far-IR emission feature located below 200 cm(-1). (c) 2014 Elsevier Inc. All rights reserved. C1 [Sebree, Joshua A.] Univ No Iowa, Dept Chem & Biochem, Cedar Falls, IA 50614 USA. [Sebree, Joshua A.; Trainer, Melissa G.; Loeffler, Mark J.; Anderson, Carrie M.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. RP Sebree, JA (reprint author), Univ No Iowa, Dept Chem & Biochem, Cedar Falls, IA 50614 USA. EM joshua.sebree@uni.edu RI Trainer, Melissa/E-1477-2012; Loeffler, Mark/C-9477-2012 FU National Aeronautics and Space Administration issued through the Planetary Atmospheres Program [10-PATM10-0027]; NASA Postdoctoral Program at the Goddard Space Flight Center FX This work was supported by the National Aeronautics and Space Administration under Grant 10-PATM10-0027 issued through the Planetary Atmospheres Program. J.A.S. 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 21 TC 6 Z9 6 U1 2 U2 14 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 JUL 1 PY 2014 VL 236 BP 146 EP 152 DI 10.1016/j.icarus.2014.03.039 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH9QR UT WOS:000336477400014 ER PT J AU Murray, CD Cooper, NJ Williams, GA Attree, NO Boyer, JS AF Murray, Carl D. Cooper, Nicholas J. Williams, Gareth A. Attree, Nicholas O. Boyer, Jeffrey S. TI The discovery and dynamical evolution of an object at the outer edge of Saturn's A ring SO ICARUS LA English DT Article DE Saturn,rings; Satellites,dynamics; Resonances,orbital ID MASSIVE RINGS; A-RING; SATELLITES; PROPELLERS; MOONLETS; MOONS AB We report on the serendipitous discovery of an unresolved, evolving, sub-km-radius object with a semimajor axis <10 km inside that of the edge of Saturn's main rings. The object has been detectable in Cassini images since at least May 2012 and its changing orbit shows evidence of a possible disruption in early 2013. (C) 2014 Elsevier Inc. All rights reserved. C1 [Murray, Carl D.; Cooper, Nicholas J.; Williams, Gareth A.; Attree, Nicholas O.] Queen Mary Univ London, Astron Unit, London E1 4NS, England. [Boyer, Jeffrey S.] CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA. RP Murray, CD (reprint author), Queen Mary Univ London, Astron Unit, Mile End Rd, London E1 4NS, England. EM C.D.Murray@qmul.ac.uk FU Science and Technology Facilities Council [ST/F007566/1]; Leverhulme Trust FX This work was supported by the Science and Technology Facilities Council (Grant No. ST/F007566/1) and we are grateful to them for financial assistance. C.D.M. is also grateful to the Leverhulme Trust for the award of a Research Fellowship. The authors thank Jenya Morrice for her help with the image analysis as well as Matthew Hedman and Matthew Tiscareno for useful discussions. We are also grateful to NASA and members of the Cassini project for their help. The original manuscript was considerably improved by helpful comments from Aurelien Crida and Sebastien Charnoz. NR 17 TC 3 Z9 3 U1 1 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUL 1 PY 2014 VL 236 BP 165 EP 168 DI 10.1016/j.icarus.2014.03.024 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH9QR UT WOS:000336477400017 ER PT J AU Hunt, RD Hickman, RR Ladd-Lively, JL Anderson, KK Collins, RT Collins, JL AF Hunt, R. D. Hickman, R. R. Ladd-Lively, J. L. Anderson, K. K. Collins, R. T. Collins, J. L. TI Production of small uranium dioxide microspheres for cermet nuclear fuel using the internal gelation process SO ANNALS OF NUCLEAR ENERGY LA English DT Article DE Internal gelation; Uranium oxide microspheres; Cermet fuel AB The U.S. National Aeronautics and Space Administration (NASA) is developing a uranium dioxide (UO2)/(tungsten cermet fuel for potential use as the nuclear cryogenic propulsion stage (NCPS). The first generation NCPS is expected to be made from dense UO2 microspheres with diameters between 75 and 150 mu m. Previously, the internal gelation process and a hood-scale apparatus with a vibrating nozzle were used to form gel spheres, which became UO2 kernels with diameters between 350 and 850 mu m. For the NASA spheres, the vibrating nozzle was replaced with a custom designed, two-fluid nozzle to produce gel spheres in the desired smaller size range. This paper describes the operational methodology used to make 3 kg of uranium oxide (UOx) microspheres. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Hunt, R. D.; Ladd-Lively, J. L.; Anderson, K. K.; Collins, R. T.; Collins, J. L.] Oak Ridge Natl Lab, Oak Ridge, TN 37831 USA. [Hickman, R. R.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35802 USA. RP Hunt, RD (reprint author), Oak Ridge Natl Lab, POB 2008, Oak Ridge, TN 37831 USA. EM huntrd@ornl.gov RI Ladd-Lively, Jennifer/I-6305-2016 OI Ladd-Lively, Jennifer/0000-0001-9353-675X NR 18 TC 3 Z9 3 U1 2 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0306-4549 J9 ANN NUCL ENERGY JI Ann. Nucl. Energy PD JUL PY 2014 VL 69 BP 139 EP 143 DI 10.1016/j.anucene.2014.02.003 PG 5 WC Nuclear Science & Technology SC Nuclear Science & Technology GA AG0LR UT WOS:000335107500018 ER PT J AU Benafan, O Garg, A Noebe, RD Bigelow, GS Padula, SA Gaydosh, DJ Schell, N Mabe, JH Vaidyanathan, R AF Benafan, O. Garg, A. Noebe, R. D. Bigelow, G. S. Padula, S. A., II Gaydosh, D. J. Schell, N. Mabe, J. H. Vaidyanathan, R. TI Mechanical and functional behavior of a Ni-rich Ni50.3Ti29.7Hf20 high temperature shape memory alloy SO INTERMETALLICS LA English DT Article DE Shape-memory effects; Diffraction; Precipitates; Phase transformation; Intermetallics; Mechanical testing ID MICROSTRUCTURE; TRANSFORMATION; TEXTURE AB The mechanical and functional behaviors of a Ni-rich Ni50.3Ti29.7Hf20 high temperature shape memory alloy were investigated through combined ex situ macroscopic experiments and in situ synchrotron X-ray diffraction. Isothermal tension and compression tests were conducted between room temperature and 260 C, while isobaric thermomechanical cycling experiments were conducted at selected stresses up to 700 MPa. Isothermal testing of the martensite phase revealed no plastic strain up to the test limit of 1 GPa and near-perfect superelastic behavior up to 3% applied strain at temperatures above the austenite finish. Excellent dimensional stability with greater than 2.5% actuation strain without accumulation of noticeable residual strains (at stresses less than or equal to -400 MPa) were observed during isobaric thermal cycling experiments. The absence of residual strain accumulation during thermomechanical cycling was confirmed by the lattice strains, determined from X-ray spectra. Even in the untrained condition, the material exhibited little or no history or path dependence in behavior, consistent with measurements of the bulk texture after thermomechanical cycling using synchrotron X-ray diffraction. Post deformation cycling revealed the limited conditions under which a slight two-way shape memory effect (TWSME) was obtained, with a maximum of 0.34% two-way shape memory strain after thermomechanical cycling under -700 MPa. Published by Elsevier Ltd. C1 [Benafan, O.; Garg, A.; Noebe, R. D.; Bigelow, G. S.; Padula, S. A., II; Gaydosh, D. J.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. [Garg, A.] Univ Toledo, Toledo, OH 43606 USA. [Gaydosh, D. J.] Ohio Aerosp Inst, Cleveland, OH 44142 USA. [Schell, N.] Helmholtz Zentrum Geesthacht, Inst Mat Res, D-21502 Geesthacht, Germany. [Mabe, J. H.] Boeing Co, Seattle, WA 98124 USA. [Vaidyanathan, R.] Univ Cent Florida, Dept Mat Sci & Engn, Adv Mat Proc & Anal Ctr, Orlando, FL 32816 USA. RP Benafan, O (reprint author), NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. EM othmane.benafan@nasa.gov FU NASA Fundamental Aeronautics Program, Aeronautical Sciences Project; [NNX08AB51A] FX Funding from the NASA Fundamental Aeronautics Program, Aeronautical Sciences Project is gratefully acknowledged. Grant NNX08AB51A to UCF is gratefully acknowledged. The authors thank A. Stark for technical support with the diffraction experiments. This work has greatly benefited from the use of the HEMS beamline at the German high-brilliance synchrotron radiation storage ring PETRA III on DESY. NR 27 TC 20 Z9 20 U1 5 U2 32 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0966-9795 EI 1879-0216 J9 INTERMETALLICS JI Intermetallics PD JUL PY 2014 VL 50 BP 94 EP 107 DI 10.1016/j.intermet.2014.02.006 PG 14 WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering GA AF8UF UT WOS:000334990400013 ER PT J AU Ryan, DF O'Flannagain, AM Aschwanden, MJ Gallagher, PT AF Ryan, Daniel F. O'Flannagain, Aidan M. Aschwanden, Markus J. Gallagher, Peter T. TI The Compatibility of Flare Temperatures Observed with AIA, GOES, and RHESSI SO SOLAR PHYSICS LA English DT Article DE Sun: corona; Sun: EUV; Sun: flares ID CLASS SOLAR-FLARES; HARD X-RAYS; MULTIWAVELENGTH OBSERVATIONS; SPATIOTEMPORAL EVOLUTION; EMISSION MEASURE; SCALING LAWS; EXPRESSIONS; DYNAMICS; EVENTS; PLASMA AB We test the compatibility and biases of multi-thermal flare DEM (differential emission measure) peak temperatures determined with AIA with those determined by GOES and RHESSI using the isothermal assumption. In a set of 149 M- and X-class flares observed during the first two years of the SDO mission, AIA finds DEM peak temperatures at the time of the peak GOES 1 -aEuro parts per thousand 8 flux to have an average of T (p)=12.0 +/- 2.9 MK and Gaussian DEM widths of log(10)(sigma (T) )=0.50 +/- 0.13. From GOES observations of the same 149 events, a mean temperature of T (p)=15.6 +/- 2.4 MK is inferred, which is systematically higher by a factor of T (GOES)/T (AIA)=1.4 +/- 0.4. We demonstrate that this discrepancy results from the isothermal assumption in the inversion of the GOES filter ratio. From isothermal fits to photon spectra at energies of I mu a parts per thousand 6 -aEuro parts per thousand 12 keV of 61 of these events, RHESSI finds the temperature to be higher still by a factor of T (RHESSI)/T (AIA)=1.9 +/- 1.0. We find that this is partly a consequence of the isothermal assumption. However, RHESSI is not sensitive to the low-temperature range of the DEM peak, and thus RHESSI samples only the high-temperature tail of the DEM function. This can also contribute to the discrepancy between AIA and RHESSI temperatures. The higher flare temperatures found by GOES and RHESSI imply correspondingly lower emission measures. We conclude that self-consistent flare DEM temperatures and emission measures require simultaneous fitting of EUV (AIA) and soft X-ray (GOES and RHESSI) fluxes. C1 [Ryan, Daniel F.; O'Flannagain, Aidan M.; Gallagher, Peter T.] Univ Dublin Trinity Coll, Sch Phys, Dublin 2, Ireland. [Ryan, Daniel F.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Solar Phys Lab Code 671, Greenbelt, MD 20771 USA. [Ryan, Daniel F.] Catholic Univ Amer, Washington, DC 20064 USA. [Aschwanden, Markus J.] Lockheed Martin Adv Technol Ctr, Dept A021S, Solar & Astrophys Lab, Palo Alto, CA 94304 USA. RP Aschwanden, MJ (reprint author), Lockheed Martin Adv Technol Ctr, Dept A021S, Solar & Astrophys Lab, Bldg 252,3251 Hanover St, Palo Alto, CA 94304 USA. EM aschwanden@lmsal.com RI Gallagher, Peter/C-7717-2011 OI Gallagher, Peter/0000-0001-9745-0400 FU NASA of the SDO/AIA instrument [NNG04EA00C]; Fulbright Association; Irish Research Council; Catholic University of America FX The authors would like to thank the following for supporting this research: NASA (contract NNG04EA00C of the SDO/AIA instrument to LMSAL), the Fulbright Association, Catholic University of America, and the Irish Research Council. Thanks must also go to Richard A. Schwartz for his helpful discussions. NR 28 TC 11 Z9 11 U1 0 U2 6 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 JUL PY 2014 VL 289 IS 7 BP 2547 EP 2563 DI 10.1007/s11207-014-0492-z PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE7TI UT WOS:000334201400009 ER PT J AU De Pontieu, B Title, AM Lemen, JR Kushner, GD Akin, DJ Allard, B Berger, T Boerner, P Cheung, M Chou, C Drake, JF Duncan, DW Freeland, S Heyman, GF Hoffman, C Hurlburt, NE Lindgren, RW Mathur, D Rehse, R Sabolish, D Seguin, R Schrijver, CJ Tarbell, TD Wulser, JP Wolfson, CJ Yanari, C Mudge, J Nguyen-Phuc, N Timmons, R van Bezooijen, R Weingrod, I Brookner, R Butcher, G Dougherty, B Eder, J Knagenhjelm, V Larsen, S Mansir, D Phan, L Boyle, P Cheimets, PN DeLuca, EE Golub, L Gates, R Hertz, E McKillop, S Park, S Perry, T Podgorski, WA Reeves, K Saar, S Testa, P Tian, H Weber, M Dunn, C Eccles, S Jaeggli, SA Kankelborg, CC Mashburn, K Pust, N Springer, L Carvalho, R Kleint, L Marmie, J Mazmanian, E Pereira, TMD Sawyer, S Strong, J Worden, SP Carlsson, M Hansteen, VH Leenaarts, J Wiesmann, M Aloise, J Chu, KC Bush, RI Scherrer, PH Brekke, P Martinez-Sykora, J Lites, BW McIntosh, SW Uitenbroek, H Okamoto, TJ Gummin, MA Auker, G Jerram, P Pool, P Waltham, N AF De Pontieu, B. Title, A. M. Lemen, J. R. Kushner, G. D. Akin, D. J. Allard, B. Berger, T. Boerner, P. Cheung, M. Chou, C. Drake, J. F. Duncan, D. W. Freeland, S. Heyman, G. F. Hoffman, C. Hurlburt, N. E. Lindgren, R. W. Mathur, D. Rehse, R. Sabolish, D. Seguin, R. Schrijver, C. J. Tarbell, T. D. Wuelser, J. -P. Wolfson, C. J. Yanari, C. Mudge, J. Nguyen-Phuc, N. Timmons, R. van Bezooijen, R. Weingrod, I. Brookner, R. Butcher, G. Dougherty, B. Eder, J. Knagenhjelm, V. Larsen, S. Mansir, D. Phan, L. Boyle, P. Cheimets, P. N. DeLuca, E. E. Golub, L. Gates, R. Hertz, E. McKillop, S. Park, S. Perry, T. Podgorski, W. A. Reeves, K. Saar, S. Testa, P. Tian, H. Weber, M. Dunn, C. Eccles, S. Jaeggli, S. A. Kankelborg, C. C. Mashburn, K. Pust, N. Springer, L. Carvalho, R. Kleint, L. Marmie, J. Mazmanian, E. Pereira, T. M. D. Sawyer, S. Strong, J. Worden, S. P. Carlsson, M. Hansteen, V. H. Leenaarts, J. Wiesmann, M. Aloise, J. Chu, K. -C. Bush, R. I. Scherrer, P. H. Brekke, P. Martinez-Sykora, J. Lites, B. W. McIntosh, S. W. Uitenbroek, H. Okamoto, T. J. Gummin, M. A. Auker, G. Jerram, P. Pool, P. Waltham, N. TI The Interface Region Imaging Spectrograph (IRIS) SO SOLAR PHYSICS LA English DT Article DE Heating, chromospheric; Heating, coronal; Chromosphere, models; Chromosphere, active; Corona, active; Magnetic fields, chromosphere; Instrumentation and data management; Spectrum, ultraviolet ID MG-II-H; FARLEY-BUNEMAN INSTABILITY; DYNAMICS-OBSERVATORY SDO; SOLAR CORONA; K-LINES; ACTIVE-REGION; ALFVEN WAVES; SPECTROSCOPIC OBSERVATIONS; OSO-8 OBSERVATIONS; PROPAGATING WAVES AB The Interface Region Imaging Spectrograph (IRIS) small explorer spacecraft provides simultaneous spectra and images of the photosphere, chromosphere, transition region, and corona with 0.33 -aEuro parts per thousand 0.4 arcsec spatial resolution, two-second temporal resolution, and 1 km s(-1) velocity resolution over a field-of-view of up to 175 arcsec x 175 arcsec. IRIS was launched into a Sun-synchronous orbit on 27 June 2013 using a Pegasus-XL rocket and consists of a 19-cm UV telescope that feeds a slit-based dual-bandpass imaging spectrograph. IRIS obtains spectra in passbands from 1332 -aEuro parts per thousand 1358 , 1389 -aEuro parts per thousand 1407 , and 2783 -aEuro parts per thousand 2834 , including bright spectral lines formed in the chromosphere (Mg ii h 2803 and Mg ii k 2796 ) and transition region (C ii 1334/1335 and Si iv 1394/1403 ). Slit-jaw images in four different passbands (C ii 1330, Si iv 1400, Mg ii k 2796, and Mg ii wing 2830 ) can be taken simultaneously with spectral rasters that sample regions up to 130 arcsec x 175 arcsec at a variety of spatial samplings (from 0.33 arcsec and up). IRIS is sensitive to emission from plasma at temperatures between 5000 K and 10 MK and will advance our understanding of the flow of mass and energy through an interface region, formed by the chromosphere and transition region, between the photosphere and corona. This highly structured and dynamic region not only acts as the conduit of all mass and energy feeding into the corona and solar wind, it also requires an order of magnitude more energy to heat than the corona and solar wind combined. The IRIS investigation includes a strong numerical modeling component based on advanced radiative-MHD codes to facilitate interpretation of observations of this complex region. Approximately eight Gbytes of data (after compression) are acquired by IRIS each day and made available for unrestricted use within a few days of the observation. C1 [De Pontieu, B.; Title, A. M.; Lemen, J. R.; Kushner, G. D.; Akin, D. J.; Allard, B.; Berger, T.; Boerner, P.; Cheung, M.; Chou, C.; Drake, J. F.; Duncan, D. W.; Freeland, S.; Heyman, G. F.; Hoffman, C.; Hurlburt, N. E.; Lindgren, R. W.; Mathur, D.; Rehse, R.; Sabolish, D.; Seguin, R.; Schrijver, C. J.; Tarbell, T. D.; Wuelser, J. -P.; Wolfson, C. J.; Yanari, C.; Martinez-Sykora, J.] Lockheed Martin Adv Technol Ctr, Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [De Pontieu, B.; Pereira, T. M. D.; Carlsson, M.; Hansteen, V. H.; Leenaarts, J.; Wiesmann, M.] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway. [Berger, T.; Uitenbroek, H.] Natl Solar Observ, Sunspot, NM 88349 USA. [Mudge, J.; Nguyen-Phuc, N.; Timmons, R.; van Bezooijen, R.; Weingrod, I.] Lockheed Martin Adv Technol Ctr, Palo Alto, CA 94304 USA. [Brookner, R.; Butcher, G.; Dougherty, B.; Eder, J.; Knagenhjelm, V.; Larsen, S.; Mansir, D.; Phan, L.; Boyle, P.] Lockheed Martin, Sunnyvale, CA 94089 USA. [Cheimets, P. N.; DeLuca, E. E.; Golub, L.; Gates, R.; Hertz, E.; McKillop, S.; Park, S.; Perry, T.; Podgorski, W. A.; Reeves, K.; Saar, S.; Testa, P.; Tian, H.; Weber, M.] Harvard Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Dunn, C.; Eccles, S.; Jaeggli, S. A.; Kankelborg, C. C.; Mashburn, K.; Pust, N.; Springer, L.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Carvalho, R.; Kleint, L.; Marmie, J.; Mazmanian, E.; Pereira, T. M. D.; Sawyer, S.; Strong, J.; Worden, S. P.] NASA, Ames Res Ctr, Moffett Field, CA 94305 USA. [Kleint, L.; Martinez-Sykora, J.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Aloise, J.; Chu, K. -C.; Bush, R. I.; Scherrer, P. H.] Stanford Univ, WW Hansen Expt Phys Lab, Ctr Space Sci & Astrophys, Stanford, CA 94305 USA. [Brekke, P.] Norwegian Space Ctr, N-0212 Oslo, Norway. [Lites, B. W.; McIntosh, S. W.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Okamoto, T. J.] ISAS JAXA, Sagamihara, Kanagawa 2525210, Japan. [Gummin, M. A.] Alias Aerosp Inc, St Helena, CA 94584 USA. [Auker, G.; Jerram, P.; Pool, P.] E2v Technol, Chelmsford CM1 2QU, Essex, England. [Waltham, N.] Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. RP De Pontieu, B (reprint author), Lockheed Martin Adv Technol Ctr, Lockheed Martin Solar & Astrophys Lab, Org A021S,Bldg 252,3251 Hanover St, Palo Alto, CA 94304 USA. EM bdp@lmsal.com RI Pereira, Tiago/G-4079-2014; Reeves, Katharine/P-9163-2014; DeLuca, Edward/L-7534-2013; OI Pereira, Tiago/0000-0003-4747-4329; DeLuca, Edward/0000-0001-7416-2895; Leenaarts, Jorrit/0000-0003-4936-4211 FU NASA [NNG09FA40C]; Lockheed Martin Independent Research Program; Norwegian Space Centre (NSC) through an ESA PRODEX contract FX The effort required to build a mission such as IRIS requires a large, skillful, and dedicated team. We wish to acknowledge many individuals who contributed to the success of IRIS: Geoff Andrews, Nate Caditan, Brock Carpenter, Jay Dusenbury, Cliff Evans, Chuck Fischer, Scott Green, George Dankiewicz, Robert Honeycutt, James Irwin, Harjeet Janda, Dwana Kacensky, Pete Kacensky, Noah Katz, Mike Marticorena, Mark Ridley, John Serafin, David Schiff, Richard Shine, Araya Silpikul, Greg Slater, Shanti Varaitch, Leah Wang, Ross Yamamoto and Kent Zikuhr (Lockheed Martin). We are grateful to Mats Lofdahl for providing his IDL phase-diversity code and teaching us how to use it. We would like to thank Nicholas Chrissotimos, Gregory Frazier, Eric Ianson, Christine Hinkle, and Valerie Mackritis from the NASA GSFC Explorers Office for their support throughout the entire IRIS mission. We would also like to thank Jeff Newmark, Joseph Davila, and Adrian Daw at NASA for their support and encouragement. This work is supported by NASA under contract NNG09FA40C and the Lockheed Martin Independent Research Program. The data downlink to Svalbard is funded by the Norwegian Space Centre (NSC) through an ESA PRODEX contract. We would like to thank Bo Andersen for his efforts in making the NSC downlink support possible. NR 82 TC 235 Z9 235 U1 2 U2 17 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD JUL PY 2014 VL 289 IS 7 BP 2733 EP 2779 DI 10.1007/s11207-014-0485-y PG 47 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AE7TI UT WOS:000334201400020 ER PT J AU Cantrell, JH AF Cantrell, John H. TI Elastic constants of solids and fluids with initial pressure via a unified approach based on equations-of-state SO ULTRASONICS LA English DT Article DE Elastic constants; Fluids; Solids; Nonlinearity parameters; Initial pressure ID ACOUSTIC-RADIATION STRESS; FINITE-AMPLITUDE WAVES; NONLINEARITY PARAMETERS AB The second and third-order Brugger elastic constants are obtained for liquids and ideal gases having an initial hydrostatic pressure p(1). For liquids the second-order elastic constants are C-11 = A + p(1), C-12 = A - p(1), and the third-order constants are C-111 = - (B + 5A + 3p(1)), C-112 = - (B + A - p(1)), and C-123 = A - B - p(1), where A and B are the Beyer expansion coefficients in the liquid equation of state. For ideal gases the second-order constants are C-11 = p(1)gamma + p(1), C-12 = p(1)gamma - p(1), and the third-order constants are C-111 = - p(1)(gamma(2) + 4 gamma + 3), C-112 = -p(1)(gamma(2) - 1), and C-123 = -p(1) (gamma(2) - 2 gamma + 1), where c is the ratio of specific heats. The inequality of C-11 and C-12 results in a nonzero shear constant C-44 = (1/2)(C-11 - C-12) = p(1) for both liquids and gases. For water at standard temperature and pressure the ratio of terms p(1)/A contributing to the second-order constants is approximately 4.3 - 10(-5). For atmospheric gases the ratio of corresponding terms is approximately 0.7. Analytical expressions that include initial stresses are derived for the material 'nonlinearity parameters' associated with harmonic generation and acoustoelasticity for fluids and solids of arbitrary crystal symmetry. The expressions are used to validate the relationships for the elastic constants of fluids. Published by Elsevier B. V. C1 NASA Langley Res Ctr, Res Directorate, Hampton, VA 23681 USA. RP Cantrell, JH (reprint author), NASA Langley Res Ctr, Res Directorate, Hampton, VA 23681 USA. EM john.h.cantrell@nasa.gov NR 40 TC 2 Z9 2 U1 0 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0041-624X EI 1874-9968 J9 ULTRASONICS JI Ultrasonics PD JUL PY 2014 VL 54 IS 5 BP 1323 EP 1331 DI 10.1016/j.ultras.2014.01.012 PG 9 WC Acoustics; Radiology, Nuclear Medicine & Medical Imaging SC Acoustics; Radiology, Nuclear Medicine & Medical Imaging GA AE1XK UT WOS:000333766300024 PM 24502870 ER PT J AU Ni, WJ Sun, GQ Ranson, KJ Zhang, ZY He, YT Huang, WL Guo, ZF AF Ni, Wenjian Sun, Guoqing Ranson, Kenneth Jon Zhang, Zhiyu He, Yating Huang, Wenli Guo, Zhifeng TI Model-Based Analysis of the Influence of Forest Structures on the Scattering Phase Center at L-Band SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Canopy height; depth of scattering phase center (DSPC); forest structure; height of scattering phase center (HSPC); interferometric synthetic aperture radar (InSAR) ID INTERFEROMETRIC SAR; RADAR BACKSCATTER; BOREAL FOREST; P-BAND; HEIGHT; INVERSION; CANOPIES AB The estimation of forest biomass from synthetic aperture radar (SAR) data is limited by the lack of forest structure information. Interferometric synthetic aperture radar (InSAR) provides a means for the extraction of forest structure. The crucial issue in InSAR application is to parameterize forest structure and to link the parameter with InSAR observations. Model-based analysis enables exploring the theoretical linkages between InSAR observations and forest structure free from temporal decorrelation effects. In this paper, a semicoherent model (SCSR) was first developed and verified. A series of simulations at L-band was then made for both homogeneous and heterogeneous forests generated from a forest growth model. The forest structure was parameterized by four height indices. Aside from the height of scattering phase center (HSPC), the depth of scattering phase center (DSPC) was also proposed to characterize the scattering phase center of InSAR. The results showed that the behavior of homogeneous forest on InSAR data was quite different from that of heterogeneous forest. Special care was needed when the retrieval algorithms of forest biomass developed on a homogeneous forest were applied to a heterogeneous forest. Crown size-weighted height (CWH) and Lorey's height were correlated with the HSPC at all polarizations and with the DSPC at copolarization in both cases of homogeneous and heterogeneous forests. These findings indicated that CWH could be an alternative biomass indicator of the Lorey's height for biomass estimation, which can be derived from the combination of InSAR data and the elevation of the forest canopy top from lidar or high-resolution stereo images. C1 [Ni, Wenjian; Zhang, Zhiyu; Guo, Zhifeng] Chinese Acad Sci, Inst Remote Sensing & Digital Earth, State Key Lab Remote Sensing Sci, Beijing 100101, Peoples R China. [Ni, Wenjian; Zhang, Zhiyu; Guo, Zhifeng] Beijing Normal Univ, Beijing 100101, Peoples R China. [Sun, Guoqing; Huang, Wenli] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Ranson, Kenneth Jon] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [He, Yating] Chinese Acad Agr Sci, Inst Agr Resources & Reg Planning, Beijing 100081, Peoples R China. RP Zhang, ZY (reprint author), Chinese Acad Sci, Inst Remote Sensing & Digital Earth, State Key Lab Remote Sensing Sci, Beijing 100101, Peoples R China. EM zhangzy@irsa.ac.cn RI rslab, hiwater/O-7037-2015; Ranson, Kenneth/G-2446-2012; rslab, water/O-7043-2015 OI Ranson, Kenneth/0000-0003-3806-7270; FU National Basic Research Program of China [2013CB733404]; National Natural Science Foundation of China [41001208, 40971203, 41171283, 91125003]; National High-Tech R&D Program of China [2012AA12A306]; Strategic Priority Research Program-Climate Change: Carbon Budget and Related Issues of the Chinese Academy of Sciences [XDA05050100]; Terrestrial Ecology Program [NNX09AG66G] FX This work was supported in part by the National Basic Research Program of China under Grant 2013CB733404, by the National Natural Science Foundation of China under Grants 41001208, 40971203, 41171283, and 91125003, by the National High-Tech R&D Program of China under Grant 2012AA12A306, by the Strategic Priority Research Program-Climate Change: Carbon Budget and Related Issues of the Chinese Academy of Sciences under Grant XDA05050100, and by the Terrestrial Ecology Program under Grant NNX09AG66G. NR 23 TC 3 Z9 3 U1 0 U2 30 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 JUL PY 2014 VL 52 IS 7 BP 3937 EP 3946 DI 10.1109/TGRS.2013.2278171 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 AC5YO UT WOS:000332597100016 ER PT J AU Kuze, A Taylor, TE Kataoka, F Bruegge, CJ Crisp, D Harada, M Helmlinger, M Inoue, M Kawakami, S Kikuchi, N Mitomi, Y Murooka, J Naitoh, M O'Brien, DM O'Dell, CW Ohyama, H Pollock, H Schwandner, FM Shiomi, K Suto, H Takeda, T Tanaka, T Urabe, T Yokota, T Yoshida, Y AF Kuze, Akihiko Taylor, Thomas E. Kataoka, Fumie Bruegge, Carol J. Crisp, David Harada, Masatomo Helmlinger, Mark Inoue, Makoto Kawakami, Shuji Kikuchi, Nobuhiro Mitomi, Yasushi Murooka, Jumpei Naitoh, Masataka O'Brien, Denis M. O'Dell, Christopher W. Ohyama, Hirofumi Pollock, Harold Schwandner, Florian M. Shiomi, Kei Suto, Hiroshi Takeda, Toru Tanaka, Tomoaki Urabe, Tomoyuki Yokota, Tatsuya Yoshida, Yukio TI Long-Term Vicarious Calibration of GOSAT Short-Wave Sensors: Techniques for Error Reduction and New Estimates of Radiometric Degradation Factors SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Carbon dioxide (CO2); Greenhouse gases Observing SATellite (GOSAT); short-wave infrared (SWIR); Thermal And Near infrared Sensor for carbon Observations (TANSO); vicarious calibration ID GASES OBSERVING SATELLITE; CO2 RETRIEVAL ALGORITHM; MODELS; TANSO AB This work describes the radiometric calibration of the short-wave infrared (SWIR) bands of two instruments aboard the Greenhouse gases Observing SATellite (GOSAT), the Thermal And Near infrared Sensor for carbon Observations Fourier Transform Spectrometer (TANSO-FTS) and the Cloud and Aerosol Imager (TANSO-CAI). Four vicarious calibration campaigns (VCCs) have been performed annually since June 2009 at Railroad Valley, NV, USA, to estimate changes in the radiometric response of both sensors. While the 2009 campaign (VCC2009) indicated significant initial degradation in the sensors compared to the prelaunch values, the results presented here show that the stability of the sensors has improved with time. The largest changes were seen in the 0.76 mu m oxygen A-band for TANSO-FTS and in the 0.380 and 0.674 mu m bands for TANSO-CAI. This paper describes techniques used to optimize the vicarious calibration of the GOSAT SWIR sensors. We discuss error reductions, relative to previous work, achieved by using higher quality and more comprehensive in situ measurements and proper selection of reference remote sensing products from the Moderate Resolution Imaging Spectroradiometer used in radiative transfer calculations to model top-of-the-atmosphere radiances. In addition, we present new estimates of TANSO-FTS radiometric degradation factors derived by combining the new vicarious calibration results with the time-dependent model provided by Yoshida et al. (2012), which is based on analysis of on-board solar diffuser data. We conclude that this combined model provides a robust correction for TANSO-FTS Level 1B spectra. A detailed error budget for TANSO-FTS vicarious calibration is also provided. C1 [Kuze, Akihiko; Harada, Masatomo; Kawakami, Shuji; Murooka, Jumpei; Naitoh, Masataka; Ohyama, Hirofumi; Shiomi, Kei; Suto, Hiroshi; Takeda, Toru; Tanaka, Tomoaki; Urabe, Tomoyuki] Japan Aerosp Explorat Agcy, Tsukuba, Ibaraki 3058505, Japan. [Taylor, Thomas E.; O'Brien, Denis M.] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA. [Kataoka, Fumie; Mitomi, Yasushi] Remote Sensing Technol Ctr Japan, Tsukuba, Ibaraki 3050032, Japan. [Bruegge, Carol J.; Crisp, David; Helmlinger, Mark; Pollock, Harold; Schwandner, Florian M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Inoue, Makoto; Kikuchi, Nobuhiro; Yokota, Tatsuya; Yoshida, Yukio] Natl Inst Environm Studies, Tsukuba, Ibaraki 3058506, Japan. [O'Dell, Christopher W.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. RP Kuze, A (reprint author), Japan Aerosp Explorat Agcy, Tsukuba, Ibaraki 3058505, Japan. EM kuze.akihiko@jaxa.jp RI Inoue, Makoto/M-8505-2014; KUZE, AKIHIKO/J-2074-2016; Schwandner, Florian/B-4027-2009 OI Inoue, Makoto/0000-0002-6826-5334; KUZE, AKIHIKO/0000-0001-5415-3377; Schwandner, Florian/0000-0002-0260-4727 FU NASA [1439002] FX The authors would like to thank two anonymous reviewers for providing helpful comments. The authors would also like to thank the following individuals for helping with the planning and measurements: N. Goto from the Japan Aerospace Exploration Agency; H. Tan and J. Laderos from the National Aeronautics and Space Administration (NASA)'s Jet Propulsion Laboratory (JPL); E. Yates, L. Iraci, M. Lowenstein, and E. Sheffner from NASA's Ames Research Team; and the H211 Alpha Team, consisting of pilots K. Ambrose, D. Simmons, and R. Simone and ground staff B. Quiambao, R. Fisher, and J. Lee. The authors would also like to thank V. Gandarillas from Purdue University; R. Rosenberg from the California Institute of Technology; R. O. Knuteson, J. Roman, and E. Garms from the University of Wisconsin; and K. Schiro from the University of California Los Angeles. The authors would also like to thank T. Matsunaga, A. Kamei, and the Level 2 Data Teams of the National Institute for Environmental Studies and Atmospheric Carbon Observations from Space (ACOS). Part of the research described here was carried out at JPL, California Institute of Technology, under a contract with NASA. The Colorado State University contributions to the ACOS task were supported by NASA Contract 1439002. NR 14 TC 15 Z9 15 U1 3 U2 22 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 JUL PY 2014 VL 52 IS 7 BP 3991 EP 4004 DI 10.1109/TGRS.2013.2278696 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 AC5YO UT WOS:000332597100021 ER PT J AU Hensley, S Oveisgharan, S Saatchi, S Simard, M Ahmed, R AF Hensley, Scott Oveisgharan, Shadi Saatchi, Sassan Simard, Marc Ahmed, Razi TI An Error Model for Biomass Estimates Derived From Polarimetric Radar Backscatter SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Backscatter error model; forest biomass; polarimetry; synthetic aperture radar (SAR) ID VEGETATION STRUCTURE; SAR AB Estimating the amount of above ground biomass in forested areas and the measurement of carbon flux through the quantification of disturbance and regrowth are critical to develop a better understanding of ecosystem processes. Well-resolved and globally consistent inventories of forest carbon must rely on remote sensing measurements, particularly from polarimetric radars. While a wide variety of studies conducted over the past three decades have shown how radar polarimetric measurements can be used to estimate above ground carbon for regions with less than 100 Mg of biomass per hectare, there is no established methodology for assessing biomass estimation accuracy based on a priori instrument and mission parameters. In this paper, a framework for assessing biomass estimation accuracy is presented that is a blend of the basic imaging physics and empirically derived parameters that describe various relationships between biomass and radar polarimetric observable quantities. The implications of this error model on the design and performance of a polarimetric radar are explored using instrument, mission, and science parameters from a notional Earth observing mission. C1 [Hensley, Scott; Oveisgharan, Shadi; Saatchi, Sassan; Simard, Marc; Ahmed, Razi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Hensley, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM shelsey@jpl.nasa.gov RI Simard, Marc/H-3516-2013 OI Simard, Marc/0000-0002-9442-4562 FU National Aeronautics and Space Administration FX This research was conducted at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 15 TC 4 Z9 4 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 JUL PY 2014 VL 52 IS 7 BP 4065 EP 4082 DI 10.1109/TGRS.2013.2279400 PG 18 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA AC5YO UT WOS:000332597100029 ER PT J AU Wang, ZP Xiong, XX Choi, TY Link, D AF Wang, Zhipeng Xiong, Xiaoxiong Choi, Taeyoung Link, Daniel TI On-Orbit Characterization of MODIS Modulation Transfer Function Using the Moon SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Calibration; edge spread function (ESF); MODerate resolution Imaging Spectroradiometer (MODIS); modulation transfer function (MTF); moon; spatial characterization ID CALIBRATION AB The high-contrast edge of the Moon has been used for the on-orbit measurement of the modulation transfer function (MTF) of remote sensing instruments with a lunar observation capability. With the lunar edge as a target, the classical edge method is applied to the National Aeronautics and Space Administration's MODerate resolution Imaging Spectroradiometer (MODIS) on board the Terra and Aqua satellites. One of the major difficulties encountered during the calculation is that the spatial resolution of MODIS is too coarse to capture the fine structure of the edge spread function (ESF), which is required to calculate the MTF. To produce the MODIS ESF in high resolution, lunar images of a selected edge acquired by multiple instrument scans need to be superposed by aligning the edge positions accurately. In this paper, an algorithm is developed to perform the alignment, based on the lunar position data generated by the MODIS geolocation algorithm and recorded scan by scan. The positions of the lunar edges at the focal plane are calculated scan by scan, allowing the construction of a high-quality ESF for MTF derivation. The algorithm is applied to all MODIS bands with 250-m, 500-m, and 1-km spatial resolutions in both along-scan and along-track directions. The along-track MTF results are particularly valuable because the onboard SpectroRadiometric Calibration Assembly can only monitor the along-scan MTF. The trending results show that the along-track MTF of MODIS has been stable throughout the MODIS lifetime and is well above the design specification for all bands. The limitation of the algorithm is analyzed. The algorithm developed in this paper can be applied to other instruments with similar design features. C1 [Wang, Zhipeng; Choi, Taeyoung; Link, Daniel] Sigma Space Corp, Lanham, MD 20706 USA. [Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wang, ZP (reprint author), Sigma Space Corp, Lanham, MD 20706 USA. EM zhipeng.wang@sigmaspace.com; XiaoxiongXiong-1@nasa.gov RI Choi, Taeyoung/E-4437-2016; OI Choi, Taeyoung/0000-0002-4596-989X; Wang, Zhipeng/0000-0002-9108-9009 NR 18 TC 6 Z9 9 U1 0 U2 12 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD JUL PY 2014 VL 52 IS 7 BP 4112 EP 4121 DI 10.1109/TGRS.2013.2279610 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 AC5YO UT WOS:000332597100033 ER PT J AU Utku, C Le Vine, DM AF Utku, Cuneyt Le Vine, David M. TI Topographic Signatures in Aquarius Radiometer and Scatterometer Response SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Aquarius; microwave radiometry; topography effects ID SOIL-MOISTURE; MICROWAVE EMISSION; SURFACE; SALINITY; MISSION; IMPACT; SMOS; SPACE AB Theory suggests that topography (large-scale roughness) will affect thermal emission at L-band and could impact remote sensing of surface parameters, such as soil moisture from space. Evidence is presented here for the existence of effects due to topography using data from the L-band radiometers and scatterometer aboard the recently launched Aquarius. The correlation with the slope standard deviation at the topographic scale is presented for data over North Africa and Australia. In the case of the radiometer, brightness temperature is observed to increase at horizontal polarization and decrease at vertical polarization. In the case of the scatterometer, an increase with topographic roughness is observed for both polarizations. The presence of the scatterometer provides an independent verification that the behavior observed is due to topography and the observations are consistent with predictions based on Monte Carlo simulations. C1 [Utku, Cuneyt] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Le Vine, David M.] NASA, Cryospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Utku, C (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 30 TC 2 Z9 2 U1 3 U2 11 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 JUL PY 2014 VL 52 IS 7 BP 4141 EP 4154 DI 10.1109/TGRS.2013.2280015 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 AC5YO UT WOS:000332597100035 ER PT J AU Jaruwatanadilok, S Stiles, BW AF Jaruwatanadilok, Sermsak Stiles, Bryan W. TI Trends and Variation in Ku-Band Backscatter of Natural Targets on Land Observed in QuikSCAT Data SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Calibration; natural target; QuikSCAT; scatterometer ID RADAR; SCATTEROMETER AB It has been well known that a few areas on the Earth's surface have a relatively constant backscattering coefficient and can serve as radar calibration targets. Examples include the Amazon rain forest, the Greenland ice sheet, parts of Antarctica, etc. However, there has not been any extensive investigation and quantitative evaluation of these targets in terms of their time variation, isotropy, and spatial variation. Here, we have analyzed a consistent set of Ku-band radar measurements for more than ten years from the QuikSCAT mission. This valuable set of data provides an unprecedented opportunity for us to study the long-term variability of observed backscattering from the Earth's surface at Ku-band. In this paper, we performed a global survey of potential constant land targets and evaluated their variability. Quantitative measurements of temporal and spatial variabilities (homogeneity) and isotropy are used to identify the locations of the best natural calibration targets. We also discuss annual and long-term trends in the data and offer potential explanations for these trends. We examine small regions with the least overall variation. By concentrating on low-variation areas, we can identify useful calibration targets for future radar missions and for intercalibration between existing radars. At the same time, by focusing on regions with little spatial or temporal heterogeneity, we can analyze the temporal variation on diurnal, seasonal, and decadal scales in homogenous natural terrain types including rain forest, dry brushy areas, and ice sheets. We found that rain forest targets in the Amazon and Congo are very stable in time and homogeneous. However, they are subjected to diurnal difference. On the other hand, the Antarctica ice sheet is another good candidate for stable target, but it has seasonal variability. The Greenland ice sheet shows a significant trend in backscatter in recent years, and therefore, may not be a suitable calibration site anymore. Another location for a good stable target is a dry brushy area in the Sahara, which shows comparable stability and isotropy with those of the Amazon, Congo, and Antarctica. C1 [Jaruwatanadilok, Sermsak; Stiles, Bryan W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Jaruwatanadilok, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM jaruwata@jpl.nasa.gov 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 11 TC 3 Z9 3 U1 0 U2 13 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 JUL PY 2014 VL 52 IS 7 BP 4383 EP 4390 DI 10.1109/TGRS.2013.2281722 PG 8 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA AC5YO UT WOS:000332597100054 ER PT J AU Prikryl, P Jayachandran, PT Mushini, SC Richardson, IG AF Prikryl, Paul Jayachandran, P. Thayyil Mushini, Sajan C. Richardson, Ian G. TI High-latitude GPS phase scintillation and cycle slips during high-speed solar wind streams and interplanetary coronal mass ejections: a superposed epoch analysis SO EARTH PLANETS AND SPACE LA English DT Article DE Ionosphere; Ionospheric irregularities; GPS scintillation; Solar wind disturbances; Space weather forecasting ID IONOSPHERIC SCINTILLATIONS; GEOMAGNETIC STORM; FLUCTUATIONS; PROPAGATION; CLIMATOLOGY; INDEX AB Results of a superposed epoch (SPE) analysis of occurrence of phase scintillation and cycle slips at high latitudes keyed by arrival times of high-speed solar wind streams (HSS) and interplanetary coronal mass ejections (ICME) for years 2008 to 2012 are presented. Phase scintillation index sigma(phi) is obtained in real time from L1 signal recorded at the rate of 50 Hz by specialized global positioning system (GPS) ionospheric scintillation and total electron content (TEC) monitors (GISTMs) deployed as a part of the Canadian High Arctic Ionospheric Network (CHAIN). The phase scintillation, mapped as a function of magnetic latitude and magnetic local time, occurs predominantly on the dayside in the cusp and in the nightside auroral oval. The scintillation occurrence peaks on days of HSS or ICME impacts at the Earth's magnetosphere and tapers off a few days later, which is similar to day-to-day variability of geomagnetic activity and riometer absorption at high latitudes. ICMEs that are identified as magnetic clouds are significantly more geoeffective than HSSs and ICMEs with no or weak magnetic cloud characteristics. On their arrival day, magnetic clouds result in higher occurrence, and thus probability, of scintillation in the nightside auroral zone. The SPE analysis results are used to obtain cumulative probability distribution functions for the phase scintillation occurrence that can be employed in probabilistic forecast of phase scintillation at high latitudes. C1 [Prikryl, Paul] Nat Resources Canada, Geomagnet Lab, Ottawa, ON K1A 0E7, Canada. [Jayachandran, P. Thayyil] Univ New Brunswick, Dept Phys, Fredericton, NB E3B 5A3, Canada. [Mushini, Sajan C.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Richardson, Ian G.] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Richardson, Ian G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Richardson, Ian G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Prikryl, P (reprint author), Nat Resources Canada, Geomagnet Lab, 2617 Anderson Rd, Ottawa, ON K1A 0E7, Canada. EM paul.prikryl@nrcan.gc.ca OI Richardson, Ian/0000-0002-3855-3634 FU Canada Foundation for Innovation; New Brunswick Innovation Foundation; Public Safety Geosciences program of the Natural Resources Canada, Earth Sciences Sector [20130496] FX Infrastructure funding for CHAIN was provided by the Canada Foundation for Innovation and the New Brunswick Innovation Foundation. CHAIN operation is conducted in collaboration with the Canadian Space Agency (CSA). The solar wind data were obtained from Goddard Space Flight Center Space Physics Data Facility OMNIWeb (http://omniweb.gsfc.nasa.gov/). This work was supported by the Public Safety Geosciences program of the Natural Resources Canada, Earth Sciences Sector (NRCan ESS Contribution Number 20130496). NR 36 TC 10 Z9 10 U1 0 U2 18 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1880-5981 J9 EARTH PLANETS SPACE JI Earth Planets Space PD JUN 30 PY 2014 VL 66 AR 62 DI 10.1186/1880-5981-66-62 PG 10 WC Geosciences, Multidisciplinary SC Geology GA AL9TY UT WOS:000339485900001 ER PT J AU Bhatia, AK AF Bhatia, A. K. TI D-wave electron-H, -He+, and -Li2+ elastic scattering and photoabsorption in P states of two-electron systems SO PHYSICAL REVIEW A LA English DT Article ID PHASE-SHIFTS; ACCURATE CALCULATION; POLARIZED ORBITALS; HYDROGEN; HELIUM; PHOTOIONIZATION; COLLISIONS; THRESHOLD AB In previous papers [A. K. Bhatia, Phys. Rev. A 85, 052708 (2012); 86, 032709 (2012); 87, 042705 (2013)] electron-H, -He+, and -Li2+ P-wave scattering phase shifts were calculated using the variational polarized orbital theory. This method is now extended to the singlet and triplet D-wave scattering in the elastic region. The long-range correlations are included in the Schrodinger equation by using the method of polarized orbitals variationally. Phase shifts are compared to those obtained by other methods. The present calculation provides results which are rigorous lower bonds to the exact phase shifts. Using the presently calculated D-wave and previously calculated S-wave continuum functions, photoionization of singlet and triplet P states of He and Li+ are also calculated, along with the radiative recombination rate coefficients at various electron temperatures. C1 NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP Bhatia, AK (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA. NR 22 TC 0 Z9 0 U1 2 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 JUN 30 PY 2014 VL 89 IS 6 AR 062720 DI 10.1103/PhysRevA.89.062720 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AL3RX UT WOS:000339047700010 ER PT J AU 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 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 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 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 Krishnan, B 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 Leonor, I 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 Martelli, F Martin, IW Martin, RM Martinelli, L Martynov, D Marx, JN Mason, K Masserot, A Massinger, TJ Matichard, F Matone, L Mavalvala, N May, G Mazumder, N Mazzolo, G McCarthy, R McClelland, DE McGuire, SC McIntyre, G McIver, J Mclin, K Meacher, D Meadors, GD Mehmet, M Meidam, J Meinders, M Melatos, A Mendell, G Mercer, RA Meshkov, S Messenger, C Meyer, MS Meyers, PM Mezzani, F Miao, H Michel, C Mikhailov, EE Milano, L Miller, J Minenkov, Y Mingarelli, CMF Mishra, C Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Moe, B Moggi, A Mohan, M Mohapatra, SRP Moraru, D Moreno, G Morgado, N Morriss, SR Mossavi, K Mours, B Mow-Lowry, CM Mueller, CL Mueller, G Mukherjee, S Mullavey, A Munch, J Murphy, D Murray, PG Mytidis, A Nagy, MF Nardecchia, I Naticchioni, L Nayak, RK Necula, V Nelemans, G Neri, I Neri, M Newton, G Nguyen, T Nielsen, AB Nissanke, S Nitz, AH Nocera, F Nolting, D Normandin, MEN Nuttall, LK Ochsner, E O'Dell, J Oelker, E Oh, JJ Oh, SH Ohme, F Omar, S Oppermann, P Oram, R O'Reilly, B Ortega, W O'Shaughnessy, R Osthelder, C Ottaway, DJ Ottens, RS Overmier, H Owen, BJ Padilla, C Pai, A Palashov, O Palomba, C Pan, H Pan, Y Pankow, C Paoletti, F Papa, MA Paris, H Pasqualetti, A Passaquieti, R Passuello, D Pedraza, M Pele, A Penn, S Perreca, A Phelps, M Pichot, M Pickenpack, M Piergiovanni, F Pierro, V Pinard, L Pinto, IM Pitkin, M Poeld, J Poggiani, R Poteomkin, A 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Van Heijningen, J. Van Veggel, A. A. Vass, S. Vasuth, M. Vaulin, R. Vecchio, A. Vedovato, G. Veitch, J. Veitch, P. J. Venkateswara, K. Verkindt, D. Vetrano, F. Vicere, A. Vincent-Finley, R. Vinet, J. -Y. Vitale, S. Vo, T. Vocca, H. Vorvick, C. Vousden, W. D. Vyachanin, S. P. Wade, A. R. Wade, L. Wade, M. Walker, M. Wallace, L. Walsh, S. 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. D. Williamson, A. R. Willis, J. L. Willke, B. Wimmer, M. Winkler, W. Wipf, C. C. Wiseman, A. G. Wittel, H. Woan, G. Wolovick, N. Worden, J. Wu, Y. Yablon, J. Yakushin, I. Yam, W. Yamamoto, H. Yancey, C. C. Yang, H. Yoshida, S. Yvert, M. Zadrozny, A. Zanolin, M. Zendri, J. -P. Zhang, Fan Zhang, L. Zhao, C. Zhu, H. Zhu, X. J. Zucker, M. E. Zuraw, S. Zweizig, J. Aptekar, R. L. Atteia, J. L. Cline, T. Connaughton, V. Frederiks, D. D. Golenetskii, S. V. Hurley, K. Krimm, H. A. Marisaldi, M. Pal'shin, V. D. Palmer, D. Svinkin, D. S. Terada, Y. Von Kienlin, A. CA LIGO Sci Collaboration Virgo Collaboration IPN Collaboration TI Search for Gravitational Waves Associated with gamma-ray Bursts Detected by the Interplanetary Network SO PHYSICAL REVIEW LETTERS LA English DT Article ID 25 APRIL 1998; SCIENCE RUN; SHORT-DURATION; GIANT FLARE; MASS-DISTRIBUTION; UNUSUAL SUPERNOVA; LIGO OBSERVATIONS; GRB 051103; REPEATER; REDSHIFT AB We present the results of a search for gravitational waves associated with 223 gamma-ray bursts (GRBs) detected by the InterPlanetary Network (IPN) in 2005-2010 during LIGO's fifth and sixth science runs and Virgo's first, second, and third science runs. The IPN satellites provide accurate times of the bursts and sky localizations that vary significantly from degree scale to hundreds of square degrees. We search for both a well-modeled binary coalescence signal, the favored progenitor model for short GRBs, and for generic, unmodeled gravitational wave bursts. Both searches use the event time and sky localization to improve the gravitational wave search sensitivity as compared to corresponding all-time, all-sky searches. We find no evidence of a gravitational wave signal associated with any of the IPN GRBs in the sample, nor do we find evidence for a population of weak gravitational wave signals associated with the GRBs. For all IPN-detected GRBs, for which a sufficient duration of quality gravitational wave data are available, we place lower bounds on the distance to the source in accordance with an optimistic assumption of gravitational wave emission energy of 10(-2)M(circle dot)c(2) at 150 Hz, and find a median of 13 Mpc. For the 27 short-hard GRBs we place 90% confidence exclusion distances to two source models: a binary neutron star coalescence, with a median distance of 12 Mpc, or the coalescence of a neutron star and black hole, with a median distance of 22 Mpc. Finally, we combine this search with previously published results to provide a population statement for GRB searches in first-generation LIGO and Virgo gravitational wave detectors and a resulting examination of prospects for the advanced gravitational wave detectors. C1 [Aasi, J.; Abbott, B. P.; Abbott, R.; Abernathy, M. R.; Adhikari, R. X.; Anderson, R. A.; Anderson, S. B.; Arai, K.; Araya, M. C.; Barayoga, J. C.; Barish, B. C.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; 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. K.; Hall, E. D.; Hamilton, W.; Harms, J.; Heptonstall, A. W.; Hodge, K. A.; Ivanov, A.; Jacobson, M.; Kalmus, P.; Kanner, J. B.; Kells, W.; King, P. J.; Kondrashov, V.; Korth, W. Z.; Kozak, D. B.; Lazzarini, A.; Lewis, J.; Li, T. G. F.; Libbrecht, K.; Mageswaran, M.; Mailand, K.; Maros, E.; Martynov, D.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Osthelder, C.; Pedraza, M.; Phelps, M.; Price, L. R.; Privitera, S.; Quintero, E.; Raymond, V.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Sannibale, V.; Shao, Z.; Singer, A.; Singer, L.; Smith, M. R.; Smith, R. J. E.; Smith-Lefebvre, N. D.; Taylor, R.; Thirugnanasambandam, M. P.; Thrane, E.; Torrie, C. I.; Vass, S.; Wallace, L.; Weinstein, A. J.; Williams, R.; Yamamoto, H.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Abbott, T.; Corbitt, T. R.; DeRosa, R. T.; Effler, A.; Giaime, J. A.; Gonzalez, G.; Johnson, W. W.; Kokeyama, K.; Macleod, D. M.; May, G.; Mullavey, A.; Singh, R.; Tao, J.; Walker, M.; Wilkinson, C.] Louisiana State Univ, Baton Rouge, LA 70803 USA. 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G.; Kim, S.] Korea Inst Sci & Technol Informat, Taejon 305 806, 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, CET Campus, Trivandrum 695016, Kerala, India. [Khazanov, E. A.; Palashov, O.; Poteomkin, A.; Sergeev, A.] Inst Phys Appl, Nizhnii Novgorod 603950, Russia. [Kim, K.; Lee, H. K.; Lee, J.] Hanyang Univ, Seoul 133791, South Korea. [Krolak, A.; Kutynia, A.; Zadrozny, A.] NCBJ, PL-05400 Otwock, Poland. [Krolak, A.] IM PAN, PL-00956 Warsaw, Poland. [Kumar, A.] Inst Plasma Res, Gandhinagar 382428, 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. [Lopez, E.] Louisiana Tech Univ, Ruston, LA 71272 USA. [Loriette, V.; Maksimovic, I.] CNRS, ESPCI, F-75005 Paris, France. [Marchesoni, F.] Univ Camerino, Dipartimento Fis, I-62032 Camerino, Italy. [McGuire, S. C.; Vincent-Finley, R.; Williams, K.] S Univ & A& M Coll, Baton Rouge, LA 70813 USA. [Nayak, R. K.] IISER Kolkata, Kolkata 741252, W Bengal, India. [Oh, J. J.; 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. [Rajalakshmi, G.; Unnikrishnan, C. S.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. [Reid, S.] Univ W 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, ICTP S Amer Inst Fundamental Res, Inst Fis Teorica, 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. [Whelan, J. T.] Rochester Inst Technol, Rochester, NY 14623 USA. [Williams, T. D.; Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA. [Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA. [Aptekar, R. L.; Frederiks, D. D.; Golenetskii, S. V.; Pal'shin, V. D.; Svinkin, D. S.] AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia. [Atteia, J. L.] Univ Toulouse, UPS OMP, IRA, Toulouse, France. [Atteia, J. L.] CNRS, IRAP, F-31400 Toulouse, France. [Connaughton, V.] Univ Alabama Huntsville, CSPAR, Huntsville, AL 35899 USA. [Hurley, K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Krimm, H. A.] CRESST, Greenbelt, MD 20771 USA. [Krimm, H. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21046 USA. [Pal'shin, V. D.] INAF IASF Bologna, I-40129 Bologna, Italy. [Pal'shin, V. D.] St Petersburg State Polytechn Univ, St Petersburg 195251, Russia. [Palmer, D.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Terada, Y.] Saitama Univ, Grad Sch Sci & Engn, Saitama, Japan. [Von Kienlin, A.] Max Planck Inst f extraterrest Phys, D-85748 Garching, Germany. RP Leroy, N (reprint author), Univ Paris 11, IN2P3, CNRS, LAL, F-91898 Orsay, France. EM leroy@lal.in2p3.fr RI 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; 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; Ott, Christian/G-2651-2011; Marchesoni, Fabio/A-1920-2008; 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; McClelland, David/E-6765-2010; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Strigin, Sergey/I-8337-2012; Leonardi, Matteo/G-9694-2015; Sigg, Daniel/I-4308-2015; Puppo, Paola/J-4250-2012; Tacca, Matteo/J-1599-2015; 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; Hild, Stefan/A-3864-2010; Danilishin, Stefan/K-7262-2012; Gammaitoni, Luca/B-5375-2009; Iyer, Bala R./E-2894-2012; Canuel, Benjamin/C-7459-2014; Prokhorov, Leonid/I-2953-2012; Lee, Chang-Hwan/B-3096-2015; Aptekar, Raphail/B-3456-2015; Golenetskii, Sergey/B-3818-2015; Pal'shin, Valentin/F-3973-2014; Svinkin, Dmitry/C-1934-2014; Khalili, Farit/D-8113-2012; Gorodetsky, Michael/C-5938-2008; Bell, Angus/E-7312-2011; Costa, Cesar/G-7588-2012; Wu, Ying/B-7283-2009; Steinlechner, Sebastian/D-5781-2013; Kumar, Prem/B-6691-2009; prodi, giovanni/B-4398-2010; Lam, Ping Koy/A-5276-2008; Huerta, Eliu/J-5426-2014; Gemme, Gianluca/C-7233-2008; Losurdo, Giovanni/K-1241-2014 OI Murphy, David/0000-0002-8538-815X; Veitch, John/0000-0002-6508-0713; 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; 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; Ott, Christian/0000-0003-4993-2055; Marchesoni, Fabio/0000-0001-9240-6793; calloni, enrico/0000-0003-4819-3297; Scott, Jamie/0000-0001-6701-6515; Sorazu, Borja/0000-0002-6178-3198; Allen, Bruce/0000-0003-4285-6256; Vitale, Salvatore/0000-0003-2700-0767; Swinkels, Bas/0000-0002-3066-3601; Guidi, Gianluca/0000-0002-3061-9870; Drago, Marco/0000-0002-3738-2431; Collette, Christophe/0000-0002-4430-3703; Pierro, Vincenzo/0000-0002-6020-5521; Coccia, Eugenio/0000-0002-6669-5787; Vetrano, Flavio/0000-0002-7523-4296; Denker, Timo/0000-0003-1259-5315; Naticchioni, Luca/0000-0003-2918-0730; Vedovato, Gabriele/0000-0001-7226-1320; Boschi, Valerio/0000-0001-8665-2293; Matichard, Fabrice/0000-0001-8982-8418; Papa, M.Alessandra/0000-0002-1007-5298; Frederiks, Dmitry/0000-0002-1153-6340; Aulbert, Carsten/0000-0002-1481-8319; Pinto, Innocenzo M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200; Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Ciani, Giacomo/0000-0003-4258-9338; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Ward, Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447; Dolique, Vincent/0000-0001-5644-9905; Whelan, John/0000-0001-5710-6576; McClelland, David/0000-0001-6210-5842; Vecchio, Alberto/0000-0002-6254-1617; Sigg, Daniel/0000-0003-4606-6526; Puppo, Paola/0000-0003-4677-5015; Tacca, Matteo/0000-0003-1353-0441; 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; Lee, Chang-Hwan/0000-0003-3221-1171; Gorodetsky, Michael/0000-0002-5159-2742; Bell, Angus/0000-0003-1523-0821; Steinlechner, Sebastian/0000-0003-4710-8548; prodi, giovanni/0000-0001-5256-915X; Lam, Ping Koy/0000-0002-4421-601X; Gemme, Gianluca/0000-0002-1127-7406; Losurdo, Giovanni/0000-0003-0452-746X FU 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; Carnegie Trust; Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation; Alfred P. Sloan Foundation; NASA [NNX06AI36G, NNX08AB84G, NNX08AZ85G, NNX09AV61G, NNX10AR12G, NNG06GI89G, NNX07AJ65G, NNX08AN23G, NNX09AO97G, NNX10AI23G, NNG06GE69G, NNX07AQ22G, NNX08AC90G, NNX08AX95G, NNX09AR28G]; Russian Space Agency; RFBR [12-02-00032-a, 13-02-12017-ofi_m] 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, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation. K. H. acknowledges IPN support from the following sources: NASA NNX06AI36G, NNX08AB84G, NNX08AZ85G, NNX09AV61G, and NNX10AR12G ( Suzaku), NASA NNG06GI89G, NNX07AJ65G, NNX08AN23G, NNX09AO97G, NNX10AI23G ( Swift), NASA NNG06GE69G, NNX07AQ22G, NNX08AC90G, NNX08AX95G, NNX09AR28G ( INTEGRAL). The Konus-Wind experiment is partially supported by a Russian Space Agency contract and RFBR Grants No. 12-02-00032-a and No. 13-02-12017-ofi_m. This document has been assigned LIGO Laboratory document number LIGO-P1300226-v10. NR 55 TC 15 Z9 16 U1 3 U2 58 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 JUN 30 PY 2014 VL 113 IS 1 AR 011102 DI 10.1103/PhysRevLett.113.011102 PG 14 WC Physics, Multidisciplinary SC Physics GA AL4GW UT WOS:000339091900001 PM 25032916 ER PT J AU Lehnert, H Stone, RP AF Lehnert, Helmut Stone, Robert P. TI Aleutian Ancorinidae (Porifera, Astrophorida): Description of three new species from the genera Stelletta and Ancorina SO ZOOTAXA LA English DT Article DE new demosponges; Aleutian Islands; Alaska; North Pacific; Bering Sea AB Two new species of the genus Stelletta and one new species of Ancorina are described from the Aleutian Islands of Alaska and compared to congeners of the region. This is the first record of the genus Ancorina in the North Pacific Ocean. Stelletta ovalae Tanita 1965 is also reported for the first time from the Bering Sea and Alaska. C1 [Lehnert, Helmut] LMU Munchen, GeoBio Ctr, D-80333 Munich, Germany. [Stone, Robert P.] NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK 99801 USA. RP Lehnert, H (reprint author), Eichenstr 14, D-86507 Oberottmarshausen, Germany. EM Lehnert@spongetaxonomics.de; bob.stone@noaa.gov FU Alaska Fisheries Science Center of NOAA/NMFS FX We thank the RACE Groundfish and Shellfish Assessment Programs of NOAA's Alaska Fisheries Science Center (AFSC) especially Jim Stark and Brian Knoth (both of NOAA Fisheries, AFSC) and the captains and crews of the FV Ocean Explorer and FV Sea Storm for their assistance collecting biological samples for this study. Thanks also to the Zoologische Staatssammlung, Munchen for providing access to the SEM, especially to Enrico Schwabe for help operating the SEM. We thank Michele Masuda (Alaska Fisheries Science Center, Auke Bay Laboratory) for providing Figure 1. Helmut Lehnert was supported by a contract from the Alaska Fisheries Science Center of NOAA/NMFS. The findings and conclusions in this paper are those of the authors and do not necessarily represent the views of the National Marine Fisheries Service. NR 30 TC 5 Z9 5 U1 1 U2 8 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JUN 30 PY 2014 VL 3826 IS 2 BP 341 EP 355 PG 15 WC Zoology SC Zoology GA AK0OG UT WOS:000338112800004 PM 24990051 ER PT J AU Klink, K Wiersma, JJ Crawford, CJ Stuthman, DD AF Klink, Katherine Wiersma, Jochum J. Crawford, Christopher J. Stuthman, Deon D. TI Impacts of temperature and precipitation variability intheNorthern Plains of the United States and Canada ontheproductivity of spring barley and oat SO INTERNATIONAL JOURNAL OF CLIMATOLOGY LA English DT Article DE barley; oat; crop yield; climate change; Minnesota ID CLIMATE-CHANGE; WHEAT; YIELD; CEREALS; WEATHER; GROWTH; TRENDS AB Increasing temperatures and changes in precipitation are expected to effect a change in production of cool-season crops such as spring barley and oat. To determine whether observed changes may already have had an impact on these crops in the Northern Plains of the United States and Canada, first-differences of growing-season temperature and precipitation and of annual yield data were analysed via multiple linear regression for 1980-2012 for the genetically stable cultivars of Robust' spring barley (Hordeum vulgare L.) at three sites in Minnesota, and for Gopher' oats (Avena sativa L.) at five sites in Minnesota and neighbouring states and provinces. Temperature and precipitation impacts also were assessed for the top-three yielding barley and oat cultivars at each site to assess whether newer varieties responded similarly to the older varieties. Barley yield at the coolest site showed a modest relationship with climate while the warmer sites showed stronger relationships between climate variability and barley yield, particularly for negative impacts of high temperatures. Climate variability also had a significant impact on yield at the five oat sites. Warm pre-sowing temperatures enhanced yields at cooler sites while high temperatures later in the growing season reduced yields across the sites. Results for the top-three barley and oat cultivars often were similar to those for the older cultivars. Our results suggest that observed climate changes have contributed to the relative decrease in barley and oat yields in the region, that more recent releases have partially compensated for the negative impacts of observed temperature and precipitation trends, and that model projected changes in temperature and precipitation will continue to present both benefits and challenges for barley and oat production in the Northern Plains. C1 [Klink, Katherine] Univ Minnesota, Dept Geog Environm & Soc, Minneapolis, MN USA. [Wiersma, Jochum J.; Stuthman, Deon D.] Univ Minnesota, Dept Agron & Plant Genet, St Paul, MN 55108 USA. [Crawford, Christopher J.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. RP Wiersma, JJ (reprint author), Univ Minnesota, Dept Agron & Plant Genet, 411 Borlaug Hall,1991 Upper Buford Circle, St Paul, MN 55108 USA. EM wiers002@umn.edu OI Klink, Katherine/0000-0002-0377-2378 FU Center for Urban and Regional Affairs at the University of Minnesota; University of Minnesota College of Liberal Arts FX This work was supported in part by a grant from the Center for Urban and Regional Affairs at the University of Minnesota. Additional funding was provided by the University of Minnesota College of Liberal Arts. Thanks to Matt Taraldsen for drafting Figure 3 and especially to the reviewers for their helpful suggestions and probing questions. NR 34 TC 1 Z9 1 U1 1 U2 27 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 JUN 30 PY 2014 VL 34 IS 8 BP 2805 EP 2818 DI 10.1002/joc.3877 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ4SU UT WOS:000337667100020 ER PT J AU Moores, JE McConnochie, TH Ming, DW Archer, PD Schuerger, AC AF Moores, John E. McConnochie, Timothy H. Ming, Douglas W. Archer, Paul Douglas, Jr. Schuerger, Andrew C. TI The Siding Spring cometary encounter with Mars: A natural experiment for the Martian atmosphere? SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID INTERPLANETARY DUST PARTICLES; C/2013 A1; METHANE; CLOUDS; MESOSPHERE; ABUNDANCE; DELIVERY; LIFE; COMA AB On 19 October 2014 comet C/2013 A1 will encounter Mars. The planet is anticipated to pass through the coma resulting in a greater than four order-of-magnitude increase in the accretion of dust with 430 tonnes of dust with diameters between 1 m and 12.4 mm surviving atmospheric passage. At high altitude, the dust would impact temperature and may affect limb dust extinction and cloud formation. The UV photolysis of the organic carbon content of the dust, 1.9 to 4.6 tonnes, would have a negligible effect on atmospheric methane. Should C/2013 A1 brighten, increases in upper atmospheric accretion of coma particles will exceed the background dust and the population of small coma particles may be constrained from orbital measurements. For M-1<-1.3, methane produced might be measurable by the Sample Analysis at Mars Tunable Laser Spectrometer instrument onboard Curiosity. C1 [Moores, John E.] York Univ, Ctr Res Earth & Space Sci, Toronto, ON M3J 2R7, Canada. [McConnochie, Timothy H.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Ming, Douglas W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Archer, Paul Douglas, Jr.] NASA, Lyndon B Johnson Space Ctr, Jacobs, Houston, TX 77058 USA. [Schuerger, Andrew C.] Univ Florida, Dept Plant Pathol, Gainesville, FL 32611 USA. RP Moores, JE (reprint author), York Univ, Ctr Res Earth & Space Sci, Toronto, ON M3J 2R7, Canada. EM jmoores@yorku.ca NR 37 TC 4 Z9 4 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 28 PY 2014 VL 41 IS 12 BP 4109 EP 4117 DI 10.1002/2014GL060610 PG 9 WC Geosciences, Multidisciplinary SC Geology GA AN0SM UT WOS:000340294300002 ER PT J AU Duller, RA Warner, NH McGonigle, C De Angelis, S Russell, AJ Mountney, NP AF Duller, Robert A. Warner, Nicholas H. McGonigle, Christopher De Angelis, Silvio Russell, Andrew J. Mountney, Nigel P. TI Landscape reaction, response, and recovery following the catastrophic 1918 Katla jokulhlaup, southern Iceland SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID FLOOD; ENVIRONMENTS; SCALES; TIME; ICE AB One of the largest recorded glacier outburst floods (jokulhlaups) occurred in 1918, generated by the last major subglacial eruption of Katla volcano in southern Iceland. Using digitized historical topographic surveys and field observations from the main proglacial outwash plain (Myrdalssandur), we document the reaction of Myrdalssandur to the 1918 event and subsequent response and recovery. Our analysis highlights the longevity of elevated topography, over the recovery period, and the complete reorganization of the main perennial meltwater channel system, both of which will affect and condition the flow routing and impact of future jokulhlaups. The jokulhlaup deposited approximately 2 km(3) of sediment onto Myrdalssandur immediately after the event and extended the coastline by several kilometers. However, 80% of this material by volume has since been removed by surface and subsurface water flow on the main sandur and by marine reworking at the coast. By 2007, the surface elevation at specific locations on the outwash plain and the position of the coastline were similar to those in 1904, indicating near-complete recovery of the landscape. Despite this, the Myrdalssandur coastline has experienced net advance over the past 1000 years. Using our calculated characteristic landscape response and recovery values following the 1918 event (60 years and 120 years) we deduce that the landscape has been in a dominant state of transience, with regard to forcing frequency and timescale of recovery, over the past 1000 years, which has facilitated long-term landscape growth. C1 [Duller, Robert A.; De Angelis, Silvio] Univ Liverpool, Dept Earth Ocean & Ecol Sci, Liverpool L69 3BX, Merseyside, England. [Warner, Nicholas H.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA USA. [McGonigle, Christopher] Univ Ulster, Sch Environm Sci, Coleraine BT52 1SA, Londonderry, North Ireland. [Russell, Andrew J.] Newcastle Univ, Sch Geog Polit & Sociol, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. [Mountney, Nigel P.] Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England. RP Duller, RA (reprint author), Univ Liverpool, Dept Earth Ocean & Ecol Sci, Liverpool L69 3BX, Merseyside, England. EM rduller@liv.ac.uk RI Mountney, Nigel/O-9054-2016; OI Mountney, Nigel/0000-0002-8356-9889; McGonigle, Chris/0000-0002-0262-0559; De Angelis, Silvio/0000-0003-2636-3056 FU Earthwatch Institute; Jet Propulsion Laboratory-California Institute of Technology; NASA FX The Earthwatch Institute provided funding for R. D., A. R. and N.M. N.W. was partially supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory-California Institute of Technology, administered by the Oak Ridge Associated Universities through a contract with NASA. R. D. and N.W. thank Philip Allen, Sanjeev Gupta, and Dave Hodgson for partial financial support during the writing of this paper. We thank Chris Paola and Paul Carling for thoughtful reviews. Data associated with this manuscript are available upon request from R.D. NR 22 TC 3 Z9 3 U1 4 U2 37 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 JUN 28 PY 2014 VL 41 IS 12 BP 4214 EP 4221 DI 10.1002/2014GL060090 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AN0SM UT WOS:000340294300015 ER PT J AU Polashenski, C Courville, Z Benson, C Wagner, A Chen, J Wong, G Hawley, R Hall, D AF Polashenski, Chris Courville, Zoe Benson, Carl Wagner, Anna Chen, Justin Wong, Gifford Hawley, Robert Hall, Dorothy TI Observations of pronounced Greenland ice sheet firn warming and implications for runoff production SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SEA-LEVEL RISE; MELT EXTENT; MODIS; ACCUMULATION; VARIABILITY AB Field measurements of shallow borehole temperatures in firn across the northern Greenland ice sheet are collected during May 2013. Sites first measured in 1952-1955 are revisited, showing long-term trends in firn temperature. Results indicate a pattern of substantial firn warming (up to +5.7 degrees C) at midlevel elevations (1400-2500 m) and little temperature change at high elevations (>2500 m). We find that latent heat transport into the firn due to meltwater percolation drives the observed warming. Modeling shows that heat is stored at depth for several years, and energy delivered from consecutive melt events accumulates in the firn. The observed warming is likely not yet in equilibrium with recent melt production rates but captures the progression of sites in the percolation facies toward net runoff production. C1 [Polashenski, Chris; Wagner, Anna] US Army Cold Reg Res & Engn Lab, Ft Wainwright, AK 99703 USA. [Polashenski, Chris; Courville, Zoe] Dartmouth Coll, Thayer Sch Engn, Hanover, NH 03755 USA. [Courville, Zoe] US Army Cold Reg Res & Engn Lab, Hanover, NH USA. [Benson, Carl] Univ Alaska Fairbanks, Inst Geophys, Fairbanks, AK 99775 USA. [Chen, Justin] Hanover High Sch, Hanover, NH USA. [Wong, Gifford; Hawley, Robert] Dartmouth Coll, Dept Earth Sci, Hanover, NH 03755 USA. [Hall, Dorothy] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Polashenski, C (reprint author), US Army Cold Reg Res & Engn Lab, Ft Wainwright, AK 99703 USA. EM chris.polashenski@gmail.com FU National Science Foundation Division of Polar Programs, the NSF award [1204145] FX We would like to acknowledge the support provided by the National Science Foundation Division of Polar Programs, the NSF award 1204145, the able and cheerful assistance of Michael Stewart, Nathan Stewart, and Thomas Overly in the collection of temperature data, and the logistics provided by CH2MHill Polar Field Services and Stanford Research Institute teams. We thank Koni Steffen for sharing up to date GC-Net Data used to extend relevant analyses. All data used in this publication can be accessed in the National Snow and Ice Data Center Advanced Cooperative Arctic Data and Information Service website: nsidc.org/acadis. The authors thank two anonymous reviewers for their helpful comments in improving this paper. NR 48 TC 7 Z9 7 U1 3 U2 19 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 JUN 28 PY 2014 VL 41 IS 12 BP 4238 EP 4246 DI 10.1002/2014GL059806 PG 9 WC Geosciences, Multidisciplinary SC Geology GA AN0SM UT WOS:000340294300018 ER PT J AU Parkinson, CL AF Parkinson, Claire L. TI Spatially mapped reductions in the length of the Arctic sea ice season SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MELT SEASON; INTERANNUAL VARIABILITY; AMPLIFICATION; THICKNESS; DECLINE; TRENDS; COVER; AREAS AB Satellite data are used to determine the number of days having sea ice coverage in each year 1979-2013 and to map the trends in these ice-season lengths. Over the majority of the Arctic seasonal sea ice zone, the ice season shortened at an average rate of at least 5 days/decade between 1979 and 2013, and in a small area in the northeastern Barents Sea the rate of shortening reached over 65 days/decade. The only substantial non-coastal area with lengthening sea ice seasons is the Bering Sea, where the ice season lengthened by 5-15 days/decade. Over the Arctic as a whole, the area with ice seasons shortened by at least 5 days/decade is 12.4 x 10(6) km(2), while the area with ice seasons lengthened by at least 5 days/decade is only 1.1 x 10(6) km(2). The contrast is even greater, percentage-wise, for higher rates. C1 NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. RP Parkinson, CL (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. EM Claire.L.Parkinson@nasa.gov FU NASA Cryospheric Sciences Program FX The author thanks Nick DiGirolamo of Science Systems and Applications Incorporated (SSAI) for his help in the generation of the figures, two anonymous reviewers and GRL editor Julienne Stroeve for their reviews of the manuscript, and the NASA Cryospheric Sciences Program for funding the work. The satellite passive-microwave data used for generating the results are available at the National Snow and Ice Data Center (NSIDC), Boulder, Colorado. NR 32 TC 20 Z9 21 U1 1 U2 23 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 28 PY 2014 VL 41 IS 12 BP 4316 EP 4322 DI 10.1002/2014GL060434 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AN0SM UT WOS:000340294300028 ER PT J AU Ma, Q Boulet, C Tipping, RH AF Ma, Q. Boulet, C. Tipping, R. H. TI Effects on calculated half-widths and shifts from the line coupling for asymmetric-top molecules SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID SEMICLASSICAL CALCULATIONS; MICROWAVE-ABSORPTION; WATER-VAPOR; H2O LINES; LINEWIDTHS; COLLISIONS; N-2 AB The refinement of the Robert-Bonamy formalism by considering the line coupling for linear molecules developed in our previous studies [Q. Ma, C. Boulet, and R. H. Tipping, J. Chem. Phys. 139, 034305 (2013); 140, 104304 (2014)] have been extended to asymmetric-top molecules. For H2O immersed in N-2 bath, the line coupling selection rules applicable for the pure rotational band to determine whether two specified lines are coupled or not are established. Meanwhile, because the coupling strengths are determined by relative importance of off-diagonal matrix elements versus diagonal elements of the operator -iS(1) - S-2, quantitative tools are developed with which one is able to remove weakly coupled lines from consideration. By applying these tools, we have found that within reasonable tolerances, most of the H2O lines in the pure rotational band are not coupled. This reflects the fact that differences of energy levels of the H2O states are pretty large. But, there are several dozen strongly coupled lines and they can be categorized into different groups such that the line couplings occur only within the same groups. In practice, to identify those strongly coupled lines and to confine them into sub-linespaces are crucial steps in considering the line coupling. We have calculated half-widths and shifts for some groups, including the line coupling. Based on these calculations, one can conclude that for most of the H2O lines, it is unnecessary to consider the line coupling. However, for several dozens of lines, effects on the calculated half-widths from the line coupling are small, but remain noticeable and reductions of calculated half-widths due to including the line coupling could reach to 5%. Meanwhile, effects on the calculated shifts are very significant and variations of calculated shifts could be as large as 25%. (C) 2014 AIP Publishing LLC. C1 [Ma, Q.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Ma, Q.] Columbia Univ, Dept Appl Phys & Appl, New York, NY 10025 USA. [Boulet, C.] CNRS, UMR8214, ISMO, F-91405 Orsay, France. [Boulet, C.] Univ Paris 11, F-91405 Orsay, France. [Tipping, R. H.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA. RP Ma, Q (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. FU NSF [1228861]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231] FX Two of the authors (Q. Ma and R. H. Tipping) acknowledge financial support from NSF under Grant No. 1228861. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. NR 24 TC 1 Z9 1 U1 1 U2 5 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 JUN 28 PY 2014 VL 140 IS 24 AR 244301 DI 10.1063/1.4883058 PG 14 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA AK7UW UT WOS:000338634200023 PM 24985632 ER PT J AU Samuels-Crow, KE Galewsky, J Hardy, DR Sharp, ZD Worden, J Braun, C AF Samuels-Crow, Kimberly E. Galewsky, Joseph Hardy, Douglas R. Sharp, Zachary D. Worden, John Braun, Carsten TI Upwind convective influences on the isotopic composition of atmospheric water vapor over the tropical Andes SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID OUTGOING LONGWAVE RADIATION; SEA-SURFACE TEMPERATURE; LAST GLACIAL MAXIMUM; ICE CORE EVIDENCE; CLIMATE-CHANGE; SOUTH-AMERICA; STABLE-ISOTOPES; DELTA-D; PRECIPITATION; VARIABILITY AB We take advantage of the spatial coverage provided by the Tropospheric Emission Spectrometer on-board the Aura satellite to evaluate processes that control seasonal variations in atmospheric water vapor HDO/H2O values (delta D-vapor) over the tropical Andes. delta D-vapor is lower in austral summer (December, January, and February, DJF) than austral winter (June, July, and August, JJA), which is broadly consistent with precipitation studies and with delta O-18(snow) preserved in tropical Andean glaciers. In DJF, 64% of delta D-vapor measurements over the tropical Andes are lower than predicted by Rayleigh distillation while 40% of JJA delta D-vapor measurements are lower than predicted by Rayleigh distillation. Air that has lower delta D-vapor than predicted by Rayleigh distillation at a given water vapor concentration (q) encounters low minimum outgoing longwave radiation (<240 W m(-2)) en route to the tropical Andes, suggesting convective intensity controls the isotopic ratios of these measurements. The broad regional coverage of the satellite data allows us to map the spatial extent of the region where isotopic ratios reflect convective processes in different seasons. In DJF, convection strongly influences delta D-vapor in the central tropical Andes. In JJA, convection influences delta D-vapor north of the tropical Andes. This pattern suggests that monsoon convection controls delta D-vapor in austral summer while large-scale advective mixing controls Andean delta D-vapor in austral winter. C1 [Samuels-Crow, Kimberly E.; Galewsky, Joseph; Sharp, Zachary D.] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [Hardy, Douglas R.] Univ Massachusetts, Climate Syst Res Ctr, Amherst, MA 01003 USA. [Worden, John] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Braun, Carsten] Westfield State Univ, Westfield, MA USA. RP Samuels-Crow, KE (reprint author), Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. EM samuels@unm.edu FU National Aeronautics and Space Administration; NM EPSCoR FX Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. AIRS data were obtained from the Mirador online database, developed and maintained by GES DISC. The authors gratefully acknowledge the NOAA Air Resources Laboratory (ARL) for the provision of the HYSPLIT transport and dispersion model. Thanks to Vicencio Expeditions for making field work at Quelccaya both possible and pleasant. We thank three anonymous reviewers for their constructive suggestions. Funding for Samuels-Crow was provided by NM EPSCoR. NR 69 TC 16 Z9 16 U1 3 U2 8 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 JUN 27 PY 2014 VL 119 IS 12 BP 7051 EP 7063 DI 10.1002/2014JD021487 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN0BP UT WOS:000340247000003 ER PT J AU Lewis, SC LeGrande, AN Schmidt, GA Kelley, M AF Lewis, Sophie C. LeGrande, Allegra N. Schmidt, Gavin A. Kelley, Maxwell TI Comparison of forced ENSO-like hydrological expressions in simulations of the preindustrial and mid-Holocene SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID EL-NINO/SOUTHERN OSCILLATION; NINO-SOUTHERN-OSCILLATION; SEA-SURFACE TEMPERATURE; INTERANNUAL VARIABILITY; TROPICAL PRECIPITATION; GLOBAL PRECIPITATION; PACIFIC CLIMATE; GISS MODELE; HOLOCENE; ISOTOPES AB Using the water isotope-and vapor source distribution (VSD) tracer-enabled Goddard Institute for Space Studies ModelE-R, we examine changing El Nino-Southern Oscillation (ENSO)-like expressions in the hydrological cycle in a suite of model experiments. We apply strong surface temperature anomalies associated with composite observed El Nino and La Nina events as surface boundary conditions to preindustrial and mid-Holocene model experiments in order to investigate ENSO-like expressions in the hydrological cycle under varying boundary conditions. We find distinct simulated hydrological anomalies associated with El Nino-like ("ENSOWARM") and La Nina-like ("ENSOCOOL") conditions, and the region-specific VSD tracers show hydrological differences across the Pacific basin between El Nino-like and La Nina-like events. The application of ENSOCOOL forcings does not produce climatological anomalies that represent the equal but opposite impacts of the ENSOWARM experiment, as the isotopic anomalies associated with ENSOWARM conditions are generally stronger than with ENSOCOOL and the spatial patterns of change distinct. Also, when the same ENSO-like surface temperature anomalies are imposed on the mid-Holocene, the hydrological response is muted, relative to the preindustrial. Mid-Holocene changes in moisture sources to the analyzed regions across the Pacific reveal potentially complex relationships between ENSO-like conditions and boundary conditions. Given the complex impacts of ENSO-like conditions on various aspects of the hydrological cycle, we suggest that proxy record insights into paleo-ENSO variability are most likely to be robust when synthesized from a network of many spatially diverse archives, which can account for the potential nonstationarity of ENSO teleconnections under different boundary conditions. C1 [Lewis, Sophie C.] Univ Melbourne, Sch Earth Sci, Parkville, Vic 3052, Australia. [Lewis, Sophie C.] ARC Ctr Excellence Climate Syst Sci, Canberra, ACT, Australia. [LeGrande, Allegra N.; Schmidt, Gavin A.; Kelley, Maxwell] Columbia Univ, NASA Goddard Inst Space Studies, New York, NY USA. [LeGrande, Allegra N.; Schmidt, Gavin A.; Kelley, Maxwell] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. RP Lewis, SC (reprint author), Univ Melbourne, Sch Earth Sci, Parkville, Vic 3052, Australia. EM sophie.lewis@unimelb.edu.au RI Schmidt, Gavin/D-4427-2012; Lewis, Sophie/H-4968-2011 OI Schmidt, Gavin/0000-0002-2258-0486; Lewis, Sophie/0000-0001-6416-0634 FU NSF [ATM 07-53868]; Australian Research Council Centre of Excellence for Climate System Science [CE 110001028] FX We thank NASA GISS for institutional support; resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Center for Climate Simulation (NCCS) at Goddard Space Flight Center. We also thank the NASA Modeling and Analysis Program for climate model development. NSF ATM 07-53868 supports A.N.L. and partial travel for S. C. L. S. C. L. is supported by funding from the Australian Research Council Centre of Excellence for Climate System Science (grant CE 110001028). We also thank the producers of observational data products that assisted this study. The GPCP-combined precipitation data were provided by the NASA/Goddard Space Flight Center's Laboratory for Atmospheres, which develops and computes the data set as a contribution to the GEWEX Global Precipitation Climatology Project. We are also grateful to four anonymous reviewers, whose comments greatly improved this manuscript. NR 58 TC 3 Z9 3 U1 2 U2 11 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 JUN 27 PY 2014 VL 119 IS 12 BP 7064 EP 7082 DI 10.1002/2013JD020961 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN0BP UT WOS:000340247000004 ER PT J AU Zhang, YF Hoar, TJ Yang, ZL Anderson, JL Toure, AM Rodell, M AF Zhang, Yong-Fei Hoar, Tim J. Yang, Zong-Liang Anderson, Jeffrey L. Toure, Ally M. Rodell, Matthew TI Assimilation of MODIS snow cover through the Data Assimilation Research Testbed and the Community Land Model version 4 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID NUMERICAL WEATHER PREDICTION; WATER EQUIVALENT; SURFACE MODEL; PRODUCTS; DEPTH; SIMULATIONS; UNCERTAINTY; STREAMFLOW; MONSOON AB To improve snowpack estimates in Community Land Model version 4 (CLM4), the Moderate Resolution Imaging Spectroradiometer (MODIS) snow cover fraction (SCF) was assimilated into the Community Land Model version 4 (CLM4) via the Data Assimilation Research Testbed (DART). The interface between CLM4 and DART is a flexible, extensible approach to land surface data assimilation. This data assimilation system has a large ensemble (80-member) atmospheric forcing that facilitates ensemble-based land data assimilation. We use 40 randomly chosen forcing members to drive 40 CLM members as a compromise between computational cost and the data assimilation performance. The localization distance, a parameter in DART, was tuned to optimize the data assimilation performance at the global scale. Snow water equivalent (SWE) and snow depth are adjusted via the ensemble adjustment Kalman filter, particularly in regions with large SCF variability. The root-mean-square error of the forecast SCF against MODIS SCF is largely reduced. In DJF (December-January-February), the discrepancy between MODIS and CLM4 is broadly ameliorated in the lower-middle latitudes (23 degrees-45 degrees N). Only minimal modifications are made in the higher-middle (45 degrees-66 degrees N) and high latitudes, part of which is due to the agreement between model and observation when snow cover is nearly 100%. In some regions it also reveals that CLM4-modeled snow cover lacks heterogeneous features compared to MODIS. In MAM (March-April-May), adjustments to snow move poleward mainly due to the northward movement of the snowline (i.e., where largest SCF uncertainty is and SCF assimilation has the greatest impact). The effectiveness of data assimilation also varies with vegetation types, with mixed performance over forest regions and consistently good performance over grass, which can partly be explained by the linearity of the relationship between SCF and SWE in the model ensembles. The updated snow depth was compared to the Canadian Meteorological Center (CMC) data. Differences between CMC and CLM4 are generally reduced in densely monitored regions. C1 [Zhang, Yong-Fei; Yang, Zong-Liang] Univ Texas Austin, Dept Geol Sci, John A & Katherine G Jackson Sch Geosci, Austin, TX 78712 USA. [Hoar, Tim J.; Anderson, Jeffrey L.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Toure, Ally M.] Univ Space Res Assoc, Columbia, MD USA. [Toure, Ally M.; Rodell, Matthew] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Yang, ZL (reprint author), Univ Texas Austin, Dept Geol Sci, John A & Katherine G Jackson Sch Geosci, Austin, TX 78712 USA. EM liang@jsg.utexas.edu RI Yang, Zong-Liang/B-4916-2011; Rodell, Matthew/E-4946-2012 OI Rodell, Matthew/0000-0003-0106-7437 FU NASA [NNX09AJ48G, NNX11AJ43G]; NCAR Advanced Study Program; NSFC [91337217] FX This work is funded by NASA grants NNX09AJ48G and NNX11AJ43G, the NCAR Advanced Study Program, and NSFC grant 91337217. Andrew Fox is thanked for discussing the implementation of DART/CLM4. The DART/CAM4 reanalysis data are prepared by Kevin Raeder (raeder@ucar.edu). Nancy Collins is thanked for part of the coding with DART. MODIS snow data and CMC snow depth data are provided by the National Snow and Ice Data Center. We would like to thank Barton Forman and two anonymous reviewers for their constructive comments. NR 46 TC 11 Z9 11 U1 0 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 27 PY 2014 VL 119 IS 12 BP 7091 EP 7103 DI 10.1002/2013JD021329 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN0BP UT WOS:000340247000006 ER PT J AU Schafer, JS Eck, TF Holben, BN Thornhill, KL Anderson, BE Sinyuk, A Giles, DM Winstead, EL Ziemba, LD Beyersdorf, AJ Kenny, PR Smirnov, A Slutsker, I AF Schafer, J. S. Eck, T. F. Holben, B. N. Thornhill, K. L. Anderson, B. E. Sinyuk, A. Giles, D. M. Winstead, E. L. Ziemba, L. D. Beyersdorf, A. J. Kenny, P. R. Smirnov, A. Slutsker, I. TI Intercomparison of aerosol single-scattering albedo derived from AERONET surface radiometers and LARGE in situ aircraft profiles during the 2011 DRAGON-MD and DISCOVER-AQ experiments SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SKY RADIANCE MEASUREMENTS; OPTICAL-PROPERTIES; LIGHT-ABSORPTION; WAVELENGTH DEPENDENCE; ATMOSPHERIC AEROSOLS; UNITED-STATES; RETRIEVAL; NETWORK; CARBON; DUST AB Single-scattering albedo (SSA) retrievals obtained with CIMEL Sun-sky radiometers from the Aerosol Robotic Network (AERONET) aerosol monitoring network were used to make comparisons with simultaneous in situ sampling from aircraft profiles carried out by the NASA Langley Aerosol Group Experiment (LARGE) team in the summer of 2011 during the coincident DRAGON-MD (Distributed Regional Aerosol Gridded Observational Network-Maryland) and DISCOVER-AQ (Deriving Information on Surface conditions from Column and Vertically Resolved Observations Relevant to Air Quality) experiments. The single-scattering albedos (interpolated to 550 nm) derived from AERONET measurements for aerosol optical depth (AOD) at 440 nm >= 0.4 (mean SSA: 0.979) were on average 0.011 lower than the values derived from the LARGE profile measurements (mean SSA: 0.99). The maximum difference observed was 0.023 with all the observed differences within the combined uncertainty for the stated SSA accuracy (0.03 for AERONET; 0.02 for LARGE). Single-scattering albedo averages were also analyzed for lower aerosol loading conditions (AOD >= 0.2) and a dependence on aerosol optical depth was noted with significantly lower single-scattering albedos observed for lower AOD in both AERONET and LARGE data sets. Various explanations for the SSA trend were explored based on other retrieval products including volume median radius and imaginary refractive index as well as column water vapor measurements. Additionally, these SSA trends with AOD were evaluated for one of the DRAGON-MD study sites, Goddard Space Flight Center, and two other Mid-Atlantic AERONET sites over the long-term record dating to 1999. C1 [Schafer, J. S.; Eck, T. F.; Holben, B. N.; Sinyuk, A.; Giles, D. M.; Kenny, P. R.; Smirnov, A.; Slutsker, I.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Schafer, J. S.; Sinyuk, A.; Giles, D. M.; Kenny, P. R.; Smirnov, A.; Slutsker, I.] Sigma Space Corp, Lanham, MD USA. [Eck, T. F.] Univ Space Res Assoc, Columbia, MD USA. [Thornhill, K. L.; Anderson, B. E.; Winstead, E. L.; Ziemba, L. D.; Beyersdorf, A. J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Schafer, JS (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM joel.schafer@nasa.gov RI Smirnov, Alexander/C-2121-2009 OI Smirnov, Alexander/0000-0002-8208-1304 FU Radiation Sciences Program (NASA); EOS project office (NASA); Joint Polar Satellite System program (NOAA) FX The AERONET project is supported by the Radiation Sciences Program (NASA), the EOS project office (NASA), and the Joint Polar Satellite System program (NOAA). We would like to thank the summer interns who installed and maintained the 40+ CIMEL Sun photometers; Anastasia Sorokine, Chris McPartland, Christopher Blackwell, Sarah Dickerson, and Christina Justice as well as the many local elementary schools and high schools that hosted our instrumentation for several months. Additionally, we would like to recognize the contributions of Jennifer Hains, Ryan Auvil, and others at the Maryland Department of the Environment who allowed us to operate our equipment at their facilities. The data used in this paper are available at 'http://aeronet.gsfc.nasa.gov/new_web/DRAGON-USA_2011_DC_Maryland.html' NR 32 TC 12 Z9 12 U1 3 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 27 PY 2014 VL 119 IS 12 BP 7439 EP 7452 DI 10.1002/2013JD021166 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN0BP UT WOS:000340247000026 ER PT J AU Vergados, P Mannucci, AJ Ao, CO AF Vergados, Panagiotis Mannucci, Anthony J. Ao, Chi O. TI Assessing the performance of GPS radio occultation measurements in retrieving tropospheric humidity in cloudiness: A comparison study with radiosondes, ERA-Interim, and AIRS data sets SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID NUMERICAL WEATHER-PREDICTION; PRECIPITABLE WATER-VAPOR; RADIATION DRY BIAS; TEMPERATURE; ECMWF; ASSIMILATION; REFRACTIVITY; VALIDATION; SIGNALS; AIRS/AMSU/HSB AB We assess the impact that the Global Positioning System radio occultations (GPSRO) measurements have on complementing different data sets in characterizing the lower-to-middle tropospheric humidity in cloudy conditions over both land and oceans using data from 1 August 2006 to 31 October 2006. We use observations from rawinsondes, Global Positioning System radio occultations (GPSRO), Atmospheric Infrared Sounder (AIRS), and the European Center for Medium-Range Weather Forecasts Reanalysis Interim (ERA-Interim). During the selected time period, Constellation Observing System for Meteorology, Ionosphere, and Climate data were not assimilated in ERA-Interim. From each data set, we estimate a zonally averaged tropospheric specific humidity profile at tropical, middle, and high latitudes. Over land, we use rawinsondes as the ground truth and quantify the specific humidity differences and root-mean-square-errors (RMSEs) of the GPSRO, AIRS, and ERA-Interim profiles. GPSRO are beneficial in retrieving lower tropospheric humidity than upper tropospheric profiles, due to their loss of sensitivity at high altitudes. Blending GPSRO with ERA-Interim produces profiles with smaller humidity biases outside the tropics, but GPSRO data do not improve the humidity RMSE when compared to rawinsondes. Combining GPSRO with AIRS leads to smaller humidity bias at the tropics and high latitudes, while reducing humidity's RMSEs. Over oceans, no rawinsonde information is available, and we use ERA-Interim as a reference. Combining GPSRO with AIRS leads to smaller humidity RMSEs than AIRS. We conclude that cross-comparisons and synergies among multi-instrument observations are promising in advancing our knowledge of the tropospheric humidity in cloudy conditions. GPSRO data can contribute to improving humidity retrievals over cloud-covered regions, especially over land and within the boundary layer. C1 [Vergados, Panagiotis; Mannucci, Anthony J.; Ao, Chi O.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91125 USA. RP Vergados, P (reprint author), CALTECH, NASA Jet Prop Lab, Pasadena, CA 91125 USA. EM Panagiotis.Vergados@jpl.nasa.gov FU National Aeronautics and Space Administration FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. P. Vergados acknowledges the NPP program administered by the Oak Ridge Associated Universities (ORAU). We would like to thank all reviewers for their extensive comments, which greatly helped us on the presentation of this research paper and for emphasizing upon the significance of our results. NR 48 TC 5 Z9 6 U1 2 U2 21 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 JUN 27 PY 2014 VL 119 IS 12 BP 7718 EP 7731 DI 10.1002/2013JD021398 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN0BP UT WOS:000340247000041 ER PT J AU Wecht, KJ Jacob, DJ Frankenberg, C Jiang, Z Blake, DR AF Wecht, Kevin J. Jacob, Daniel J. Frankenberg, Christian Jiang, Zhe Blake, Donald R. TI Mapping of North American methane emissions with high spatial resolution by inversion of SCIAMACHY satellite data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID UNITED-STATES; SENTINEL-5 PRECURSOR; SURFACE MEASUREMENTS; CONTROL SPACE; GEOS-CHEM; CH4; OZONE; MODEL; ASSIMILATION; SEASONALITY AB We estimate methane emissions from North America with high spatial resolution by inversion of Scanning Imaging Absorption Spectrometer for Atmospheric Chartography (SCIAMACHY) satellite observations using the Goddard Earth Observing System Chemistry (GEOS-Chem) chemical transport model and its adjoint. The inversion focuses on summer 2004 when data from the Intercontinental Chemical Transport Experiment-North America (INTEX-A) aircraft campaign over the eastern U. S. are available to validate the SCIAMACHY retrievals and evaluate the inversion. From the INTEX-A data we identify and correct a water vapor-dependent bias in the SCIAMACHY data. We conduct an initial inversion of emissions on the horizontal grid of GEOS-Chem (1/2 degrees x 2/3 degrees) to identify correction tendencies relative to the Emission Database for Global Atmospheric Research (EDGAR) v4.2 emission inventory used as a priori. We then cluster these grid cells with a hierarchical algorithm to extract the maximum information from the SCIAMACHY observations. A 1000 cluster ensemble can be adequately constrained, providing similar to 100 km resolution across North America. Analysis of results indicates that the Hudson Bay Lowland wetlands source is 2.1 Tg a(-1), lower than the a priori but consistent with other recent estimates. Anthropogenic U. S. emissions are 30.1 +/- 1.3 Tg a(-1), compared to 25.8 Tg a(-1) and 28.3 Tg a(-1) in the EDGAR v4.2 and Environmental Protection Agency (EPA) inventories, respectively. We find that U. S. livestock emissions are 40% greater than in these two inventories. No such discrepancy is apparent for overall U. S. oil and gas emissions, although this may reflect some compensation between overestimate of emissions from storage/distribution and underestimate from production. We find that U. S. livestock emissions are 70% greater than the oil and gas emissions, in contrast to the EDGAR v4.2 and EPA inventories where these two sources are of comparable magnitude. C1 [Wecht, Kevin J.; Jacob, Daniel J.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Frankenberg, Christian; Jiang, Zhe] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Blake, Donald R.] Univ Calif Irvine, Dept Chem, Irvine, CA 92717 USA. RP Wecht, KJ (reprint author), Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. EM wecht@fas.harvard.edu RI Chem, GEOS/C-5595-2014; Frankenberg, Christian/A-2944-2013 OI Frankenberg, Christian/0000-0002-0546-5857 FU NASA Carbon Monitoring System (CMS); NASA Atmospheric Composition Modeling and Analysis Program (ACMAP); NASA FX This work was supported by the NASA Carbon Monitoring System (CMS), the NASA Atmospheric Composition Modeling and Analysis Program (ACMAP), and by a NASA Earth System Science Fellowship to K.J.W. We thank Tom Wirth (U.S. EPA) for providing information on seasonality in the EPA emission inventory. The INTEX-A data are available through NASA's LaRC Airborne Science Data for Atmospheric Composition: ftp://ftp-air.larc.nasa.gov/pub/INTEXA/DC8_AIRCRAFT/. The SCIAMACHY data are available upon request through the SCIAMACHY website: http://www.sciamachy.org/products/index.php. Instructions for downloading and running the GEOS-Chem CTM are available at http://geos-chem.org/ and for the GEOS-Chem adjoint at http://wiki.seas.harvard.edu/geos-chem/index.php/GEOS-Chem_Adjoint. NR 68 TC 25 Z9 25 U1 1 U2 46 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 JUN 27 PY 2014 VL 119 IS 12 BP 7741 EP 7756 DI 10.1002/2014JD021551 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN0BP UT WOS:000340247000043 ER PT J AU Sharp, WE Zaccheo, TS Browell, EV Ismail, S Dobler, JT Llewellyn, EJ AF Sharp, William E. Zaccheo, T. Scott Browell, Edward V. Ismail, Syed Dobler, Jeremy T. Llewellyn, Edward J. TI Impact of ambient O-2(a(1)Delta(g)) on satellite-based laser remote sensing of O-2 columns using absorption lines in the 1.27 mu m region SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID AIRBORNE LIDAR MEASUREMENTS; EMISSION SOUNDER SMILES; OZONE PROFILES; RAMAN-SPECTROSCOPY; LOWER THERMOSPHERE; ATOMIC OXYGEN; BAND; CO2; MODEL; MESOSPHERE AB Determination of CO2 mixing ratio columns from space using Laser Absorption Spectroscopy (LAS) requires simultaneous measurements of CO2 number density columns and knowledge of the dry atmospheric surface pressure. One approach to determining the surface pressure is to make an LAS column measurement of O-2 number density in the 7857.3-7921.7 cm(-1) (1.27 mu m) region of the O-2((1)Delta) state. A complicating factor in the LAS O-2 measurement is the presence of a permanent but spatially variable natural source of airglow from the O-2((1)Delta) state. In addition, the laser radiation can induce stimulated emission from the ambient O-2((1)Delta) state and also cause stimulated absorption and emission from the ground state O-2 molecules as the laser beam passes through the atmosphere. Finally, the upwelling surface-reflected solar radiation is an additional source of background radiation. The effects of these additional radiation sources on the LAS measurement of O-2 are examined. The surface-reflected solar radiation produces the largest background at 3 orders of magnitude more intense than the laser backscatter signal, while the airglow is of the same order of magnitude as the laser backscatter. The stimulated emission from ambient O-2(a(1)Delta(g)) is found to be about the same order of magnitude as the laser radiation. These effects are evaluated under noon, twilight, and midnight conditions at midlatitudes, the equator, and the pole. The stimulated emission is in the same direction and in phase with the laser signal, its contamination of the LAS O-2 measurement prevents a full sunlight determination of surface pressure. C1 [Sharp, William E.] Sharp Technol LLC, Ann Arbor, MI 48103 USA. [Zaccheo, T. Scott] AER, Lexington, MA USA. [Browell, Edward V.] NASA, STARSS Affiliate 2, LaRC, Hampton, VA USA. [Ismail, Syed] NASA, LaRC, Hampton, VA USA. [Dobler, Jeremy T.] Exelis, Ft Wayne, IN USA. [Llewellyn, Edward J.] Univ Saskatchewan, Dept Phys & Engn Phys, Saskatoon, SK, Canada. RP Sharp, WE (reprint author), Sharp Technol LLC, Ann Arbor, MI 48103 USA. EM wsharp01@comcast.net FU NASA Langley Research Center from Science Systems and Applications, Inc. Lanham, MD [21101.CY2.A069] FX This work was supported by NASA Langley Research Center under subcontract 21101.CY2.A069 from Science Systems and Applications, Inc. Lanham, MD, to Sharp Technologies LLC. Data for the generation of the figures and tables is available from the author. We thank Ian McDade and an anonymous reviewer for their helpful comments. NR 57 TC 0 Z9 0 U1 4 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 27 PY 2014 VL 119 IS 12 BP 7757 EP 7772 DI 10.1002/2013JD021324 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AN0BP UT WOS:000340247000044 ER PT J AU Dougherty, MJ Tran, HM Stavila, V Knierim, B George, A Auer, M Adams, PD Hadi, MZ AF Dougherty, Michael J. Tran, Huu M. Stavila, Vitalie Knierim, Bernhard George, Anthe Auer, Manfred Adams, Paul D. Hadi, Masood Z. TI Cellulosic Biomass Pretreatment and Sugar Yields as a Function of Biomass Particle Size SO PLOS ONE LA English DT Article ID IONIC LIQUID PRETREATMENT; 1-ETHYL-3-METHYLIMIDAZOLIUM ACETATE; ENZYMATIC SACCHARIFICATION; LIGNIN CONTENT; CORN STOVER; HYDROLYSIS; DECONSTRUCTION; DIGESTIBILITY; CELLULASE; ACID AB Three lignocellulosic pretreatment techniques (ammonia fiber expansion, dilute acid and ionic liquid) are compared with respect to saccharification efficiency, particle size and biomass composition. In particular, the effects of switchgrass particle size (32-200) on each pretreatment regime are examined. Physical properties of untreated and pretreated samples are characterized using crystallinity, surface accessibility measurements and scanning electron microscopy (SEM) imaging. At every particle size tested, ionic liquid (IL) pretreatment results in greater cell wall disruption, reduced crystallinity, increased accessible surface area, and higher saccharification efficiencies compared with dilute acid and AFEX pretreatments. The advantages of using IL pretreatment are greatest at larger particle sizes (>75 mu m). C1 [Dougherty, Michael J.; Tran, Huu M.; Knierim, Bernhard; George, Anthe; Auer, Manfred; Adams, Paul D.; Hadi, Masood Z.] Joint BioEnergy Inst, Emeryville, CA USA. [Dougherty, Michael J.; Tran, Huu M.; Stavila, Vitalie; George, Anthe; Hadi, Masood Z.] Sandia Natl Labs, Livermore, CA USA. [Knierim, Bernhard; Auer, Manfred; Adams, Paul D.] Lawrence Berkeley Natl Lab, Phys Biosci Div, Berkeley, CA USA. [Adams, Paul D.] Univ Calif Berkeley, Dept Bioengn, Berkeley, CA 94720 USA. RP Hadi, MZ (reprint author), NASA, Ames Res Ctr, Space BioSci Div, Synthet Biol Program, Moffett Field, CA 94035 USA. EM Masood.Hadi@NASA.gov RI Adams, Paul/A-1977-2013 OI Adams, Paul/0000-0001-9333-8219 FU U. S. Department of Energy, Office of Science, Office of Biological and Environmental Research [DE-AC02-05CH11231] FX This work was part of the DOE Joint BioEnergy Institute (http://www.jbei.org) supported by the U. S. Department of Energy, Office of Science, Office of Biological and Environmental Research, through contract DE-AC02-05CH11231 between Lawrence Berkeley National Laboratory and the U. S. Department of Energy. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 21 TC 5 Z9 5 U1 4 U2 33 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 JUN 27 PY 2014 VL 9 IS 6 AR e100836 DI 10.1371/journal.pone.0100836 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AK6BK UT WOS:000338512200067 PM 24971883 ER PT J AU 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 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 Cain, J 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 Fotopoulos, N 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 Gill, C Gleason, J Goetz, E Goetz, R Gondan, L Gonzalez, G Gordon, N Gorodetsky, ML Gossan, S Gossler, S Gouaty, R Graf, C Graff, PB Granata, M Grant, A Gras, S Gray, C Greenhalgh, RJS Gretarsson, AM Groot, P Grote, H Grover, K Grunewald, S Guidi, GM Guido, 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 Haris, K 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, G Jones, R Jonker, RJG Ju, L 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 Krishnan, B 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 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 Martelli, F Martin, IW Martin, RM Martinelli, L Martynov, D Marx, JN Mason, K Masserot, A Massinger, TJ Matichard, F 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Zendri, JP Zhang, F Zhang, L Zhao, C Zhu, H Zhu, XJ Zucker, ME Zuraw, S Zweizig, J AF Aasi, J. 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Unnikrishnan, C. S. Urban, A. L. Usman, S. A. Vahlbruch, H. Vajente, G. Valdes, G. Vallisneri, M. van Beuzekom, M. van den Brand, J. F. J. Van den Broeck, C. van der Sluys, M. V. van Heijningen, J. van Veggel, A. A. Vass, S. Vasuth, M. Vaulin, R. Vecchio, A. Vedovato, G. Veitch, J. Veitch, P. J. Venkateswara, K. Verkindt, D. Vetrano, F. Vicere, A. Vincent-Finley, R. Vinet, J. -Y. Vitale, S. Vo, T. Vocca, H. Vorvick, C. Vousden, W. D. Vyachanin, S. P. Wade, A. R. Wade, L. Wade, M. Walker, M. Wallace, L. Walsh, S. 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. D. Williamson, A. R. Willis, J. L. Willke, B. Wimmer, M. Winkler, W. Wipf, C. C. Wiseman, A. G. Wittel, H. Woan, G. Wolovick, N. Worden, J. Wu, Y. Yablon, J. Yakushin, I. Yam, W. Yamamoto, H. Yancey, C. C. Yang, H. Yoshida, S. Yvert, M. Zadrozny, A. Zanolin, M. Zendri, J. -P. Zhang, Fan Zhang, L. Zhao, C. Zhu, H. Zhu, X. J. Zucker, M. E. Zuraw, S. Zweizig, J. CA LIGO Sci Collaboration Virgo Collaboration TI Methods and results of a search for gravitational waves associated with gamma-ray bursts using the GEO 600, LIGO, and Virgo detectors SO PHYSICAL REVIEW D LA English DT Article ID NEUTRON-STARS; LOCAL UNIVERSE; SHORT-DURATION; GIANT FLARE; SCIENCE RUN; GRB 051103; SWIFT ERA; REDSHIFT; MISSION; ORIGIN AB In this paper we report on a search for short-duration gravitational wave bursts in the frequency range 64 Hz-1792 Hz associated with gamma-ray bursts (GRBs), using data from GEO 600 and one of the LIGO or Virgo detectors. We introduce the method of a linear search grid to analyze GRB events with large sky localization uncertainties, for example the localizations provided by the Fermi Gamma-ray Burst Monitor (GBM). Coherent searches for gravitational waves (GWs) can be computationally intensive when the GRB sky position is not well localized, due to the corrections required for the difference in arrival time between detectors. Using a linear search grid we are able to reduce the computational cost of the analysis by a factor of O(10) for GBM events. Furthermore, we demonstrate that our analysis pipeline can improve upon the sky localization of GRBs detected by the GBM, if a high-frequency GW signal is observed in coincidence. We use the method of the linear grid in a search for GWs associated with 129 GRBs observed satellite-based gamma-ray experiments between 2006 and 2011. The GRBs in our sample had not been previously analyzed for GW counterparts. A fraction of our GRB events are analyzed using data from GEO 600 while the detector was using squeezed-light states to improve its sensitivity; this is the first search for GWs using data from a squeezed-light interferometric observatory. We find no evidence for GW signals, either with any individual GRB in this sample or with the population as a whole. For each GRB we place lower bounds on the distance to the progenitor, under an assumption of a fixed GW emission energy of 10(-2)M circle dot c(2), with a median exclusion distance of 0.8 Mpc for emission at 500 Hz and 0.3 Mpc at 1 kHz. The reduced computational cost associated with a linear search grid will enable rapid searches for GWs associated with Fermi GBM events once the advanced LIGO and Virgo detectors begin operation. C1 [Aasi, J.; Abbott, B. P.; Abbott, R.; Abernathy, M. R.; Adhikari, R. X.; Anderson, R. A.; Anderson, S. B.; Arai, K.; Araya, M. C.; 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.; Fotopoulos, N.; Gushwa, K.; Gustafson, E. K.; Hall, E. D.; Harms, J.; Heptonstall, A. W.; Hodge, K. A.; Ivanov, A.; Jacobson, M.; Kalmus, P.; Kanner, J. B.; Kells, W.; King, P. J.; Kondrashov, V.; Korth, W. Z.; Kozak, D. B.; Lewis, J.; Li, T. G. F.; Libbrecht, K.; Mageswaran, M.; Mailand, K.; Maros, E.; Martynov, D.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Osthelder, C.; Patel, P.; Pedraza, M.; Phelps, M.; Price, L. R.; Privitera, S.; Quintero, E.; Raymond, V.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Sannibale, V.; Shao, Z.; Singer, A.; Singer, L.; Smith, M. R.; Smith, R. J. E.; Smith-Lefebvre, N. D.; Taylor, R.; Thirugnanasambandam, M. P.; Thrane, E.; Torrie, C. I.; Vass, S.; Wallace, L.; Weinstein, A. J.; Williams, R.; Yamamoto, H.; Zhang, L.; Zweizig, J.] CALTECH, LIGO, Pasadena, CA 91125 USA. [Abbott, T.; Corbitt, T. R.; DeRosa, R. T.; Effler, A.; Giaime, J. A.; Gonzalez, G.; Hamilton, W.; Johnson, W. W.; Kokeyama, K.; Macleod, D. 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J.; Hanson, J.; Heintze, M.; Holt, K.; Huynh-Dinh, T.; Katzman, W.; Kinzel, D. L.; Le Roux, A.; Lormand, M.; Meyer, M. S.; Nolting, D.; Oram, R.; O'Reilly, B.; Overmier, H.; Ramet, C.; Riesen, R.; Roddy, S. B.; Romie, J. H.; Sellers, D.; Stuver, A. L.; Thomas, M.; Thorne, K. A.; Traylor, G.; Welborn, T.; Yakushin, I.] LIGO Livingston Observ, Livingston, LA 70754 USA. [Adams, T.; Cadonati, L.; Edwards, M.; Fairhurst, S.; Hannam, M. D.; Hopkins, P.; Jones, G.; Macdonald, E. P.; Ohme, F.; Predoi, V.; Puerrer, M.; Sathyaprakash, B. S.; Schmidt, P.; Schutz, B. F.; Williamson, A. R.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales. [Addesso, P.; Castaldi, G.; Croce, R. P.; DeSalvo, R.; Pierro, V.; Pinto, I. M.] Univ Sannio Benevento, I-82100 Benevento, Italy. [Addesso, P.; Castaldi, G.; Croce, R. P.; DeSalvo, R.; Pierro, V.; Pinto, I. M.] Ist Nazl Fis Nucl, Sez Napoli, I-80100 Naples, Italy. [Affeldt, C.; Allen, B.; Aulbert, C.; Bauchrowitz, J.; Baune, C.; Bergmann, G.; Bock, O.; Bogan, C.; Born, M.; Brinkmann, M.; Dahl, K.; Dal Canton, T.; Damjanic, M.; Danzmann, K.; Denker, T.; Dent, T.; Di Palma, I.; Dooley, K. L.; Eberle, T.; Eggenstein, H. -B.; Fehrmann, H.; Frede, M.; Fricke, T. T.; Goetz, E.; Gossler, S.; Grote, H.; Hanke, M.; Heurs, M.; Hewitson, M.; Kawazoe, F.; Keitel, D.; Keppel, D. G.; Khalaidovski, A.; Koehlenbeck, S.; Kringel, V.; Krishnan, B.; Kuehn, G.; Leong, J. R.; Lueck, H.; Lundgren, A. P.; Machenschalk, B.; Manca, G. M.; Mazzolo, G.; Mehmet, M.; Mossavi, K.; Mow-Lowry, C. M.; Nielsen, A. B.; Oppermann, P.; Pickenpack, M.; Poeld, J.; Ruediger, A.; Salemi, F.; Schilling, R.; Schnabel, R.; Schreiber, E.; Schuette, D.; Shaltev, M.; Simakov, D.; Steinke, M.; Steinlechner, J.; Steinlechner, S.; Tarabrin, S. P.; Tuennermann, H.; Was, M.; Weinert, M.; Wessels, P.; Westphal, T.; Wette, K.; Wiesner, K.; Willke, B.; Wimmer, M.; Winkler, W.; Wittel, H.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. [Agathos, M.; Bauer, Th. S.; Beker, M. G.; Bertolini, A.; Bloemen, S.; Bulten, H. J.; Del Pozzo, W.; Ghosh, S.; Jonker, R. J. G.; Mailand, K.; Nelemans, G.; Rabeling, D. S.; Shah, S.; van Beuzekom, M.; van den Brand, J. F. J.; Van den Broeck, C.; van der Sluys, M. V.; van Heijningen, J.; Veitch, J.] Nikhef, NL-1098 XG Amsterdam, Netherlands. [Aggarwal, N.; Barsotti, L.; Biscans, S.; Bodiya, T. P.; Buikema, A.; Donovan, F.; Essick, R.; Evans, M.; Fritschel, P.; Gras, S.; Isogai, T.; Katsavounidis, E.; Lee, P. J.; Libson, A.; Macleod, D. M.; Mason, K.; Matichard, F.; Mavalvala, N.; Miller, J.; Mittleman, R.; Oelker, E.; Sankar, S.; Shoemaker, D. H.; Vaulin, R.; Vitale, S.; Weiss, R.; Wipf, C. C.; Yam, W.; Zhang, Fan; Zucker, M. E.] MIT, LIGO, Cambridge, MA 02139 USA. 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[Cagnoli, G.; Degallaix, J.; Dolique, V.; Flaminio, R.; Granata, M.; Hofman, D.; Michel, C.; Morgado, N.; Pinard, L.; Saracco, E.; Sassolas, B.; Straniero, N.] Univ Lyon, CNRS, IN2P3, Lab Materiaux Avances, F-69622 Lyon, France. [Calderon Bustillo, J.; Husa, S.; Jimenez-Forteza, F.; Sintes, A. M.; Trias, M.] Univ Illes Balears, E-07122 Palma de Mallorca, Spain. [Calloni, E.; De Rosa, R.; Garufi, F.; Milano, L.] Univ Naples Federico II, I-80126 Naples, Italy. [Cannon, K. C.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Cao, J.; Du, Z.; Ji, Y.; Lebigot, E. O.; Wang, X.; Zhang, Fan] Tsinghua Univ, Beijing 100084, Peoples R China. [Caride, S.; Gustafson, R.; Meadors, G. D.; Riles, K.; Sanders, J. R.] Univ Michigan, Ann Arbor, MI 48109 USA. [Cesarini, E.; D'Antonio, S.; Fafone, V.; Lorenzini, M.; Malvezzi, V.; Minenkov, Y.; Nardecchia, I.; Re, V.; Rocchi, A.; Sequino, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. 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Strigin, Sergey/I-8337-2012; Leonardi, Matteo/G-9694-2015; Sigg, Daniel/I-4308-2015; Bell, Angus/E-7312-2011; Costa, Cesar/G-7588-2012; Hild, Stefan/A-3864-2010; Danilishin, Stefan/K-7262-2012; Gammaitoni, Luca/B-5375-2009; Huerta, Eliu/J-5426-2014; Gemme, Gianluca/C-7233-2008; Losurdo, Giovanni/K-1241-2014; Wu, Ying/B-7283-2009; Steinlechner, Sebastian/D-5781-2013; Kumar, Prem/B-6691-2009; prodi, giovanni/B-4398-2010; Lam, Ping Koy/A-5276-2008; Strain, Kenneth/D-5236-2011; Miao, Haixing/O-1300-2013; 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; 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; Travasso, Flavio/J-9595-2016 OI Murphy, David/0000-0002-8538-815X; Pitkin, Matthew/0000-0003-4548-526X; Veitch, John/0000-0002-6508-0713; Davies, Gareth/0000-0002-4289-3439; Gendre, Bruce/0000-0002-9077-2025; Allen, Bruce/0000-0003-4285-6256; Granata, Massimo/0000-0003-3275-1186; Kanner, Jonah/0000-0001-8115-0577; Freise, Andreas/0000-0001-6586-9901; Mandel, Ilya/0000-0002-6134-8946; Whiting, Bernard F/0000-0002-8501-8669; Puppo, Paola/0000-0003-4677-5015; Tacca, Matteo/0000-0003-1353-0441; Graef, Christian/0000-0002-4535-2603; Garufi, Fabio/0000-0003-1391-6168; Deleglise, Samuel/0000-0002-8680-5170; 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; 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; O'Shaughnessy, Richard/0000-0001-5832-8517; Collette, Christophe/0000-0002-4430-3703; Coccia, Eugenio/0000-0002-6669-5787; Vetrano, Flavio/0000-0002-7523-4296; Addesso, Paolo/0000-0003-0895-184X; Denker, Timo/0000-0003-1259-5315; Howell, Eric/0000-0001-7891-2817; Fairhurst, Stephen/0000-0001-8480-1961; Husa, Sascha/0000-0002-0445-1971; Papa, M.Alessandra/0000-0002-1007-5298; Vocca, Helios/0000-0002-1200-3917; Aulbert, Carsten/0000-0002-1481-8319; 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; Drago, Marco/0000-0002-3738-2431; Boschi, Valerio/0000-0001-8665-2293; Pierro, Vincenzo/0000-0002-6020-5521; Naticchioni, Luca/0000-0003-2918-0730; Ward, Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447; Dolique, Vincent/0000-0001-5644-9905; Whelan, John/0000-0001-5710-6576; Vedovato, Gabriele/0000-0001-7226-1320; Punturo, Michele/0000-0001-8722-4485; Cella, Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167; Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Ciani, Giacomo/0000-0003-4258-9338; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Matichard, Fabrice/0000-0001-8982-8418; calloni, enrico/0000-0003-4819-3297; Iyer, Bala R./0000-0002-4141-5179; Lee, Chang-Hwan/0000-0003-3221-1171; Gorodetsky, Michael/0000-0002-5159-2742; McClelland, David/0000-0001-6210-5842; M, Manjunath/0000-0001-8710-0730; Vecchio, Alberto/0000-0002-6254-1617; Sigg, Daniel/0000-0003-4606-6526; Bell, Angus/0000-0003-1523-0821; Danilishin, Stefan/0000-0001-7758-7493; Gammaitoni, Luca/0000-0002-4972-7062; Gemme, Gianluca/0000-0002-1127-7406; Losurdo, Giovanni/0000-0003-0452-746X; Steinlechner, Sebastian/0000-0003-4710-8548; prodi, giovanni/0000-0001-5256-915X; Lam, Ping Koy/0000-0002-4421-601X; Strain, Kenneth/0000-0002-2066-5355; Miao, Haixing/0000-0003-4101-9958; 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; Frasconi, Franco/0000-0003-4204-6587; Groot, Paul/0000-0002-4488-726X; Lazzaro, Claudia/0000-0001-5993-3372; Ferrante, Isidoro/0000-0002-0083-7228; Travasso, Flavio/0000-0002-4653-6156 FU 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 and the 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; Alfred P. Sloan Foundation FX We are indebted to the observers of the electromagnetic events and the Gamma-ray burst Coordinates Network for providing us with valuable data. 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 GEO 600 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, and the Alfred P. Sloan Foundation. We also gratefully acknowledge the team of graduate students and scientists who maintained the H2 instrument during the Astrowatch epoch, without whom a substantial fraction of our events would not have been analyzed. This paper has been assigned LIGO Document No. LIGO-P1300086. NR 96 TC 12 Z9 12 U1 3 U2 52 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD JUN 25 PY 2014 VL 89 IS 12 AR 122004 DI 10.1103/PhysRevD.89.122004 PG 17 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AK8FY UT WOS:000338664000002 ER PT J AU Robinson, TD Maltagliati, L Marley, MS Fortney, JJ AF Robinson, Tyler D. Maltagliati, Luca Marley, Mark S. Fortney, Jonathan J. TI Titan solar occultation observations reveal transit spectra of a hazy world SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE transit spectroscopy; extrasolar planet ID SUPER-EARTH GJ1214B; EXTRASOLAR PLANET ATMOSPHERE; HUBBLE-SPACE-TELESCOPE; EXOPLANET GJ 1214B; TRANSMISSION SPECTRUM; SPECTROSCOPY; CLOUDS; RETRIEVAL; MASS; ULTRAVIOLET AB High-altitude clouds and hazes are integral to understanding exoplanet observations, and are proposed to explain observed featureless transit spectra. However, it is difficult to make inferences from these data because of the need to disentangle effects of gas absorption from haze extinction. Here, we turn to the quintessential hazy world, Titan, to clarify how high-altitude hazes influence transit spectra. We use solar occultation observations of Titan's atmosphere from the Visual and Infrared Mapping Spectrometer aboard National Aeronautics and Space Administration's (NASA) Cassini spacecraft to generate transit spectra. Data span 0.88-5 mu m at a resolution of 12-18 nm, with uncertainties typically smaller than 1%. Our approach exploits symmetry between occultations and transits, producing transit radius spectra that inherently include the effects of haze multiple scattering, refraction, and gas absorption. We use a simple model of haze extinction to explore how Titan's haze affects its transit spectrum. Our spectra show strong methane-absorption features, and weaker features due to other gases. Most importantly, the data demonstrate that high-altitude hazes can severely limit the atmospheric depths probed by transit spectra, bounding observations to pressures smaller than 0.1-10 mbar, depending on wavelength. Unlike the usual assumption made when modeling and interpreting transit observations of potentially hazy worlds, the slope set by haze in our spectra is not flat, and creates a variation in transit height whose magnitude is comparable to those from the strongest gaseous-absorption features. These findings have important consequences for interpreting future exoplanet observations, including those from NASA's James Webb Space Telescope. C1 [Robinson, Tyler D.; Marley, Mark S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Robinson, Tyler D.] NASA, Virtual Planetary Lab, Astrobiol Inst, Seattle, WA 98195 USA. [Maltagliati, Luca] Univ Paris 06, CNRS, Observ Paris, Lab Etud Spatiales & Instrumentat Astrophys, F-92195 Meudon, France. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Robinson, TD (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM tyler.d.robinson@nasa.gov RI Marley, Mark/I-4704-2013; OI Marley, Mark/0000-0002-5251-2943 FU NASA Postdoctoral Program at NASA Ames Research Center; Agence Nationale de la Recherche (ANR Project "Analysis of Photometric Observations for the Study of Titan Climate", France) [11BS56002]; NASA's Planetary Atmospheres program; National Science Foundation FX We thank W. B. Hubbard, P. Muirhead, and an anonymous referee for friendly and constructive feedback on earlier versions of this work. T.D.R. acknowledges support from an appointment to the NASA Postdoctoral Program at NASA Ames Research Center, administered by Oak Ridge Affiliated Universities. L.M. thanks the Agence Nationale de la Recherche (ANR Project "Analysis of Photometric Observations for the Study of Titan Climate" 11BS56002, France). M.S.M. and J.J.F. acknowledge support from NASA's Planetary Atmospheres program. J.J.F. also acknowledges support from the National Science Foundation. NR 60 TC 9 Z9 10 U1 1 U2 11 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 JUN 24 PY 2014 VL 111 IS 25 BP 9042 EP 9047 DI 10.1073/pnas.1403473111 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AJ5WJ UT WOS:000337760600024 PM 24876272 ER PT J AU Guanter, L Zhang, YG Jung, M Joiner, J Voigt, M Berry, JA Frankenberg, C Huete, AR Zarco-Tejada, P Lee, JE Moran, MS Ponce-Campos, G Beer, C Camps-Valls, G Buchmann, N Gianelle, D Klumpp, K Cescatti, A Baker, JM Griffis, TJ AF Guanter, Luis Zhang, Yongguang Jung, Martin Joiner, Joanna Voigt, Maximilian Berry, Joseph A. Frankenberg, Christian Huete, Alfredo R. Zarco-Tejada, Pablo Lee, Jung-Eun Moran, M. Susan Ponce-Campos, Guillermo Beer, Christian Camps-Valls, Gustavo Buchmann, Nina Gianelle, Damiano Klumpp, Katja Cescatti, Alessandro Baker, John M. Griffis, Timothy J. TI Reply to Magnani et al.: Linking large-scale chlorophyll fluorescence observations with cropland gross primary production SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter C1 [Guanter, Luis; Zhang, Yongguang; Voigt, Maximilian] Free Univ Berlin, Inst Space Sci, D-12165 Berlin, Germany. [Jung, Martin] Max Planck Inst Biogeochem, Dept Biogeochem Syst, D-07745 Jena, Germany. [Joiner, Joanna] NASA, Goddard Space Flight Ctr, Lab Atmospher Chem & Dynam, Greenbelt, MD 20771 USA. [Berry, Joseph A.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. [Frankenberg, Christian] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Huete, Alfredo R.] Univ Technol Sydney, Plant Funct Biol & Climate Change Cluster, Sydney, NSW 2007, Australia. [Zarco-Tejada, Pablo] CSIC, Inst Agr Sostenible, Cordoba 14004, Spain. [Lee, Jung-Eun] Brown Univ, Providence, RI 02912 USA. [Moran, M. Susan; Ponce-Campos, Guillermo] ARS, Southwest Watershed Res, USDA, Tucson, AZ 85719 USA. [Beer, Christian] Stockholm Univ, Dept Appl Environm Sci, S-10691 Stockholm, Sweden. [Beer, Christian] Stockholm Univ, Bolin Ctr Climate Res, S-10691 Stockholm, Sweden. [Camps-Valls, Gustavo] Univ Valencia, Image Proc Lab, Valencia 46980, Spain. [Buchmann, Nina] ETH, CH-8092 Zurich, Switzerland. [Gianelle, Damiano] Fdn Edmund Mach, Res & Innovat Ctr, Sustainable Agroecosyst & Bioresources Dept, I-38010 San Michele All Adige, Italy. [Klumpp, Katja] INRA, Grassland Ecosyst Res Unit, F-63122 Clermont Ferrand, France. [Cescatti, Alessandro] Commiss European Communities, Joint Res Ctr, Inst Environm & Sustainabil, I-20127 Ispra, Italy. [Baker, John M.] ARS, USDA, St Paul, MN 55108 USA. [Griffis, Timothy J.] Univ Minnesota, Dept Soil Water & Climate, St Paul, MN 55108 USA. RP Guanter, L (reprint author), Free Univ Berlin, Inst Space Sci, D-12165 Berlin, Germany. EM luis.guanter@wew.fu-berlin.de RI Frankenberg, Christian/A-2944-2013; Griffis, Timothy/A-5707-2011; Zarco-Tejada, Pablo J./A-6874-2012; Guanter, Luis/I-1588-2015; Buchmann, Nina/E-6095-2011; Huete, Alfredo/C-1294-2008; Beer, Christian/D-2296-2013; Gianelle, Damiano/G-9437-2011 OI Frankenberg, Christian/0000-0002-0546-5857; Zhang, Yongguang/0000-0001-8286-300X; Zarco-Tejada, Pablo J./0000-0003-1433-6165; Guanter, Luis/0000-0002-8389-5764; Huete, Alfredo/0000-0003-2809-2376; Gianelle, Damiano/0000-0001-7697-5793 NR 5 TC 3 Z9 3 U1 3 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 JUN 24 PY 2014 VL 111 IS 25 BP E2511 EP E2511 DI 10.1073/pnas.1406996111 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AJ5WJ UT WOS:000337760600002 PM 25093229 ER PT J AU Magnani, F Raddi, S Mohammed, G Middleton, EM AF Magnani, Federico Raddi, Sabrina Mohammed, Gina Middleton, Elizabeth M. TI Let's exploit available knowledge on vegetation fluorescence SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter ID CHLOROPHYLL FLUORESCENCE; PHOTOSYNTHESIS C1 [Magnani, Federico] Univ Bologna, Dept Agr Sci, I-40127 Bologna, Italy. [Raddi, Sabrina] Univ Florence, Dept Agr Food & Forest Syst Management, I-50145 Florence, Italy. [Mohammed, Gina] P&M Technol, Marie, ON P6A 6S7, Canada. [Middleton, Elizabeth M.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. RP Magnani, F (reprint author), Univ Bologna, Dept Agr Sci, I-40127 Bologna, Italy. EM federico.magnani@unibo.it RI Magnani, Federico/A-2448-2011 OI Magnani, Federico/0000-0003-4479-0916 NR 5 TC 3 Z9 3 U1 3 U2 23 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 JUN 24 PY 2014 VL 111 IS 25 BP E2510 EP E2510 DI 10.1073/pnas.1406600111 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AJ5WJ UT WOS:000337760600001 PM 24927587 ER PT J AU Soebiyanto, RP Clara, W Jara, J Castillo, L Sorto, OR Marinero, S de Antinori, MEB McCracken, JP Widdowson, MA Azziz-Baumgartner, E Kiang, RK AF Soebiyanto, Radina P. Clara, Wilfrido Jara, Jorge Castillo, Leticia Rene Sorto, Oscar Marinero, Sidia Barnett de Antinori, Maria E. McCracken, John P. Widdowson, Marc-Alain Azziz-Baumgartner, Eduardo Kiang, Richard K. TI The Role of Temperature and Humidity on Seasonal Influenza in Tropical Areas: Guatemala, El Salvador and Panama, 2008-2013 SO PLOS ONE LA English DT Article ID RELATIVE-HUMIDITY; TRANSMISSION; VIRUS; SURVEILLANCE; SURVIVAL; EPIDEMICS; COUNTRIES; PATTERNS; DRIVERS; CENTERS AB Background: The role of meteorological factors on influenza transmission in the tropics is less defined than in the temperate regions. We assessed the association between influenza activity and temperature, specific humidity and rainfall in 6 study areas that included 11 departments or provinces within 3 tropical Central American countries: Guatemala, El Salvador and Panama. Method/Findings: Logistic regression was used to model the weekly proportion of laboratory-confirmed influenza positive samples during 2008 to 2013 (excluding pandemic year 2009). Meteorological data was obtained from the Tropical Rainfall Measuring Mission satellite and the Global Land Data Assimilation System. We found that specific humidity was positively associated with influenza activity in El Salvador (Odds Ratio (OR) and 95% Confidence Interval of 1.18 (1.07-1.31) and 1.32 (1.08-1.63)) and Panama (OR = 1.44 (1.08-1.93) and 1.97 (1.34-2.93)), but negatively associated with influenza activity in Guatemala (OR = 0.72 (0.6-0.86) and 0.79 (0.69-0.91)). Temperature was negatively associated with influenza in El Salvador's west-central departments (OR = 0.80 (0.7-0.91)) whilst rainfall was positively associated with influenza in Guatemala's central departments (OR = 1.05 (1.01-1.09)) and Panama province (OR = 1.10 (1.05-1.14)). In 4 out of the 6 locations, specific humidity had the highest contribution to the model as compared to temperature and rainfall. The model performed best in estimating 2013 influenza activity in Panama and west-central El Salvador departments (correlation coefficients: 0.5-0.9). Conclusions/Significance: The findings highlighted the association between influenza activity and specific humidity in these 3 tropical countries. Positive association with humidity was found in El Salvador and Panama. Negative association was found in the more subtropical Guatemala, similar to temperate regions. Of all the study locations, Guatemala had annual mean temperature and specific humidity that were lower than the others. C1 [Soebiyanto, Radina P.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res GESTAR, Columbia, MD USA. [Soebiyanto, Radina P.; Kiang, Richard K.] NASA, Global Change Data Ctr, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Clara, Wilfrido] Ctr Dis Control & Prevent CDC, Reg Off Cent Amer Reg, Influenza Program, Guatemala City, Guatemala. [Jara, Jorge; McCracken, John P.] Univ Valle Guatemala, Influenza Unit, Ctr Hlth Studies, Guatemala City, Guatemala. [Castillo, Leticia] Minist Hlth Guatemala, Natl Influenza Ctr, Guatemala City, Guatemala. [Rene Sorto, Oscar] Minist Hlth El Salvador, Hlth Surveillance Div, San Salvador, El Salvador. [Marinero, Sidia] Minist Environm & Nat Resources El Salvador, Div Meteorol, Natl Environm Observ, San Salvador, El Salvador. [Barnett de Antinori, Maria E.] Gorgas Mem Inst Hlth Studies, Natl Influenza Ctr, Panama City, Panama. [Widdowson, Marc-Alain; Azziz-Baumgartner, Eduardo] Ctr Dis Control & Prevent CDC, Influenza Div, Atlanta, GA USA. RP Kiang, RK (reprint author), NASA, Global Change Data Ctr, Goddard Space Flight Ctr, Code 610-2, Greenbelt, MD 20771 USA. EM richard.kiang@nasa.gov FU NASA Applied Science - Public Health program; CDC Influenza Division FX This study was supported by NASA Applied Science - Public Health program and CDC Influenza Division. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 51 TC 11 Z9 11 U1 1 U2 2 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 JUN 23 PY 2014 VL 9 IS 6 AR e100659 DI 10.1371/journal.pone.0100659 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AL1WV UT WOS:000338917900078 PM 24956184 ER PT J AU Han, JW Moon, DI Oh, JS Choi, YK Meyyappan, M AF Han, Jin-Woo Moon, Dong-Il Oh, Jae Sub Choi, Yang-Kyu Meyyappan, M. TI Vacuum gate dielectric gate-all-around nanowire for hot carrier injection and bias temperature instability free transistor SO APPLIED PHYSICS LETTERS LA English DT Article ID MOSFET AB A gate-all-around (GAA) field effect transistor with vacuum gate dielectric is presented as a structure free from hot-carrier injection and bias temperature instability. A conventional GAA fabrication process is used along with selective removal of the sacrificial gate oxide as an extra process step. The lowered dielectric constant in vacuum gate dielectric can be compensated by the nature of the nanowire and physical oxide thickness reduction. As the nanowire channel is fully surrounded by empty space, reliability issues relevant to the gate dielectric can be completely cleared. (C) 2014 AIP Publishing LLC. C1 [Han, Jin-Woo; Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. [Moon, Dong-Il; Choi, Yang-Kyu] Korea Adv Inst Sci & Technol, Dept Elect Engn, Taejon 305701, South Korea. [Oh, Jae Sub] Natl Nanofab Ctr, Taejon 305701, South Korea. RP Han, JW (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. EM jin-woo.han@nasa.gov NR 15 TC 3 Z9 3 U1 2 U2 22 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0003-6951 EI 1077-3118 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD JUN 23 PY 2014 VL 104 IS 25 AR 253506 DI 10.1063/1.4885595 PG 3 WC Physics, Applied SC Physics GA AK6CQ UT WOS:000338515900093 ER PT J AU Strekalov, DV Kowligy, AS Huang, YP Kumar, P AF Strekalov, Dmitry V. Kowligy, Abijith S. Huang, Yu-Ping Kumar, Prem TI Progress towards interaction-free all-optical devices SO PHYSICAL REVIEW A LA English DT Article ID QUANTUM; MICRODISKS; CAVITY AB We present an all-optical control device in which coupling a weak control optical field into a high-Q lithium niobate whispering-gallery-mode microcavity decouples it from a signal field due to nonlinear optical interactions. This results in switching and modulation of the signal with low-power control pulses. In the quantum limit, the underlying nonlinear-optical process corresponds to the quantum Zeno blockade. Its "interaction-free" nature effectively alleviates loss and decoherence for the signal waves. This work therefore presents experimental progress towards acquiring large phase shifts with few photons or even at the single-photon level. C1 [Strekalov, Dmitry V.] CALTECH, Jet Prop Lab, Pasadena, CA 91108 USA. [Kowligy, Abijith S.; Huang, Yu-Ping; Kumar, Prem] Northwestern Univ, Ctr Photon Commun & Comp, Evanston, IL 60208 USA. RP Strekalov, DV (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91108 USA. RI Kumar, Prem/B-6691-2009 FU DARPA Zeno-based Opto-Electronics program [W31P4Q-09-1-0014] FX This work was supported by the DARPA Zeno-based Opto-Electronics program (Grant No. W31P4Q-09-1-0014). It was partly carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We thank J. U. Furst and T. Beckmann for useful discussions. NR 22 TC 2 Z9 3 U1 0 U2 16 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 JUN 23 PY 2014 VL 89 IS 6 AR 063820 DI 10.1103/PhysRevA.89.063820 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AK6CM UT WOS:000338515400010 ER PT J AU Zhang, ZD Astrakharchik, GE Aveline, DC Choi, S Perrin, H Bergeman, TH Olshanii, M AF Zhang, Z. D. Astrakharchik, G. E. Aveline, D. C. Choi, S. Perrin, H. Bergeman, T. H. Olshanii, M. TI Breakdown of scale invariance in the vicinity of the Tonks-Girardeau limit SO PHYSICAL REVIEW A LA English DT Article ID BOSE-GAS; ATOMS; FERMIONS AB In this article, we consider the monopole excitations of a harmonically trapped Bose gas in the vicinity of the Tonks-Girardeau limit. Using Girardeau's Fermi-Bose duality and subsequently an effective fermion-fermion odd-wave interaction, we obtain the dominant correction to the scale-invariance-protected value of the excitation frequency, for microscopically small excitation amplitudes. We produce a series of diffusion Monte Carlo results that confirm our analytic prediction for three particles. And less expectedly, our result stands in excellent agreement with the result of a hydrodynamic simulation (with the Lieb-Liniger equation of state as an input) of the microscopically large but macroscopically small excitations. We also show that the frequency we obtain coincides with the upper bound derived by Menotti and Stringari using sum rules. Surprisingly, however, we found that the usually successful hydrodynamic perturbation theory predicts a shift that is 9/4 higher than its ab initio numerical counterpart. We conjecture that the sharp boundary of the cloud in local density approximation-characterized by an infinite density gradient-renders the perturbation inapplicable. All our results also directly apply to the three-dimensional p-wave-interacting waveguide-confined fermions. C1 [Zhang, Z. D.; Bergeman, T. H.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Astrakharchik, G. E.] Univ Politecn Cataluna, Dept Fis & Engn Nucl, E-08034 Barcelona, Spain. [Aveline, D. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Choi, S.; Olshanii, M.] Univ Massachusetts, Dept Phys, Boston, MA 02125 USA. [Perrin, H.] Univ Paris 13, Sorbonne Paris Cite, CNRS, Lab Phys Lasers, F-93430 Villetaneuse, France. RP Zhang, ZD (reprint author), SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. EM zhedong.zhang@stonybrook.edu RI Astrakharchik, Gregory/L-6181-2014; Olshanii, Maxim/M-2830-2013; Perrin, Helene/A-3428-2013 OI Astrakharchik, Gregory/0000-0003-0394-8094; Olshanii, Maxim/0000-0003-3629-6002; Perrin, Helene/0000-0001-5624-4133 FU Institut Francilien de Recherche sur les Atomes Froids (IFRAF); MEC (Spain) through the Ramon y Cajal fellowship program; DGI (Spain) [FIS2011-25275]; Generalitat de Catalunya [2009SGR-1003]; NSF [PHY-0968905, PHY-1019197]; Office of Naval Research [N00014-12-1-0400] FX We acknowledge support from the Institut Francilien de Recherche sur les Atomes Froids (IFRAF). G.E.A. acknowledges financial support from MEC (Spain) through the Ramon y Cajal fellowship program, DGI (Spain) Grant No. FIS2011-25275 and Generalitat de Catalunya Grant No. 2009SGR-1003. Z.D.Z. and T.B. were supported by the NSF Grant No. PHY-0968905. M.O. was supported by grants from the Office of Naval Research (Grant No. N00014-12-1-0400) and the NSF Grant No. PHY-1019197. Laboratoire de Physique des Lasers is UMR 7538 of CNRS and Paris 13 University. NR 36 TC 5 Z9 5 U1 1 U2 5 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 JUN 23 PY 2014 VL 89 IS 6 AR 063616 DI 10.1103/PhysRevA.89.063616 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AK6CM UT WOS:000338515400008 ER PT J AU Tam, CKW Pastouchenko, NN Jones, MG Watson, WR AF Tam, Christopher K. W. Pastouchenko, Nikolai N. Jones, Michael G. Watson, Willie R. TI Experimental validation of numerical simulations for an acoustic liner in grazing flow: Self-noise and added drag SO JOURNAL OF SOUND AND VIBRATION LA English DT Article ID FINITE-DIFFERENCE SCHEMES; PRESSURE OSCILLATIONS; BOUNDARY-CONDITIONS; IMPEDANCE; RESONATORS; ORIFICE; AEROACOUSTICS; CAVITIES; LAYER AB A coordinated experimental and numerical simulation effort is carried out to improve our understanding of the physics of acoustic liners in a grazing flow as well our computational aeroacoustics (CAA) method prediction capability. A numerical simulation code based on advanced CAA methods is developed. In a parallel effort, experiments are performed using the Grazing Flow Impedance Tube at the NASA Langley Research Center. In the experiment, a liner is installed in the upper wall of a rectangular flow duct with a 2 in. by 2.5 in. cross section. Spatial distribution of sound pressure levels and relative phases are measured on the wall opposite the liner in the presence of a Mach 0.3 grazing flow. The computer code is validated by comparing computed results with experimental measurements. Good agreements are found. The numerical simulation code is then used to investigate the physical properties of the acoustic liner. It is shown that an acoustic liner can produce self-noise in the presence of a grazing flow and that a feedback acoustic resonance mechanism is responsible for the generation of this liner self-noise. In addition, the same mechanism also creates additional liner drag. An estimate, based on numerical simulation data, indicates that for a resonant liner with a 10 percent open area ratio, the drag increase would be about 4 percent of the turbulent boundary layer drag over a flat wall. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Tam, Christopher K. W.; Pastouchenko, Nikolai N.] Florida State Univ, Tallahassee, FL 32306 USA. [Jones, Michael G.; Watson, Willie R.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Tam, CKW (reprint author), Florida State Univ, Tallahassee, FL 32306 USA. EM tam@math.fsu.edu FU NASA Langley Research Center through a Phase II SBIR contract FX CKWT and NNP wish to acknowledge the support of NASA Langley Research Center through a Phase II SBIR contract. NR 33 TC 8 Z9 8 U1 1 U2 16 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0022-460X EI 1095-8568 J9 J SOUND VIB JI J. Sound Vibr. PD JUN 23 PY 2014 VL 333 IS 13 BP 2831 EP 2854 DI 10.1016/j.jsv.2014.02.019 PG 24 WC Acoustics; Engineering, Mechanical; Mechanics SC Acoustics; Engineering; Mechanics GA AG2VB UT WOS:000335274100011 ER PT J AU Lindeman, MA Bonetti, JA Bumble, B Day, PK Eom, BH Holmes, WA Kleinsasser, AW AF Lindeman, M. A. Bonetti, J. A. Bumble, B. Day, P. K. Eom, B. H. Holmes, W. A. Kleinsasser, A. W. TI Arrays of membrane isolated yttrium-barium-copper-oxide kinetic inductance bolometers SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID THIN-FILMS; ION-BOMBARDMENT; RESONATORS; DEPOSITION; NOISE; SI AB We are developing of arrays of membrane isolated resonator-bolometers, each with a kinetic inductance device (KID) to measure the temperature of the membrane. The KIDs are fabricated out of the high temperature superconductor YBCO to allow operation at relatively high temperatures. The bolometers are designed to offer higher sensitivity than sensors operating at 300 K, but they require less expensive and lighter weight cooling than even more sensitive conventional superconducting detectors operating at lower temperatures. The bolometer arrays are applicable as focal planes in infrared imaging spectrometers, such as for planetary science missions or earth observing satellites. We describe the devices and present measurements of their sensitivity. C1 [Lindeman, M. A.; Bonetti, J. A.; Bumble, B.; Day, P. K.; Holmes, W. A.; Kleinsasser, A. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Eom, B. H.] CALTECH, Pasadena, CA 91125 USA. RP Lindeman, MA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mark.a.lindeman@jpl.nasa.gov FU NASA FX This research was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. IBAD deposition of MgO was performed by I-Beam Materials. The YBCO was deposited by Ceraco Ceramic Coating and patterned by Star Cryoelectronics. The authors would like to thank Vince Kotsubo for useful discussions. NR 28 TC 3 Z9 3 U1 0 U2 10 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-8979 EI 1089-7550 J9 J APPL PHYS JI J. Appl. Phys. PD JUN 21 PY 2014 VL 115 IS 23 AR 234509 DI 10.1063/1.4884437 PG 4 WC Physics, Applied SC Physics GA AK0MB UT WOS:000338106000077 ER PT J AU Dwek, E Staguhn, J Arendt, RG Kovacks, A Su, T Benford, DJ AF Dwek, Eli Staguhn, Johannes Arendt, Richard G. Kovacks, Attila Su, Ting Benford, Dominic J. TI DUST FORMATION, EVOLUTION, AND OBSCURATION EFFECTS IN THE VERY HIGH-REDSHIFT UNIVERSE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE dust, extinction; galaxies: evolution; galaxies: high-redshift; galaxies: individual (MACS1149-JD); nuclear reactions, nucleosynthesis, abundances ID INTERSTELLAR DUST; SOLAR NEIGHBORHOOD; SDSS J1148+5251; GALAXIES; ORIGIN; SUPERNOVAE; EMISSION; STARS; MODEL AB The evolution of dust at redshifts z greater than or similar to 9, and consequently the dust properties, differs greatly from that in the local universe. In contrast to the local universe, core collapse supernovae (CCSNe) are the only source of thermally condensed dust. Because of the low initial dust-to-gas mass ratio, grain destruction rates are low, so that CCSNe are net producers of interstellar dust. Galaxies with large initial gas mass or high mass infall rate will therefore have a more rapid net rate of dust production compared to galaxies with lower gas mass, even at the same star formation rate. The dust composition is dominated by silicates, which exhibit a strong rise in the UV opacity near the Lyman break. This "silicate-UV break" may be confused with the Lyman break, resulting in a misidentification of a galaxy's photometric redshift. In this Letter we demonstrate these effects by analyzing the spectral energy distribution of MACS1149-JD, a lensed galaxy at z = 9.6. A potential 2 mm counterpart of MACS1149-JD has been identified with GISMO. While additional observations are required to corroborate this identification, we use this possible association to illustrate the physical processes and the observational effects of dust in the very high-redshift universe. C1 [Dwek, Eli; Staguhn, Johannes; Arendt, Richard G.; Kovacks, Attila; Su, Ting; Benford, Dominic J.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Staguhn, Johannes; Su, Ting] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Arendt, Richard G.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA. [Kovacks, Attila] CALTECH, Dept Astron, Pasadena, CA 90025 USA. [Kovacks, Attila] Univ Minnesota, Dept Astron, St Paul, MN 12345 USA. RP Dwek, E (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. EM eli.dwek@nasa.gov RI Kovacs, Attila/C-1171-2010; Benford, Dominic/D-4760-2012; OI Kovacs, Attila/0000-0001-8991-9088; Benford, Dominic/0000-0002-9884-4206; Arendt, Richard/0000-0001-8403-8548 FU NSF ATI [1020981, 1106284]; INSU/CNRS (France); MPG (Germany); IGN (Spain); [NASA-ROSES-ATP2012] FX This work was supported through NSF ATI grants 1020981 and 1106284 (J.S., T.S., A.K. and the GISMO observations). IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). E.D. and R.G.A. acknowledges support of NASA-ROSES-ATP2012. We acknowledge the comments made by the referee which have led to a more detailed discussion on the origin of dust in the early universe. E.D. thanks Rachel Somerville for a helpful discussion. NR 34 TC 11 Z9 11 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 JUN 20 PY 2014 VL 788 IS 2 AR L30 DI 10.1088/2041-8205/788/2/L30 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK5YX UT WOS:000338504500011 ER PT J AU Obenberger, KS Taylor, GB Hartman, JM Dowell, J Ellingson, SW Helmboldt, JF Henning, PA Kavic, M Schinzel, FK Simonetti, JH Stovall, K Wilson, TL AF Obenberger, K. S. Taylor, G. B. Hartman, J. M. Dowell, J. Ellingson, S. W. Helmboldt, J. F. Henning, P. A. Kavic, M. Schinzel, F. K. Simonetti, J. H. Stovall, K. Wilson, T. L. TI DETECTION OF RADIO EMISSION FROM FIREBALLS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE meteorites; meteors; meteoroids ID ORIGIN; BURST AB We present the findings from the Prototype All-Sky Imager, a back end correlator of the first station of the Long Wavelength Array, which has recorded over 11,000 hr of all-sky images at frequencies between 25 and 75 MHz. In a search of this data for radio transients, we have found 49 long-duration (10 s of seconds) transients. Ten of these transients correlate both spatially and temporally with large meteors (fireballs), and their signatures suggest that fireballs emit a previously undiscovered low frequency, non-thermal pulse. This emission provides a new probe into the physics of meteors and identifies a new form of naturally occurring radio transient foreground. C1 [Obenberger, K. S.; Taylor, G. B.; Dowell, J.; Henning, P. A.; Schinzel, F. K.; Stovall, K.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Hartman, J. M.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Ellingson, S. W.] Virginia Tech, Bradley Dept Elect Engn, Blacksburg, VA 24061 USA. [Helmboldt, J. F.; Wilson, T. L.] US Naval Res Lab, Washington, DC 20375 USA. [Kavic, M.] Long Isl Univ, Dept Phys, Brooklyn, NY 11201 USA. [Simonetti, J. H.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. RP Obenberger, KS (reprint author), Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. RI Helmboldt, Joseph/C-8105-2012 FU Office of Naval Research [N00014-07-C-0147]; National Science Foundation [AST-1139963, AST-1139974] FX Construction of LWA1 has been 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 Observatory program. NR 25 TC 8 Z9 8 U1 0 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 JUN 20 PY 2014 VL 788 IS 2 AR L26 DI 10.1088/2041-8205/788/2/L26 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK5YX UT WOS:000338504500007 ER PT J AU Sterling, AC Moore, RL Falconer, DA Knox, JM AF Sterling, Alphonse C. Moore, Ronald L. Falconer, David A. Knox, Javon M. TI NEW ASPECTS OF A LID-REMOVAL MECHANISM IN THE ONSET OF AN ERUPTION SEQUENCE THAT PRODUCED A LARGE SOLAR ENERGETIC PARTICLE (SEP) EVENT SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: coronal mass ejections (CMEs); Sun: filaments, prominences; Sun: flares; Sun: magnetic fields; Sun: particle emission ID CORONAL MASS EJECTIONS; EMISSION MEASURES; FLARES; FILAMENT; HINODE; STEREO; SUN; SDO; RECONNECTION; TEMPERATURES AB We examine a sequence of two ejective eruptions from a single active region on 2012 January 23, using magnetograms and EUV images from the Solar Dynamics Observatory's (SDO) Helioseismic and Magnetic Imager (HMI) and Atmospheric and Imaging Assembly (AIA), and EUV images from STEREO/EUVI. This sequence produced two coronal mass ejections (CMEs) and a strong solar energetic particle event (SEP); here we focus on the magnetic onset of this important space weather episode. Cheng et al. showed that the first eruption's ("Eruption 1") flux rope was apparent only in "hotter" AIA channels, and that it removed overlying field that allowed the second eruption ("Eruption 2") to begin via ideal MHD instability; here we say that Eruption 2 began via a "lid removal" mechanism. We show that during Eruption 1's onset, its flux rope underwent a "tether weakening" (TW) reconnection with field that arched from the eruption-source active region to an adjacent active region. Standard flare loops from Eruption 1 developed over Eruption 2's flux rope and enclosed filament, but these overarching new loops were unable to confine that flux rope/filament. Eruption 1's flare loops, from both TW reconnection and standard-flare-model internal reconnection, were much cooler than Eruption 2's flare loops (GOES thermal temperatures of similar to 7.5 MK and 9 MK, compared to similar to 14 MK). The corresponding three sequential GOES flares were, respectively, due to TW reconnection plus earlier phase Eruption 1 tether-cutting reconnection, Eruption 1 later-phase tether-cutting reconnection, and Eruption 2 tether-cutting reconnection. C1 [Sterling, Alphonse C.; Moore, Ronald L.; Falconer, David A.] Heliophys & Planetary Sci Off, Marshall Space Flight Ctr, ZP13, Huntsville, AL 35812 USA. [Moore, Ronald L.; Falconer, David A.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. [Falconer, David A.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Knox, Javon M.] Norfolk State Univ, Dept Phys, Norfolk, VA 23504 USA. RP Sterling, AC (reprint author), Heliophys & Planetary Sci Off, Marshall Space Flight Ctr, ZP13, Huntsville, AL 35812 USA. EM alphonse.sterling@nasa.gov; ron.moore@nasa.gov FU Heliophysics Division of NASA's Science Mission Directorate through the Living With a Star Targeted Research and Technology Program; Hinode Project; NSF FX We thank the referee for improving the presentation, and for an insightful suggestion regarding the speed of the second eruption. A.C.S. and R.L.M. were supported by funding from the Heliophysics Division of NASA's Science Mission Directorate through the Living With a Star Targeted Research and Technology Program, and the Hinode Project. J.M.K. was supported by NSF's Research Experience for Undergraduates Program. NR 46 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 20 PY 2014 VL 788 IS 2 AR L20 DI 10.1088/2041-8205/788/2/L20 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK5YX UT WOS:000338504500001 ER PT J AU Wirstrom, ES Charnley, SB Persson, CM Buckle, JV Cordiner, MA Takakuwa, S AF Wirstrom, E. S. Charnley, S. B. Persson, C. M. Buckle, J. V. Cordiner, M. A. Takakuwa, S. TI COLD WATER VAPOR IN THE BARNARD 5 MOLECULAR CLOUD SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: individual objects (Barnard 5); ISM: molecules; stars: formation; submillimeter: ISM ID WAVE-ASTRONOMY-SATELLITE; STAR-FORMING REGIONS; ROTATIONAL-EXCITATION; RADIATIVE-TRANSFER; LINE OBSERVATIONS; DENSE CLOUDS; HERSCHEL; EMISSION; CORES; CH3OH AB After more than 30 yr of investigations, the nature of gas-grain interactions at low temperatures remains an unresolved issue in astrochemistry. Water ice is the dominant ice found in cold molecular clouds; however, there is only one region where cold (similar to 10 K) water vapor has been detected-L1544. This study aims to shed light on ice desorption mechanisms under cold cloud conditions by expanding the sample. The clumpy distribution of methanol in dark clouds testifies to transient desorption processes at work-likely to also disrupt water ice mantles. Therefore, the Herschel HIFI instrument was used to search for cold water in a small sample of prominent methanol emission peaks. We report detections of the ground-state transition of o-H2O (J = 1(10)-1(01)) at 556.9360 GHz toward two positions in the cold molecular cloud, Barnard 5. The relative abundances of methanol and water gas support a desorption mechanism which disrupts the outer ice mantle layers, rather than causing complete mantle removal. C1 [Wirstrom, E. S.; Persson, C. M.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden. [Charnley, S. B.; Cordiner, M. A.] NASA Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20770 USA. [Charnley, S. B.; Cordiner, M. A.] NASA Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20770 USA. [Buckle, J. V.] Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Buckle, J. V.] Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Cordiner, M. A.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Takakuwa, S.] Acad Sinica, Inst Astron & Astrophys, Tokyo 106, Japan. RP Wirstrom, ES (reprint author), Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden. EM eva.wirstrom@chalmers.se OI Wirstrom, Eva/0000-0002-0656-876X FU NASA's Exobiology Program; Goddard Center for Astrobiology; Swedish National Space Board FX Part of this work was supported by NASA's Exobiology Program and The Goddard Center for Astrobiology. E. S. W. and C. M. P. acknowledge generous support from the Swedish National Space Board. NR 39 TC 2 Z9 2 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 JUN 20 PY 2014 VL 788 IS 2 AR L32 DI 10.1088/2041-8205/788/2/L32 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK5YX UT WOS:000338504500013 ER PT J AU Archambault, S Arlen, T Aune, T Beilicke, M Benbow, W Bird, R Bottcher, M Bouvier, A Buckley, JH Bugaev, V Ciupik, L Collins-Hughes, E Connolly, MP Cui, W Dickherber, R Dumm, J Errando, M Falcone, A Federici, S Feng, Q Finley, JP Fortson, L Furniss, A Galante, N Gall, D Garson, AI Gillanders, GH Griffin, S Grube, J Gusbar, C Gyuk, G Hanna, D Holder, J Hughes, G Kaaret, P Kertzman, M Khassen, Y Kieda, D Krawczynski, H Lamerato, A Lang, MJ Li, K Madhavan, AS Maier, G Majumdar, P McArthur, S McCann, A Millis, J Moriarty, P Mukherjee, R Nieto, D De Bhroithe, AO Ong, RA Orr, M Otte, AN Park, N Perkins, JS Pohl, M Popkow, A Prokoph, H Quinn, J Ragan, K Reynolds, PT Richards, GT Roache, E Roustazadeh, P Saxon, DB Sembroski, GH Senturk, GD Skole, C Staszak, D Telezhinsky, I Tesic, G Theiling, M Varlotta, A Vassiliev, VV Vincent, S Wakely, SP Weinstein, A Welsing, R Williams, DA Zitzer, B AF Archambault, S. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Bird, R. Boettcher, M. Bouvier, A. Buckley, J. H. Bugaev, V. Ciupik, L. Collins-Hughes, E. Connolly, M. P. Cui, W. Dickherber, R. Dumm, J. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fortson, L. Furniss, A. Galante, N. Gall, D. Garson, A. III. Gillanders, G. H. Griffin, S. Grube, J. Gusbar, C. Gyuk, G. Hanna, D. Holder, J. Hughes, G. Kaaret, P. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Lamerato, A. Lang, M. J. Li, K. Madhavan, A. S. Maier, G. Majumdar, P. McArthur, S. McCann, A. Millis, J. Moriarty, P. Mukherjee, R. Nieto, D. De Bhroithe, A. O'Faolain Ong, R. A. Orr, M. Otte, A. N. Park, N. Perkins, J. S. Pohl, M. Popkow, A. Prokoph, H. Quinn, J. Ragan, K. Reynolds, P. T. Richards, G. T. Roache, E. Roustazadeh, P. Saxon, D. B. Sembroski, G. H. Senturk, G. D. Skole, C. Staszak, D. Telezhinsky, I. Tesic, G. Theiling, M. Varlotta, A. Vassiliev, V. V. Vincent, S. Wakely, S. P. Weinstein, A. Welsing, R. Williams, D. A. Zitzer, B. TI TEST OF MODELS OF THE COSMIC INFRARED BACKGROUND WITH MULTIWAVELENGTH OBSERVATIONS OF THE BLAZAR 1ES 1218+30.4 IN 2009 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: general; BL Lacertae objects: individual (1ES1218+30.4); cosmic background radiation; diffuse radiation; galaxies: jets; gamma rays: galaxies ID GAMMA-RAY OBSERVATIONS; EXTRAGALACTIC MAGNETIC-FIELDS; ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; X-RAY; TEV BLAZARS; PARTICLE-ACCELERATION; VERITAS OBSERVATIONS; TIMING EXPLORER; STRONG FLARES AB We present the results of a multi-wavelength campaign targeting the blazar 1ES 1218+30.4 with observations with the 1.3 m McGraw-Hill optical telescope, the Rossi X-ray Timing Explorer (RXTE), the Fermi Gamma-Ray Space Telescope, and the Very Energetic Radiation Imaging Telescope Array System (VERITAS). The RXTE and VERITAS observations were spread over a 13 day period and revealed clear evidence for flux variability, and a strong X-ray and gamma-ray flare on 2009 February 26 (MJD 54888). The campaign delivered a well-sampled broadband energy spectrum with simultaneous RXTE and VERITAS very high energy (VHE, > 100 GeV) observations, as well as contemporaneous optical and Fermi observations. The 1ES 1218+30.4 broadband energy spectrum-the first with simultaneous X-ray and VHE gamma-ray energy spectra-is of particular interest as the source is located at a high cosmological redshift for a VHE source (z = 0.182), leading to strong absorption of VHE gamma rays by photons from the optical/infrared extragalactic background light (EBL) via gamma VHE +gamma EBL -> e(+) e(-)pair-creation processes. We model the data with a one-zone synchrotron self-Compton (SSC) emission model and with the extragalactic absorption predicted by several recent EBL models. We find that the observations are consistent with the SSC scenario and all the EBL models considered in this work. We discuss observational and theoretical avenues to improve on the EBL constraints. C1 [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Staszak, D.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Arlen, T.; Aune, T.; Ong, R. A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Garson, A. III.; Krawczynski, H.; Li, K.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bird, R.; Collins-Hughes, E.; Khassen, Y.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Boettcher, M.; Gusbar, C.; Gyuk, G.; Lamerato, A.; Roustazadeh, P.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. [Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Ciupik, L.; Grube, J.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Cui, W.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Dumm, J.; Fortson, L.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Errando, M.; Mukherjee, R.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Federici, S.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Skole, C.; Telezhinsky, I.; Vincent, S.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Federici, S.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam Golm, Germany. [Gall, D.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Holder, J.; Saxon, D. B.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Holder, J.; Saxon, D. B.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Madhavan, A. S.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Majumdar, P.] Saha Inst Nucl Phys, Kolkata 700064, India. [McArthur, S.; Park, N.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Nieto, D.; Senturk, G. D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Perkins, J. S.] NASA, GSFC, CRESST, Greenbelt, MD 20771 USA. [Perkins, J. S.] NASA, GSFC, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. [Perkins, J. S.] Univ Maryland, Baltimore, MD 21250 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. RP Archambault, S (reprint author), McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. 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; Lang, Mark/0000-0003-4641-4201; Bird, Ralph/0000-0002-4596-8563 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U.K FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748), and by STFC in the U.K. 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 72 TC 1 Z9 1 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 JUN 20 PY 2014 VL 788 IS 2 AR 158 DI 10.1088/0004-637X/788/2/158 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200061 ER PT J AU Chomiuk, L Nelson, T Mukai, K Sokoloski, JL Rupen, MP Page, KL Osborne, JP Kuulkers, E Mioduszewski, AJ Roy, N Weston, J Krauss, MI AF Chomiuk, Laura Nelson, Thomas Mukai, Koji Sokoloski, J. L. Rupen, Michael P. Page, Kim L. Osborne, Julian P. Kuulkers, Erik Mioduszewski, Amy J. Roy, Nirupam Weston, Jennifer Krauss, Miriam I. TI THE 2011 OUTBURST OF RECURRENT NOVA T Pyx: X-RAY OBSERVATIONS EXPOSE THE WHITE DWARF MASS AND EJECTION DYNAMICS SO ASTROPHYSICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; stars: individual (T Pyxidis); white dwarfs; X-rays: stars ID CLASSICAL NOVAE; RS-OPHIUCHI; SPECTROSCOPIC EVOLUTION; INTERSTELLAR-MEDIUM; SPECTRAL EVOLUTION; ORBITAL PERIOD; CENTRAL REGION; HERCULIS 1991; ATOMIC DATA; BLAST WAVE AB The recurrent nova T Pyx underwent its sixth historical outburst in 2011, and became the subject of an intensive multi-wavelength observational campaign. We analyze data from the Swift and Suzaku satellites to produce a detailed X-ray light curve augmented by epochs of spectral information. X-ray observations yield mostly non-detections in the first four months of outburst, but both a super-soft and hard X-ray component rise rapidly after Day 115. The super-soft X-ray component, attributable to the photosphere of the nuclear-burning white dwarf, is relatively cool (similar to 45 eV) and implies that the white dwarf in T Pyx is significantly below the Chandrasekhar mass (similar to 1 M similar to). The late turn-on time of the super-soft component yields a large nova ejecta mass (greater than or similar to 10-5 M ), consistent with estimates at other wavelengths. The hard X-ray component is well fit by a similar to 1 keV thermal plasma, and is attributed to shocks internal to the 2011 nova ejecta. The presence of a strong oxygen line in this thermal plasma on Day 194 requires a significantly super-solar abundance of oxygen and implies that the ejecta are polluted by white dwarf material. The X-ray light curve can be explained by a dual-phase ejection, with a significant delay between the first and second ejection phases, and the second ejection finally released two months after outburst. A delayed ejection is consistent with optical and radio observations of T Pyx, but the physical mechanism producing such a delay remains a mystery. C1 [Chomiuk, Laura] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Chomiuk, Laura; Rupen, Michael P.; Mioduszewski, Amy J.; Krauss, Miriam I.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Nelson, Thomas] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Mukai, Koji] CRESST, Greenbelt, MD 20771 USA. [Mukai, Koji] NASA GSFC, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Mukai, Koji] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Sokoloski, J. L.; Weston, Jennifer] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Page, Kim L.; Osborne, Julian P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Kuulkers, Erik] European Space Astron Ctr ESA ESAC, Sci Operat Dept, E-28691 Madrid, Spain. [Roy, Nirupam] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Chomiuk, L (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. EM chomiuk@pa.msu.edu RI XRAY, SUZAKU/A-1808-2009 FU UK Space Agency; NSF [AST-1211778] FX We are grateful to R. Williams, A. Ederoclite, M. Bode, R. Smith, and U. Munari for useful conversations. We thank the Suzaku mission for the generous allocation of target-of-opportunity time to observe T Pyx. We also thank Neil Gehrels and the Swift mission team for their support of the target-of-opportunity program for this nova. We acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this research. This work made use of the HEASARC archive, data supplied by the UK Swift Science Data Centre at the University of Leicester, and observations obtained with the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. L. Chomiuk is a Jansky Fellow of the National Radio Astronomy Observatory. J. Osborne and K. Page acknowledge the support of the UK Space Agency. J. L. Sokoloski and J. Weston acknowledge support from NSF award AST-1211778. NR 79 TC 11 Z9 11 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 JUN 20 PY 2014 VL 788 IS 2 AR 130 DI 10.1088/0004-637X/788/2/130 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200033 ER PT J AU Gershman, DJ Fisk, LA Gloeckler, G Raines, JM Slavin, JA Zurbuchen, TH Solomon, SC AF Gershman, Daniel J. Fisk, Lennard A. Gloeckler, George Raines, Jim M. Slavin, James A. Zurbuchen, Thomas H. Solomon, Sean C. TI THE VELOCITY DISTRIBUTION OF PICKUP He+ MEASURED AT 0.3 AU BY MESSENGER SO ASTROPHYSICAL JOURNAL LA English DT Article DE diffusion; ISM: atoms; methods: data analysis; scattering; solar wind; Sun: corona ID HELIUM FOCUSING CONE; ION-CYCLOTRON WAVES; PITCH-ANGLE SCATTERING; SOLAR-WIND; INTERSTELLAR HELIUM; INNER HELIOSPHERE; ALFVENIC FLUCTUATIONS; RADIAL EVOLUTION; LO OBSERVATIONS; PARAMETERS AB During its interplanetary trajectory in 2007-2009, the MErcury Surface, Space ENvrionment, GEochemistry, and Ranging ( MESSENGER) spacecraft passed through the gravitational focusing cone for interstellar helium multiple times at a heliocentric distance R approximate to 0.3 AU. Observations of He+ interstellar pickup ions made by the Fast Imaging Plasma Spectrometer sensor on MESSENGER during these transits provide a glimpse into the structure of newly formed inner heliospheric pickup- ion distributions. This close to the Sun, these ions are picked up in a nearly radial interplanetary magnetic field. Compared with the near- Earth environment, pickup ions observed near 0.3 AU will not have had sufficient time to be energized substantially. Such an environment results in a nearly pristine velocity distribution function that should depend only on pickup- ion injection velocities ( related to the interstellar gas), pitch- angle scattering, and cooling processes. From measured energy- per- charge spectra obtained during multiple spacecraft observational geometries, we have deduced the phase- space density of He+ as a function of magnetic pitch angle. Our measurements are most consistent with a distribution that decreases nearly monotonically with increasing pitch angle, rather than the more commonly modeled isotropic or hemispherically symmetric forms. These results imply that pitch- angle scattering of He+ may not be instantaneous, as is often assumed, and instead may reflect the velocity distribution of initially injected particles. In a slow solar wind stream, we find a parallel- scattering mean free path of lambda(parallel to) similar to 0.1 AU and a He+ production rate of similar to 0.05 m(-3) s(- 1) within 0.3 AU. C1 [Gershman, Daniel J.] NASA Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Gershman, Daniel J.; Fisk, Lennard A.; Gloeckler, George; Raines, Jim M.; Slavin, James A.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. RP Gershman, DJ (reprint author), NASA Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA. EM djgersh@umich.edu RI Slavin, James/H-3170-2012 OI Slavin, James/0000-0002-9206-724X FU NASA [NAS5-97271, NASW-00002]; NASA Postdoctoral Program at Goddard Space Flight Center 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 theCarnegie Institution ofWashington. D.J.G. is supported by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities. NR 69 TC 6 Z9 6 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 JUN 20 PY 2014 VL 788 IS 2 AR 124 DI 10.1088/0004-637X/788/2/124 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200027 ER PT J AU Gotthelf, EV Tomsick, JA Halpern, JP Gelfand, JD Harrison, FA Boggs, SE Christensen, FE Craig, WW Hailey, JC Kaspi, VM Stern, DK Zhang, WW AF Gotthelf, E. V. Tomsick, J. A. Halpern, J. P. Gelfand, J. D. Harrison, F. A. Boggs, S. E. Christensen, F. E. Craig, W. W. Hailey, J. C. Kaspi, V. M. Stern, D. K. Zhang, W. W. TI NuSTAR DISCOVERY OF A YOUNG, ENERGETIC PULSAR ASSOCIATED WITH THE LUMINOUS GAMMA-RAY SOURCE HESS J1640-465 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (G338.3-0.0, HESS J1640-465, 1FHL J1640.5-4634, AX J1640.7-4632, XMMU J164045.4-463131); ISM: supernova remnants; pulsars: individual (PSR J1640-4631); stars: neutron ID X-RAY; SUPERNOVA REMNANT; NEUTRON-STAR; WIND NEBULAE; CATALOG; CLUSTER; POPULATION; PROGENITOR; MAGNETAR; WESTERLUND-1 AB We report the discovery of a 206 ms pulsar associated with the TeV gamma-ray source HESS J1640-465 using the Nuclear Spectroscopic Telescope Array (NuSTAR) X-ray observatory. PSR J1640-4631 lies within the shelltype supernova remnant (SNR) G338.3-0.0, and coincides with an X-ray point source and putative pulsar wind nebula (PWN) previously identified in XMM-Newton and Chandra images. It is spinning down rapidly with period derivative P = 9.758(44) x 10(-13), yielding a spin-down luminosity E = 4.4 x 10(36) erg s(-1), characteristic age tau(c) = P/2P. = 3350 yr, and surface dipole magnetic field strength B-s = 1.4x10(13) G. For the measured distance of 12 kpc to G338.3-0.0, the 0.2-10 TeV luminosity of HESS J1640-465 is 6% of the pulsar's present E . The Fermi source 1FHL J1640.5-4634 is marginally coincident with PSR J1640-4631, but we find no gamma - ray pulsations in a search using five years of Fermi Large Area Telescope (LAT) data. The pulsar energetics support an evolutionary PWN model for the broadband spectrum of HESS J1640-465, provided that the pulsar's braking index is n approximate to 2, and that its initial spin period was P-0 similar to 15 ms. C1 [Gotthelf, E. V.; Halpern, J. P.; Hailey, J. C.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Tomsick, J. A.; Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Gelfand, J. D.] NYU Abu Dhabi, Abu Dhabi, U Arab Emirates. [Gelfand, J. D.] NYU, Ctr Cosmol & Particle Phys, New York, NY USA. [Harrison, F. A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Christensen, F. E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Kaspi, V. M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Stern, D. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gotthelf, EV (reprint author), Columbia Univ, Columbia Astrophys Lab, 550 West 120th St, New York, NY 10027 USA. EM eric@astro.columbia.edu RI Boggs, Steven/E-4170-2015; Gelfand, Joseph/F-1110-2015 OI Boggs, Steven/0000-0001-9567-4224; Gelfand, Joseph/0000-0003-4679-1058 FU National Aeronautics and Space Administration; NASA through Chandra Award [SAO GO2-13097X, GO1-12068A]; NASA [NAS8-03060]; Fermi Guest Investigator [NNX12AO89G]; Australian Research Council; Science Foundation for Physics within The University of Sydney FX This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. This work has also made use of archival data from the Chandra X-ray Observatory. Partial support for E.V.G. and J.A.T were provided by NASA through Chandra Award Numbers SAO GO2-13097X and GO1-12068A, respectively, 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. E.V.G acknowledges support by Fermi Guest Investigator Grant NNX12AO89G. Radio contours were obtained from Molonglo Observatory Synthesis Telescope (MOST) data provided by the University of Sydney with support from the Australian Research Council and the Science Foundation for Physics within The University of Sydney. NR 42 TC 13 Z9 13 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 JUN 20 PY 2014 VL 788 IS 2 AR 155 DI 10.1088/0004-637X/788/2/155 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200058 ER PT J AU Gronoff, G Maggiolo, R Wedlund, CS Mertens, CJ Norman, RB Bell, J Bernard, D Parkinson, CJ Vidal-Madjar, A AF Gronoff, G. Maggiolo, R. Wedlund, C. Simon Mertens, C. J. Norman, R. B. Bell, J. Bernard, D. Parkinson, C. J. Vidal-Madjar, A. TI THEORETICAL UV ABSORPTION SPECTRA OF HYDRODYNAMICALLY ESCAPING O-2/CO2-RICH EXOPLANETARY ATMOSPHERES SO ASTROPHYSICAL JOURNAL LA English DT Article DE molecular data; planets and satellites: atmospheres; planets and satellites: detection; ultraviolet: planetary systems ID CROSS-SECTION MEASUREMENTS; VENUS THERMOSPHERE; HD 209458B; HYDROGEN; CARBON; MODEL; O-2; CO2; NM AB Characterizing Earth- and Venus-like exoplanets' atmospheres to determine if they are habitable and how they are evolving (e.g., equilibrium or strong erosion) is a challenge. For that endeavor, a key element is the retrieval of the exospheric temperature, which is a marker of some of the processes occurring in the lower layers and controls a large part of the atmospheric escape. We describe a method to determine the exospheric temperature of an O-2- and/or CO2-rich transiting exoplanet, and we simulate the respective spectra of such a planet in hydrostatic equilibrium and hydrodynamic escape. The observation of hydrodynamically escaping atmospheres in young planets may help constrain and improve our understanding of the evolution of the solar system's terrestrial planets' atmospheres. We use the dependency of the absorption spectra of the O-2 and CO2 molecules on the temperature to estimate the temperature independently of the total absorption of the planet. Combining two observables (two parts of the UV spectra that have a different temperature dependency) with the model, we are able to determine the thermospheric density profile and temperature. If the slope of the density profile is inconsistent with the temperature, then we infer the hydrodynamic escape. We address the question of the possible biases in the application of the method to future observations, and we show that the flare activity should be cautiously monitored to avoid large biases. C1 [Gronoff, G.; Mertens, C. J.; Norman, R. B.] NASA LaRC, Hampton, VA 23681 USA. [Gronoff, G.] SSAI, Hampton, VA USA. [Maggiolo, R.] BIRA IASB, B-1180 Brussels, Belgium. [Wedlund, C. Simon] Aalto Univ, Sch Elect Engn, Dept Radio Sci & Engn, FI-00076 Aalto, Finland. [Bell, J.] Natl Inst Aerosp, Hampton, VA USA. [Bernard, D.] IPAG, Grenoble, France. [Parkinson, C. J.] Univ Michigan, Ann Arbor, MI 48109 USA. [Vidal-Madjar, A.] Observ Paris, F-75014 Paris, France. RP Gronoff, G (reprint author), NASA LaRC, Hampton, VA 23681 USA. EM Guillaume.P.Gronoff@nasa.gov RI Norman, Ryan/D-5095-2017; OI Norman, Ryan/0000-0002-9103-7225; Gronoff, Guillaume/0000-0002-0331-7076 NR 43 TC 0 Z9 0 U1 2 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 JUN 20 PY 2014 VL 788 IS 2 AR 191 DI 10.1088/0004-637X/788/2/191 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200094 ER PT J AU Jones, BM Kaiser, RI Strazzulla, G AF Jones, Brant M. Kaiser, Ralf I. Strazzulla, Giovanni TI CARBONIC ACID AS A RESERVE OF CARBON DIOXIDE ON ICY MOONS: THE FORMATION OF CARBON DIOXIDE (CO2) IN A POLAR ENVIRONMENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: laboratory: solid state; planets and satellites: composition; planets and satellites: surfaces; planet-star interactions; solid state: volatile ID INFRARED SPECTRAL PROPERTIES; PROTON IRRADIATED H2O+CO2; COSMIC-RAY PARTICLES; SOLAR-SYSTEM ICES; ION IRRADIATION; WATER-ICE; GALILEAN SATELLITES; INTERSTELLAR ICES; IONIZATION RADIATION; LABORATORY SPECTRA AB Carbon dioxide (CO2) has been detected on the surface of several icy moons of Jupiter and Saturn via observation of the nu(3) band with the Near-Infrared Mapping Spectrometer on board the Galileo spacecraft and the Visible-Infrared Mapping Spectrometer on board the Cassini spacecraft. Interestingly, the CO2 band for several of these moons exhibits a blueshift along with a broader profile than that seen in laboratory studies and other astrophysical environments. As such, numerous attempts have been made in order to clarify this abnormal behavior; however, it currently lacks an acceptable physical or chemical explanation. We present a rather surprising result pertaining to the synthesis of carbon dioxide in a polar environment. Here, carbonic acid was synthesized in a water (H2O)-carbon dioxide (CO2) (1:5) ice mixture exposed to ionizing radiation in the form of 5 keV electrons. The irradiated ice mixture was then annealed, producing pure carbonic acid which was then subsequently irradiated, recycling water and carbon dioxide. However, the observed carbon dioxide nu(3) band matches almost exactly with that observed on Callisto; subsequent temperature program desorption studies reveal that carbon dioxide synthesized under these conditions remains in solid form until 160 K, i.e., the sublimation temperature of water. Consequently, our results suggest that carbon dioxide on Callisto as well as other icy moons is indeed complexed with water rationalizing the shift in peak frequency, broad profile, and the solid state existence on these relatively warm moons. C1 [Jones, Brant M.; Kaiser, Ralf I.] Univ Hawaii Manoa, WM Keck Res Lab Astrochem, Honolulu, HI 96822 USA. [Jones, Brant M.; Kaiser, Ralf I.] Univ Hawaii Manoa, Dept Chem, Honolulu, HI 96822 USA. [Jones, Brant M.; Kaiser, Ralf I.] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA. [Strazzulla, Giovanni] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy. RP Jones, BM (reprint author), Univ Hawaii Manoa, WM Keck Res Lab Astrochem, Honolulu, HI 96822 USA. EM brantmj@hawaii.edu FU W.M. Keck Foundation; University of Hawai'i at Manoa; National Aeronautics and Space Administration through NASA Astrobiology Institute [NNA09DA77A] FX B.M.J and R.I.K would like to thank W.M. Keck Foundation and The University of Hawai'i at Manoa for their financial support. G.S. would like to acknowledge support from the National Aeronautics and Space Administration through the NASA Astrobiology Institute (Cooperative Agreement No. NNA09DA77A issued through the Office of Space Science). NR 84 TC 6 Z9 6 U1 5 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 JUN 20 PY 2014 VL 788 IS 2 AR 170 DI 10.1088/0004-637X/788/2/170 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200073 ER PT J AU Kawakita, H Dello Russo, N Vervack, R Kobayashi, H DiSanti, MA Opitom, C Jehin, E Weaver, HA Cochran, AL Harris, WM Bockelee-Morvan, D Biver, N Crovisier, J Mckay, AJ Manfroid, J Gillon, M AF Kawakita, Hideyo Dello Russo, Neil Vervack, Ron, Jr. Kobayashi, Hitomi DiSanti, Mike A. Opitom, Cyrielle Jehin, Emmanuel Weaver, Harold A. Cochran, Anita L. Harris, Walter M. Bockelee-Morvan, Dominique Biver, Nicolas Crovisier, Jacques Mckay, Adam J. Manfroid, Jean Gillon, Michael TI EXTREMELY ORGANIC-RICH COMA OF COMET C/2010 G2 ( HILL) DURING ITS OUTBURST IN 2012 SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets: general; comets: individual (C/2010 G2 (Hill); ISM: molecules; protoplanetary disks ID FORBIDDEN OXYGEN LINES; O1 HALE-BOPP; CHEMICAL-COMPOSITION; 103P/HARTLEY 2; GAS-RELEASE; KECK II; 17P/HOLMES; APPARITION; NIRSPEC; NUCLEI AB We performed high-dispersion near-infrared spectroscopic observations of comet C/2010 G2 (Hill) at 2.5 AU from the Sun using NIRSPEC (R approximate to 25,000) at the Keck II Telescope on UT 2012 January 9 and 10, about a week after an outburst had occurred. Over the two nights of our observations, prominent emission lines of CH4 and C2H6, along with weaker emission lines of H2O, HCN, CH3OH, and CO were detected. The gas production rate of CO was comparable to that of H2O during the outburst. The mixing ratios of CO, HCN, CH4, C2H6, and CH3OH with respect to H2O were higher than those for normal comets by a factor of five or more. The enrichment of CO and CH4 in comet Hill suggests that the sublimation of these hypervolatiles sustained the outburst of the comet. Some fraction of water in the inner coma might exist as icy grains that were likely ejected from nucleus by the sublimation of hypervolatiles. Mixing ratios of volatiles in comet Hill are indicative of the interstellar heritage without significant alteration in the solar nebula. C1 [Kawakita, Hideyo; Kobayashi, Hitomi] Kyoto Sangyo Univ, Koyama Astron Observ, Kita Ku, Kyoto 6038555, Japan. [Dello Russo, Neil; Vervack, Ron, Jr.; Weaver, Harold A.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [DiSanti, Mike A.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [Opitom, Cyrielle; Jehin, Emmanuel; Manfroid, Jean; Gillon, Michael] Univ Liege, Inst Astrophys & Geophys, FRS FNRS, B-4000 Liege, Belgium. [Cochran, Anita L.] McDonald Observ, Austin, TX 78712 USA. [Harris, Walter M.] Univ Calif Davis, Dept Appl Sci, Davis, CA 95616 USA. [Bockelee-Morvan, Dominique; Biver, Nicolas; Crovisier, Jacques] Univ Paris Diderot, UPMC, CNRS, LESIA,Observ Paris, F-92195 Meudon, France. [Mckay, Adam J.] New Mexico State Univ, Las Cruces, NM 88001 USA. RP Kawakita, H (reprint author), Kyoto Sangyo Univ, Koyama Astron Observ, Kita Ku, Kyoto 6038555, Japan. EM kawakthd@cc.kyoto-su.ac.jp RI Dello Russo, Neil/G-2727-2015; Vervack, Ronald/C-2702-2016; Weaver, Harold/D-9188-2016 OI Dello Russo, Neil/0000-0002-8379-7304; Vervack, Ronald/0000-0002-8227-9564; FU NASA Keck PI Data Award; MEXT [22540257] FX This work was supported by a NASA Keck PI Data Award administered by the NASA Exoplanet Science Institute. Data presented here were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The observatory was made possible by the generous financial support of the W. M. Keck Foundation. 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 work was also financially supported by MEXT under Grant-in-Aid for Scientific Research 22540257 (H. Kawakita). NR 35 TC 5 Z9 5 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 JUN 20 PY 2014 VL 788 IS 2 AR 110 DI 10.1088/0004-637X/788/2/110 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200013 ER PT J AU Materese, CK Cruikshank, DP Sandford, SA Imanaka, H Nuevo, M White, DW AF Materese, Christopher K. Cruikshank, Dale P. Sandford, Scott A. Imanaka, Hiroshi Nuevo, Michel White, Douglas W. TI ICE CHEMISTRY ON OUTER SOLAR SYSTEM BODIES: CARBOXYLIC ACIDS, NITRILES, AND UREA DETECTED IN REFRACTORY RESIDUES PRODUCED FROM THE UV PHOTOLYSIS OF N2: CH4: CO-CONTAINING ICES SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; Kuiper belt: general; molecular data; molecular processes; planets and satellites: surfaces; solid state: refractory ID CHARGED-PARTICLE IRRADIATION; TRANS-NEPTUNIAN OBJECTS; ADVANCED LIGHT-SOURCE; ULTRAVIOLET PHOTOIRRADIATION; OPTICAL-CONSTANTS; BUTYLDIMETHYLSILYL DERIVATIVES; INFRARED-SPECTROSCOPY; PREBIOTIC MOLECULES; SOLID NITROGEN; ANALOGS AB Radiation processing of the surface ices of outer solar system bodies may result in the production of new chemical species even at low temperatures. Many of the smaller, more volatile molecules that are likely produced by the photolysis of these ices have been well characterized by laboratory experiments. However, the more complex refractory material formed in these experiments remains largely uncharacterized. In this work, we present a series of laboratory experiments in which low-temperature (15-20 K) N2: CH4: CO ices in relative proportions 100: 1: 1 are subjected to UV irradiation, and the resulting materials are studied with a variety of analytical techniques including infrared spectroscopy, X-ray absorption near-edge structure spectroscopy, gas chromatography coupled with mass spectrometry, and high-resolution mass spectroscopy. Despite the simplicity of the reactants, these experiments result in the production of a highly complex mixture of molecules from relatively low-mass volatiles (tens of daltons) to high-mass refractory materials (hundreds of daltons). These products include various carboxylic acids, nitriles, and urea, which are also expected to be present on the surface of outer solar system bodies, including Pluto and other transneptunian objects. If these compounds occur in sufficient concentrations in the ices of outer solar system bodies, their characteristic bands may be detectable in the near-infrared spectra of these objects. C1 [Materese, Christopher K.; Cruikshank, Dale P.; Sandford, Scott A.; Imanaka, Hiroshi; Nuevo, Michel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Materese, Christopher K.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. [Imanaka, Hiroshi] SETI Inst, Mountain View, CA 94043 USA. [Imanaka, Hiroshi] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Nuevo, Michel] Bay Area Environm Res Inst, Petaluma, CA 94952 USA. [White, Douglas W.] Jacksonville State Univ, Jacksonville, AL 36265 USA. RP Materese, CK (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA. OI Materese, Christopher/0000-0003-2146-4288 NR 58 TC 15 Z9 15 U1 0 U2 17 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2014 VL 788 IS 2 DI 10.1088/0004-637X/788/2/111 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200014 ER PT J AU Ofek, EO Arcavi, I Tal, D Sullivan, M Gal-Yam, A Kulkarni, SR Nugent, PE Ben-Ami, S Bersier, D Cao, Y Cenko, SB De Cia, A Filippenko, AV Fransson, C Kasliwal, MM Laher, R Surace, J Quimby, R Yaron, O AF Ofek, Eran O. Arcavi, Iair Tal, David Sullivan, Mark Gal-Yam, Avishay Kulkarni, Shrinivas R. Nugent, Peter E. Ben-Ami, Sagi Bersier, David Cao, Yi Cenko, S. Bradley De Cia, Annalisa Filippenko, Alexei V. Fransson, Claes Kasliwal, Mansi M. Laher, Russ Surace, Jason Quimby, Robert Yaron, Ofer TI INTERACTION-POWERED SUPERNOVAE: RISE-TIME VERSUS PEAK-LUMINOSITY CORRELATION AND THE SHOCK-BREAKOUT VELOCITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: massive; stars: mass-loss; supernovae: general ID DENSE MASS-LOSS; X-RAY-EMISSION; LIGHT CURVES; SN 2009IP; CIRCUMSTELLAR MEDIUM; LOW-RESOLUTION; CORE-COLLAPSE; STAR; WIND; OUTBURST AB Interaction of supernova (SN) ejecta with the optically thick circumstellar medium (CSM) of a progenitor star can result in a bright, long-lived shock-breakout event. Candidates for such SNe include Type IIn and superluminous SNe. If some of these SNe are powered by interaction, then there should be a specific relation between their peak luminosity, bolometric light-curve rise time, and shock-breakout velocity. Given that the shock velocity during shock breakout is not measured, we expect a correlation, with a significant spread, between the rise time and the peak luminosity of these SNe. Here, we present a sample of 15 SNe IIn for which we have good constraints on their rise time and peak luminosity from observations obtained using the Palomar Transient Factory. We report on a possible correlation between the R-band rise time and peak luminosity of these SNe, with a false-alarm probability of 3%. Assuming that these SNe are powered by interaction, combining these observables and theory allows us to deduce lower limits on the shock-breakout velocity. The lower limits on the shock velocity we find are consistent with what is expected for SNe (i.e., similar to 10(4) km s(-1)). This supports the suggestion that the early-time light curves of SNe IIn are caused by shock breakout in a dense CSM. We note that such a correlation can arise from other physical mechanisms. Performing such a test on other classes of SNe ( e. g., superluminous SNe) can be used to rule out the interaction model for a class of events. C1 [Ofek, Eran O.; Arcavi, Iair; Tal, David; Gal-Yam, Avishay; Ben-Ami, Sagi; De Cia, Annalisa; Yaron, Ofer] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Sullivan, Mark] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Kulkarni, Shrinivas R.; Cao, Yi] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Nugent, Peter E.; Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Bersier, David] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Cenko, S. Bradley] NASA Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Fransson, Claes] Stockholm Univ, AlbaNova Univ Ctr, Oskar Klein Ctr, Dept Astron, SE-10691 Stockholm, Sweden. [Kasliwal, Mansi M.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Laher, Russ; Surace, Jason] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Quimby, Robert] Univ Tokyo, Kavli IPMU WPI, Kashiwa, Chiba 2778583, Japan. RP Ofek, EO (reprint author), Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. OI Sullivan, Mark/0000-0001-9053-4820; Gal-Yam, Avishay/0000-0002-3653-5598 FU Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ); Israeli Ministry of Science; I-CORE Program of the Planning and Budgeting Committee; ISF; BSF; GIF; Minerva; EU/FP7 via ERC grant [307260]; Israel Science Foundation; Israel Science Foundation, Minerva, Weizmann-UK; Hubble Fellowship; Carnegie-Princeton Fellowship; Christopher R.Redlich Fund; Richard and Rhoda Goldman Fund; TABASGO Foundation; NSF [AST-1211916] FX We thank Dan Perley for obtaining some spectra. E.O.O. thanks Ehud Nakar and Orly Gnat for discussions. This paper is based on observations obtained with the Samuel Oschin Telescope as part of the Palomar Transient Factory project, a scientific collaboration between the California Institute of Technology, Columbia University, Las Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scientific Computing Center, the University of Oxford, and the Weizmann Institute of Science. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We are grateful for excellent staff assistance at Palomar, Lick, and Keck Observatories. E.O.O. is incumbent of the Arye Dissentshik career development chair and is grateful to support by grants from the Willner Family Leadership Institute Ilan Gluzman (Secaucus NJ), Israeli Ministry of Science, Israel Science Foundation, Minerva, Weizmann-UK and the I-CORE Program of the Planning and Budgeting Committee and The Israel Science Foundation. A. G-Y. acknowledge grants from the ISF, BSF, GIF, Minerva, the EU/FP7 via ERC grant (307260), and the I-CORE program of the Planning and Budgeting Committee and The Israel Science Foundation. M.M.K. acknowledges generous support from the Hubble Fellowship and Carnegie-Princeton Fellowship. A.V.F.'s SN group at UC Berkeley has received generous financial assistance from Gary and Cynthia Bengier, the Christopher R.Redlich Fund, the Richard and Rhoda Goldman Fund, the TABASGO Foundation, and NSF grant AST-1211916. NR 61 TC 16 Z9 16 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 JUN 20 PY 2014 VL 788 IS 2 AR 154 DI 10.1088/0004-637X/788/2/154 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200057 ER PT J AU Rangwala, N Maloney, PR Glenn, J Wilson, CD Kamenetzky, J Schirm, MRP Spinoglio, L Santaella, MP AF Rangwala, Naseem Maloney, Philip R. Glenn, Jason Wilson, Christine D. Kamenetzky, Julia Schirm, Maximilien R. P. Spinoglio, Luigi Santaella, Miguel Pereira TI FIRST EXTRAGALACTIC DETECTION OF SUBMILLIMETER CH ROTATIONAL LINES FROM THE HERSCHEL SPACE OBSERVATORY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: ISM; galaxies: starburst; ISM: molecules; line: identification; techniques: spectroscopic ID DIFFUSE INTERSTELLAR-MEDIUM; STAR-FORMING REGIONS; MOLECULAR GAS; ABSORPTION-LINES; NGC 1068; CLOUDS; SPIRE; EMISSION; SPECTRUM; ARP-220 AB We present the first extragalactic detections of several CH rotational transitions in the far-infrared in four nearby galaxies, NGC 1068, Arp 220, M82, and NGC 253, using the Herschel Space Observatory. The CH lines in all four galaxies are a factor of 2-4 brighter than the adjacent HCN and HCO+ J = 6-5 lines (also detected in the same spectra). In the star-formation-dominated galaxies, M82, NGC 253, and Arp 220, the CH/CO abundance ratio is low (similar to 10(-5)), implying that the CH is primarily arising in diffuse and translucent gas where the chemistry is driven by UV radiation as found in the Milky Way interstellar matter. In NGC 1068, which has a luminous active galactic nucleus (AGN), the CH/CO ratio is an order of magnitude higher, suggesting that CH formation is driven by an X-ray-dominated region (XDR). Our XDR models show that both the CH and CO abundances in NGC 1068 can be explained by an XDR-driven chemistry for gas densities and molecular hydrogen column densities that are well constrained by the CO observations. We conclude that the CH/CO ratio may a good indicator of the presence of AGN in galaxies. We also discuss the feasibility of detecting CH in intermediate-to high-z galaxies with ALMA. C1 [Rangwala, Naseem; Maloney, Philip R.; Glenn, Jason; Kamenetzky, Julia] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80303 USA. [Rangwala, Naseem] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. [Wilson, Christine D.; Schirm, Maximilien R. P.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Spinoglio, Luigi; Santaella, Miguel Pereira] INAF, Ist Fis Spazio Interplanetario, I-00133 Rome, Italy. RP Rangwala, N (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, 1255 38th St, Boulder, CO 80303 USA. OI Pereira Santaella, Miguel/0000-0002-4005-9619 NR 26 TC 3 Z9 3 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 JUN 20 PY 2014 VL 788 IS 2 AR 147 DI 10.1088/0004-637X/788/2/147 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200050 ER PT J AU Rappaport, S Swift, J Levine, A Joss, M Sanchis-Ojeda, R Barclay, T Still, M Handler, G Olah, K Muirhead, PS Huber, D Vida, K AF Rappaport, S. Swift, J. Levine, A. Joss, M. Sanchis-Ojeda, R. Barclay, T. Still, M. Handler, G. Olah, K. Muirhead, P. S. Huber, D. Vida, K. TI M-DWARF RAPID ROTATORS AND THE DETECTION OF RELATIVELY YOUNG MULTIPLE M-STAR SYSTEMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: general; stars: activity; stars: late-type; stars: rotation; starspots; techniques: photometric ID FIELD M-DWARFS; DIFFERENTIAL ROTATION; BAYESIAN-APPROACH; MAGNETIC BRAKING; PLANET-CANDIDATE; ERROR-CORRECTION; TRANSIT SURVEY; MAIN-SEQUENCE; LIGHT CURVES; HR ORBIT AB We have searched the Kepler light curves of similar to 3900 M-star targets for evidence of periodicities that indicate, by means of the effects of starspots, rapid stellar rotation. Several analysis techniques, including Fourier transforms, inspection of folded light curves, "sonograms," and phase tracking of individual modulation cycles, were applied in order to distinguish the periodicities due to rapid rotation from those due to stellar pulsations, eclipsing binaries, or transiting planets. We find 178 Kepler M-star targets with rotation periods, P-rot, of < 2 days, and 110 with P-rot < 1 day. Some 30 of the 178 systems exhibit two or more independent short periods within the same Kepler photometric aperture, while several have 3 or more short periods. Adaptive optics imaging and modeling of the Kepler pixel response function for a subset of our sample support the conclusion that the targets with multiple periods are highly likely to be relatively young physical binary, triple, and even quadruple M star systems. We explore in detail the one object with four incommensurate periods all less than 1.2 days, and show that two of the periods arise from one of a close pair of stars, while the other two arise from the second star, which itself is probably a visual binary. If most of these M-star systems with multiple periods turn out to be bound M stars, this could prove a valuable way discovering young hierarchical M-star systems; the same approach may also be applicable to G and K stars. The similar to 5% occurrence rate of rapid rotation among the similar to 3900 M star targets is consistent with spin evolution models that include an initial contraction phase followed by magnetic braking, wherein a typical M star can spend several hundred Myr before spinning down to periods longer than 2 days. C1 [Rappaport, S.; Joss, M.; Sanchis-Ojeda, R.] MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Swift, J.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Swift, J.] CALTECH, Dept Planetary Sci, Pasadena, CA 91125 USA. [Levine, A.] 37 575 MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Barclay, T.; Still, M.] NASA, Ames Res Ctr, BAER Inst, Moffett Field, CA 94035 USA. [Handler, G.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Olah, K.; Vida, K.] MTA CSFK, Konkoly Observ, H-1525 Budapest, Hungary. [Muirhead, P. S.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Huber, D.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP Rappaport, S (reprint author), MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. EM sar@mit.edu; jswift@astro.caltech.edu; aml@space.mit.edu; mattjoss@mit.edu; rsanchis86@gmail.com; thomas.barclay@nasa.gov; martin.d.still@nasa.gov; gerald@camk.edu.pl; olah@konkoly.hu; philipm@bu.edu; daniel.huber@nasa.gov; vidakris@konkoly.hu RI Muirhead, Philip/H-2273-2014 OI Muirhead, Philip/0000-0002-0638-8822 FU NASA support through the Kepler Participating Scientist Program [NNX14AB92]; Kepler Participating Scientist Program; NASA Origins Program [NNX12AC76G, NNX11AG85]; Hubble Fellowship Program; NASA through Hubble Fellowship [HST-HF-51326.01-A]; STScI FX We acknowledge several useful discussions about the particular M star(s) KIC 7740983 with Robert Szabo and Katrien Kolenberg. We also thank Cristina Rodriguez-Lopez, Jim MacDonald, Jerome Quintin, Alex Brown, Gunter Houdek, and Lucianne Walkowicz for important discussions about the possibility of observing M-star pulsations with Kepler. Arthur Delarue wrote a very helpful code for automatically extracting significant incommensurate frequencies from FTs. We thank Sasha Hinkley and Benjamin Montet for performing a subset of our Keck AO observations. We are grateful to the Kepler team for providing such valuable data to the community. D. H. acknowledges NASA support through the Kepler Participating Scientist Program under grant NNX14AB92G.R.S.O. acknowledges support through the Kepler Participating Scientist Program and the NASA Origins Program under grants NNX12AC76G and NNX11AG85 G.P.S.M. acknowledges support from the Hubble Fellowship Program, provided by NASA through Hubble Fellowship grant HST-HF-51326.01-A awarded by the STScI, which is operated by the AURA, Inc., for NASA, under contract NAS 5-26555. G. H. is grateful for support by the Polish NCN grant 2011/01/B/ST9/05448. K. O. and K. V. acknowledge support from the Hungarian OTKA grants K-81421 and K-109276, and from "Lend "ulet-2012"Young Researchers' Programs of the Hungarian Academy of Sciences. This research has made use of the NASA Exoplanet Archive, and theMikulski Archive for Space Telescopes ( MAST). We made use of J-band images that were obtained with the United Kingdom Infrared Telescope ( UKIRT) which is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the U. K. 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. We acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community, and we are most fortunate to have the opportunity to conduct observations from this mountain. NR 58 TC 10 Z9 10 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 JUN 20 PY 2014 VL 788 IS 2 AR 114 DI 10.1088/0004-637X/788/2/114 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200017 ER PT J AU Schorghofer, N Aharonson, O AF Schorghofer, Norbert Aharonson, Oded TI THE LUNAR THERMAL ICE PUMP SO ASTROPHYSICAL JOURNAL LA English DT Article DE diffusion; molecular processes; Moon ID WATER ICE; POLAR-REGIONS; MOON; POLES AB It has long been suggested that water ice can exist in extremely cold regions near the lunar poles, where sublimation loss is negligible. The geographic distribution of H-bearing regolith shows only a partial or ambiguous correlation with permanently shadowed areas, thus suggesting that another mechanism may contribute to locally enhancing water concentrations. We show that under suitable conditions, water molecules can be pumped down into the regolith by day-night temperature cycles, leading to an enrichment of H2O in excess of the surface concentration. Ideal conditions for pumping are estimated and found to occur where the mean surface temperature is below 105 K and the peak surface temperature is above 120 K. These conditions complement those of the classical cold traps that are roughly defined by peak temperatures lower than 120 K. On the present-day Moon, an estimated 0.8% of the global surface area experiences such temperature variations. Typically, pumping occurs on pole-facing slopes in small areas, but within a few degrees of each pole the equator-facing slopes are preferred. Although pumping of water molecules is expected over cumulatively large areas, the absolute yield of this pump is low; at best, a few percent of the H2O delivered to the surface could have accumulated in the near-surface layer in this way. The amount of ice increases with vapor diffusivity and is thus higher in the regolith with large pore spaces. C1 [Schorghofer, Norbert] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Schorghofer, Norbert] Univ Hawaii, NASA Astrobiol Inst, Honolulu, HI 96822 USA. [Aharonson, Oded] Weizmann Inst Sci, Dept Earth & Planetary Sci, Helen Kimmel Ctr Planetary Sci, IL-76100 Rehovot, Israel. RP Schorghofer, N (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM norbert@hawaii.edu FU National Aeronautics and Space Administration through NASA Astrobiology Institute under Cooperative FX This material is in part based upon work supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement No. NNA09DA77A issued through the Office of Space Science, as well as by the Lunar Reconnaissance Orbiter project. We also thank the Diviner Science Team for sharing their data. NR 20 TC 8 Z9 8 U1 2 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 JUN 20 PY 2014 VL 788 IS 2 AR 169 DI 10.1088/0004-637X/788/2/169 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AJ2DT UT WOS:000337466200072 ER PT J AU Immerman, DA Goetz, FW AF Immerman, Douglas A. Goetz, Frederick W. TI The activation and cryopreservation of sablefish (Anoplopoma fimbria) sperm SO AQUACULTURE LA English DT Article DE Cryopreservation; Sablefish; Sperm; Marine teleost; Sperm activation; CASA ID COD GADUS-MORHUA; FRESH-WATER TELEOSTS; SEA-URCHIN SPERM; SCOPHTHALMUS-MAXIMUS; MARINE FISH; MOTILITY; SPERMATOZOA; EGGS; CHEMOTAXIS; OSMOLALITY AB Sablefish (Anoplopoma fimbria) is a deep-water marine species in the Pacific Ocean with a high commercial value. Limited information is available about male reproductive development and sperm physiology in sablefish or how to optimize fertilization and sperm storage in this species for aquaculture. In the present study the conditions required for sablefish sperm activation were investigated and an optimized regime for cryopreservation of sablefish sperm was developed. In all experiments, the assessment of sablefish sperm was conducted using a computer assisted sperm analysis (CASA) system that determined the velocity and linearity of motile sperm as well as the percent motile. A modified Cortland's solution was used as an extender in all activation and cryopreservation tests. Sperm were activated with ionic (NaCl, KCl, MgSO4 and CaCl2) and non-ionic (urea and glucose) solutions of varying osmolalities. KCl and NaCl activated sperm at the lowest osmolalities, followed by MgSO4, urea, glucose, and CaCl2. Compared to NaCl and KCl, non-ionic solutions required higher osmolalities for activation. The results indicate that the primary stimulus for sablefish sperm activation is increased osmolality and not the presence/absence of a specific ion. The effects of several cryoprotectants including dimethyl sulfoxide, propylene glycol and glycerol at two concentrations (5% and 10%) and three freezing rates (- 2.5, - 5 and - 7.5 degrees C/min) were tested on the cryopreservation of sperm using a Crysalys cryogenic programmable freezing system. There were differences observed in the motility maintained following freezing between all cryoprotectants, but the highest motility after freezing was observed with 10% dimethyl sulfoxide at all freezing rates. Sperm, cryopreserved with 10% DMSO, fertilized eggs but at rates lower than with fresh milt. Published by Elsevier B.V. C1 [Immerman, Douglas A.] Univ Washington, Sch Aquat & Fishery Sci, Seattle, WA 98195 USA. [Goetz, Frederick W.] Natl Marine Fisheries Serv, Resource Enhancement & Utilizat Technol Div, NW Fisheries Sci Ctr, NOAA,Manchester Res Stn, Manchester, WA 98366 USA. RP Goetz, FW (reprint author), Natl Marine Fisheries Serv, Resource Enhancement & Utilizat Technol Div, NW Fisheries Sci Ctr, NOAA,Manchester Res Stn, 7305 E Beach Dr, Manchester, WA 98366 USA. EM Immerd@uw.edu; Rick.Goetz@NOAA.gov FU Joint Institute for the Study of the Atmosphere and Ocean (JISAO) under NOAA Cooperative Agreement [NA10OAR4320148, 2230] FX This publication is partially funded by the Joint Institute for the Study of the Atmosphere and Ocean (JISAO) under NOAA Cooperative Agreement NA10OAR4320148, Contribution No. 2230. The authors would like to thank Ken Massee, Tom Wade, Matt Cook, Cort Jensen and Sean Oden for their help in collecting and maintaining the sablefish and milt used for these studies; Charles Muller for advice and guidance on sperm motility and cryopreservation; and Loveday Conquest for advice and guidance on statistical interpretations. NR 51 TC 2 Z9 2 U1 2 U2 25 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0044-8486 EI 1873-5622 J9 AQUACULTURE JI Aquaculture PD JUN 20 PY 2014 VL 430 BP 211 EP 217 DI 10.1016/j.aquaculture.2014.04.010 PG 7 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA AI0UG UT WOS:000336564900029 ER PT J AU Ade, PAR Aikin, RW Barkats, D Benton, SJ Bischoff, CA Bock, JJ Brevik, JA Buder, I Bullock, E Dowell, CD Duband, L Filippini, JP Fliescher, S Golwala, SR Halpern, M Hasselfield, M Hildebrandt, SR Hilton, GC Hristov, VV Irwin, KD Karkare, KS Kaufman, JP Keating, BG Kernasovskiy, SA Kovac, JM Kuo, CL Leitch, EM Lueker, M Mason, P Netterfield, CB Nguyen, HT O'Brient, R Ogburn, RW Orlando, A Pryke, C Reintsema, CD Richter, S Schwarz, R Sheehy, CD Staniszewski, ZK Sudiwala, RV Teply, GP Tolan, JE Turner, AD Vieregg, AG Wong, CL Yoon, KW AF Ade, P. A. R. Aikin, R. W. Barkats, D. Benton, S. J. Bischoff, C. A. Bock, J. J. Brevik, J. A. Buder, I. Bullock, E. Dowell, C. D. Duband, L. Filippini, J. P. Fliescher, S. Golwala, S. R. Halpern, M. Hasselfield, M. Hildebrandt, S. R. Hilton, G. C. Hristov, V. V. Irwin, K. D. Karkare, K. S. Kaufman, J. P. Keating, B. G. Kernasovskiy, S. A. Kovac, J. M. Kuo, C. L. Leitch, E. M. Lueker, M. Mason, P. Netterfield, C. B. Nguyen, H. T. O'Brient, R. Ogburn, R. W. Orlando, A. Pryke, C. Reintsema, C. D. Richter, S. Schwarz, R. Sheehy, C. D. Staniszewski, Z. K. Sudiwala, R. V. Teply, G. P. Tolan, J. E. Turner, A. D. Vieregg, A. G. Wong, C. L. Yoon, K. W. CA BICEP2 Collaboration TI Detection of B-Mode Polarization at Degree Angular Scales by BICEP2 SO PHYSICAL REVIEW LETTERS LA English DT Article ID MICROWAVE BACKGROUND POLARIZATION; PROBE WMAP OBSERVATIONS; INFLATIONARY UNIVERSE SCENARIO; SPT-SZ SURVEY; POWER SPECTRA; SYMMETRY-BREAKING; PHASE-TRANSITION; CMB POLARIMETRY; GRAVITY-WAVES; ANISOTROPY AB We report results from the BICEP2 experiment, a cosmic microwave background (CMB) polarimeter specifically designed to search for the signal of inflationary gravitational waves in the B-mode power spectrum around l similar to 80. The telescope comprised a 26 cm aperture all-cold refracting optical system equipped with a focal plane of 512 antenna coupled transition edge sensor 150 GHz bolometers each with temperature sensitivity of approximate to 300 mu K-CMB root s. BICEP2 observed from the South Pole for three seasons from 2010 to 2012. A low-foreground region of sky with an effective area of 380 square deg was observed to a depth of 87 nK deg in Stokes Q and U. In this paper we describe the observations, data reduction, maps, simulations, and results. We find an excess of B-mode power over the base lensed-ACDM expectation in the range 30 < l < 150, inconsistent with the null hypothesis at a significance of > 5 sigma. Through jackknife tests and simulations based on detailed calibration measurements we show that systematic contamination is much smaller than the observed excess. Cross correlating against WMAP 23 GHz maps we find that Galactic synchrotron makes a negligible contribution to the observed signal. We also examine a number of available models of polarized dust emission and find that at their default parameter values they predict power similar to(5-10)x smaller than the observed excess signal (with no significant cross-correlation with our maps). However, these models are not sufficiently constrained by external public data to exclude the possibility of dust emission bright enough to explain the entire excess signal. Cross correlating BICEP2 against 100 GHz maps from the BICEP1 experiment, the excess signal is confirmed with 3 sigma significance and its spectral index is found to be consistent with that of the CMB, disfavoring dust at 1.7 sigma. The observed B-mode power spectrum is well fit by a lensed-ACDM + tensor theoretical model with tensor-to-scalar ratio r = 0.20(-0.05)(+0.07), with r = 0 disfavored at 7.0 sigma. Accounting for the contribution of foreground, dust will shift this value downward by an amount which will be better constrained with upcoming data sets. C1 [Ade, P. A. R.; Sudiwala, R. V.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Aikin, R. W.; Bock, J. J.; Brevik, J. A.; Filippini, J. P.; Golwala, S. R.; Hildebrandt, S. R.; Hristov, V. V.; Lueker, M.; Mason, P.; Staniszewski, Z. K.; Teply, G. P.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [Barkats, D.] Joint ALMA Observ, Santiago, Chile. [Benton, S. J.; Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Bischoff, C. A.; Buder, I.; Karkare, K. S.; Kovac, J. M.; Richter, S.; Vieregg, A. G.; Wong, C. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bock, J. J.; Dowell, C. D.; Hildebrandt, S. R.; Nguyen, H. T.; O'Brient, R.; Staniszewski, Z. K.; Turner, A. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bullock, E.; Pryke, C.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. [Duband, L.] CEA, Serv Basses Temp, F-38054 Grenoble, France. [Fliescher, S.; Pryke, C.; Schwarz, R.; Sheehy, C. D.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Halpern, M.; Hasselfield, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Hilton, G. C.; Irwin, K. D.; Reintsema, C. D.] NIST, Boulder, CO 80305 USA. [Irwin, K. D.; Kernasovskiy, S. A.; Kuo, C. L.; Ogburn, R. W.; Tolan, J. E.; Yoon, K. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Irwin, K. D.; Kuo, C. L.; Ogburn, R. W.; Yoon, K. W.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Kaufman, J. P.; Keating, B. G.; Orlando, A.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Leitch, E. M.; Orlando, A.; Sheehy, C. D.; Vieregg, A. G.] Univ Chicago, Chicago, IL 60637 USA. [Netterfield, C. B.] Canadian Inst Adv Res, Toronto, ON M5G 1Z8, Canada. RP Ade, PAR (reprint author), Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. EM jmkovac@cfa.harvard.edu; pryke@physics.umn.edu OI Orlando, Angiola/0000-0001-8004-5054; Karkare, Kirit/0000-0002-5215-6993; Barkats, Denis/0000-0002-8971-1954 FU U.S. National Science Foundation [ANT-0742818, ANT-1044978, ANT-0742592, ANT-1110087]; NASA APRA [06-ARPA206-0040, 10-SAT10-0017]; SAT programs; Gordon and Betty Moore Foundation at Caltech; Canada Foundation for Innovation grant; W. M. Keck Foundation; FAS Science Division Research Computing Group at Harvard University; U.S. Department of Energy Office of Science FX BICEP2 was supported by the U.S. National Science Foundation under Grants No. ANT-0742818 and No. ANT-1044978 (Caltech and Harvard) and ANT-0742592 and ANT-1110087 (Chicago and Minnesota). The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and Grants No. 06-ARPA206-0040 and No. 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The receiver development was supported in part by a grant from the W. M. Keck Foundation. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and SLAC is partially supported by the U.S. Department of Energy Office of Science. Tireless administrative support was provided by Irene Coyle and Kathy Deniston. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. We thank all those who have contributed past efforts to the BICEP-Keck Array series of experiments, including the BICEP1 and Keck Array teams. We thank all those in the astrophysics community who have contributed feedback on the public preprint of this paper, and particularly two anonymous referees for their detailed and constructive recommendations. This work would not have been possible without the late Andrew Lange, whom we sorely miss. NR 103 TC 793 Z9 794 U1 11 U2 82 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 JUN 19 PY 2014 VL 112 IS 24 AR 241101 DI 10.1103/PhysRevLett.112.241101 PG 25 WC Physics, Multidisciplinary SC Physics GA AO0MN UT WOS:000341003800002 PM 24996078 ER PT J AU Kent, ST Cushman, M Howard, G Judd, SE Crosson, WL Al-Hamdan, MZ McClure, LA AF Kent, Shia T. Cushman, Mary Howard, George Judd, Suzanne E. Crosson, William L. Al-Hamdan, Mohammad Z. McClure, Leslie A. TI Sunlight exposure and cardiovascular risk factors in the REGARDS study: a cross-sectional split-sample analysis SO BMC NEUROLOGY LA English DT Article DE Sunlight; Temperature; Weather; Climate; Environment; Blood pressure; Lipids and lipoproteins ID CHRONIC KIDNEY-DISEASE; VITAMIN-D DEFICIENCY; BLOOD-PRESSURE; OUTDOOR TEMPERATURE; SEASONAL-VARIATION; SOLAR-RADIATION; STROKE; MORTALITY; PARTICIPANTS; INFLAMMATION AB Background: Previous research has suggested that vitamin D and sunlight are related to cardiovascular outcomes, but associations between sunlight and risk factors have not been investigated. We examined whether increased sunlight exposure was related to improved cardiovascular risk factor status. Methods: Residential histories merged with satellite, ground monitor, and model reanalysis data were used to determine previous-year sunlight radiation exposure for 17,773 black and white participants aged 45+ from the US. Exploratory and confirmatory analyses were performed by randomly dividing the sample into halves. Logistic regression models were used to examine relationships with cardiovascular risk factors. Results: The lowest, compared to the highest quartile of insolation exposure was associated with lower high-density lipoprotein levels in adjusted exploratory (-2.7 mg/dL [95% confidence interval: -4.2, -1.2]) and confirmatory (-1.5 mg/dL [95% confidence interval: -3.0, -0.1]) models. The lowest, compared to the highest quartile of insolation exposure was associated with higher systolic blood pressure levels in unadjusted exploratory and confirmatory, as well as the adjusted exploratory model (2.3 mmHg [95% confidence interval: 0.8, 3.8]), but not the adjusted confirmatory model (1.6 mg/dL [95% confidence interval: -0.5, 3.7]). Conclusions: The results of this study suggest that lower long-term sunlight exposure has an association with lower high-density lipoprotein levels. However, all associations were weak, thus it is not known if insolation may affect cardiovascular outcomes through these risk factors. C1 [Kent, Shia T.] Univ Alabama Birmingham, Dept Epidemiol, Birmingham, AL 35294 USA. [Cushman, Mary] Univ Vermont, Coll Med, Dept Med, Burlington, VT 05405 USA. [Howard, George; Judd, Suzanne E.; McClure, Leslie A.] Univ Alabama Birmingham, Dept Biostat, Birmingham, AL 35294 USA. [Crosson, William L.; Al-Hamdan, Mohammad Z.] NASA Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. RP McClure, LA (reprint author), Univ Alabama Birmingham, Dept Biostat, 1665 Univ Blvd, Birmingham, AL 35294 USA. EM lmcclure@uab.edu RI McClure, Leslie/P-2929-2015 FU National Institute of Neurological Disorders and Stoke [U01 NS041588]; National Aeronautics and Space Administration [NNX09AV81G] FX The NLDAS hourly data used in this study were acquired as part of the mission of NASA's Earth Science Division and archived and distributed by the Goddard Earth Sciences (GES) Data and Information Services Center (DISC). This work was supported by the National Institute of Neurological Disorders and Stoke [U01 NS041588]; and the National Aeronautics and Space Administration [grant# NNX09AV81G]. NR 41 TC 0 Z9 0 U1 0 U2 1 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2377 J9 BMC NEUROL JI BMC Neurol. PD JUN 19 PY 2014 VL 14 AR 133 DI 10.1186/1471-2377-14-133 PG 9 WC Clinical Neurology SC Neurosciences & Neurology GA AK4HK UT WOS:000338384400002 PM 24946776 ER PT J AU Fortenberry, RC Huang, XC McCarthy, MC Crawford, TD Lee, TJ AF Fortenberry, Ryan C. Huang, Xinchuan McCarthy, Michael C. Crawford, T. Daniel Lee, Timothy J. TI Fundamental Vibrational Frequencies and Spectroscopic Constants of cis- and trans-HOCS, HSCO, and Isotopologues via Quartic Force Fields SO JOURNAL OF PHYSICAL CHEMISTRY B LA English DT Article ID SHELL HARTREE-FOCK; CORRELATED MOLECULAR CALCULATIONS; GAUSSIAN-BASIS SETS; ELECTRON-AFFINITIES; WAVE-FUNCTIONS; CHEMISTRY; ENERGIES; INTERMEDIATE; GRADIENTS; HYDROGEN AB Highly accurate, coupled-cluster-based quartic force fields (QFFs) have been employed recently to provide spectroscopic reference for a myriad of molecules. Here, we are extending the same approach to provide vibrational and rotational spectroscopic reference data for the sulfur analogues of HOCO, HSCO, and HOCS, in both the cis and trans conformations as well as the D and S-34 isotopologues of each system. The resulting energies corroborate previous computations showing that trans-HSCO is the lowest-energy isomer for this system. The vibrational frequencies are computed with both second-order vibrational perturbation theory (VPT2) and vibrational configuration interaction (VCI) methods. The VPT2 and VCI QFF frequencies largely agree with one another to better than 5.0 cm(-1) (often better than 1.0 cm(-1)) and are also consistent with the type of behavior exhibited in previous studies. As such, the reference data provided here should assist in analysis of environments in which these sulfur systems may be found, including the interstellar medium, combustion flames, or laboratory simulations of either. C1 [Fortenberry, Ryan C.] Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA. [Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA. [McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Crawford, T. Daniel] Virginia Tech, Dept Chem, Blacksburg, VA 24061 USA. [Fortenberry, Ryan C.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Fortenberry, RC (reprint author), Georgia So Univ, Dept Chem, Statesboro, GA 30460 USA. EM rfortenberry@georgiasouthern.edu; Timothy.J.Lee@nasa.gov RI Lee, Timothy/K-2838-2012; HUANG, XINCHUAN/A-3266-2013; Crawford, Thomas/A-9271-2017; OI Crawford, Thomas/0000-0002-7961-7016; McCarthy, Michael/0000-0001-9142-0008 FU RCF; NASA; Georgia Southern University; NASA [NNX13AE59G, 10-APRA10-0167]; NSF [CHE-1058420]; NASA/SETI Institute [NNX12AG96A]; NSF Multi-User Chemistry Research Instrumentation and Facility (CRIF:MU) Award [CHE-0741927]; NASA's Laboratory Astrophysics 'Carbon in the Galaxy' Consortium Grant [NNH10ZDA001N] FX The authors would like to acknowledge the following sources of funding: RCF, the NASA Postdoctoral Program administered by Oak Ridge Associated Universities, as well as Georgia Southern University for start-up funds; M.C.M., NASA Award NNX13AE59G; T.D.C., NSF Award CHE-1058420; XI I., NASA/SETI Institute Cooperative Agreement NNX12AG96A; T.J.L., NASA Grant 10-APRA10-0167; R.C.F. and T.D.C., NSF Multi-User Chemistry Research Instrumentation and Facility (CRIF:MU) Award CHE-0741927; and R.C.F., X.H., and T.J.L., NASA's Laboratory Astrophysics 'Carbon in the Galaxy' Consortium Grant (NNH10ZDA001N). NR 52 TC 5 Z9 5 U1 3 U2 12 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1520-6106 J9 J PHYS CHEM B JI J. Phys. Chem. B PD JUN 19 PY 2014 VL 118 IS 24 SI SI BP 6498 EP 6510 DI 10.1021/jp412362h PG 13 WC Chemistry, Physical SC Chemistry GA AJ6FC UT WOS:000337784100017 PM 24635494 ER PT J AU Hofmann, DC Roberts, S Otis, R Kolodziejska, J Dillon, RP Suh, JO Shapiro, AA Liu, ZK Borgonia, JP AF Hofmann, Douglas C. Roberts, Scott Otis, Richard Kolodziejska, Joanna Dillon, R. Peter Suh, Jong-ook Shapiro, Andrew A. Liu, Zi-Kui Borgonia, John-Paul TI Developing Gradient Metal Alloys through Radial Deposition Additive Manufacturing SO SCIENTIFIC REPORTS LA English DT Article ID MICROSTRUCTURAL EVOLUTION; TITANIUM-VANADIUM; LASER DEPOSITION; COMPONENTS AB Interest in additive manufacturing (AM) has dramatically expanded in the last several years, owing to the paradigm shift that the process provides over conventional manufacturing. Although the vast majority of recent work in AM has focused on three-dimensional printing in polymers, AM techniques for fabricating metal alloys have been available for more than a decade. Here, laser deposition (LD) is used to fabricate multifunctional metal alloys that have a strategically graded composition to alter their mechanical and physical properties. Using the technique in combination with rotational deposition enables fabrication of compositional gradients radially from the center of a sample. A roadmap for developing gradient alloys is presented that uses multi-component phase diagrams as maps for composition selection so as to avoid unwanted phases. Practical applications for the new technology are demonstrated in low-coefficient of thermal expansion radially graded metal inserts for carbon-fiber spacecraft panels. C1 [Hofmann, Douglas C.; Roberts, Scott; Otis, Richard; Kolodziejska, Joanna; Dillon, R. Peter; Suh, Jong-ook; Shapiro, Andrew A.; Borgonia, John-Paul] CALTECH, Jet Prop Lab, Engn & Sci Directorate, Pasadena, CA 91109 USA. [Hofmann, Douglas C.; Roberts, Scott; Kolodziejska, Joanna; Shapiro, Andrew A.] CALTECH, Keck Lab Engn Sci, Pasadena, CA 91125 USA. [Otis, Richard; Liu, Zi-Kui] Penn State Univ, Dept Mat Sci & Engn, University Pk, PA 16802 USA. RP Hofmann, DC (reprint author), CALTECH, Jet Prop Lab, Engn & Sci Directorate, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM dch@jpl.nasa.gov RI Liu, Zi-Kui/A-8196-2009; OI Liu, Zi-Kui/0000-0003-3346-3696; Otis, Richard/0000-0002-1147-9032 FU Office of the Chief Technologist FX This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA) and funded through the Office of the Chief Technologist. The authors acknowledge G. Agnes, C. Bradford, P. Gardner, C. Morandi, J. Mulder, P. Willis, and RPM for useful discussions. The authors cite no conflict of interest. NR 25 TC 14 Z9 15 U1 4 U2 67 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2045-2322 J9 SCI REP-UK JI Sci Rep PD JUN 19 PY 2014 VL 4 AR 5357 DI 10.1038/srep05357 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AJ2PF UT WOS:000337499400006 PM 24942329 ER PT J AU Navarro, RE Moya, PS Munoz, V Araneda, JA Vinas, AF Valdivia, JA AF Navarro, R. E. Moya, P. S. Munoz, V. Araneda, J. A. Vinas, A. F. Valdivia, J. A. TI Solar Wind Thermally Induced Magnetic Fluctuations SO PHYSICAL REVIEW LETTERS LA English DT Article ID PROTON TEMPERATURE ANISOTROPY; COULOMB COLLISIONS; LINEAR-THEORY; INSTABILITY; WAVES; DISSIPATION AB A kinetic description of Alfven-cyclotron magnetic fluctuations for anisotropic electron-proton quasistable plasmas is studied. An analytical treatment, based on the fluctuation-dissipation theorem, consistently shows that spontaneous fluctuations in plasmas with stable distributions significantly contribute to the observed magnetic fluctuations in the solar wind, as seen, for example, in [S. D. Bale et al., Phys. Rev. Lett. 103, 211101 (2009)], even far below from the instability thresholds. Furthermore, these results, which do not require any adjustable parameters or wave excitations, are consistent with the results provided by hybrid simulations. It is expected that this analysis contributes to our understanding of the nature of magnetic fluctuations in the solar wind. C1 [Navarro, R. E.; Munoz, V.; Valdivia, J. A.] Univ Chile, Fac Ciencias, Dept Fis, Santiago, Chile. [Moya, P. S.; Vinas, A. F.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Geospace Phys Lab, Greenbelt, MD 20771 USA. [Moya, P. S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Araneda, J. A.] Univ Concepcion, Dept Fis, Concepcion 4070386, Chile. [Valdivia, J. A.] CEIBA Complejidad, Ctr Estudios Interdisciplinarios Basicos & Aplica, Bogota, Colombia. [Valdivia, J. A.] CEDENNA, Ctr Desarrollo Nanociencia & Nanotecnol, Santiago, Chile. RP Navarro, RE (reprint author), Univ Chile, Fac Ciencias, Dept Fis, Casilla 653, Santiago, Chile. EM roberto.navarro@ug.uchile.cl RI Moya, Pablo/C-3163-2011; Valdivia, Juan/A-3631-2008; Navarro, Roberto/F-7045-2014; Araneda, Jaime/J-9245-2015; Munoz, Victor/A-2255-2008 OI Moya, Pablo/0000-0002-9161-0888; Valdivia, Juan/0000-0003-3381-9904; Navarro, Roberto/0000-0003-0782-1904; FU FONDECyT [1110135, 1110729, 1121144, 1110880]; CONICYT-Becas Chile Postdoctoral Fellowship; CONICyT [21100691]; CEDENNA; NASA's Wind/SWE program FX This project has been financially supported by FONDECyT under Contracts No. 1110135 (J. A. V.), No. 1110729 (J. A. V.), No. 1121144 (V. M.), and No. 1110880 (J. A). P. S. M. received support from a CONICYT-Becas Chile Postdoctoral Fellowship. R. N. received support from a CONICyT Fellowship No. 21100691. J. A. V. also thanks to CEDENNA and A. F. V. thanks to NASA's Wind/SWE program for their support. NR 31 TC 13 Z9 13 U1 2 U2 9 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 JUN 18 PY 2014 VL 112 IS 24 AR 245001 DI 10.1103/PhysRevLett.112.245001 PG 5 WC Physics, Multidisciplinary SC Physics GA AK6KJ UT WOS:000338536200012 PM 24996092 ER PT J AU Renault, C Koehne, J Ricco, AJ Crooks, RM AF Renault, Christophe Koehne, Jessica Ricco, Antonio J. Crooks, Richard M. TI Three-Dimensional Wax Patterning of Paper Fluidic Devices SO LANGMUIR LA English DT Article ID MICROFLUIDIC DEVICES; LOW-COST; IMMUNODEVICE; FABRICATION AB In this paper we describe a method for three-dimensional wax patterning of microfluidic paper-based analytical devices (mu PADs). The method is rooted in the fundamental details of wax transport in paper and provides a simple way to fabricate complex channel architectures such as hemichannels and fully enclosed channels. We show that three-dimensional mu PADs can be fabricated with half as much paper by using hemichannels rather than ordinary open channels. We also provide evidence that fully enclosed channels are efficiently isolated from the exterior environment, decreasing contamination risks, simplifying the handling of the device, and slowing evaporation of solvents. C1 [Renault, Christophe; Crooks, Richard M.] Univ Texas Austin, Dept Chem, Ctr Nano & Mol Sci & Technol, Austin, TX 78712 USA. [Koehne, Jessica] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. [Ricco, Antonio J.] NASA, Ames Res Ctr, Small Payloads & Instruments Grp, Moffett Field, CA 94035 USA. RP Crooks, RM (reprint author), Univ Texas Austin, Dept Chem, Ctr Nano & Mol Sci & Technol, 105 East 24th St,Stop A5300, Austin, TX 78712 USA. EM crooks@cm.utexas.edu OI Ricco, Antonio/0000-0002-2355-4984 FU Defense Advanced Research Projects Agency Diagnostics on Demand program [HR0011-12-2-0003]; Robert A. Welch Foundation [F-0032] FX We gratefully acknowledge sponsorship of this project by the Defense Advanced Research Projects Agency Diagnostics on Demand program (Contract HR0011-12-2-0003). We also thank the Robert A. Welch Foundation (Grant F-0032) for sustained research support. NR 29 TC 32 Z9 32 U1 9 U2 76 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0743-7463 J9 LANGMUIR JI Langmuir PD JUN 17 PY 2014 VL 30 IS 23 BP 7030 EP 7036 DI 10.1021/la501212b PG 7 WC Chemistry, Multidisciplinary; Chemistry, Physical; Materials Science, Multidisciplinary SC Chemistry; Materials Science GA AJ4KD UT WOS:000337644200048 PM 24896490 ER PT J AU Lyatskaya, S Lyatsky, W Khazanov, GV AF Lyatskaya, Sonya Lyatsky, Wladislaw Khazanov, George V. TI Effect of Interhemispheric Field-Aligned Currents on Region-1 Currents SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CONJUGATE HEMISPHERES; DOUBLE OVAL; MODEL; SUBSTORM; SATELLITE; JOULE; MAGNETOSPHERE; IONOSPHERE; DYNAMICS; DUSK AB An asymmetry in ionospheric conductivity between two hemispheres results in the formation of additional, interhemispheric field-aligned currents (FACs) flowing between conjugate ionospheres within two auroral zones. These interhemispheric currents are especially significant during summer-winter conditions when there is a significant asymmetry in ionospheric conductivity in two hemispheres. In such conditions, these currents may be comparable in magnitude with the Region 1 (R1) field-aligned currents. In this case, the R1 current is the sum of two FACs: one is going from/to the solar wind, and another is flowing between conjugate ionospheres. These interhemispheric currents can also cause the formation of auroras extended along the nightside polar cap boundary, which may be related to the so-called "double auroral oval." In this study, we present the results of analytical and numerical solutions for the interhemispheric currents and their effect on the Region 1 currents. C1 [Lyatskaya, Sonya] Howard Community Coll, Columbia, MD 21044 USA. [Lyatsky, Wladislaw] Catholic Univ Amer, Washington, DC 20064 USA. [Lyatskaya, Sonya; Lyatsky, Wladislaw; Khazanov, George V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lyatskaya, S (reprint author), Howard Community Coll, Columbia, MD 21044 USA. EM lyatsky@hotmail.com RI feggans, john/F-5370-2012 FU National Science Foundation [ANT-1204019] FX This study is supported by the National Science Foundation under Award ANT-1204019. NR 43 TC 6 Z9 6 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 16 PY 2014 VL 41 IS 11 BP 3731 EP 3737 DI 10.1002/2014GL060413 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AL6YP UT WOS:000339280200007 ER PT J AU Poppe, AR Fatemi, S Halekas, JS Holmstrom, M Delory, GT AF Poppe, A. R. Fatemi, S. Halekas, J. S. Holmstrom, M. Delory, G. T. TI ARTEMIS observations of extreme diamagnetic fields in the lunar wake SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SOLAR-WIND; MAGNETIC-FIELD; MOON AB We present two Acceleration, Reconnection, Turbulence, and Electrodynamics of the Moon's Interaction with the Sun ( ARTEMIS) observations of diamagnetic fields in the lunar wake at strengths exceeding twice the ambient magnetic field during high plasma beta conditions. The first observation was 350 km from the lunar surface while the Moon was located in the terrestrial magnetosheath with elevated particle temperatures. The second observation was in the solar wind ranging from 500 to 2000 km downstream, with a relatively low magnetic field strength of approximately 1.6 nT. In both cases, the plasma beta exceeded 10. We discuss the observations and compare the data to hybrid plasma simulations in order to validate the model under such extreme conditions and to elucidate the global structure of the lunar wake during these observations. The extreme nature of the diamagnetic field in the lunar wake provides an important end-member test case for theoretical and modeling studies of the various plasma processes operating in the lunar wake. C1 [Poppe, A. R.; Halekas, J. S.; Delory, G. T.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Poppe, A. R.; Halekas, J. S.; Delory, G. T.] NASA, Solar Syst Explorat Res Virtual Inst, Ames Res Ctr, Moffett Field, CA USA. [Fatemi, S.; Holmstrom, M.] Swedish Inst Space Phys, S-98128 Kiruna, Sweden. [Fatemi, S.; Holmstrom, M.] Lulea Univ Technol, Dept Comp Sci Elect & Space Engn, S-95187 Lulea, Sweden. RP Poppe, AR (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM poppe@ssl.berkeley.edu OI Poppe, Andrew/0000-0001-8137-8176; Halekas, Jasper/0000-0001-5258-6128 FU NASA's Solar System Exploration Research Virtual Institute (SSERVI); NASA [NAS5-02099]; German Ministry for Economy and Technology; German Center for Aviation and Space (DLR) [50 OC 0302] FX A.R.P, J.S.H, and G.T.D. gratefully acknowledge support from NASA's Solar System Exploration Research Virtual Institute (SSERVI). This publication is SSERVI contribution SSERVI-2014-093. The ARTEMIS mission is funded and operated under NASA grant NAS5-02099, and we specifically acknowledge J. P. McFadden for the use of ESA data and K.-H. Glassmeier, U. Auster, and W. Baumjohann for the use of FGM data provided under the lead of the Technical University of Braunschweig and with financial support through the German Ministry for Economy and Technology and the German Center for Aviation and Space (DLR) under contract 50 OC 0302. All ARTEMIS data necessary to reproduce this work are publicly available at http://artemis.ssl.berkeley.edu. The authors also acknowledge the International Space Science Institute (ISSI) for hosting a workshop series that in part inspired this work. The hybrid modeling was conducted using resources provided by the Swedish National Infrastructure for Computing (SNIC) at the High Performance Computing Center North (HPC2N), Umea University, Sweden. The software used in this work was in part developed by the DOE NNSA-ASC OASCR Flash Center at the University of Chicago. The authors thank two reviewers for helpful and constructive comments. NR 22 TC 4 Z9 4 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 16 PY 2014 VL 41 IS 11 BP 3766 EP 3773 DI 10.1002/2014GL060280 PG 8 WC Geosciences, Multidisciplinary SC Geology GA AL6YP UT WOS:000339280200012 ER PT J AU Sims, DW Wyrick, DY Ferrill, DA Morris, AP Collins, GC Pappalardo, RT Colton, SL AF Sims, Darrell W. Wyrick, Danielle Y. Ferrill, David A. Morris, Alan P. Collins, Geoffrey C. Pappalardo, Robert T. Colton, Shannon L. TI Physical models of grooved terrain tectonics on Ganymede SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID HIGH-RESOLUTION; EXTENSIONAL INSTABILITY; GEOLOGY AB Grooved terrain on Ganymede consists of distinct areas of parallel to subparallel ridges and troughs at a variety of spatial scales. Grooved terrain has been interpreted as the product of tectonism in the form of fault-accommodated distributed lithospheric extension. We use physical analog methods to test the formation of grooved terrain by imbricate normal faulting in response to distributed extension. Faults and fault systems produced in the models are geometrically and kinematically similar to patterns inferred for some grooved terrains on Ganymede. The high degree of similarity between model structures and those observed on Ganymede indicates that rotational half-graben brittle block faulting can explain at least some tectonic resurfacing on Ganymede and that 20% extension is sufficient to form structures analogous to grooved terrain. C1 [Sims, Darrell W.; Wyrick, Danielle Y.; Ferrill, David A.; Morris, Alan P.] Southwest Res Inst, San Antonio, TX USA. [Collins, Geoffrey C.] Wheaton Coll, Phys & Astron Dept, Norton, MA 02766 USA. [Pappalardo, Robert T.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Colton, Shannon L.] NuStar Energy LP, San Antonio, TX USA. RP Pappalardo, RT (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM robert.pappalardo@jpl.nasa.gov OI Ferrill, David/0000-0002-3486-5526 FU National Aeronautics and Space Administration through the Outer Planets Research Program [NNG05GH47G]; National Aeronautics and Space Administration FX We thank G. Walter and two anonymous reviewers for comments that improved the manuscript and C. Patton for manuscript preparation. This material is based upon work supported by the National Aeronautics and Space Administration under grant NNG05GH47G issued through the Outer Planets Research Program. The portion of this work performed by R. T. P. 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 1 Z9 1 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 16 PY 2014 VL 41 IS 11 BP 3774 EP 3778 DI 10.1002/2014GL060359 PG 5 WC Geosciences, Multidisciplinary SC Geology GA AL6YP UT WOS:000339280200013 ER PT J AU Pagano, TS Olsen, ET Nguyen, H Ruzmaikin, A Jiang, X Perkins, L AF Pagano, Thomas S. Olsen, Edward T. Hai Nguyen Ruzmaikin, Alexander Jiang, Xun Perkins, Lori TI Global variability of midtropospheric carbon dioxide as measured by the Atmospheric Infrared Sounder SO JOURNAL OF APPLIED REMOTE SENSING LA English DT Article DE Atmospheric Infrared Sounder; carbon dioxide; midtroposphere; Moderate Resolution Imaging Spectroradiometer; seasonal cycle ID FTS MEASUREMENTS; CO2 VARIABILITY; SATELLITE DATA; CLIMATE; MODEL; PRODUCTS; NETWORK; SCIENCE; MISSION; SURFACE AB The Atmospheric Infrared Sounder (AIRS) on the EOS Aqua spacecraft provides accurate and consistent measurements of midtropospheric carbon dioxide (CO2) with global monthly coverage. The data are widely used for studies of vertical transport of CO2 due to large-scale dynamics (e.g., ENSO, MJO, and the Walker Circulation). The purpose of this paper is to characterize the response of CO2 in the midtroposphere, at the altitudes where AIRS is most sensitive, to geophysical changes at the surface across the globe. Our findings confirm that surface factors, as well as weather and climate patterns, impact the global variability of midtropospheric CO2 as observed by AIRS. Despite a phase lag and a reduction in the seasonal amplitude observed in AIRS CO2 relative to surface CO2 measurements in the Northern Hemisphere, a significant correlation is observed between regional variability of CO2 from AIRS and Moderate Resolution Imaging Spectroradiometer (MODIS)-derived Gross Primary Productivity at the surface, primarily in the high-latitude boreal forests during the peak of the growing season (July). A video of global AIRS CO2 and MODIS vegetation index clearly shows the seasonal drawdown of CO2 from the midtroposphere over highly vegetated areas in the northern latitudes. In the Southern Hemisphere, we see higher amplitude in the seasonal cycle, with the phase leading that of the surface. Both are indicative of interhemispheric transport. (C) 2014 Society of Photo-Optical Instrumentation Engineers (SPIE) C1 [Pagano, Thomas S.; Olsen, Edward T.; Hai Nguyen; Ruzmaikin, Alexander] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Jiang, Xun] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX 77204 USA. [Perkins, Lori] NASA, Goddard Space Flight Ctr, Sci Visualizat Studios, Greenbelt, MD 20771 USA. RP Pagano, TS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM tpagano@jpl.nasa.gov NR 41 TC 3 Z9 3 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 JUN 16 PY 2014 VL 8 AR 084984 DI 10.1117/1.JRS.8.084984 PG 18 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AK5XN UT WOS:000338500400001 ER PT J AU Schmidt, A Thordarson, T Oman, LD Robock, A Self, S AF Schmidt, Anja Thordarson, Thorvaldur Oman, Luke D. Robock, Alan Self, Stephen TI Reply to comment by Cole-Dai et al. on "Climatic impact of the long-lasting Laki eruption: Inapplicability of mass-independent sulfur isotope composition measurements" SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Laki eruption; sulfur MIF; sulfur isotopes; Laki climate ID BASALTIC FISSURE ERUPTIONS; VOLCANIC-ERUPTIONS; TEMPERATURE-CHANGES; ATMOSPHERIC IMPACT; FRACTIONATION; SULFATE; AEROSOL C1 [Schmidt, Anja] Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England. [Thordarson, Thorvaldur] Univ Iceland, Fac Earth Sci, Reykjavik, Iceland. [Oman, Luke D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Robock, Alan] Rutgers State Univ, Dept Environm Sci, New Brunswick, NJ 08903 USA. [Self, Stephen] Open Univ, Dept Earth & Environm Sci, Milton Keynes MK7 6AA, Bucks, England. RP Schmidt, A (reprint author), Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England. EM a.schmidt@leeds.ac.uk RI Oman, Luke/C-2778-2009; Schmidt, Anja/C-9617-2012; Thordarson, Thorvaldur/M-2422-2015; Robock, Alan/B-6385-2016; OI Oman, Luke/0000-0002-5487-2598; Thordarson, Thorvaldur/0000-0003-4011-7185; Schmidt, Anja/0000-0001-8759-2843 NR 23 TC 0 Z9 0 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 16 PY 2014 VL 119 IS 11 BP 6636 EP 6637 DI 10.1002/2013JD021440 PG 2 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ8RK UT WOS:000337974500024 ER PT J AU Kleinbohl, A Khosravi, M Urban, J Canty, T Salawitch, RJ Toon, GC Kullmann, H Notholt, J AF Kleinboehl, Armin Khosravi, Maryam Urban, Joachim Canty, Timothy Salawitch, Ross J. Toon, Geoffrey C. Kuellmann, Harry Notholt, Justus TI Constraints for the photolysis rate and the equilibrium constant of ClO-dimer from airborne and balloon-borne measurements of chlorine compounds SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE chlorine monoxide; ClO-dimer; submillimeter measurements; photolysis; equilibrium constant; Arctic winter ID ABSORPTION CROSS-SECTIONS; ARCTIC POLAR VORTEX; STRATOSPHERIC OZONE LOSS; IN-SITU MEASUREMENTS; ANTARCTIC OZONE; CLO/CL2O2 EQUILIBRIUM; WINTER 1999/2000; SELF-REACTION; PEROXIDE; KINETICS AB We analyze measurements of ClO across the terminator taken by the Airborne Submillimeter Radiometer (ASUR) in the activated vortices of the Arctic winters of 1995/1996, 1996/1997, and 1999/2000 to evaluate the plausibility of various determinations of the ClO-dimer photolysis cross section and the rate constant controlling the thermal equilibrium between ClO-dimer and ClO. We use measured ClO during sunlit conditions to estimate total active chlorine (ClOx). As the measurements suggest nearly full chlorine activation in winter 1999/2000, we compare ClOx estimates based on various photolysis frequencies of ClO-dimer with total available inorganic chlorine (Cly), estimated from an N2O-Cly correlation established by a balloon-borne MkIV interferometer measurement. Only ClO-dimer cross sections leading to the fastest photolysis frequencies in the literature (including the latest evaluation by the Jet Propulsion Laboratory) give ClOx mixing ratios that overlap with the estimated range of available Cly. Slower photolysis rates lead to ClOx values that are higher than available Cly. We use the ClOx calculated from sunlit ClO measurements to estimate ClO in darkness based on different equilibrium constants, and compare it with ASUR ClO measurements before sunrise at high solar zenith angles. Calculations with equilibrium constants published in recent evaluations of the Jet Propulsion Laboratory give good agreement with observed ClO mixing ratios. Equilibrium constants leading to a higher ClO/ClOx ratio in darkness yield ClO values that tend to exceed observed abundances. Perturbing the rates for the ClO+BrO reaction in a manner that increases OClO formation and decreases BrCl formation leads to lower ClO values calculated for twilight conditions after sunset, resulting in better agreement with ASUR measurements. C1 [Kleinboehl, Armin; Toon, Geoffrey C.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Khosravi, Maryam; Urban, Joachim] Chalmers, Dept Earth & Space Sci, S-41296 Gothenburg, Sweden. [Canty, Timothy; Salawitch, Ross J.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Salawitch, Ross J.] Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA. [Salawitch, Ross J.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Kuellmann, Harry; Notholt, Justus] Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany. RP Kleinbohl, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Armin.Kleinboehl@jpl.nasa.gov RI Urban, Jo/F-9172-2010; Salawitch, Ross/B-4605-2009; Canty, Timothy/F-2631-2010; Notholt, Justus/P-4520-2016 OI Urban, Jo/0000-0001-7026-793X; Salawitch, Ross/0000-0001-8597-5832; Canty, Timothy/0000-0003-0618-056X; Notholt, Justus/0000-0002-3324-885X FU aircraft crew; Atmospheric Composition, Modeling, and Analysis Program of the National Aeronautics and Space Administration; National Aeronautics and Space Administration FX We are grateful to H. Bremer and M. Sinnhuber for their contributions to data acquisition and retrieval of ASUR data. We would like to acknowledge V. Eyring for performing initial analyses of the flights from 1996 and 1997, and we would like to thank Y. Tijani for re-integrating the ASUR measurements of the 1996/1997 flights. We are grateful to K. Kunzi for providing the opportunity to perform measurements with ASUR on board of research aircraft. We also thank G. Naveke, N. Whyborn, H. Golstein, and H. Schaeffer for their excellent technical support prior to and during the ASUR aircraft campaigns. We are thankful to R. M. Stimpfle, D. M. Wilmouth, and J. G. Anderson for providing their ClO and ClNO3 measurements from the ER-2 via the NASA ESPO archive. We thank the aircraft crew of the DLR Falcon for their support during the 1996/1997 campaigns. We are grateful for the opportunity to participate on board the NASA DC-8 during SOLVE and thank the aircraft crew for their support. We want to express our gratitude to J.-F. L. Blavier, D. Petterson, and J. Landeros for their contributions to the balloon flight from Esrange. We thank NASA CSBF for performing the balloon launch and for their support during the campaign. We acknowledge GMAO and NCEP for providing meteorological analyses. T. Canty and R. Salawitch appreciate support from the Atmospheric Composition, Modeling, and Analysis Program of the National Aeronautics and Space Administration. Work at the Jet Propulsion Laboratory, California Institute of Technology, is performed under a contract with the National Aeronautics and Space Administration. NR 81 TC 1 Z9 1 U1 2 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 16 PY 2014 VL 119 IS 11 BP 6916 EP 6937 DI 10.1002/2013JD021433 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ8RK UT WOS:000337974500041 ER PT J AU Duderstadt, KA Dibb, JE Jackman, CH Randall, CE Solomon, SC Mills, MJ Schwadron, NA Spence, HE AF Duderstadt, Katharine A. Dibb, Jack E. Jackman, Charles H. Randall, Cora E. Solomon, Stanley C. Mills, Michael J. Schwadron, Nathan A. Spence, Harlan E. TI Nitrate deposition to surface snow at Summit, Greenland, following the 9 November 2000 solar proton event SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE solar proton; nitrate; WACCM; SPE; Summit ID COMMUNITY CLIMATE MODEL; COSMIC-RAY EVENTS; POLAR ICE CORES; ODD NITROGEN; PARTICLE-PRECIPITATION; MIDDLE ATMOSPHERE; FOREST-FIRES; VEGETATION EMISSIONS; ARCTIC STRATOSPHERE; WINTER STRATOSPHERE AB This study considers whether spikes in nitrate in snow sampled at Summit, Greenland, from August 2000 to August 2002 are related to solar proton events. After identifying tropospheric sources of nitrate on the basis of correlations with sulfate, ammonium, sodium, and calcium, we use the three-dimensional global Whole Atmosphere Community Climate Model (WACCM) to examine unaccounted for nitrate spikes. Model calculations confirm that solar proton events significantly impact HOx, NOx, and O3 levels in the mesosphere and stratosphere during the weeks and months following the major 9 November 2000 solar proton event. However, solar proton event (SPE)-enhanced NOy calculated within the atmospheric column is too small to account for the observed nitrate peaks in surface snow. Instead, our WACCM results suggest that nitrate spikes not readily accounted for by measurement correlations are likely of anthropogenic origin. These results, consistent with other recent studies, imply that nitrate spikes in ice cores are not suitable proxies for individual SPEs and motivate the need to identify alternative proxies. C1 [Duderstadt, Katharine A.; Dibb, Jack E.; Schwadron, Nathan A.; Spence, Harlan E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Jackman, Charles H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Randall, Cora E.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. [Solomon, Stanley C.; Mills, Michael J.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. RP Duderstadt, KA (reprint author), Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. EM duderstadtk@gust.sr.unh.edu RI Solomon, Stanley/J-4847-2012; Jackman, Charles/D-4699-2012; Randall, Cora/L-8760-2014; Mills, Michael/B-5068-2010 OI Solomon, Stanley/0000-0002-5291-3034; Randall, Cora/0000-0002-4313-4397; Mills, Michael/0000-0002-8054-1346 FU NSF [1135432]; National Science Foundation; Office of Science (BER) of the U.S. Department of Energy FX This work was supported by NSF grant 1135432 to the University of New Hampshire. We 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 [Computational and Information Systems Laboratory, 2012; The NCAR Command Language, 2013]. The CESM project is supported by the National Science Foundation and the Office of Science (BER) of the U.S. Department of Energy. The model results and observations used to produce the analysis and figures within this study are available upon request from the corresponding author. We thank the reviewers of the manuscript for their helpful comments and suggestions. NR 107 TC 9 Z9 9 U1 1 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 16 PY 2014 VL 119 IS 11 BP 6938 EP 6957 DI 10.1002/2013JD021389 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ8RK UT WOS:000337974500042 ER PT J AU Neu, JL Hegglin, MI Tegtmeier, S Bourassa, A Degenstein, D Froidevaux, L Fuller, R Funke, B Gille, J Jones, A Rozanov, A Toohey, M von Clarmann, T Walker, KA Worden, JR AF Neu, J. L. Hegglin, M. I. Tegtmeier, S. Bourassa, A. Degenstein, D. Froidevaux, L. Fuller, R. Funke, B. Gille, J. Jones, A. Rozanov, A. Toohey, M. von Clarmann, T. Walker, K. A. Worden, J. R. TI The SPARC Data Initiative: Comparison of upper troposphere/lower stratosphere ozone climatologies from limb-viewing instruments and the nadir-viewing Tropospheric Emission Spectrometer SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE ozone climatologies; upper troposphere; lower stratosphere; satellite measurements ID TROPICAL TROPOPAUSE; SATELLITE-OBSERVATIONS; ERROR ANALYSIS; ANNUAL CYCLE; TES; RETRIEVALS; VALIDATION; O-3; CIRCULATION; RESOLUTION AB We present the first comprehensive intercomparison of currently available satellite ozone climatologies in the upper troposphere/lower stratosphere (UTLS) (300-70hPa) as part of the Stratosphere-troposphere Processes and their Role in Climate (SPARC) Data Initiative. The Tropospheric Emission Spectrometer (TES) instrument is the only nadir-viewing instrument in this initiative, as well as the only instrument with a focus on tropospheric composition. We apply the TES observational operator to ozone climatologies from the more highly vertically resolved limb-viewing instruments. This minimizes the impact of differences in vertical resolution among the instruments and allows identification of systematic differences in the large-scale structure and variability of UTLS ozone. We find that the climatologies from most of the limb-viewing instruments show positive differences (ranging from 5 to 75%) with respect to TES in the tropical UTLS, and comparison to a zonal mean ozonesonde climatology indicates that these differences likely represent a positive bias for p100hPa. In the extratropics, there is good agreement among the climatologies regarding the timing and magnitude of the ozone seasonal cycle (differences in the peak-to-peak amplitude of <15%) when the TES observational operator is applied, as well as very consistent midlatitude interannual variability. The discrepancies in ozone temporal variability are larger in the tropics, with differences between the data sets of up to 55% in the seasonal cycle amplitude. However, the differences among the climatologies are everywhere much smaller than the range produced by current chemistry-climate models, indicating that the multiple-instrument ensemble is useful for quantitatively evaluating these models. C1 [Neu, J. L.; Froidevaux, L.; Fuller, R.; Worden, J. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Hegglin, M. I.] Univ Reading, Dept Meteorol, Reading, Berks, England. [Tegtmeier, S.; Toohey, M.] GEOMAR Helmholtz Ctr Ocean Res, Kiel, Germany. [Bourassa, A.; Degenstein, D.] Univ Saskatchewan, Dept Phys & Engn Phys, Saskatoon, SK, Canada. [Funke, B.] CSIC, Inst Astrofis Andalucia, Granada, Spain. [Gille, J.] Univ Colorado, Dept Ocean & Atmospher Sci, Boulder, CO 80309 USA. [Jones, A.; Walker, K. A.] Univ Toronto, Dept Phys, Toronto, ON, Canada. [Rozanov, A.] Univ Bremen, Dept Phys & Elect Engn, D-28359 Bremen, Germany. [von Clarmann, T.] Karlsruhe Inst Technol, Dept Phys, D-76021 Karlsruhe, Germany. RP Neu, JL (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM jessica.l.neu@jpl.nasa.gov RI Funke, Bernd/C-2162-2008; Toohey, Matthew/G-3129-2010; Hegglin, Michaela/D-7528-2017 OI Funke, Bernd/0000-0003-0462-4702; Toohey, Matthew/0000-0002-7070-405X; Hegglin, Michaela/0000-0003-2820-9044 FU National Aeronautics and Space Administration; NASA [NAS5-97046]; CSA; ESA; Spanish MINECO [AYA2011-23552]; EC FEDER funds; German Aerospace Agency (DLR) within the project SADOS [50EE1105]; state and University of Bremen; Canadian Space Agency (CSA); Canadian Foundation for Climate and Atmospheric Sciences FX The authors thank the relevant instrument teams and space agencies for their data and support. We also thank the ISSI in Bern for facilitating two successful team meetings in Bern as part of the ISSI International Team activity program, and the SPARC Toronto office and SPARC/WCRP for travel support. Work at the Jet Propulsion Laboratory, California Institute of Technology, was performed under contract from the National Aeronautics and Space Administration. John Gille and the work of the HIRDLS team in the U.S. was supported by NASA contract NAS5-97046. Michaela I Hegglin's work within the SPARC Data Initiative was supported by the CSA and ESA. IAA was supported by the Spanish MINECO under grant AYA2011-23552 and EC FEDER funds. The work of the University of Bremen team on the SCIAMACHY ozone climatology was funded in part by the German Aerospace Agency (DLR) within the project SADOS (50EE1105) and by the state and University of Bremen. ACE is a Canadian-led mission mainly supported by the Canadian Space Agency (CSA). Development of the ACE-FTS climatologies was supported by grants from the Canadian Foundation for Climate and Atmospheric Sciences and the CSA. The ozonesonde climatology and ACCMIP model results were provided by Paul Young of Lancaster University and Kevin Bowman of the Jet Propulsion Laboratory, respectively. NR 46 TC 5 Z9 5 U1 1 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 16 PY 2014 VL 119 IS 11 BP 6971 EP 6990 DI 10.1002/2013JD020822 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ8RK UT WOS:000337974500044 ER PT J AU Alerstam, E AF Alerstam, Erik TI Anisotropic diffusive transport: Connecting microscopic scattering and macroscopic transport properties SO PHYSICAL REVIEW E LA English DT Article ID NEMATIC LIQUID-CRYSTALS; MULTIPLE LIGHT-SCATTERING; RANDOM-MEDIA; PROPAGATION AB This work concerns the modeling of radiative transfer in anisotropic turbid media using diffusion theory. A theory for the relationship between microscopic scattering properties (i.e., an arbitrary differential scattering cross-section) and the macroscopic diffusion tensor, in the limit of independent scatterers, is presented. The theory is accompanied by a numerical method capable of performing the calculations. In addition, a boundary condition appropriate for modeling systems with anisotropic radiance is derived. It is shown that anisotropic diffusion theory, when based on these developments, indeed can describe radiative transfer in anisotropic turbid media. More specifically, it is reported that solutions to the anisotropic diffusion equation are in excellent agreement with Monte Carlo simulations, both in steady-state and time-domain. This stands in contrast to previous work on the topic, where inadequate boundary conditions and/or incorrect relations between microscopic scattering properties and the diffusion tensor have caused disagreement between simulations and diffusion theory. The present work thus falsify previous claims that anisotropic diffusion theory cannot describe anisotropic radiative transfer, and instead open for accurate quantitative diffusion-based modeling of anisotropic turbid materials. C1 [Alerstam, Erik] Lund Univ, Dept Phys, Div Atom Phys, S-22100 Lund, Sweden. RP Alerstam, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM erik.alerstam@jpl.nasa.gov FU Swedish Research Council FX Part of this work was supported and generously funded by Stefan Andersson-Engels using grants from the Swedish Research Council. Tomas Svensson is gratefully acknowledged for interesting discussions, constant encouragement, and invaluable help improving the manuscript. The author is also grateful to Kevin Vynck, Matteo Burresi, and Corey Cochrane for reading and helping to improve the manuscript. NR 28 TC 8 Z9 9 U1 0 U2 11 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1539-3755 EI 1550-2376 J9 PHYS REV E JI Phys. Rev. E PD JUN 16 PY 2014 VL 89 IS 6 AR 063202 DI 10.1103/PhysRevE.89.063202 PG 10 WC Physics, Fluids & Plasmas; Physics, Mathematical SC Physics GA AJ5OJ UT WOS:000337733900009 PM 25019904 ER PT J AU Kato, S Rose, FG Liu, X Wielicki, BA Mlynczak, MG AF Kato, Seiji Rose, Fred G. Liu, Xu Wielicki, Bruce A. Mlynczak, Martin G. TI Retrieval of Atmospheric and Cloud Property Anomalies and Their Trend from Temporally and Spatially Averaged Infrared Spectra Observed from Space SO JOURNAL OF CLIMATE LA English DT Article AB A surface, atmospheric, and cloud (fraction, height, optical thickness, and particle size) property anomaly retrieval from highly averaged longwave spectral radiances is simulated using 28 years of reanalysis. Instantaneous nadir-view spectral radiances observed from an instrument on a 90 inclination polar orbit are computed. Spectral radiance changes caused by surface, atmospheric, and cloud property perturbations are also computed and used for the retrieval. This study's objectives are 1) to investigate whether or not separating clear sky from cloudy sky reduces the retrieval error and 2) to estimate the error in a trend of retrieved properties. This simulation differs from earlier studies in that annual 10 latitude zonal cloud and atmospheric property anomalies defined as the deviation from 28-yr climatological means are retrieved instead of the difference of these properties from two time periods. The root-mean-square (RMS) difference of temperature and humidity anomalies retrieved from all-sky radiance anomalies is similar to the RMS difference derived from clear-sky radiance anomalies computed by removing clouds. This indicates that the cloud property anomaly retrieval error does not affect the retrieved temperature and humidity anomalies. When retrieval errors are nearly random, the error in the trend of retrieved properties is small. Approximately 30% of 10 latitude zones meet conditions that the true temperature and water vapor amount trends are within a 95% confidence interval of retrieved trends, and that the standard deviation of retrieved anomalies sigma(ret) is within 20% of the standard deviation of true anomalies sigma(n). If sigma(ret)/sigma(n) - 1 is within +/- 0.2, 91% of the true trends fall within the 95% confidence interval of the corresponding retrieved trend. C1 [Kato, Seiji; Liu, Xu; Wielicki, Bruce A.; Mlynczak, Martin G.] NASA, Sci Directorate, Langley Res Ctr, Hampton, VA 23681 USA. [Rose, Fred G.] Sci Syst & Applicat Inc, Hampton, VA USA. RP Kato, S (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA. EM seiji.kato@nasa.gov RI Richards, Amber/K-8203-2015; OI Rose, Fred G/0000-0003-0769-0772 FU NASA Science Directorate through the CLARREO project FX We thank Drs. Stephen Leroy, Xianglei Huang, Oleg Dubovic, Norman Loeb, and Steven Platnick for helpful discussions and suggestions and Ms. Amber Richards for proofreading the manuscript. The work was supported by the NASA Science Directorate through the CLARREO project. NR 27 TC 3 Z9 3 U1 0 U2 6 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD JUN 15 PY 2014 VL 27 IS 12 BP 4403 EP 4420 DI 10.1175/JCLI-D-13-00566.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ4PV UT WOS:000337659200005 ER PT J AU Neena, JM Lee, JY Waliser, D Wang, B Jiang, XN AF Neena, J. M. Lee, June Yi Waliser, Duane Wang, Bin Jiang, Xianan TI Predictability of the Madden-Julian Oscillation in the Intraseasonal Variability Hindcast Experiment (ISVHE) SO JOURNAL OF CLIMATE LA English DT Article ID GENERAL-CIRCULATION MODEL; EXTENDED RANGE FORECASTS; MULTIVARIATE MJO INDEX; AIR-SEA INTERACTIONS; COUPLED MODEL; ENSEMBLE PREDICTION; CLIMATE MODELS; PART I; SKILL; OCEAN AB The Madden-Julian oscillation (MJO) represents a primary source of predictability on the intraseasonal time scales and its influence extends from seasonal variations to weather and extreme events. While the last decade has witnessed marked improvement in dynamical MJO prediction, an updated estimate of MJO predictability from a contemporary suite of dynamic models, in conjunction with an estimate of their corresponding prediction skill, is crucial for guiding future research and development priorities. In this study, the predictability of the boreal winter MJO is revisited based on the Intraseasonal Variability Hindcast Experiment (ISVHE), a set of dedicated extended-range hindcasts from eight different coupled models. Two estimates of MJO predictability are made, based on single-member and ensemble-mean hindcasts, giving values of 20-30 days and 35-45 days, respectively. Exploring the dependence of predictability on the phase of MJO during hindcast initiation reveals a slightly higher predictability for hindcasts initiated from MJO phases 2, 3, 6, or 7 in three of the models with higher prediction skill. The estimated predictability of MJO initiated in phases 2 and 3 (i.e., convection in Indian Ocean with subsequent propagation across Maritime Continent) being equal to or higher than other MJO phases implies that the so-called Maritime Continent prediction barrier may not actually be an intrinsic predictability limitation. For most of the models, the skill for single-member (ensemble mean) hindcasts is less than the estimated predictability limit by about 5-10 days (15-25 days), implying that significantly more skillful MJO forecasts can be afforded through further improvements of dynamical models and ensemble prediction systems (EPS). C1 [Neena, J. M.; Waliser, Duane; Jiang, Xianan] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA. [Lee, June Yi; Wang, Bin] Univ Hawaii Manoa, Int Pacific Res Ctr, Honolulu, HI 96822 USA. [Lee, June Yi] Pusan Natl Univ, Inst Environm Studies, Pusan, South Korea. [Waliser, Duane] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. 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/Climate Program Office Climate Test Bed [GC10-287a]; ONR Marine Meteorology Program [ONRBAA12-001]; NSF Climate and Large-Scale Dynamics Program [AGS-1221013, AGS-1228302]; NOAA/MAPP Program [NA12OAR4310075]; APEC Climate Center, Global Research Laboratory (GRL) [MEST 2011-0021927]; IPRC; JAMSTEC; NOAA; NASA FX The authors thank all the participating members of ISVHE project for the dataset. We acknowledge support from the NOAA/Climate Program Office Climate Test Bed under Project GC10-287a, ONR Marine Meteorology Program under Project ONRBAA12-001, NSF Climate and Large-Scale Dynamics Program under Awards AGS-1221013 and AGS-1228302, and NOAA/MAPP Program under Award NA12OAR4310075. The contribution from D. Waliser was performed on behalf of JIFRESSE and the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with the National Aeronautics and Space Administration. J.-Y. Lee and B. Wang acknowledge support from APEC Climate Center, Global Research Laboratory (GRL) Grant MEST 2011-0021927, and IPRC, which is in part supported by JAMSTEC, NOAA, and NASA. NR 77 TC 28 Z9 34 U1 1 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 JUN 15 PY 2014 VL 27 IS 12 BP 4531 EP 4543 DI 10.1175/JCLI-D-13-00624.1 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ4PV UT WOS:000337659200013 ER PT J AU Min, QL Li, R Lin, B Joseph, E Morris, V Hu, Y Li, SW Wang, S AF Min, Q-L. Li, R. Lin, B. Joseph, E. Morris, V. Hu, Y. Li, S. W. Wang, S. TI Impacts of mineral dust on ice clouds in tropical deep convection systems SO ATMOSPHERIC RESEARCH LA English DT Article DE Ice cloud; Mineral dust aerosol; Heterogeneous nucleation; Homogeneous nucleation; Effective diameter; Satellite observation ID VERTICAL TRANSPORT; AEROSOL; SATELLITE; PRECIPITATION; LIQUID; OCEANS; STORMS AB Multi-platform and multi-sensor observations are used to study the impacts of mineral dust on ice clouds of tropical deep convection systems based on one massive Sahara dust event. The comparisons of cloud properties between dust-laden and dust-free conditions support the hypothesis that the presence of large concentrations of mineral dust produces more ice particles at warmer temperature through heterogeneous nucleation processes. Water vapor competition limits ice particles' growth and results in relatively small sizes of ice particles and a narrow distribution of effective particle diameter in non-precipitating ice clouds, particularly at upper layer with temperatures colder than -40 to -50 degrees C. On the other hand, precipitating ice clouds with sufficient water vapor supply have greater ice water paths under dust-laden conditions than under dust-free conditions. The results also suggest that mineral dusts may invigorate the convection and enhance water vapor supply in deep convective precipitating clouds, lifting ice particles to higher altitudes. Additional study illustrates that the observed microphysical changes of ice clouds in the deep convection systems are not simply due to the differences of large-scale dynamics and thermodynamics. (C) 2014 Elsevier B.V. All rights reserved. C1 [Min, Q-L.; Li, R.; Li, S. W.; Wang, S.] State Univ New York, Atmospher Sci Res Ctr, New York, NY 10016 USA. [Li, R.] Univ Sci & Technol China, CAS, Sch Earth & Space Sci, Key Lab Atmospher Composit & Opt Radiat, Hefei, Anhui, Peoples R China. [Lin, B.; Hu, Y.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA USA. [Joseph, E.; Morris, V.; Li, S. W.] Howard Univ, NOAA, Ctr Atmospher Sci, Washington, DC USA. [Wang, S.] Nanjing Univ, Coll Atmospher Sci, Nanjing, Jiangsu, Peoples R China. RP Min, QL (reprint author), State Univ New York, Atmospher Sci Res Ctr, New York, NY 10016 USA. EM qmin@albany.edu RI Hu, Yongxiang/K-4426-2012 FU US NSF [AGS-1138495]; DOE's Atmospheric System Research Program (Office of Science, OBER) [DE-FG02-03ER63531]; NOAA Educational Partnership Program; Minority Serving Institutions (EPP/MSI) [NA17AE1625, NA17AE1623]; National Natural Science Foundation of China (NSFC) [41375148]; Jiangsu Collaborative Innovation Center for Climate Change FX This work was supported by the US NSF under contract AGS-1138495, by the DOE's Atmospheric System Research Program (Office of Science, OBER) under contract DE-FG02-03ER63531, by the NOAA Educational Partnership Program with Minority Serving Institutions (EPP/MSI) under cooperative agreements NA17AE1625 and NA17AE1623, by the National Natural Science Foundation of China (NSFC) under contract 41375148, and by the Jiangsu Collaborative Innovation Center for Climate Change. NR 34 TC 3 Z9 3 U1 1 U2 12 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0169-8095 EI 1873-2895 J9 ATMOS RES JI Atmos. Res. PD JUN 15 PY 2014 VL 143 BP 64 EP 72 DI 10.1016/j.atmosres.2014.01.026 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH4OY UT WOS:000336109100006 ER PT J AU Tao, WK Lang, S Zeng, X Li, X Matsui, T Mohr, K Posselt, D Chern, J Peters-Lidard, C Norris, PM Kang, IS Choi, I Hou, A Lau, KM Yang, YM AF Tao, Wei-Kuo Lang, Stephen Zeng, Xiping Li, Xiaowen Matsui, Toshi Mohr, Karen Posselt, Derek Chern, Jiundar Peters-Lidard, Christa Norris, Peter M. Kang, In-Sik Choi, Ildae Hou, Arthur Lau, K. -M. Yang, Young-Min TI The Goddard Cumulus Ensemble model (GCE): Improvements and applications for studying precipitation processes SO ATMOSPHERIC RESEARCH LA English DT Article DE Cloud-resolving model; Cloud processes; Microphysics; Diurnal rain; Cloud aerosols; Multiscale modeling framework ID CLOUD-RESOLVING MODEL; TROPICAL OCEANIC CONVECTION; GENERAL-CIRCULATION MODEL; LAND INFORMATION-SYSTEM; MEASURING MISSION TRMM; PART II; WATER BUDGETS; MICROPHYSICS PARAMETERIZATION; SATELLITE-OBSERVATIONS; RADIATION INTERACTION AB Convection is the primary transport process in the Earth's atmosphere. About two-thirds of the Earth's rainfall and severe floods derive from convection. In addition, two-thirds of the global rain falls in the tropics, while the associated latent heat release accounts for three-fourths of the total heat energy for the Earth's atmosphere. Cloud-resolving models (CRMs) have been used to improve our understanding of cloud and precipitation processes and phenomena from micro-scale to cloud-scale and mesoscale as well as their interactions with radiation and surface processes. CRMs use sophisticated and realistic representations of cloud microphysical processes and can reasonably well resolve the time evolution, structure, and life cycles of clouds and cloud systems. CRMs also allow for explicit interaction between clouds, outgoing longwave (cooling) and incoming solar (heating) radiation, and ocean and land surface processes. Observations are required to initialize CRMs and to validate their results. The Goddard Cumulus Ensemble model (GCE) has been developed and improved at NASA/Goddard Space Flight Center over the past three decades. It is a multi-dimensional non-hydrostatic CRM that can simulate clouds and cloud systems in different environments. Early improvements and testing were presented in Tao and Simpson (1993) and Tao et al. (2003a). A review on the application of the GCE to the understanding of precipitation processes can be found in Simpson and Tao (1993) and Tao (2003). In this paper, recent model improvements (microphysics, radiation and land surface processes) are described along with their impact and performance on cloud and precipitation events in different geographic locations via comparisons with observations. In addition, recent advanced applications of the GCE are presented that include understanding the physical processes responsible for diurnal variation, examining the impact of aerosols (cloud condensation nuclei or CCN and ice nuclei or IN) on precipitation processes, utilizing a satellite simulator to improve the microphysics, providing better simulations for satellite-derived latent heating retrieval, and coupling with a general circulation model to improve the representation of precipitation processes. Future research is also discussed. Published by Elsevier B.V. C1 [Tao, Wei-Kuo; Lang, Stephen; Zeng, Xiping; Li, Xiaowen; Matsui, Toshi; Mohr, Karen; Chern, Jiundar] NASA, GSFC, Mesoscale Atmospher Proc Lab, Greenbelt, MD 20771 USA. [Lang, Stephen] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Zeng, Xiping; Li, Xiaowen; Chern, Jiundar] Morgan State Univ, Goddard Earth Sci Technol & Res, Baltimore, MD 21250 USA. [Matsui, Toshi] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Posselt, Derek] Univ Michigan, Ann Arbor, MI 48109 USA. [Peters-Lidard, Christa] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. [Norris, Peter M.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. [Norris, Peter M.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21044 USA. [Kang, In-Sik; Choi, Ildae; Yang, Young-Min] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea. [Hou, Arthur; Lau, K. -M.] NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA. RP Tao, WK (reprint author), NASA, GSFC, Mesoscale Atmospher Proc Lab, Greenbelt, MD 20771 USA. EM Wei-Kuo.Tao-1@nasa.gov RI 안, 민섭/D-9972-2015; Posselt, Derek/I-4912-2012; Peters-Lidard, Christa/E-1429-2012; Lau, William /E-1510-2012; Measurement, Global/C-4698-2015; Norris, Peter/H-2008-2012 OI Posselt, Derek/0000-0002-5670-5822; Peters-Lidard, Christa/0000-0003-1255-2876; Lau, William /0000-0002-3587-3691; Norris, Peter/0000-0001-6807-9884 FU NASA Precipitation Measurement Mission (PMM); NASA Modeling, Analysis, and Prediction (MAP) Program; NASA Advanced Information Systems Technology (AIST) Program FX The first author appreciates the inspiring and enthusiastic support of his mentor, Dr. Joanne Simpson, over a period of 25 years. The author is grateful to Dr. R. Kakar at NASA headquarters for his continuous support of Goddard Cumulus Ensemble model (GCE) improvements and applications. The GCE modeling is mainly supported by the NASA Precipitation Measurement Mission (PMM). The Goddard MMF, NU-WRF, and GPU work are supported by the NASA Modeling, Analysis, and Prediction (MAP) Program and the NASA Advanced Information Systems Technology (AIST) Program. We would also like to thank one anonymous reviewer for helping to improve the quality of the manuscript. Acknowledgment is also made to the NASA Ames Research Center and NASA Goddard Space Flight Center for computer time used in this research. NR 146 TC 15 Z9 15 U1 1 U2 23 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 JUN 15 PY 2014 VL 143 BP 392 EP 424 DI 10.1016/j.atmosres.2014.03.005 PG 33 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AH4OY UT WOS:000336109100030 ER PT J AU Guitreau, M Blichert-Toft, J Mojzsis, SJ Roth, ASG Bourdon, B Cates, NL Bleeker, W AF Guitreau, Martin Blichert-Toft, Janne Mojzsis, Stephen J. Roth, Antoine S. G. Bourdon, Bernard Cates, Nicole L. Bleeker, Wouter TI Lu-Hf isotope systematics of the Hadean-Eoarchean Acasta Gneiss Complex (Northwest Territories, Canada) SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID METAMORPHIC INTERNAL ZONE; CONTINENTAL-CRUST; WOPMAY OROGEN; ARCHEAN CRUST; GA; HAFNIUM; EVOLUTION; ZIRCON; CONSTRAINTS; MANTLE AB The Acasta Gneiss Complex (AGC) is a remnant Hadean-Eoarchean terrane composed of strongly deformed polyphase mafic to felsic gneisses which preserve a multi-stage history of magmatic emplacement, inheritance, and subsequent tectonothermal modifications. The complexities encountered in such an old terrane fragment have been documented in previous geochronological studies of the AGC (e.g. zircon U-Pb, Sm-147-Nd-143), and are evident also in its Lu-Hf isotope systematics. Here, we report new Lu-Hf isotope whole-rock measurements which show that some AGC gneisses were severely disturbed by migmatization and associated mineral segregation, while others preserve their Lu-Hf isotope systematics relatively intact with mostly near-to sub-chondritic initial Hf-176/Hf-177 ratios. Results reveal identifiable Eoarchean and later (Paleoarchean) magmatic events at around 3960 Ma and again at 3600 Ma, with a major metamorphism of the complex at 3750 Ma. The oldest and least disturbed gneisses have a Lu-Hf regression age of 3946 +/- 87 Ma, in good agreement with U-Pb zircon geochronology. A role of yet older crust (4000-4200 Ma) in the formation of the AGC is also evident, but seems not to have influenced to first order the Lu-Hf isotope systematics of the 3960 Ma group. The ca. 3960 Ma group is proposed to be representative of its mantle source based on the absence of correlation between epsilon(Hf(t)) and Ce/Pb. It is further suggested that these two parameters show that the ca. 3600 Ma gneisses were sourced in part from a mafic lithology belonging to the 3960 Ma group, and that multiple sources (mantle and crust) were involved in AGC formation. The identification of preserved Lu-Hf isotope systematics in AGC gneisses means that complementary geochemical and isotopic studies bearing on the petrogenesis of pre-3900 Ma rocks are possible. Despite its history of strong deformation and alteration, carefully selected domains within the AGC carry surviving information about the evolution of the mantle-crust system at the Eoarchean-Hadean boundary. Published by Elsevier Ltd. C1 [Guitreau, Martin; Blichert-Toft, Janne; Mojzsis, Stephen J.; Bourdon, Bernard] Ecole Normale Super Lyon, Lab Geol Lyon, F-69007 Lyon, France. [Guitreau, Martin; Blichert-Toft, Janne; Mojzsis, Stephen J.; Bourdon, Bernard] Univ Lyon 1, CNRS UMR 5276, F-69007 Lyon, France. [Guitreau, Martin] Univ New Hampshire, CEPS, Dept Earth Sci, Durham, NH 03824 USA. [Mojzsis, Stephen J.; Cates, Nicole L.] Univ Colorado, NASA, Lunar Sci Inst, Dept Geol Sci, Boulder, CO 80309 USA. [Mojzsis, Stephen J.; Cates, Nicole L.] Univ Colorado, Ctr Lunar Origin & Evolut, Boulder, CO 80309 USA. [Mojzsis, Stephen J.] Hungarian Acad Sci, Inst Geol & Geochem Res, H-1112 Budapest, Hungary. [Roth, Antoine S. G.] ETH, Inst Geochem & Petr, CH-8092 Zurich, Switzerland. [Bleeker, Wouter] Geol Survey Canada, Ottawa, ON K1A 0E8, Canada. RP Guitreau, M (reprint author), Univ New Hampshire, CEPS, Dept Earth Sci, 56 Coll Rd, Durham, NH 03824 USA. EM martin.guitreau@unh.edu RI Blichert-Toft, Janne/C-8280-2012; OI Blichert-Toft, Janne/0000-0002-4932-4079; Roth, Antoine/0000-0001-9772-4643 FU French Programme National de Planetologie of the Institut National des Sciences de l'Univers and Centre National d'Etudes Spatiales; French Agence Nationale de la Recherche; NASA Exobiology and Evolutionary Biology Program; NASA Lunar Science Institute (Center for Lunar Origin and Evolution, CLOE) FX We have benefitted from discussions with O. Abramov, F. Albarede, P. Peng, R. Stern, D. Trail, and O. Van Breemen. We are grateful to K. Mezger, two anonymous reviewers, and A. E. S. Huang for their constructive comments to the manuscript. Mireille Besairie and Herve Martin are thanked for help at Laboratoire Magmas et Volcans (Clermont-Ferrand, France) and Damien Mollex is thanked for thin section preparations at LGL-TPE (Lyon, France). J.B.T. acknowledges financial support from the French Programme National de Planetologie of the Institut National des Sciences de l'Univers and Centre National d'Etudes Spatiales, and from the French Agence Nationale de la Recherche (grants BEGDy - Birth and Evolution of Terrestrial GeoDynamics and M&Ms - Mantle Melting - Measurements, Models, Mechanisms). S.J.M. and N.L.C. acknowledge support from the NASA Exobiology and Evolutionary Biology Program (Investigating the Hadean Earth), and the NASA Lunar Science Institute (Center for Lunar Origin and Evolution, CLOE). Additional support to S.J.M. came from a Distinguished Visiting Professorship at the Hungarian Academy of Sciences. We are especially grateful for the logistical assistance for work in the Acasta Gneiss Complex provided by the Geological Survey of Canada and the Northwest Territories Geoscience Field Office in Yellowknife. NR 54 TC 16 Z9 16 U1 4 U2 29 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 JUN 15 PY 2014 VL 135 BP 251 EP 269 DI 10.1016/j.gca.2014.03.039 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AG8GN UT WOS:000335656900013 ER PT J AU Evirgen, A Karaman, I Santamarta, R Pons, J Noebe, RD AF Evirgen, A. Karaman, I. Santamarta, R. Pons, J. Noebe, R. D. TI Microstructural characterization and superelastic response of a Ni50.3Ti29.7Zr20 high-temperature shape memory alloy SO SCRIPTA MATERIALIA LA English DT Article DE High-temperature shape memory alloys; NiTiZr; Superelasticity; Precipitation; Microstructure ID CU-ZN-AL; MARTENSITIC-TRANSFORMATION; BEHAVIOR; ZR AB The microstructure and superelastic response of a Ni50.3Ti29.7Zr20 high-temperature shape memory alloy were studied. The alloy exhibited a recoverable strain level of 5% at 170 degrees C and near-perfect superelasticity up to 250 degrees C under 3% applied strain when fine precipitates were present. In this case, large martensite variants easily formed during the stress-induced martensitic transformation while dislocation motion was impeded. In contrast, poor superelastic response was obtained in samples containing large particles that constrain martensite formation to channels between elongated precipitates. (C) 2014 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved. C1 [Evirgen, A.; Karaman, I.] Texas A&M Univ, Dept Mat Sci & Engn, College Stn, TX 77843 USA. [Santamarta, R.; Pons, J.] Univ Illes Balears, Dept Fis, E-07122 Palma De Mallorca, Spain. [Noebe, R. D.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA. RP Karaman, I (reprint author), Texas A&M Univ, Dept Mat Sci & Engn, College Stn, TX 77843 USA. EM ikaraman@tamu.edu RI Karaman, Ibrahim/E-7450-2010; Santamarta, Ruben/K-7865-2016 OI Karaman, Ibrahim/0000-0001-6461-4958; Santamarta, Ruben/0000-0003-3341-5758 FU US Air Force Office of Scientific Research [FA9550-12-1-0218]; US National Science Foundation [DMR 08-44082]; International Materials Institute for Multi-functional Materials for Energy Conversion (IIMEC) at Texas AM University; Spanish MINECO; FEDER [MAT2011-28217-C02-01]; NASA Fundamental Aeronautics Program, Aeronautical Sciences Project FX The present work was supported by the US Air Force Office of Scientific Research, Grant No. FA9550-12-1-0218 and the US National Science Foundation under Grant No. DMR 08-44082, which supports the International Materials Institute for Multi-functional Materials for Energy Conversion (IIMEC) at Texas A&M University. Spanish MINECO and FEDER under Project Number MAT2011-28217-C02-01 are acknowledged for their partial financial support. R.D.N. gratefully acknowledges support from the NASA Fundamental Aeronautics Program, Aeronautical Sciences Project. NR 17 TC 13 Z9 13 U1 2 U2 28 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1359-6462 J9 SCRIPTA MATER JI Scr. Mater. PD JUN 15 PY 2014 VL 81 BP 12 EP 15 DI 10.1016/j.scriptamat.2014.02.012 PG 4 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA AG7TY UT WOS:000335622900004 ER PT J AU Christoffersen, BO Restrepo-Coupe, N Arain, MA Baker, IT Cestaro, BP Ciais, P Fisher, JB Galbraith, D Guan, XD Gulden, L van den Hurk, B Ichii, K Imbuzeiro, H Jain, A Levine, N Miguez-Machor, G Poulter, B Roberti, DR Sakaguchi, K Sahoo, A Schaefer, K Shi, MJ Verbeeck, H Yang, ZL Araujo, AC Kruijt, B Manzi, AO da Rocha, HR von Randow, C Muza, MN Borak, J Costa, MH de Goncalves, LGG Zeng, XB Saleska, SR AF Christoffersen, Bradley O. Restrepo-Coupe, Natalia Arain, M. Altaf Baker, Ian T. Cestaro, Bruno P. Ciais, Phillippe Fisher, Joshua B. Galbraith, David Guan, Xiaodan Gulden, Lindsey van den Hurk, Bart Ichii, Kazuhito Imbuzeiro, Hewlley Jain, Atul Levine, Naomi Miguez-Machor, Gonzalo Poulter, Ben Roberti, Debora R. Sakaguchi, Koichi Sahoo, Alok Schaefer, Kevin Shi, Mingjie Verbeeck, Hans Yang, Zong-Liang Araujo, Alessandro C. Kruijt, Bart Manzi, Antonio O. da Rocha, Humberto R. von Randow, Celso Muza, Michel N. Borak, Jordan Costa, Marcos H. Goncalves de Goncalves, Luis Gustavo Zeng, Xubin Saleska, Scott R. TI Mechanisms of water supply and vegetation demand govern the seasonality and magnitude of evapotranspiration in Amazonia and Cerrado SO AGRICULTURAL AND FOREST METEOROLOGY LA English DT Article DE Tropical forest; Evapotranspiration Deep roots; Groundwater; Canopy stomatal conductance; Intrinsic water use efficiency ID LAND-SURFACE SCHEME; ENVIRONMENT SIMULATOR JULES; CARBON-CYCLE FEEDBACKS; STOMATAL CONDUCTANCE; REGIONAL EVAPOTRANSPIRATION; ATMOSPHERE INTERACTIONS; MODEL DESCRIPTION; BIOSPHERE MODEL; BOUNDARY-LAYER; CLIMATE MODEL AB Evapotranspiration (E) in the Amazon connects forest function and regional climate via its role in precipitation recycling However, the mechanisms regulating water supply to vegetation and its demand for water remain poorly understood, especially during periods of seasonal water deficits In this study, we address two main questions: First, how do mechanisms of water supply (indicated by rooting depth and groundwater) and vegetation water demand (indicated by stomatal conductance and intrinsic water use efficiency) control evapotranspiration (E) along broad gradients of climate and vegetation from equatorial Amazonia to Cerrado, and second, how do these inferred mechanisms of supply and demand compare to those employed by a suite of ecosystem models? We used a network of eddy covariance towers in Brazil coupled with ancillary measurements to address these questions With respect to the magnitude and seasonality of E, models have much improved in equatorial tropical forests by eliminating most dry season water limitation, diverge in performance in transitional forests where seasonal water deficits are greater, and mostly capture the observed seasonal depressions in E at Cerrado However, many models depended universally on either deep roots or groundwater to mitigate dry season water deficits, the relative importance of which we found does not vary as a simple function of climate or vegetation In addition, canopy stomatal conductance (g's) regulates dry season vegetation demand for water at all except the wettest sites even as the seasonal cycle of E follows that of net radiation In contrast, some models simulated no seasonality in gs, even while matching the observed seasonal cycle of E. We suggest that canopy dynamics mediated by leaf phenology may play a significant role in such seasonality, a process poorly represented in models Model bias in gs and E, in turn, was related to biases arising from the simulated light response (gross primary productivity, GPP) or the intringic water use efficiency of photosynthesis (iWUE). We identified deficiencies in models which would not otherwise be apparent based on a simple comparison of simulated and observed rates of E. While some deficiencies can be remedied by parameter tuning, in most models they highlight the need for continued process development of belowground hydrology and in particular, the biological processes of root dynamics and leaf phenology, which via their controls on E, mediate vegetation-climate feedbacks in the tropics. (C) 2014 Elsevier B.V. All rights reserved. C1 [Christoffersen, Bradley O.; Restrepo-Coupe, Natalia; Saleska, Scott R.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ USA. [Christoffersen, Bradley O.; Sakaguchi, Koichi; Zeng, Xubin] Univ Arizona, Dept Atmospher Sci, Tucson, AZ USA. [Restrepo-Coupe, Natalia] Univ Technol Sydney, Plant Funct Biol & Climate Change Cluster, Sydney, NSW 2007, Australia. [Arain, M. Altaf] McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON, Canada. [Baker, Ian T.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA. [Cestaro, Bruno P.; da Rocha, Humberto R.] Univ Sao Paulo, IAG, Dept Ciencias Atmosfer, Sao Paulo, Brazil. [Fisher, Joshua B.] LSCE CEA CNRS UVSQ, F-91191 Gif Sur Yvette, France. [Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Galbraith, David] Univ Oxford, Sch Geog & Environm, Environm Change Inst, Oxford OX1 3QY, England. [Galbraith, David] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. [Guan, Xiaodan; Gulden, Lindsey; Shi, Mingjie; Yang, Zong-Liang] Univ Texas Austin, Dept Geol Sci, Ctr Integrated Earth Syst Sci, Austin, TX USA. [Gulden, Lindsey] ExxonMobil Upstream Res Co, Houston, TX USA. [van den Hurk, Bart] Royal Netherlands Meteorol Inst KNMI, De Bilt, Netherlands. [Ichii, Kazuhito] Fukushima Univ, Fac Symbiot Syst Sci, Fukushima, Japan. [Imbuzeiro, Hewlley; Costa, Marcos H.] Univ Fed Vicosa, Dep Agr Engn, Vicosa, MG, Brazil. [Jain, Atul] Univ Illinois, Dept Atmospher Sci, Urbana, IL USA. [Levine, Naomi] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Miguez-Machor, Gonzalo] Univ Santiago de Compostela, Fac Phys, Santiago De Compostela, Galicia, Spain. [Poulter, Ben] Swiss Fed Res Inst WSL, Birmensdorf, Switzerland. [Roberti, Debora R.] Univ Santa Maria, Dept Phys, Santa Maria, RS, Brazil. [Sahoo, Alok] IGES, Ctr Res Environm & Water, Calverton, MD USA. [Schaefer, Kevin] Univ Colorado, Cooperat Inst Res Environm Sci, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA. [Verbeeck, Hans] Univ Ghent, Plant Ecol Lab, B-9000 Ghent, Belgium. [Araujo, Alessandro C.] Embrapa Amazonia Oriental, Belem, Para, Brazil. [Kruijt, Bart] Wageningen Univ & Res Ctr, Wageningen, Netherlands. [Manzi, Antonio O.] INPA, Manaus, Amazonas, Brazil. [von Randow, Celso] INPE, CCST, Cachoeira Paulista, SP, Brazil. [Muza, Michel N.; Goncalves de Goncalves, Luis Gustavo] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Muza, Michel N.; Goncalves de Goncalves, Luis Gustavo] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD USA. [Borak, Jordan; Goncalves de Goncalves, Luis Gustavo] INPE, CPTEC, Cachoeira Paulista, SP, Brazil. RP Christoffersen, BO (reprint author), Univ Edinburgh, Sch GeoSci, Crew Bldg,Kings Bldg, Edinburgh EH9 3JN, Midlothian, Scotland. EM bchristo@email.arizona.edu RI Yang, Zong-Liang/B-4916-2011; Costa, Marcos/A-5695-2009; Ichii, Kazuhito/D-2392-2010; Restrepo-Coupe, Natalia/C-3507-2015; Jain, Atul/D-2851-2016 OI Zeng, Xubin/0000-0001-7352-2764; Fisher, Joshua/0000-0003-4734-9085; Levine, Naomi/0000-0002-4963-0535; Poulter, Benjamin/0000-0002-9493-8600; Costa, Marcos/0000-0001-6874-9315; Ichii, Kazuhito/0000-0002-8696-8084; Restrepo-Coupe, Natalia/0000-0003-3921-1772; Jain, Atul/0000-0002-4051-3228 FU National Aeronautics and Space Administration (NASA) [NNX09AL52G]; National Science Foundation (Amazon-PIRE, NSF award) [OISE-0730305]; Gordon and Betty Moore Foundation's Andes-Amazon Initiative; FAPESP [08-581203]; Graduate Research Environmental Fellowship (GREF)-U.S. DOE Global Change Education Program, FX This research was funded by the National Aeronautics and Space Administration (NASA) (LBA investigation CD-32 and the LBA-DMIP project, award #NNX09AL52G), the National Science Foundation (Amazon-PIRE, NSF award #OISE-0730305), and the Gordon and Betty Moore Foundation's Andes-Amazon Initiative. HRdR acknowledges FAPESP (08-581203) for aiding field data collection. Soil moisture data for the RJA field site were collected under the ABRACOS project and made available by the UK Institute of Hydrology and the Instituto Nacional de Pesquisas Espaciais (Brazil). ABRACOS was a collaboration between the Agencia Brasileira de Cooperacao and the UK Overseas Development Administration. B.O.C. acknowledges support from a Graduate Research Environmental Fellowship (GREF)-U.S. DOE Global Change Education Program, as well as an NSF Amazon-PIRE fellowship. J.B.F. contributed to this paper from the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We thank Reto Stoeckli for initial generation of gap-filled meteorological driver data, and Enrique Rosero for discussions helping to frame some analyses for this paper. We are indebted to both LBA and ABRACOS projects, and their field technicians, without whose efforts to establish and preserve the quality of datasets used here, this paper would not have been possible. We are grateful to two anonymous reviewers whose comments greatly improved the clarity of this paper. NR 82 TC 19 Z9 21 U1 5 U2 88 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-1923 EI 1873-2240 J9 AGR FOREST METEOROL JI Agric. For. Meteorol. PD JUN 15 PY 2014 VL 191 BP 33 EP 50 DI 10.1016/j.agrformet.2014.02.008 PG 18 WC Agronomy; Forestry; Meteorology & Atmospheric Sciences SC Agriculture; Forestry; Meteorology & Atmospheric Sciences GA AG4YT UT WOS:000335427000004 ER PT J AU Zhang, QY Cheng, YB Lyapustin, AI Wang, YJ Xiao, XM Suyker, A Verma, S Tan, B Middleton, EM AF Zhang, Qingyuan Cheng, Yen-Ben Lyapustin, Alexei I. Wang, Yujie Xiao, Xiangming Suyker, Andrew Verma, Shashi Tan, Bin Middleton, Elizabeth M. TI Estimation of crop gross primary production (GPP): I. impact of MODIS observation footprint and impact of vegetation BRDF characteristics SO AGRICULTURAL AND FOREST METEOROLOGY LA English DT Article DE Daily GPP; MODIS; Chlorophyll; Footprint; BRDF ID LIGHT-USE EFFICIENCY; NET PRIMARY PRODUCTION; SURFACE PARAMETERIZATION SIB2; REMOTE ESTIMATION; SATELLITE DATA; EO-1 HYPERION; LANDSAT DATA; LEAF-AREA; FOREST; MODEL AB Accurate estimation of gross primary production (GPP) is essential for carbon cycle and climate change studies. Three AmeriFlux crop sites of maize and soybean were selected for this study. Two of the sites were irrigated and the other one was rainfed. The normalized difference vegetation index (NDVI), the enhanced vegetation index (EVI), the green band chlorophyll index (CIgreen) and the green band wide dynamic range vegetation index (WDRVIgreen) were computed from the moderate resolution imaging spectroradiometer (MODIS) surface reflectance data. We examined the impacts of the MODIS observation footprint and the vegetation bidirectional reflectance distribution function (BRDF) on crop daily GPP estimation with the four spectral vegetation indices (VIs - NDVI, EVI, WDRVIgreen and CIgreen, where GPP was) predicted with two linear models, with and without offset: GPP = alpha x VI x PAR and GPP = alpha x VI x PAR + b. Model performance was evaluated with coefficient of determination (R-2), root mean square error (RMSE), and coefficient of variation (CV). The MODIS data were filtered into four categories and four experiments were conducted to assess the impacts. The first experiment included all observations. The second experiment only included observations with view zenith angle (VZA) <= 35 to constrain growth of the footprint size,which achieved a better grid cell match with the agricultural fields. The third experiment included only forward scatter observations with VZA <= 35 degrees. The fourth experiment included only backscatter observations with VZA <= 35 degrees. Overall, the EVI yielded the most consistently strong relationships to daily GPP under all examined conditions. The model GPP = a x VI x PAR + b had better performance than the model GPP = alpha x VI x PAR, and the offset was significant for most cases. Better performance was obtained for the irrigated field than its counterpart rainfed field. Comparison of experiment 2 vs. experiment 1 was used to examine the observation footprint impact whereas comparison of experiment 4 vs. experiment 3 was used to examine the BRDF impact. Changes in R2, RMSE,CV and changes in model coefficients "a" and "b" (experiment 2 vs. experiment 1; and experiment 4 vs. experiment 3) were indicators of the impacts. The second experiment produced better performance than the first experiment, increasing R-2(up arrow 0.13) and reducing RMSE (down arrow 0.68 g Cm-2 d(-1)) and CV (down arrow 9%). For each VI, the slope of GPP = a x VI x PAR in the second experiment for each crop type changed little while the slope and intercept of GPP = a x VI x PAR + b varied field by field. The Cl-green was least affected by the MODIS observation footprint in estimating crop daily GPP (R-2, up arrow 0.08; RMSE, down arrow 0.42 g Cm-2 d(-1); and CV, down arrow 7%) Footprint most affected the NDVI (R-2, up arrow 0.15; CV, down arrow 10%) and the EVI (RMSE, down arrow 0.84 g Cm-2 d(-1)). The vegetation BRDF impact also caused variation of model performance and change of model coefficients. Significantly different slopes were obtained for forward vs. backscatter observations, especially for the Clgreen and the NDVI. Both the footprint impact and the BRDF impact varied with crop types, irrigation options, model options and VI options. (C) 2014 Elsevier B.V. All rights reserved. C1 [Zhang, Qingyuan] Unvers Space Res Assoc, Columbia, MD 21044 USA. [Zhang, Qingyuan; Cheng, Yen-Ben; Wang, Yujie; Middleton, Elizabeth M.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA. [Cheng, Yen-Ben] Earth Resources Technol Inc, Laurel, MD 20707 USA. [Lyapustin, Alexei I.] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD 20771 USA. [Wang, Yujie] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Xiao, Xiangming] Univ Oklahoma, Ctr Spatial Anal, Norman, OK 73019 USA. [Suyker, Andrew; Verma, Shashi] Univ Nebraska, Sch Nat Resources, Lincoln, NE 68588 USA. [Tan, Bin] Sigma Space Corp, Lanham, MD 20706 USA. RP Zhang, QY (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA. EM qyz72@yahoo.com RI Lyapustin, Alexei/H-9924-2014 OI Lyapustin, Alexei/0000-0003-1105-5739 FU NASA Terrestrial Ecology Program [NNX12AJ51G] FX The authors would like to thank the support and the use of facilities and equipment provided by the Center for Advanced Land Management Information Technologies and the Carbon Sequestration program, University of Nebraska-Lincoln. The authors also would like to thank the anonymous reviewers and Dr. Anatoly A. Gitelson who have provided helpful suggestion and comments for this paper. This work was supported by the NASA Terrestrial Ecology Program (Grant # NNX12AJ51G, PI: Q. Zhang). NR 70 TC 13 Z9 15 U1 4 U2 51 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-1923 EI 1873-2240 J9 AGR FOREST METEOROL JI Agric. For. Meteorol. PD JUN 15 PY 2014 VL 191 BP 51 EP 63 DI 10.1016/j.agrformet.2014.02.002 PG 13 WC Agronomy; Forestry; Meteorology & Atmospheric Sciences SC Agriculture; Forestry; Meteorology & Atmospheric Sciences GA AG4YT UT WOS:000335427000005 ER PT J AU Vu, TH Cable, ML Choukroun, M Hodyss, R Beauchamp, P AF Tuan Hoang Vu Cable, Morgan L. Choukroun, Mathieu Hodyss, Robert Beauchamp, Patricia TI Formation of a New Benzene-Ethane Co-Crystalline Structure Under Cryogenic Conditions SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID VIBRATIONAL FREQUENCIES; CHEMICAL-COMPOSITION; ACETYLENE; SPECTRA; ENERGY; HEXAFLUOROBENZENE; COMPLEXES; CLUSTERS; TITAN; WATER AB We report the first experimental finding of a solid molecular complex between benzene and ethane, two small apolar hydrocarbons, at atmospheric pressure and cryogenic temperatures. Considerable amounts of ethane are found to be incorporated inside the benzene lattice upon the addition of liquid ethane onto solid benzene at 90-150 K, resulting in formation of a distinctive co-crystalline structure that can be detected via micro-Raman spectroscopy. Two new features characteristic of these co-crystals are observed in the Raman spectra at 2873 and 1455 cm(-1), which are red-shifted by 12 cm(-1) from the upsilon(1) (a(1g)) and upsilon(11) (e(g)) stretching modes of liquid ethane, respectively. Analysis of benzene and ethane vibrational bands combined with quantum mechanical modeling of isolated molecular dimers reveal an interaction between the aromatic ring of benzene and the hydrogen atoms of ethane in a C-H center dot center dot center dot pi fashion. The most favored configuration for the benzene-ethane dimer is the monodentate-contact structure, with a calculated interaction energy of 9.33 kJ/mol and an equilibrium bonding distance of 2.66 angstrom. These parameters are comparable to those for a T-shaped co-crystalline complex between benzene and acetylene that has been previously reported in the literature. These results are relevant for understanding the hydrocarbon cycle of Titan, where benzene and similar organics may act as potential hydrocarbon reservoirs due to this incorporation mechanism. C1 [Tuan Hoang Vu; Cable, Morgan L.; Choukroun, Mathieu; Hodyss, Robert; Beauchamp, Patricia] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA. RP Hodyss, R (reprint author), CALTECH, NASA Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM robert.p.hodyss@jpl.nasa.gov RI Choukroun, Mathieu/F-3146-2017; Vu, Tuan/F-5223-2017 OI Choukroun, Mathieu/0000-0001-7447-9139; Vu, Tuan/0000-0001-6839-9765 FU NASA; NASA Astrobiology Institute (Titan node); NASA Astrobiology Science and Technology Instrument Development Program (ASTID); NASA Outer Planets Research Program (OPR); NASA Postdoctoral Program FX This work was conducted at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Support from the NASA Astrobiology Institute (Titan node), the NASA Astrobiology Science and Technology Instrument Development Program (ASTID), the NASA Outer Planets Research Program (OPR), the NASA Postdoctoral Program (administered by Oak Ridge Associated Universities), and government sponsorship are gratefully acknowledged. NR 33 TC 4 Z9 4 U1 3 U2 16 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD JUN 12 PY 2014 VL 118 IS 23 BP 4087 EP 4094 DI 10.1021/jp501698j PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA AJ2ON UT WOS:000337497300010 PM 24809894 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 Bavigadda, V 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 Clark, JA Cleva, F Coccia, E Cohadon, PF Colla, A Collette, C Colombini, M Cominsky, L Constancio, M Conte, A Cook, D Corbitt, TR Cordier, M Cornish, N Corpuz, A Corsi, A Costa, CA Coughlin, MW Coughlin, S Coulon, JP Countryman, S Couvares, P Coward, DM Cowart, M Coyne, DC Coyne, R Craig, K Creighton, JDE Crowder, SG Cumming, A Cunningham, L Cuoco, E Dahl, K Dal Canton, T Damjanic, M Danilishin, SL D'Antonio, S Danzmann, K Dattilo, V Daveloza, H Davier, M Davies, GS Daw, EJ Day, R Dayanga, T Debreczeni, G Degallaix, J Deleglise, S Del Pozzo, W Denker, T Dent, T Dereli, H Dergachev, V De Rosa, R DeRosa, RT DeSalvo, R Dhurandhar, S Diaz, M Di Fiore, L Di Lieto, A Di Palma, I Di Virgilio, A Donath, A Donovan, F Dooley, KL Doravari, S Dossa, 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, H Ehrens, P Eichholz, J Eikenberry, SS Endroczi, G Essick, R Etzel, T Evans, M Evans, T Factourovich, M Fafone, V Fairhurst, S Fang, Q Farinon, S Farr, B Farr, WM Favata, M Fehrmann, H Fejer, MM Feldbaum, D Feroz, F Ferrante, I Ferrini, F Fidecaro, F Finn, LS Fiori, I Fisher, RP Flaminio, R Fournier, JD Franco, S Frasca, S Frasconi, F Frede, M Frei, Z Freise, A Frey, R Fricke, TT Fritschel, P Frolov, VV Fulda, P Fyffe, M Gair, J Gammaitoni, L Gaonkar, S Garufi, F Gehrels, N Gemme, G Genin, E Gennai, A Ghosh, S Giaime, JA Giardina, KD Giazotto, A Gill, C Gleason, J Goetz, E Goetz, R Gondan, L Gonzalez, G Gordon, N Gorodetsky, ML Gossan, S Gossler, S Gouaty, R Graf, C Graff, PB Granata, M Grant, A Gras, S Gray, C Greenhalgh, RJS Gretarsson, AM Groot, P Grote, H Grover, K Grunewald, S Guidi, GM Guido, C Gushwa, K Gustafson, EK Gustafson, R Hammer, D Hammond, G Hanke, M Hanks, J Hanna, C Hanson, J Harms, J Harry, GM Harry, IW Harstad, ED Hart, M Hartman, MT Haster, CJ Haughian, K Heidmann, A Heintze, M Heitmann, H Hello, P Hemming, G Hendry, M Heng, IS Heptonstall, AW Heurs, M Hewitson, M Hild, S Hoak, D Hodge, KA Holt, K Hooper, S Hopkins, P Hosken, DJ Hough, J Howell, EJ Hu, Y Huerta, E Hughey, B Husa, S Huttner, SH Huynh, M Huynh-Dinh, T Ingram, DR Inta, R Isogai, T Ivanov, A Iyer, BR Izumi, K Jacobson, M James, E 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 Kawabe, K Kawazoe, F Kefelian, F Keiser, GM Keitel, D Kelley, DB Kells, W Khalaidovski, A Khalili, FY Khazanov, EA Kim, C Kim, K Kim, NG Kim, N Kim, YM King, EJ King, PJ Kinzel, DL Kissel, JS Klimenko, S Kline, J Koehlenbeck, S Kokeyama, K Kondrashov, V Koranda, S Korth, WZ Kowalska, I Kozak, DB Kremin, A Kringel, V Krishnan, B Krolak, A Kuehn, G Kumar, A Kumar, P Kumar, R Kuo, L Kutynia, A Kwee, P Landry, M Lantz, B Larson, S Lasky, PD Lawrie, C Lazzarini, A Lazzaro, C Leaci, P Leavey, S Lebigot, EO Lee, CH Lee, HK Lee, HM Lee, J Leonardi, M Leong, JR Le Roux, A Leroy, N Letendre, N Levin, Y Levine, B Lewis, J Li, TGF Libbrecht, K Libson, A Lin, AC 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CA LIGO Sci Collaboration Virgo Collaboration TI Search for gravitational radiation from intermediate mass black hole binaries in data from the second LIGO-Virgo joint science run SO PHYSICAL REVIEW D LA English DT Article ID X-RAY SOURCES; GLOBULAR-CLUSTERS; VARIABILITY AB This paper reports on an unmodeled, all-sky search for gravitational waves from merging intermediate mass black hole binaries (IMBHB). The search was performed on data from the second joint science run of the LIGO and Virgo detectors (July 2009-October 2010) and was sensitive to IMBHBs with a range up to similar to 200 Mpc, averaged over the possible sky positions and inclinations of the binaries with respect to the line of sight. No significant candidate was found. Upper limits on the coalescence-rate density of nonspinning IMBHBs with total masses between 100 and 450 M-circle dot and mass ratios between 0.25 and 1 were placed by combining this analysis with an analogous search performed on data from the first LIGO-Virgo joint science run (November 2005-October 2007). The most stringent limit was set for systems consisting of two 88 M-circle dot black holes and is equal to 0.12 Mpc(-3) Myr(-1) at the 90% confidence level. This paper also presents the first estimate, for the case of an unmodeled analysis, of the impact on the search range of IMBHB spin configurations: the visible volume for IMBHBs with nonspinning components is roughly doubled for a population of IMBHBs with spins aligned with the binary's orbital angular momentum and uniformly distributed in the dimensionless spin parameter up to 0.8, whereas an analogous population with antialigned spins decreases the visible volume by similar to 20%. 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.; Gustafson, E. K.; Harms, J.; Heptonstall, A. W.; Hodge, K. A.; Ivanov, A.; Jacobson, M.; James, E.; Kalmus, P.; Kanner, J. B.; Kells, W.; King, P. J.; Kondrashov, V.; Korth, W. Z.; Kozak, D. B.; Lazzarini, A.; Lewis, J.; Li, T. G. F.; Libbrecht, K.; Litvine, V.; Mageswaran, M.; Mailand, K.; Maros, E.; Martynov, D.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Osthelder, C.; Pedraza, M.; Phelps, M.; Price, L. R.; Privitera, S.; Quintero, E.; Raymond, V.; Reitze, D. H.; Robertson, N. A.; Rollins, J. G.; Sannibale, V.; Singer, A.; Singer, L.; Smith, M.; Smith, R. J. E.; Smith-Lefebvre, N. D.; Taylor, R.; Thirugnanasambandam, M. 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RP Aasi, J (reprint author), LIGO Calif Inst Technol, Pasadena, CA 91125 USA. RI Nelemans, Gijs/D-3177-2012; 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; 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; 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; Strain, Kenneth/D-5236-2011; Miao, Haixing/O-1300-2013; Prokhorov, Leonid/I-2953-2012; Khalili, Farit/D-8113-2012; Gehring, Tobias/A-8596-2016; Heidmann, Antoine/G-4295-2016; Mow-Lowry, Conor/F-8843-2015; 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; Hild, Stefan/A-3864-2010; Bell, Angus/E-7312-2011; Ottaway, David/J-5908-2015; Garufi, Fabio/K-3263-2015; Deleglise, Samuel/B-1599-2015; Danilishin, Stefan/K-7262-2012; Iyer, Bala R./E-2894-2012; Canuel, Benjamin/C-7459-2014; Costa, Cesar/G-7588-2012; Gemme, Gianluca/C-7233-2008; Losurdo, Giovanni/K-1241-2014; Gammaitoni, Luca/B-5375-2009; Lee, Chang-Hwan/B-3096-2015; Gorodetsky, Michael/C-5938-2008; McClelland, David/E-6765-2010; M, Manjunath/N-4000-2014; Steinlechner, Sebastian/D-5781-2013; Vecchio, Alberto/F-8310-2015; Howell, Eric/H-5072-2014; 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; OI Nelemans, Gijs/0000-0002-0752-2974; 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; Travasso, Flavio/0000-0002-4653-6156; Punturo, Michele/0000-0001-8722-4485; Cella, Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167; 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; Strain, Kenneth/0000-0002-2066-5355; Miao, Haixing/0000-0003-4101-9958; Gehring, Tobias/0000-0002-4311-2593; Heidmann, Antoine/0000-0002-0784-5175; 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; Danilishin, Stefan/0000-0001-7758-7493; Iyer, Bala R./0000-0002-4141-5179; Gemme, Gianluca/0000-0002-1127-7406; Losurdo, Giovanni/0000-0003-0452-746X; Gammaitoni, Luca/0000-0002-4972-7062; Lee, Chang-Hwan/0000-0003-3221-1171; Gorodetsky, Michael/0000-0002-5159-2742; McClelland, David/0000-0001-6210-5842; M, Manjunath/0000-0001-8710-0730; Steinlechner, Sebastian/0000-0003-4710-8548; Vecchio, Alberto/0000-0002-6254-1617; Del Pozzo, Walter/0000-0003-3978-2030; O'Shaughnessy, Richard/0000-0001-5832-8517; Allen, Bruce/0000-0003-4285-6256; Granata, Massimo/0000-0003-3275-1186; Vitale, Salvatore/0000-0003-2700-0767; 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; 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; Drago, Marco/0000-0002-3738-2431; Collette, Christophe/0000-0002-4430-3703; Pierro, Vincenzo/0000-0002-6020-5521; Coccia, Eugenio/0000-0002-6669-5787; Vetrano, Flavio/0000-0002-7523-4296; Vedovato, Gabriele/0000-0001-7226-1320; Howell, Eric/0000-0001-7891-2817; Fairhurst, Stephen/0000-0001-8480-1961; 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; Aulbert, Carsten/0000-0002-1481-8319; 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; Denker, Timo/0000-0003-1259-5315; Ward, Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447; Whelan, John/0000-0001-5710-6576; Kanner, Jonah/0000-0001-8115-0577; Freise, Andreas/0000-0001-6586-9901; Nitz, Alexander/0000-0002-1850-4587; 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 FU United States National Science Foundation for the construction and operation of the LIGO Laboratory; 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; OTKA of Hungary; 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; Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation; Alfred P. Sloan Foundation FX The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector, and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Economia y Competitividad, the Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the National Aeronautics and Space Administration, OTKA of Hungary, 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 document was assigned the LIGO number LIGO-P1300158. NR 66 TC 15 Z9 15 U1 4 U2 35 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD JUN 12 PY 2014 VL 89 IS 12 AR 122003 DI 10.1103/PhysRevD.89.122003 PG 15 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AK8EW UT WOS:000338661100001 ER PT J AU Curtis, TH McCandless, CT Carlson, JK Skomal, GB Kohler, NE Natanson, LJ Burgess, GH Hoey, JJ Pratt, HL AF Curtis, Tobey H. McCandless, Camilla T. Carlson, John K. Skomal, Gregory B. Kohler, Nancy E. Natanson, Lisa J. Burgess, George H. Hoey, John J. Pratt, Harold L., Jr. TI Seasonal Distribution and Historic Trends in Abundance of White Sharks, Carcharodon carcharias, in the Western North Atlantic Ocean SO PLOS ONE LA English DT Article ID NEW-SOUTH-WALES; GULF-OF-MEXICO; EASTERN PACIFIC; MIGRATION PATTERNS; HARBOR PORPOISE; POPULATIONS; CALIFORNIA; MOVEMENTS; PREDATION; BEHAVIOR AB Despite recent advances in field research on white sharks (Carcharodon carcharias) in several regions around the world, opportunistic capture and sighting records remain the primary source of information on this species in the northwest Atlantic Ocean (NWA). Previous studies using limited datasets have suggested a precipitous decline in the abundance of white sharks from this region, but considerable uncertainty in these studies warrants additional investigation. This study builds upon previously published data combined with recent unpublished records and presents a synthesis of 649 confirmed white shark records from the NWA compiled over a 210-year period (1800-2010), resulting in the largest white shark dataset yet compiled from this region. These comprehensive records were used to update our understanding of their seasonal distribution, relative abundance trends, habitat use, and fisheries interactions. All life stages were present in continental shelf waters year-round, but median latitude of white shark occurrence varied seasonally. White sharks primarily occurred between Massachusetts and New Jersey during summer and off Florida during winter, with broad distribution along the coast during spring and fall. The majority of fishing gear interactions occurred with rod and reel, longline,and gillnet gears. Historic abundance trends from multiple sources support a significant decline in white shark abundance in the 1970s and 1980s, but there have been apparent increases in abundance since the 1990s when a variety of conservation measures were implemented. Though the white shark's inherent vulnerability to exploitation warrants continued protections, our results suggest a more optimistic outlook for the recovery of this iconic predator in the Atlantic. C1 [Curtis, Tobey H.] NOAA, Natl Marine Fisheries Serv, Greater Atlantic Reg Fisheries Off, Gloucester, MA 01930 USA. [McCandless, Camilla T.; Kohler, Nancy E.; Natanson, Lisa J.; Hoey, John J.; Pratt, Harold L., Jr.] NOAA, Natl Marine Fisheries Serv, Northeast Fisheries Sci Ctr, Narragansett, RI USA. [Carlson, John K.] NOAA, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Panama City, FL USA. [Skomal, Gregory B.] Massachusetts Div Marine Fisheries, New Bedford, MA USA. [Burgess, George H.] Univ Florida, Florida Museum Nat Hist, Florida Program Shark Res, Gainesville, FL 32611 USA. [Pratt, Harold L., Jr.] Mote Marine Lab, Summerland Key, FL USA. RP Curtis, TH (reprint author), NOAA, Natl Marine Fisheries Serv, Greater Atlantic Reg Fisheries Off, Gloucester, MA 01930 USA. EM Tobey.Curtis@noaa.gov NR 81 TC 15 Z9 15 U1 9 U2 68 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 JUN 11 PY 2014 VL 9 IS 6 AR e99240 DI 10.1371/journal.pone.0099240 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AK7TQ UT WOS:000338631000066 PM 24918579 ER PT J AU Lindenmaier, R Dubey, MK Henderson, BG Butterfield, ZT Herman, JR Rahn, T Lee, SH AF Lindenmaier, Rodica Dubey, Manvendra K. Henderson, Bradley G. Butterfield, Zachary T. Herman, Jay R. Rahn, Thom Lee, Sang-Hyun TI Multiscale observations of CO2, (CO2)-C-13, and pollutants at Four Corners for emission verification and attribution SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE air pollution; greenhouse gases; climate change ID DIOXIDE; REGION; URBAN; GAS AB There is a pressing need to verify air pollutant and greenhouse gas emissions from anthropogenic fossil energy sources to enforce current and future regulations. We demonstrate the feasibility of using simultaneous remote sensing observations of column abundances of CO2, CO, and NO2 to inform and verify emission inventories. We report, to our knowledge, the first ever simultaneous column enhancements in CO2 (3-10 ppm) and NO2 (1-3 Dobson Units), and evidence of delta(CO2)-C-13 depletion in an urban region with two large coal-fired power plants with distinct scrubbing technologies that have resulted in Delta NOx/Delta CO2 emission ratios that differ by a factor of two. Ground-based total atmospheric column trace gas abundances change synchronously and correlate well with simultaneous in situ point measurements during plume interceptions. Emission ratios of Delta NOx/Delta CO2 and Delta SO2/Delta CO2 derived from in situ atmospheric observations agree with those reported by in-stack monitors. Forward simulations using in-stack emissions agree with remote column CO2 and NO2 plume observations after fine scale adjustments. Both observed and simulated column Delta NO2/Delta CO2 ratios indicate that a large fraction (70-75%) of the region is polluted. We demonstrate that the column emission ratios of Delta NO2/Delta CO2 can resolve changes from day-to-day variation in sources with distinct emission factors (clean and dirty power plants, urban, and fires). We apportion these sources by using NO2, SO2, and CO as signatures. Our high-frequency remote sensing observations of CO2 and coemitted pollutants offer promise for the verification of power plant emission factors and abatement technologies from ground and space. C1 [Lindenmaier, Rodica; Dubey, Manvendra K.; Henderson, Bradley G.; Butterfield, Zachary T.; Rahn, Thom; Lee, Sang-Hyun] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Herman, Jay R.] Univ Maryland, Goddard Space Flight Ctr, Joint Ctr Earth Syst Technol, Greenbelt, MD 20771 USA. RP Lindenmaier, R (reprint author), Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87545 USA. EM rodica@lanl.gov; dubey@lanl.gov RI Dubey, Manvendra/E-3949-2010; Lee, Sang-Hyun/B-5974-2013; Rahn, Thom/C-5211-2012 OI Dubey, Manvendra/0000-0002-3492-790X; FU LANL Laboratory Directed Research and Development project "Multi-Scale Science Framework for Climate Treaty Verification: Attributing & Tracking GHG Fluxes Using Co-Emitted Signatures" FX We thank TCCON (D. Wunch and P. Wennberg) for providing resources to achieve high-accuracy retrievals. We thank A. Cede and N. Abuhassan for their continuous effort to optimize and maintain the Pandora instrument. We acknowledge the New Mexico Environment Department (T. Hertel, M. Jones, and R. Szkoda), EPA (M. Sather), and Bureau of Land and Management (M. Uhl) for providing us access to the site and in situ air quality data. S.-H. L. thanks the Korean Meteorological Administration for support with supercomputing resources. We thank R. Middleton and J. Muss [Los Alamos National Laboratory (LANL)] for editorial assistance. The reported research was supported by the LANL Laboratory Directed Research and Development project "Multi-Scale Science Framework for Climate Treaty Verification: Attributing & Tracking GHG Fluxes Using Co-Emitted Signatures" (principal investigator M.K.D.). NR 16 TC 12 Z9 12 U1 1 U2 18 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 JUN 10 PY 2014 VL 111 IS 23 BP 8386 EP 8391 DI 10.1073/pnas.1321883111 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AI6IJ UT WOS:000336976000037 PM 24843169 ER PT J AU Binns, WR Bose, RG Braun, DL Brandt, TJ Daniels, WM Dowkontt, PF Fitzsimmons, SP Hahne, DJ Hams, T Israel, MH Klemic, J Labrador, AW Link, JT Mewaldt, RA Mitchell, JW Moore, P Murphy, RP Olevitch, MA Rauch, BF Sakai, K Sebastian, FS Sasaki, M Simburger, GE Stone, EC Waddington, CJ Ward, JE Wiedenbeck, ME AF Binns, W. R. Bose, R. G. Braun, D. L. Brandt, T. J. Daniels, W. M. Dowkontt, P. F. Fitzsimmons, S. P. Hahne, D. J. Hams, T. Israel, M. H. Klemic, J. Labrador, A. W. Link, J. T. Mewaldt, R. A. Mitchell, J. W. Moore, P. Murphy, R. P. Olevitch, M. A. Rauch, B. F. Sakai, K. Sebastian, F. San Sasaki, M. Simburger, G. E. Stone, E. C. Waddington, C. J. Ward, J. E. Wiedenbeck, M. E. TI THE SuperTIGER INSTRUMENT: MEASUREMENT OF ELEMENTAL ABUNDANCES OF ULTRA-HEAVY GALACTIC COSMIC RAYS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; instrumentation : detectors ID SUPERNOVA-GENERATED SUPERBUBBLES; OB ASSOCIATIONS; ENERGETIC PARTICLES; IONIZING PARTICLES; REMNANTS; ORIGIN; ACCELERATION; EMISSION; SCINTILLATORS; MICROQUASARS AB The SuperTIGER (Super Trans-Iron Galactic Element Recorder) instrument was developed to measure the abundances of galactic cosmic-ray elements from Ne-10 to Zr-40 with individual element resolution and the high statistics needed to test models of cosmic-ray origins. SuperTIGER also makes exploratory measurements of the abundances of elements with 40 <= Z <= 60 and measures the energy spectra of the more abundant elements for Z <= 30 from about 0.8 to 10 GeV/nucleon. This instrument is an enlarged and higher resolution version of the earlier TIGER instrument. It was designed to provide the largest geometric acceptance possible and to reach as high an altitude as possible, flying on a standard long-duration 1.11 million m(3) balloon. SuperTIGER was launched from Williams Field, McMurdo Station, Antarctica, on 2012 December 8, and made about 2.7 revolutions around the South Pole in 55 days of flight, returning data on over 50 x 10(6) cosmic-ray nuclei with Z <= 10, including similar to 1300 with Z > 29 and similar to 60 with Z > 49. Here, we describe the instrument, the methods of charge identification employed, the SuperTIGER balloon flight, and the instrument performance. C1 [Binns, W. R.; Bose, R. G.; Braun, D. L.; Dowkontt, P. F.; Israel, M. H.; Moore, P.; Murphy, R. P.; Olevitch, M. A.; Rauch, B. F.; Simburger, G. E.; Ward, J. E.] Washington Univ, St Louis, MO 63130 USA. [Brandt, T. J.; Daniels, W. M.; Fitzsimmons, S. P.; Hahne, D. J.; Hams, T.; Link, J. T.; Mitchell, J. W.; Sakai, K.; Sebastian, F. San; Sasaki, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Klemic, J.; Labrador, A. W.; Mewaldt, R. A.; Stone, E. C.] CALTECH, Pasadena, CA 91125 USA. [Waddington, C. J.] Univ Minnesota, Minneapolis, MN 55455 USA. [Wiedenbeck, M. E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hams, T.; Link, J. T.; Sakai, K.; Sasaki, M.] Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA. RP Binns, WR (reprint author), Washington Univ, St Louis, MO 63130 USA. EM wrb@wustl.edu OI Ward, John E/0000-0003-1973-0794 FU NASA; ROSES 2007 APRA program [NNX09AC17G]; Washington University [NNX09AC18G]; JPL NASA/GSFC [APRA07- 0146]; McDonnell Center for the Space Sciences at Washington University; Peggy and Steve Fossett Foundation; (RPM) at Washington University FX NASA supported this research under the ROSES 2007 APRA program under grants NNX09AC17G to Washington University in St. Louis and NNX09AC18G to Caltech, and JPL, and APRA07- 0146 to NASA/GSFC. WU also received support from the McDonnell Center for the Space Sciences at Washington University. We thank the NASA Columbia Scientific Balloon Facility, the NASA Balloon Program Office, and the NSF United States Antarctic Program for the excellent and highly professional efforts that resulted in the record long-duration balloon flight of SuperTIGER. We also gratefully acknowledge support from the Peggy and Steve Fossett Foundation for graduate student support (RPM) at Washington University. NR 50 TC 4 Z9 4 U1 0 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2014 VL 788 IS 1 AR 18 DI 10.1088/0004-637X/788/1/18 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200018 ER PT J AU Brenneman, LW Madejski, G Fuerst, F Matt, G Elvis, M Harrison, FA Ballantyne, DR Boggs, SE Christensen, FE Craig, WW Fabian, AC Grefenstette, BW Hailey, CJ Madsen, KK Marinucci, A Rivers, E Stern, D Walton, DJ Zhang, WW AF Brenneman, L. W. Madejski, G. Fuerst, F. Matt, G. Elvis, M. Harrison, F. A. Ballantyne, D. R. Boggs, S. E. Christensen, F. E. Craig, W. W. Fabian, A. C. Grefenstette, B. W. Hailey, C. J. Madsen, K. K. Marinucci, A. Rivers, E. Stern, D. Walton, D. J. Zhang, W. W. TI THE BROAD-BAND X-RAY SPECTRUM OF IC 4329A FROM A JOINT NuSTAR/SUZAKU OBSERVATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion; accretion disks; galaxies : active; galaxies : individual (IC 4329A); galaxies : nuclei; galaxies : Seyfert; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; SEYFERT-GALAXY IC-4329A; K-ALPHA LINES; BLACK-HOLE; XMM-NEWTON; BEPPOSAX OBSERVATIONS; COMPTON REFLECTION; EDDINGTON RATIO; TIMING-EXPLORER; ACCRETION DISK AB We have obtained a deep, simultaneous observation of the bright, nearby Seyfert galaxy IC 4329A with Suzaku and NuSTAR. Through a detailed spectral analysis, we are able to robustly separate the continuum, absorption, and distant reflection components in the spectrum. The absorbing column is found to be modest (similar to 6 x 10(21) cm(-2)), and does not introduce any significant curvature in the Fe K band. We are able to place a strong constraint on the presence of a broadened Fe K alpha line (E-rest = 6.46(-0.07)(+0.08) keV with sigma = 0.33(-0.07)(+0.08) keV and EW = 34(-7)(+8) eV), though we are not able to constrain any of the parameters of a relativistic reflection model. These results highlight the range in broad Fe K line strengths observed in nearby, bright, active galactic nuclei (roughly an order of magnitude), and imply a corresponding range in the physical properties of the inner accretion disk in these sources. We have also updated our previously reported measurement of the high-energy cutoff of the hard X-ray emission using both observatories rather than just NuSTAR alone: E-cut = 186 +/- 14 keV. This high-energy cutoff acts as a proxy for the temperature of the coronal electron plasma, enabling us to further separate this parameter from the plasma's optical depth and to update our results for these parameters as well. We derive kT = 50(-3)(+6) keV with tau = 2.34(-0.11)(+0.16) using a spherical geometry, kT = 61 +/- 1 keV with tau = 0.68 +/- 0.02 for a slab geometry, with both having an equivalent goodness-of-fit. C1 [Brenneman, L. W.; Elvis, M.] Harvard Smithsonian CfA, Cambridge, MA 02138 USA. [Madejski, G.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Fuerst, F.; Harrison, F. A.; Grefenstette, B. W.; Madsen, K. K.; Rivers, E.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Matt, G.; Marinucci, A.] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Ballantyne, D. R.] Georgia Inst Technol, Ctr Relativist Astrophys, Sch Phys, Atlanta, GA 30332 USA. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Brenneman, LW (reprint author), Harvard Smithsonian CfA, 60 Garden St,MS-67, Cambridge, MA 02138 USA. RI Boggs, Steven/E-4170-2015; XRAY, SUZAKU/A-1808-2009 OI Boggs, Steven/0000-0001-9567-4224; FU NASA [NNG08FD60C, NNX13AE90G]; National Aeronautics and Space Administration; Italian Space Agency [ASI/INAF I/037/12/0-011/13] FX This work was supported under NASA Contract No. NNG08FD60C and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). L.B. thanks Koji Mukai and the Suzaku GOF at NASA/GSFC for all their assistance in obtaining and analyzing that data, and also gratefully acknowledges funding from NASA grant NNX13AE90G. G.Matt and A.M. acknowledge financial support from Italian Space Agency under contract ASI/INAF I/037/12/0-011/13. NR 65 TC 29 Z9 29 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 JUN 10 PY 2014 VL 788 IS 1 AR 61 DI 10.1088/0004-637X/788/1/61 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200061 ER PT J AU Fukuda, T Yoshiike, S Sano, H Torii, K Yamamoto, H Acero, F Fukui, Y AF Fukuda, T. Yoshiike, S. Sano, H. Torii, K. Yamamoto, H. Acero, F. Fukui, Y. TI INTERSTELLAR PROTONS IN THE TeV gamma-RAY SNR HESS J1731-347: POSSIBLE EVIDENCE FOR THE COEXISTENCE OF HADRONIC AND LEPTONIC gamma-RAYS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; gamma rays: ISM; H II regions; ISM: clouds; ISM: individual objects (HESS J1731-347) ID REMNANT RX J1713.7-3946; YOUNG SUPERNOVA-REMNANTS; LARGE-SCALE MORPHOLOGY; GALACTIC PLANE SURVEY; LARGE-AREA TELESCOPE; 3 KPC ARM; COSMIC-RAY; ATOMIC-HYDROGEN; GAS-DYNAMICS; EMISSION AB HESS J1731-347 (G353.6-0.7) is one of the TeV. -ray supernova remnants (SNRs) that shows the shell-like morphology. We have made a new analysis of the interstellar protons toward the SNR by using both the 12CO(J = 1-0) and Hi data sets. The results indicate that the TeV gamma-ray shell shows significant spatial correlation with the interstellar protons at a velocity range from -90 km s-1 to -75 km s-1. The total mass of the interstellar medium (ISM) protons is estimated to be 6.4 x104 M-circle dot, 25% of which is atomic gas, and the distance corresponding to the velocity range is similar to 5.2 kpc, a factor of 2 larger than the previous figure, 3 kpc. We have identified the cold Hi gas observed as self-absorption which shows significant correspondence with the northeastern gamma-ray peak. While the good correspondence between the ISM protons and TeV gamma-rays in the north of the SNR lends support to the hadronic scenario for the TeV gamma-rays, the southern part of the shell shows a break in the correspondence; in particular, the southwestern rim of the SNR shell shows a significant decrease of the interstellar protons by a factor of two. We argue that this discrepancy can be explained due to leptonic gamma-rays because this region coincides well with the bright shell that emits non-thermal radio continuum emission and non-thermal X-rays, suggesting that the gamma-rays of HESS J1713-347 consist of both the hadronic and leptonic components. The leptonic contribution corresponds to similar to 20% of the total gamma-rays. C1 [Fukuda, T.; Yoshiike, S.; Sano, H.; Torii, K.; Yamamoto, H.; Fukui, Y.] Nagoya Univ, Dept Phys, Chikusa Ku, Nagoya, Aichi 4648601, Japan. [Acero, F.] NASA, Goddard Space Flight Ctr, ORAU, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Fukuda, T (reprint author), Nagoya Univ, Dept Phys, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648601, Japan. EM tfukuda@a.phys.nagoya-u.ac.jp FU (KAKENHI) MEXT (the Ministry of Education, Culture, Sports, Science, and Technology of Japan) [15071203, 21253003, 20244014, 23403001, 22540250, 22244014, 23740149-01, 22740119] FX NANTEN2 is an international collaboration of 10 universities: Nagoya University, Osaka Prefecture University, University of Cologne, University of Bonn, Seoul National University, University of Chile, University of New South Wales, Macquarie University, University of Sydney, and University of ETH Zurich. Thiswork is financially supported by a grant-in-aid for Scientific Research (KAKENHI, Nos. 15071203, 21253003, 20244014, 23403001, 22540250, 22244014, 23740149-01, and 22740119) from MEXT (the Ministry of Education, Culture, Sports, Science, and Technology of Japan). This work is also financially supported by the Young Research Overseas Visits Program for Vitalizing Brain Circulation (R2211) and the Institutional Program for Young Researcher Overseas Visits (R29) by the Japan Society for the Promotion of Science (JSPS), as well as the JSPS core-to-core program (No. 17004). We also acknowledge the support of the Mitsubishi Foundation and the Sumitomo Foundation. This research was supported by the grant-in-aid for Nagoya University Global COE Program, gQuest for Fundamental Principles in the Universe: From Particles to the Solar System and the Cosmos fromMEXT. The satellite Internet connection forNANTEN2was provided by theAustralian Research Council. NR 45 TC 7 Z9 7 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2014 VL 788 IS 1 AR 94 DI 10.1088/0004-637X/788/1/94 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200094 ER PT J AU Lang, P Wuyts, S Somerville, RS Schreiber, NMF Genzel, R Bell, EF Brammer, G Dekel, A Faber, SM Ferguson, HC Grogin, NA Kocevski, DD Koekemoer, AM Lutz, D McGrath, EJ Momcheva, I Nelson, EJ Primack, JR Rosario, DJ Skelton, RE Tacconi, LJ van Dokkum, PG Whitaker, KE AF Lang, Philipp Wuyts, Stijn Somerville, Rachel S. Schreiber, Natascha M. Foerster Genzel, Reinhard Bell, Eric F. Brammer, Gabe Dekel, Avishai Faber, Sandra M. Ferguson, Henry C. Grogin, Norman A. Kocevski, Dale D. Koekemoer, Anton M. Lutz, Dieter McGrath, Elizabeth J. Momcheva, Ivelina Nelson, Erica J. Primack, Joel R. Rosario, David J. Skelton, Rosalind E. Tacconi, Linda J. van Dokkum, Pieter G. Whitaker, Katherine E. TI BULGE GROWTH AND QUENCHING SINCE z=2.5 IN CANDELS/3D-HST SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; galaxies: stellar content; galaxies: structure ID STAR-FORMING GALAXIES; SIMILAR-TO 2; HUBBLE-SPACE-TELESCOPE; ACTIVE GALACTIC NUCLEI; CLUSTER ELLIPTIC GALAXIES; DIGITAL SKY SURVEY; PASSIVELY EVOLVING GALAXIES; EXTRAGALACTIC LEGACY SURVEY; COMPACT QUIESCENT GALAXIES; KILOPARSEC-SCALE CLUMPS AB Exploiting the deep high- resolution imaging of all five CANDELS fields, and accurate redshift information provided by 3D- HST, we investigate the relation between structure and stellar populations for a mass- selected sample of 6764 galaxies above 1010 M, spanning the redshift range 0.5 < z < 2.5. For the first time, we fit two- dimensional models comprising a single S ' ersic fit and two- component ( i. e., bulge + disk) decompositions not only to the H- band light distributions, but also to the stellar mass maps reconstructed from resolved stellar population modeling. We confirm that the increased bulge prominence among quiescent galaxies, as reported previously based on rest- optical observations, remains in place when considering the distributions of stellar mass. Moreover, we observe an increase of the typical S ' ersic index and bulge- to- total ratio ( with median B/ T reaching 40%- 50%) among star- forming galaxies above 1011 M. Given that quenching for these most massive systems is likely to be imminent, our findings suggest that significant bulge growth precedes a departure from the star- forming main sequence. We demonstrate that the bulge mass ( and ideally knowledge of the bulge and total mass) is a more reliable predictor of the star- forming versus quiescent state of a galaxy than the total stellar mass. The same trends are predicted by the state- of- the- art, semi- analytic model by Somerville et al. In this model, bulges and black holes grow hand in hand through merging and/ or disk instabilities, and feedback from active galactic nuclei shuts off star formation. Further observations will be required to pin down star formation quenching mechanisms, but our results imply that they must be internal to the galaxies and closely associated with bulge growth. C1 [Lang, Philipp; Wuyts, Stijn; Schreiber, Natascha M. Foerster; Genzel, Reinhard; Lutz, Dieter; Rosario, David J.; Tacconi, Linda J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Somerville, Rachel S.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Brammer, Gabe] European So Observ, Santiago, Chile. [Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, Ctr Astrophys & Planetary Sci, IL-91904 Jerusalem, Israel. [Faber, Sandra M.; Momcheva, Ivelina] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Ferguson, Henry C.; Grogin, Norman A.; Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kocevski, Dale D.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [McGrath, Elizabeth J.] Colby Coll, Dept Phys & Astron, Waterville, ME 04901 USA. [Nelson, Erica J.; van Dokkum, Pieter G.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Primack, Joel R.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Skelton, Rosalind E.] S African Astron Observ, ZA-7925 Cape Town, South Africa. [Whitaker, Katherine E.] Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Lang, P (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. RI Skelton, Rosalind/S-1845-2016; OI Skelton, Rosalind/0000-0001-7393-3336; Koekemoer, Anton/0000-0002-6610-2048; Bell, Eric/0000-0002-5564-9873 FU NASA through the Space Telescope Science Institute [HST-GO-12060, HST-GO-12177]; Association of Universities for Research in Astronomy, Incorporated, under NASA [NAS5-26555] FX The authors acknowledge fruitful discussions with Edmond Cheung, David C. Koo, Yu Lu, Casey J. Papovich, Mohammadtaher Safarzadeh, Benjamin J. Weiner, and Steven P. Willner. Support for Program number HST-GO-12060 and HST-GO-12177 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. NR 114 TC 68 Z9 69 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 JUN 10 PY 2014 VL 788 IS 1 AR 11 DI 10.1088/0004-637X/788/1/11 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200011 ER PT J AU Merlo, MJ Perlman, ES Nikutta, R Packham, C Elitzur, M Imanishi, M Levenson, NA Radomski, JT Aretxaga, I AF Merlo, Matthew J. Perlman, Eric S. Nikutta, Robert Packham, Christopher Elitzur, Moshe Imanishi, Masatoshi Levenson, N. A. Radomski, James T. Aretxaga, Itziar TI SUBARU SPECTROSCOPY AND SPECTRAL MODELING OF CYGNUS A SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (Cygnus A); infrared : galaxies ID ACTIVE GALACTIC NUCLEI; OBSCURING DUST TORI; SEYFERT-GALAXIES; MIDINFRARED EMISSION; INFRARED-EMISSION; CIRCINUS GALAXY; RADIO GALAXIES; IRRADIANCE CALIBRATION; SILICATE FEATURES; VLBI OBSERVATIONS AB We present high angular resolution (similar to 0 ''.5) MIR spectra of the powerful radio galaxy, Cygnus A (Cyg A), obtained with the Subaru telescope. The overall shape of the spectra agree with previous high angular resolution MIR observations, as well as previous Spitzer spectra. Our spectra, both on and off nucleus, show a deep silicate absorption feature. The absorption feature can be modeled with a blackbody obscured by cold dust or a clumpy torus. The deep silicate feature is best fit by a simple model of a screened blackbody, suggesting that foreground absorption plays a significant, if not dominant, role in shaping the spectrum of Cyg A. This foreground absorption prevents a clear view of the central engine and surrounding torus, making it difficult to quantify the extent the torus attributes to the obscuration of the central engine, but does not eliminate the need for a torus in Cyg A. C1 [Merlo, Matthew J.; Perlman, Eric S.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Nikutta, Robert] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [Nikutta, Robert; Elitzur, Moshe] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. [Packham, Christopher] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX 78249 USA. [Imanishi, Masatoshi] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Levenson, N. A.] Gemini Observ, La Serena, Chile. [Radomski, James T.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. [Aretxaga, Itziar] Inst Nacl Astrofis Opt & Electr, Puebla, Mexico. RP Merlo, MJ (reprint author), Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. OI Levenson, Nancy A./0000-0003-4209-639X FU NSF [AST-0904890, AST-0904421, AST-0904316] FX Based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. M.J.M. and E.S.P acknowledge support from NSF grant AST-0904890. C.P. acknowledges support from NFS grant AST-0904421. M.E. acknowledges support from NFS grant AST-0904316. We are pleased to acknowledge the helpful discussions with members of the Los Piratas, especially Rachel Mason and Enrique Lopez Rodriguez for intensive help with data reduction. NR 70 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 JUN 10 PY 2014 VL 788 IS 1 AR 6 DI 10.1088/0004-637X/788/1/6 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200006 ER PT J AU Miller, JM Raymond, J Kallman, TR Maitra, D Fabian, AC Proga, D Reynolds, CS Reynolds, MT Degenaar, N King, AL Cackett, EM Kennea, JA Beardmore, A AF Miller, J. M. Raymond, J. Kallman, T. R. Maitra, D. Fabian, A. C. Proga, D. Reynolds, C. S. Reynolds, M. T. Degenaar, N. King, A. L. Cackett, E. M. Kennea, J. A. Beardmore, A. TI CHANDRA SPECTROSCOPY OF MAXI J1305-704: DETECTION OF AN INFALLING BLACK HOLE DISK WIND? SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics ID X-RAY BINARIES; LY-ALPHA LINE; ACCRETION DISK; INTERSTELLAR-MEDIUM; GRO J1655-40; ABSORPTION; RADIATION; DRIVEN; JETS; SUPPRESSION AB We report on a high-resolution Chandra/HETG X-ray spectrum of the transient X-ray binary MAXI J1305-704. A rich absorption complex is detected in the Fe L band, including density-sensitive lines from Fe XX, Fe XXI, and Fe XXII. Spectral analysis over three wavelength bands with a large grid of XSTAR photoionization models generally requires a gas density of n >= 10(17) cm(-3). Assuming a luminosity of L = 10(37) erg s(-1), fits to the 10-14 angstrom band constrain the absorbing gas to lie within r = (3.9 +/- 0.7) x 10(3) km from the central engine, or about r = 520 +/- 90 (M/5M(circle dot)) r(g), where r(g) = GM/c(2). At this small distance from the compact object, gas in stable orbits should have a gravitational redshift of z = v/c similar or equal to (3 +/- 1) x 10(-3) (M/5M(circle dot)), and any tenuous inflowing gas should have a free-fall velocity of v/c similar or equal to (6 +/- 1) x 10(-2) (M/5M(circle dot))(1/2). The best-fit single-zone photoionization models measure a redshift of v/c = (2.6-3.2) x 10(-3.) Models with two absorbing zones provide significantly improved fits, and the additional zone is measured to have a redshift of v/c = (4.6-4.9) x 10(-2) (models including two zones suggest slightly different radii and may point to lower densities). Thus, the observed shifts are broadly consistent with those expected at the photoionization radius. The absorption spectrum revealed in MAXI J1305-704 may be best explained in terms of a "failed wind" like those predicted in some recent numerical simulations of black hole accretion flows. The robustness of the velocity shifts was explored through detailed simulations with the Chandra/MARX ray-tracing package and analysis of the zeroth-order ACIS-S3 spectrum. These tests are particularly important given the anomalously large angle between the source and the optical axis in this observation. The simulations and ACIS spectrum suggest that the shifts are not instrumental; however, strong caution is warranted. We discuss our results in the context of accretion flows in stellar-mass black holes and active galactic nuclei, as well as the potential role of failed winds in emerging connections between disk outflows and black hole state transitions. C1 [Miller, J. M.; Maitra, D.; Reynolds, M. T.; Degenaar, N.; King, A. L.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Raymond, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greedbelt, MD 20771 USA. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. [Proga, D.] Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Cackett, E. M.] Wayne State Univ, Dept Phys & Astron, Detroit, MI 48201 USA. [Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Beardmore, A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Miller, JM (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM jonmm@umich.edu FU Chandra Guest Observer Program; Swift; NASA through Hubble Postdoctoral Fellowship grant from the Space Telescope Science Institute [HST-HF-51287.01-A]; Swift at the University of Leicester; UK Space Agency FX We gratefully acknowledge comments from the anonymous referee that improved the clarity and content of this paper. We thank Harvey Tananbaum and Chandra for executing this observation. We are indebted to Mateusz Ruszkowski for lending computing cluster clock cycles to this project. We acknowledge Mike Nowak, David Huenemoerder, John Davis, John Houck, Norbert Schulz, and Jonathan McDowell for helpful discussions. J.M.M. gratefully acknowledges support from the Chandra Guest Observer Program and Swift. N.D. is supported by NASA through Hubble Postdoctoral Fellowship grant number HST-HF-51287.01-A from the Space Telescope Science Institute. A.P.B. acknowledges funding for Swift at the University of Leicester by the UK Space Agency. NR 57 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 JUN 10 PY 2014 VL 788 IS 1 AR 53 DI 10.1088/0004-637X/788/1/53 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200053 ER PT J AU Price, SH Kriek, M Brammer, GB Conroy, C Schreiber, NMF Franx, M Fumagalli, M Lundgren, B Momcheva, I Nelson, EJ Skelton, RE van Dokkum, PG Whitaker, KE Wuyts, S AF Price, Sedona H. Kriek, Mariska Brammer, Gabriel B. Conroy, Charlie Schreiber, Natascha M. Foerster Franx, Marijn Fumagalli, Mattia Lundgren, Britt Momcheva, Ivelina Nelson, Erica J. Skelton, Rosalind E. van Dokkum, Pieter G. Whitaker, Katherine E. Wuyts, Stijn TI DIRECT MEASUREMENTS OF DUST ATTENUATION IN z similar to 1.5 STAR-FORMING GALAXIES FROM 3D-HST: IMPLICATIONS FOR DUST GEOMETRY AND STAR FORMATION RATES SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies : evolution; galaxies : high-redshift ID MASS-METALLICITY RELATION; ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT GALAXIES; HUBBLE-SPACE-TELESCOPE; SPECTRAL ENERGY-DISTRIBUTIONS; AEGIS FIELD GALAXIES; LYMAN-BREAK GALAXIES; DIGITAL SKY SURVEY; AGN HOST GALAXIES; GREATER-THAN 1 AB The nature of dust in distant galaxies is not well understood, and until recently few direct dust measurements have been possible. We investigate dust in distant star-forming galaxies using near-infrared grism spectra of the 3D-HST survey combined with archival multi-wavelength photometry. These data allow us to make a direct comparison between dust around star-forming regions (A(V,) (HII)) and the integrated dust content (A(V, star)). We select a sample of 163 galaxies between 1.36 <= z <= 1.5 with Ha signal-to-noise ratio >= 5 and measure Balmer decrements from stacked spectra to calculate AV, Hii. First, we stack spectra in bins of A(V, star), and find that A(V, HII) = 1.86A(V,) (star), with a significance of sigma = 1.7. Our result is consistent with the two-component dust model, in which galaxies contain both diffuse and stellar birth cloud dust. Next, we stack spectra in bins of specific star formation rate (log SSFR), star formation rate (log SFR), and stellar mass (log M-*). We find that on average A(V,) (HII) increases with SFR and mass, but decreases with increasing SSFR. Interestingly, the data hint that the amount of extra attenuation decreases with increasing SSFR. This trend is expected from the two-component model, as the extra attenuation will increase once older stars outside the star-forming regions become more dominant in the galaxy spectrum. Finally, using Balmer decrements we derive dust-corrected H alpha SFRs, and find that stellar population modeling produces incorrect SFRs if rapidly declining star formation histories are included in the explored parameter space. C1 [Price, Sedona H.; Kriek, Mariska] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Brammer, Gabriel B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Conroy, Charlie] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Schreiber, Natascha M. Foerster; Wuyts, Stijn] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Franx, Marijn; Fumagalli, Mattia] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Lundgren, Britt] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Momcheva, Ivelina; Nelson, Erica J.; van Dokkum, Pieter G.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Skelton, Rosalind E.] S African Astron Observ, ZA-7935 Observatory, South Africa. [Whitaker, Katherine E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. RP Price, SH (reprint author), Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. EM sedona@berkeley.edu RI Skelton, Rosalind/S-1845-2016; OI Skelton, Rosalind/0000-0001-7393-3336; Price, Sedona/0000-0002-0108-4176 FU National Science Foundation Graduate Research Fellowship [DGE 1106400]; 3D-HST Treasury Program - NASA/ESA HST [GO 12177, 12328]; Association of Universities for Research in Astronomy, Inc., under NASA [NAS5-26555]; STScI [12117.21- A] FX We thank Edward Taylor and Nick Hand for useful discussions, and David Sobral and Daichi Kashino for sharing data for comparison. We thank the anonymous referee for constructive comments, which have improved this paper. 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. We acknowledge support from STScI grant 12117.21- A. S.P. is funded by the National Science Foundation Graduate Research Fellowship under grant No. DGE 1106400. NR 92 TC 52 Z9 52 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 JUN 10 PY 2014 VL 788 IS 1 AR 86 DI 10.1088/0004-637X/788/1/86 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200086 ER PT J AU Shporer, A O'Rourke, JG Knutson, HA Szabo, GM Zhao, M Burrows, A Fortney, J Agol, E Cowan, NB Desert, JM Howard, AW Isaacson, H Lewis, NK Showman, AP Todorov, KO AF Shporer, Avi O'Rourke, Joseph G. Knutson, Heather A. Szabo, Gyula M. Zhao, Ming Burrows, Adam Fortney, Jonathan Agol, Eric Cowan, Nicolas B. Desert, Jean-Michel Howard, Andrew W. Isaacson, Howard Lewis, Nikole K. Showman, Adam P. Todorov, Kamen O. TI ATMOSPHERIC CHARACTERIZATION OF THE HOT JUPITER KEPLER-13Ab SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: early-type; stars: individual (Kepler-13 BD+46 2629); techniques: photometric; techniques: spectroscopic ID PLANET HD 189733B; LIGHT CURVES; THERMAL EMISSION; SOPHIE VELOCIMETRY; EXTRASOLAR PLANETS; WARM-SPITZER; ELLIPSOIDAL VARIATIONS; TRANSITING COMPANION; HEAT REDISTRIBUTION; STELLAR ACTIVITY AB Kepler-13Ab (= KOI-13.01) is a unique transiting hot Jupiter. It is one of very few known short-period planets orbiting a hot A-type star, making it one of the hottest planets currently known. The availability of Kepler data allows us to measure the planet's occultation (secondary eclipse) and phase curve in the optical, which we combine with occultations observed by warm Spitzer at 4.5 mu m and 3.6 mu m and a ground-based occultation observation in the K-s band (2.1 mu m). We derive a day-side hemisphere temperature of 2750 +/- 160 K as the effective temperature of a black body showing the same occultation depths. Comparing the occultation depths with one-dimensional planetary atmosphere models suggests the presence of an atmospheric temperature inversion. Our analysis shows evidence for a relatively high geometric albedo, A(g) = 0.33(-0.06)(+0.04). While measured with a simplistic method, a high A(g) is supported also by the fact that the one-dimensional atmosphere models underestimate the occultation depth in the optical. We use stellar spectra to determine the dilution, in the four wide bands where occultation was measured, due to the visual stellar binary companion 1.'' 15 +/- 0.'' 05 away. The revised stellar parameters measured using these spectra are combined with other measurements, leading to revised planetary mass and radius estimates of M-p = 4.94-8.09 M-J and R-p = 1.406 +/- 0.038 R-J. Finally, we measure a Kepler midoccultation time that is 34.0 +/- 6.9 s earlier than expected based on the midtransit time and the delay due to light-travel time and discuss possible scenarios. C1 [Shporer, Avi; O'Rourke, Joseph G.; Knutson, Heather A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Shporer, Avi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Szabo, Gyula M.] ELTE Gothard Astrophys Observ, H-9704 Szombathely, Hungary. [Szabo, Gyula M.] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, H-1121 Budapest, Hungary. [Szabo, Gyula M.] Gothard Lendulet Res Team, H-9704 Szombathely, Hungary. [Zhao, Ming] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Fortney, Jonathan] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Cowan, Nicolas B.] Northwestern Univ, Ctr Interdisciplinary Explorat & Res Astrophys, Evanston, IL 60208 USA. [Cowan, Nicolas B.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Desert, Jean-Michel] Univ Colorado, CASA, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Isaacson, Howard] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Lewis, Nikole K.; Showman, Adam P.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Lewis, Nikole K.; Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Todorov, Kamen O.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Shporer, Avi] ETH, Inst Astron, CH-8093 Zurich, Switzerland. RP Shporer, A (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Todorov, Kamen/0000-0002-9276-8118; O'Rourke, Joseph/0000-0002-1180-996X; /0000-0002-0802-9145 FU NASA; National Science Foundation FX A. S. thanks Ehud Nakar and Jason Eastman for enlightening discussions. This work was performed in part at the Jet Propulsion Laboratory, under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. J. G. O. receives support from the National Science Foundation's Graduate Research Fellowship Program. Gy.M.Sz. was supported by the Hungarian OTKAgrants 104607 and 83790, the HUMAN MB08C 81013 grant of the MAG Zrt, and the Janos Bolyai Research Fellowship and a Lendulet-2009 grant of the Hungarian Academy of Sciences. M. Z. is supported by the Center for Exoplanets and Habitable Worlds (CEHW) at the Pennsylvania State University. The Palomar/WIRC observation was in part supported by NASA through the American Astronomical Society's Small Research Grant program. This research has made use of NASA's Astrophysics Data System Service. This work is based on observations made by the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. The Palomar 200 inch (5 m) Hale Telescope (P200) is operated by Caltech, JPL, and Cornell University. Kepler was competitively selected as the tenth NASA Discovery mission. Funding for this mission is provided by the NASA Science Mission Directorate. Some of the data presented herein were obtained at theW. 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 Keck Observatory was made possible by the generous financial support of the W. M. Keck Foundation. NR 108 TC 27 Z9 27 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2014 VL 788 IS 1 AR 92 DI 10.1088/0004-637X/788/1/92 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200092 ER PT J AU Usmanov, AV Goldstein, ML Matthaeus, WH AF Usmanov, Arcadi V. Goldstein, Melvyn L. Matthaeus, William H. TI THREE-FLUID, THREE-DIMENSIONAL MAGNETOHYDRODYNAMIC SOLAR WIND MODEL WITH EDDY VISCOSITY AND TURBULENT RESISTIVITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic fields; magnetohydrodynamics (MHD); methods : numerical; solar wind; turbulence ID INTERSTELLAR PICKUP PROTONS; PRESSURE-BALANCED STRUCTURES; ELECTRON-IMPACT IONIZATION; ALFVEN WAVES; OUTER HELIOSPHERE; 2-FLUID MODEL; TERMINATION SHOCK; DISTANT HELIOSPHERE; COROTATING STREAMS; NEUTRAL HYDROGEN AB We have developed a three-fluid, three-dimensional magnetohydrodynamic solar wind model that incorporates turbulence transport, eddy viscosity, turbulent resistivity, and turbulent heating. The solar wind plasma is described as a system of co-moving solar wind protons, electrons, and interstellar pickup protons, with separate energy equations for each species. Numerical steady-state solutions of Reynolds-averaged solar wind equations coupled with turbulence transport equations for turbulence energy, cross helicity, and correlation length are obtained by the time relaxation method in the corotating with the Sun frame of reference in the region from 0.3 to 100 AU (but still inside the termination shock). The model equations include the effects of electron heat conduction, Coulomb collisions, photoionization of interstellar hydrogen atoms and their charge exchange with the solar wind protons, turbulence energy generation by pickup protons, and turbulent heating of solar wind protons and electrons. The turbulence transport model is based on the Reynolds decomposition and turbulence phenomenologies that describe the conversion of fluctuation energy into heat due to a turbulent cascade. In addition to using separate energy equations for the solar wind protons and electrons, a significant improvement over our previous work is that the turbulence model now uses an eddy viscosity approximation for the Reynolds stress tensor and the mean turbulent electric field. The approximation allows the turbulence model to account for driving of turbulence by large-scale velocity gradients. Using either a dipole approximation for the solar magnetic field or synoptic solar magnetograms from the Wilcox Solar Observatory for assigning boundary conditions at the coronal base, we apply the model to study the global structure of the solar wind and its three-dimensional properties, including embedded turbulence, heating, and acceleration throughout the heliosphere. The model results are compared with plasma and magnetic field observations on WIND, Ulysses, and Voyager 2 spacecraft. C1 [Usmanov, Arcadi V.; Matthaeus, William H.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Usmanov, Arcadi V.; Goldstein, Melvyn L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Usmanov, AV (reprint author), Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. EM arcadi.usmanov@nasa.gov FU NSF [AST-1004035]; NASA [NNX09AH79G, NNX13AR42G]; NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at the Ames Research Center [SMD-123050, SMD-13-4027]; NASA Center for Climate Simulation (NCCS) at the Goddard Space Flight Center FX The authors are indebted to Sean Oughton for his results used in Appendix B. We also gratefully acknowledge Nobumitsu Yokoi and Robert Rubinstein for valuable discussions. The spacecraft data used in this study were obtained from the NASA/GSFC's Space Physics Data Facility's OMNIWeb service at http://omniweb.gsfc.nasa.gov.John M. Wilcox Solar Observatory data used in this study were obtained via the web site http://wso.stanford.edu courtesy of J. T. Hoeksema. The work of A.V.U. was supported by NSF grant AST-1004035 and NASA grants NNX09AH79G and NNX13AR42G to the University of Delaware. Supercomputer time allocations were provided by the NASA High-End Computing (HEC) Program awards SMD-123050 and SMD-13-4027 through the NASA Advanced Supercomputing (NAS) Division at the Ames Research Center and the NASA Center for Climate Simulation (NCCS) at the Goddard Space Flight Center. NR 98 TC 14 Z9 14 U1 1 U2 9 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 JUN 10 PY 2014 VL 788 IS 1 AR 43 DI 10.1088/0004-637X/788/1/43 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200043 ER PT J AU van der Wel, A Franx, M van Dokkum, PG Skelton, RE Momcheva, IG Whitaker, KE Brammer, GB Bell, EF Rix, HW Wuyts, S Ferguson, HC Holden, BP Barro, G Koekemoer, AM Chang, YY McGrath, EJ Haussler, B Dekel, A Behroozi, P Fumagalli, M Leja, J Lundgren, BF Maseda, MV Nelson, EJ Wake, DA Patel, SG Labbe, I Faber, SM Grogin, NA Kocevski, DD AF van der Wel, A. Franx, M. van Dokkum, P. G. Skelton, R. E. Momcheva, I. G. Whitaker, K. E. Brammer, G. B. Bell, E. F. Rix, H. -W. Wuyts, S. Ferguson, H. C. Holden, B. P. Barro, G. Koekemoer, A. M. Chang, Yu-Yen McGrath, E. J. Haeussler, B. Dekel, A. Behroozi, P. Fumagalli, M. Leja, J. Lundgren, B. F. Maseda, M. V. Nelson, E. J. Wake, D. A. Patel, S. G. Labbe, I. Faber, S. M. Grogin, N. A. Kocevski, D. D. TI 3D-HST+CANDELS: THE EVOLUTION OF THE GALAXY SIZE-MASS DISTRIBUTION SINCE z=3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : evolution; galaxies : fundamental parameters; galaxies : high-redshift; galaxies : structure ID SIMILAR-TO 2; HUBBLE-SPACE-TELESCOPE; COMPACT QUIESCENT GALAXIES; ULTRA-DEEP-FIELD; HIGH-REDSHIFT GALAXIES; STAR-FORMING GALAXIES; GREATER-THAN 1; VELOCITY-DISPERSION EVOLUTION; PASSIVELY EVOLVING GALAXIES; EXTRAGALACTIC LEGACY SURVEY AB Spectroscopic + photometric redshifts, stellar mass estimates, and rest-frame colors from the 3D-HST survey are combined with structural parameter measurements from CANDELS imaging to determine the galaxy size-mass distribution over the redshift range 0 < z < 3. Separating early-and late-type galaxies on the basis of star-formation activity, we confirm that early-type galaxies are on average smaller than late-type galaxies at all redshifts, and we find a significantly different rate of average size evolution at fixed galaxy mass, with fast evolution for the early-type population, R-eff proportional to (1 + z)(-1.48), and moderate evolution for the late-type population, R-eff proportional to (1 + z)(-0.75). The large sample size and dynamic range in both galaxy mass and redshift, in combination with the high fidelity of our measurements due to the extensive use of spectroscopic data, not only fortify previous results but also enable us to probe beyond simple average galaxy size measurements. At all redshifts the slope of the size-mass relation is shallow, R-eff proportional to M-*(0.22) , for late-type galaxies with stellar mass >3 x 10(9) M-circle dot, and steep, R-eff proportional to M-*(0.75), for early-type galaxies with stellar mass >2 x 10(10) M-circle dot. The intrinsic scatter is less than or similar to 0.2 dex for all galaxy types and redshifts. For late-type galaxies, the logarithmic size distribution is not symmetric but is skewed toward small sizes: at all redshifts and masses, a tail of small late-type galaxies exists that overlaps in size with the early-type galaxy population. The number density of massive (similar to 10(11)M(circle dot)), compact (R-eff < 2 kpc) early-type galaxies increases from z = 3 to z 1.5-2 and then strongly decreases at later cosmic times. C1 [van der Wel, A.; Rix, H. -W.; Chang, Yu-Yen; Maseda, M. V.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Franx, M.; Fumagalli, M.; Labbe, I.] Leiden Univ, Leiden Observ, NL-2300 AA Leiden, Netherlands. [van Dokkum, P. G.; Momcheva, I. G.; Leja, J.; Nelson, E. J.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Skelton, R. E.] S African Astron Observ, ZA-7935 Observatory, South Africa. [Whitaker, K. E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Brammer, G. B.; Ferguson, H. C.; Koekemoer, A. M.; Behroozi, P.; Grogin, N. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Bell, E. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Wuyts, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Holden, B. P.; Barro, G.; Faber, S. M.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [McGrath, E. J.] Colby Coll, Dept Phys & Astron, Waterville, ME USA. [Haeussler, B.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Haeussler, B.] Univ Hertfordshire, Ctr Astrophys, Hatfield AL10 9AB, Herts, England. [Haeussler, B.] Univ Hertfordshire, Technol Res Inst, Hatfield AL10 9AB, Herts, England. [Dekel, A.] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Lundgren, B. F.; Wake, D. A.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Wake, D. A.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Patel, S. G.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Kocevski, D. D.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. RP van der Wel, A (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM vdwel@mpia.de RI Skelton, Rosalind/S-1845-2016; OI Skelton, Rosalind/0000-0001-7393-3336; Leja, Joel/0000-0001-6755-1315; Koekemoer, Anton/0000-0002-6610-2048; Bell, Eric/0000-0002-5564-9873 NR 126 TC 171 Z9 171 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 JUN 10 PY 2014 VL 788 IS 1 AR 28 DI 10.1088/0004-637X/788/1/28 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200028 ER PT J AU Walton, DJ Risaliti, G Harrison, FA Fabian, AC Miller, JM Arevalo, P Ballantyne, DR Boggs, SE Brenneman, LW Christensen, FE Craig, WW Elvis, M Fuerst, F Gandhi, P Grefenstette, BW Hailey, CJ Kara, E Luo, B Madsen, KK Marinucci, A Matt, G Parker, ML Reynolds, CS Rivers, E Ross, RR Stern, D Zhang, WW AF Walton, D. J. Risaliti, G. Harrison, F. A. Fabian, A. C. Miller, J. M. Arevalo, P. Ballantyne, D. R. Boggs, S. E. Brenneman, L. W. Christensen, F. E. Craig, W. W. Elvis, M. Fuerst, F. Gandhi, P. Grefenstette, B. W. Hailey, C. J. Kara, E. Luo, B. Madsen, K. K. Marinucci, A. Matt, G. Parker, M. L. Reynolds, C. S. Rivers, E. Ross, R. R. Stern, D. Zhang, W. W. TI NuSTAR AND XMM-NEWTON OBSERVATIONS OF NGC 1365: EXTREME ABSORPTION VARIABILITY AND A CONSTANT INNER ACCRETION DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies : active; X-rays : individual (NGC 1365) ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE SPIN; X-RAY REVERBERATION; GALAXY SWIFT J2127.4+5654; PHOTON IMAGING CAMERA; SPECTRAL VARIABILITY; IRON-K; SEYFERT-GALAXIES; BEPPOSAX OBSERVATIONS; COMPTON REFLECTION AB We present a spectral analysis of four coordinated NuSTAR+ XMM-Newton observations of the Seyfert galaxy NGC 1365. These exhibit an extreme level of spectral variability, which is primarily due to variable line-of-sight absorption, revealing relatively unobscured states in this source for the first time. Despite the diverse range of absorption states, each of the observations displays the same characteristic signatures of relativistic reflection from the inner accretion disk. Through time-resolved spectroscopy, we find that the strength of the relativistic iron line and the Compton reflection hump relative to the intrinsic continuum are well correlated, which is expected if they are two aspects of the same broadband reflection spectrum. We apply self-consistent disk reflection models to these time-resolved spectra in order to constrain the inner disk parameters, allowing for variable, partially covering absorption to account for the vastly different absorption states that were observed. Each of the four observations is treated independently to test the consistency of the results obtained for the black hole spin and the disk inclination, which should not vary on observable timescales. We find both the spin and the inclination determined from the reflection spectrum to be consistent, confirming that NGC 1365 hosts a rapidly rotating black hole; in all cases the dimensionless spin parameter is constrained to be a* > 0.97 (at 90% statistical confidence or better). C1 [Walton, D. J.; Harrison, F. A.; Fuerst, F.; Grefenstette, B. W.; Madsen, K. K.; Rivers, E.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Risaliti, G.] INAF, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Risaliti, G.; Brenneman, L. W.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fabian, A. C.; Elvis, M.; Parker, M. L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Arevalo, P.] Pontificia Univ Catolica Chile, Inst Astrfis, Santiago 22, Chile. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Gandhi, P.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Luo, B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Marinucci, A.; Matt, G.] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Reynolds, C. S.] Univ Maryland, Joint Space Sci Inst JSI, College Pk, MD 20742 USA. [Ross, R. R.] Coll Holy Cross, Dept Phys, Worcester, MA 01610 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Walton, DJ (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Risaliti, Guido/0000-0002-3556-977X FU NASA [NNG08FD60C]; XMM-Newton; ESA Member States; Conicyt [ACT 1101]; STFC [ST/J00369711] FX The authors would like to thank the referee for providing useful feedback, which helped improve the manuscript. This research has made use of data obtained with the NuSTAR mission, a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL) and funded by NASA, and XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. We thank both the XMM-Newton and the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these coordinated observations. This research was supported under NASA grant No. NNG08FD60C and has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and Caltech (USA). P.A. acknowledges financial support from Conicyt ACT 1101, and P.G. acknowledges support from STFC (grant reference ST/J00369711). NR 102 TC 32 Z9 32 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2014 VL 788 IS 1 AR 76 DI 10.1088/0004-637X/788/1/76 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI7RY UT WOS:000337095200076 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 Brukner, 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 Clark, JA Cleva, F Coccia, E Cohadon, PF Colla, A Collette, C Colombini, M Cominsky, L Constancio, M Conte, A Cook, D Corbitt, TR Cordier, M Cornish, N Corpuz, A Corsi, A Costa, CA Coughlin, MW Coughlin, S Coulon, JP Countryman, S Couvares, P Coward, DM Cowart, M Coyne, DC Coyne, R Craig, K Creighton, JDE Crowder, SG Cumming, A Cunningham, L Cuoco, E Dahl, K Dal Canton, T Damjanic, M Danilishin, SL D'Antonio, S Danzmann, K Dattilo, V Daveloza, H Davier, M Davies, GS Daw, EJ Day, R Dayanga, T Debreczeni, G Degallaix, J Deleglise, S Del Pozzo, W Denker, T Dent, T Dereli, H Dergachev, V De Rosa, R DeRosa, RT DeSalvo, R Dhurandhar, S Diaz, M Di Fiore, L Di Lieto, A Di Palma, I Di Virgilio, A Donath, A Donovan, F Dooley, KL Doravari, S Dossa, S Douglas, R Downes, TP Drago, M Drever, RWP Driggers, JC Du, Z Dwyer, S Eberle, T Edo, T Edwards, M Effler, A Eggenstein, H Ehrens, P Eichholz, J Eikenberry, SS Endroczi, G Essick, R Etzel, T Evans, M Evans, T Factourovich, M Fafone, V Fairhurst, S Fang, Q Farinon, S Farr, B Farr, WM Favata, M Fehrmann, H Fejer, MM Feldbaum, D Feroz, F Ferrante, I Ferrini, F Fidecaro, F Finn, LS Fiori, I Fisher, RP Flaminio, R Fournier, JD Franco, S Frasca, S Frasconi, F Frede, M Frei, Z Freise, A Frey, R Fricke, TT Fritschel, P Frolov, VV Fulda, P Fyffe, M Gair, J Gammaitoni, L Gaonkar, S Garufi, F Gehrels, N Gemme, G Genin, E Gennai, A Ghosh, S Giaime, JA Giardina, KD Giazotto, A Gill, C Gleason, J Goetz, E Goetz, R Gondan, L Gonzalez, G Gordon, N Gorodetsky, ML Gossan, S Gossler, S Gouaty, R Graf, C Graff, PB Granata, M Grant, A Gras, S Gray, C Greenhalgh, RJS Gretarsson, AM Groot, P Grote, H Grover, K Grunewald, S Guidi, GM Guido, C Gushwa, K Gustafson, EK Gustafson, R Hammer, D Hammond, G Hanke, M Hanks, J Hanna, C Hanson, J Harms, J Harry, GM Harry, IW Harstad, ED Hart, M Hartman, MT Haster, CJ Haughian, K Heidmann, A Heintze, M Heitmann, H Hello, P Hemming, G Hendry, M Heng, IS Heptonstall, AW Heurs, M Hewitson, M Hild, S Hoak, D Hodge, KA Holt, K Hooper, S Hopkins, P Hosken, DJ Hough, J Howell, EJ Hu, Y Hughey, B Husa, S Huttner, SH Huynh, M Huynh-Dinh, T Ingram, DR Inta, R Isogai, T Ivanov, A Iyer, 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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. Whitcomb, S. E. 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. Boyle, M. Bruegmann, B. Buchman, L. T. Campanelli, M. Chu, T. Etienne, Z. B. Hannam, M. Healy, J. Hinder, I. Kidder, L. E. Laguna, P. Liu, Y. T. London, L. Lousto, C. O. Lovelace, G. MacDonald, I. Marronetti, P. Moesta, P. Mueller, D. Mundim, B. C. Nakano, H. Paschalidis, V. Pekowsky, L. Pollney, D. Pfeiffer, H. P. Ponce, M. Puerrer, M. Reifenberger, G. Reisswig, C. Santamaria, L. Scheel, M. A. Shapiro, S. L. Shoemaker, D. Sopuerta, C. F. Sperhake, U. Szilagyi, B. Taylor, N. W. Tichy, W. Tsatsin, P. Zlochower, Y. TI The NINJA-2 project: detecting and characterizing gravitational waveforms modelled using numerical binary black hole simulations SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article DE numerical relativity; gravitational-wave astronomy; binary black; holes; NINJA; LIGO; Virgo ID INSPIRALLING COMPACT BINARIES; GAMMA-RAY BURSTS; MASS-DISTRIBUTION; MERGERS; RADIATION; COSMOLOGY; EVOLUTION; PHYSICS; SEARCH; STARS AB The Numerical INJection Analysis (NINJA) project is a collaborative effort between members of the numerical relativity and gravitational-wave (GW) astrophysics communities. The purpose of NINJA is to study the ability to detect GWs emitted from merging binary black holes (BBH) and recover their parameters with next-generation GW observatories. We report here on the results of the second NINJA project, NINJA-2, which employs 60 complete BBH hybrid waveforms consisting of a numerical portion modelling the late inspiral, merger, and ringdown stitched to a post-Newtonian portion modelling the early inspiral. In a 'blind injection challenge' similar to that conducted in recent Laser Interferometer Gravitational Wave Observatory (LIGO) and Virgo science runs, we added seven hybrid waveforms to two months of data recoloured to predictions of Advanced LIGO (aLIGO) and Advanced Virgo (AdV) sensitivity curves during their first observing runs. The resulting data was analysed by GW detection algorithms and 6 of the waveforms were recovered with false alarm rates smaller than 1 in a thousand years. Parameter-estimation algorithms were run on each of these waveforms to explore the ability to constrain the masses, component angular momenta and sky position of these waveforms. We find that the strong degeneracy between the mass ratio and the BHs' angular momenta will make it difficult to precisely estimate these parameters with aLIGO and AdV. We also perform a large-scale Monte Carlo study to assess the ability to recover each of the 60 hybrid waveforms with early aLIGO and AdV sensitivity curves. Our results predict that early aLIGO and AdV will have a volume-weighted average sensitive distance of 300 Mpc (1 Gpc) for 10M circle dot + 10M circle dot (50M circle dot + 50M circle dot) BBH coalescences. We demonstrate that neglecting the component angular momenta in the waveform models used in matched-filtering will result in a reduction in sensitivity for systems with large component angular momenta. This reduction is estimated to be up to similar to 15% for 50M circle dot + 50M circle dot BBH coalescences with almost maximal angular momenta aligned with the orbit when using early aLIGO and AdV sensitivity curves. C1 [Aasi, J.; Abbott, B. 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[MacDonald, I.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Marronetti, P.; Reifenberger, G.; Tichy, W.; Tsatsin, P.] Florida Atlantic Univ, Dept Phys, Boca Raton, FL 33431 USA. [Nakano, H.] Kyoto Univ, Yukawa Inst Theoret Phys, Kyoto 6068502, Japan. [Pfeiffer, H. P.] Canadian Inst Adv Res, Toronto, ON M5G 1Z8, Canada. [Ponce, M.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. [Sopuerta, C. F.] Inst Ciencies Espai CSIC IEEC, Barcelona 08193, Spain. RP Aasi, J (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA. 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Martelli, Filippo/P-4041-2015; Branchesi, Marica/P-2296-2015; Gehring, Tobias/A-8596-2016; Canuel, Benjamin/C-7459-2014; Prokhorov, Leonid/I-2953-2012; Lee, Chang-Hwan/B-3096-2015; Khalili, Farit/D-8113-2012; Gorodetsky, Michael/C-5938-2008; McClelland, David/E-6765-2010; M, Manjunath/N-4000-2014; Vecchio, Alberto/F-8310-2015; Mow-Lowry, Conor/F-8843-2015; Strigin, Sergey/I-8337-2012; Leonardi, Matteo/G-9694-2015; Sigg, Daniel/I-4308-2015; Puppo, Paola/J-4250-2012; Gemme, Gianluca/C-7233-2008; Kumar, Prem/B-6691-2009; Luijten, Erik/E-3899-2010; Iyer, Bala R./E-2894-2012; Bell, Angus/E-7312-2011; Costa, Cesar/G-7588-2012; Losurdo, Giovanni/K-1241-2014; Steinlechner, Sebastian/D-5781-2013; prodi, giovanni/B-4398-2010; Sopuerta, Carlos/L-3835-2014; Hild, Stefan/A-3864-2010; Danilishin, Stefan/K-7262-2012; Gammaitoni, Luca/B-5375-2009 OI Del Pozzo, Walter/0000-0003-3978-2030; O'Shaughnessy, Richard/0000-0001-5832-8517; Vocca, Helios/0000-0002-1200-3917; Fairhurst, Stephen/0000-0001-8480-1961; Addesso, Paolo/0000-0003-0895-184X; Allen, Bruce/0000-0003-4285-6256; Granata, Massimo/0000-0003-3275-1186; Vetrano, Flavio/0000-0002-7523-4296; Naticchioni, Luca/0000-0003-2918-0730; calloni, enrico/0000-0003-4819-3297; Scott, Jamie/0000-0001-6701-6515; Sorazu, Borja/0000-0002-6178-3198; Bondu, Francois/0000-0001-6487-5197; Zweizig, John/0000-0002-1521-3397; 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; Nakano, Hiroyuki/0000-0001-7665-0796; Husa, Sascha/0000-0002-0445-1971; Vitale, Salvatore/0000-0003-2700-0767; Kanner, Jonah/0000-0001-8115-0577; Freise, Andreas/0000-0001-6586-9901; Nitz, Alexander/0000-0002-1850-4587; Papa, M.Alessandra/0000-0002-1007-5298; 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; Drago, Marco/0000-0002-3738-2431; Collette, Christophe/0000-0002-4430-3703; Pierro, Vincenzo/0000-0002-6020-5521; Lousto, Carlos/0000-0002-6400-9640; Coccia, Eugenio/0000-0002-6669-5787; Ward, Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447; Whelan, John/0000-0001-5710-6576; Ponce, Marcelo/0000-0001-5850-7240; Vedovato, Gabriele/0000-0001-7226-1320; Boschi, Valerio/0000-0001-8665-2293; Matichard, Fabrice/0000-0001-8982-8418; Punturo, Michele/0000-0001-8722-4485; Cella, Giancarlo/0000-0002-0752-0338; Cesarini, Elisabetta/0000-0001-9127-3167; Chow, Jong/0000-0002-2414-5402; Frey, Raymond/0000-0003-0341-2636; Ciani, Giacomo/0000-0003-4258-9338; Di Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Aulbert, Carsten/0000-0002-1481-8319; Denker, Timo/0000-0003-1259-5315; Strain, Kenneth/0000-0002-2066-5355; Miao, Haixing/0000-0003-4101-9958; Howell, Eric/0000-0001-7891-2817; Heidmann, Antoine/0000-0002-0784-5175; Nelemans, Gijs/0000-0002-0752-2974; 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; Travasso, Flavio/0000-0002-4653-6156; Tacca, Matteo/0000-0003-1353-0441; Graef, Christian/0000-0002-4535-2603; Garufi, Fabio/0000-0003-1391-6168; Deleglise, Samuel/0000-0002-8680-5170; 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; Lee, Chang-Hwan/0000-0003-3221-1171; Gorodetsky, Michael/0000-0002-5159-2742; McClelland, David/0000-0001-6210-5842; M, Manjunath/0000-0001-8710-0730; Vecchio, Alberto/0000-0002-6254-1617; Sigg, Daniel/0000-0003-4606-6526; Puppo, Paola/0000-0003-4677-5015; Gemme, Gianluca/0000-0002-1127-7406; Luijten, Erik/0000-0003-2364-1866; Iyer, Bala R./0000-0002-4141-5179; Bell, Angus/0000-0003-1523-0821; Losurdo, Giovanni/0000-0003-0452-746X; Steinlechner, Sebastian/0000-0003-4710-8548; prodi, giovanni/0000-0001-5256-915X; Sopuerta, Carlos/0000-0002-1779-4447; Danilishin, Stefan/0000-0001-7758-7493; Gammaitoni, Luca/0000-0002-4972-7062 FU United States National Science Foundation for the construction and operation of the LIGO Laboratory; 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; 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; Scottish Funding Council; National Aeronautics and Space Administration; OTKA of Hungary; 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; Leverhulme Trust; David and Lucile Packard Foundation; Research Corporation; Alfred P Sloan Foundation; National Science Foundation under NSF [PHY-1305730, PHY-1212426, PHY-1229173, AST-1028087, DRL-1136221, OCI-0832606, PHY-0903782, PHY-0929114, PHY-0969855, AST-1002667, PHY-0963136, PHY-1300903, PHY-1305387, PHY-1204334, PHY-0855315, PHY-0969111, PHY-1005426, PHY-0601459, PHY-1068881, PHY-1005655]; NASA [07-ATFP07-0158, NNX11AE11G, NNX13AH44G, NNX09AF96G, NNX09AF97G]; Marie Curie Grants of the 7th European Community Framework Programme [293412]; ERC Starting Grant [DyBHo-256667]; Science and Technology Facilities Council [ST/H008438/1, ST/I001085/1]; Sherman Fairchild Foundation; NSERC of Canada; Canada Research Chairs Program; Canadian Institute for Advanced Research; Ramon y Cajal Programme of the Ministry of Education and Science of Spain [AYA2010-15709, CSD2007-00042, CSD2009-00064]; Spanish Ministry of Science and Innovation [FPA2010-16495]; German Research Foundation [SFB/Transregio 7]; German Aerospace Center for LISA Germany; NSF [PHY-1229173, AST-1028087, DMS-0820923, PHY-0722703, PHY-09602]; BSC grant [AECT-2009- 2-0017, AECT-2010-1-0008, AECT-2010-2-0013, AECT-2010-3-0010, AECT-2011-10015, AECT-2011-2-0012]; FWF grant [P22498]; Canada Foundation for Innovation; Government of Ontario; Ontario Research Fund-Research Excellence; University of Toronto; Compute Canada; CESGA-ICTS-2010-200; Scottish Universities Physics Alliance; Royal Society; Istituto Nazionale di Fisica Nucleare of Italy; [MIRG-CT-2007-205005/PHY] 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, OTKA of Hungary, 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.; We gratefully acknowledge support from the National Science Foundation under NSF grants PHY-1305730, PHY-1212426, PHY-1229173, AST-1028087, DRL-1136221, OCI-0832606, PHY-0903782, PHY-0929114, PHY-0969855, AST-1002667, PHY-0963136, PHY-1300903, PHY-1305387, PHY-1204334, PHY-0855315, PHY-0969111, PHY-1005426, PHY-0601459, PHY-1068881, PHY-1005655, PHY-0653443, PHY-0855892, PHY-0914553, PHY-0941417, PHY-0903973, PHY-0955825, by NASA grants 07-ATFP07-0158, NNX11AE11G, NNX13AH44G, NNX09AF96G, NNX09AF97G, by Marie Curie Grants of the 7th European Community Framework Programme FP7-PEOPLE-2011-CIG CBHEO No. 293412, by the DyBHo-256667 ERC Starting Grant, and MIRG-CT-2007-205005/PHY, and Science and Technology Facilities Council grants ST/H008438/1 and ST/I001085/1. Further funding was provided by the Sherman Fairchild Foundation, NSERC of Canada, the Canada Research Chairs Program, the Canadian Institute for Advanced Research, the Ramon y Cajal Programme of the Ministry of Education and Science of Spain, contracts AYA2010-15709, CSD2007-00042, CSD2009-00064 and FPA2010-16495 of the Spanish Ministry of Science and Innovation, the German Research Foundation, grant SFB/Transregio 7, the German Aerospace Center for LISA Germany, and the Grand-in-Aid for Scientific Research (24103006). Computations were carried out on Teragrid machines Lonestar, Ranger, Trestles and Kraken under Teragrid allocations TG-PHY060027N, TG-MCA99S008, TG-PHY090095, TG-PHY100051, TG-PHY990007N, TG-PHY090003, TG-MCA08X009. Computations were also performed on the clusters "HLRB-2'at LRZ Munich, 'NewHorizons' and 'Blue Sky'at RIT (funded by NSF grant nos PHY-1229173, AST-1028087, DMS-0820923 and PHY-0722703), 'Zwicky' at Caltech (funded by NSF MRI award PHY-0960291), 'Finis Terrae'(funded by CESGA-ICTS-2010-200), 'Caesaraugusta'(funded by BSC grant nos AECT-2011-2-0006, AECT-2011-3-0007), 'MareNostrum'( funded by BSC grant nos. AECT-2009- 2-0017, AECT-2010-1-0008, AECT-2010-2-0013, AECT-2010-3-0010, AECT-2011-10015, AECT-2011-2-0012), 'VSC' in Vienna (funded by FWF grant P22498), 'Force' at GaTech, and on the GPC supercomputer at the SciNet HPC Consortium [150]; 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 133 TC 22 Z9 22 U1 4 U2 63 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD JUN 7 PY 2014 VL 31 IS 11 AR 115004 DI 10.1088/0264-9381/31/11/115004 PG 45 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AI3YT UT WOS:000336802600004 ER PT J AU Choi, T Xiong, XX Angal, A Chander, G Qu, JJ AF Choi, Taeyoung Xiong, Xiaoxiong Angal, Amit Chander, Gyanesh Qu, John J. TI Assessment of the spectral stability of Libya 4, Libya 1, and Mauritania 2 sites using Earth Observing One Hyperion SO JOURNAL OF APPLIED REMOTE SENSING LA English DT Article DE average deviation; calibration; CEOS; Hyperion; Libya 1; Libya 4; Mauritania 2; PICS; RSR; SAM; spectral stability ID DESERT SITES; CALIBRATION; SPECTROMETER AB The objective of this paper is to formulate a methodology to assess the spectral stability of the Libya 4, Libya 1, and Mauritania 2 pseudo-invariant calibration sites (PICS) using Earth Observing One (EO-1) Hyperion sensor. All the available Hyperion collections, downloaded from the Earth Explorer website, were utilized for the three PICS. In each site, a reference spectrum is selected at a specific day in the vicinity of the region of interest (ROI) defined by Committee on Earth Observation Satellites (CEOS). A series of ROIs are predefined in the along-track direction with 196 spectral top-of-atmosphere reflectance values in each ROI. Based on the reference ROI spectrum, the spectral stability of these ROIs is evaluated by average deviations (ADs) and spectral angle mapper (SAM) methods in the specific ranges of time and geo-spatial locations. Time and ROI location-dependent SAM and AD results are very stable within +/- 2 deg and +/- 1.7% of 1 sigma standard deviations. Consequently, the Libya 4, Mauritania 2, and Libya 1 CEOS selected PICS are spectrally stable targets within the time and spatial swath ranges of the Hyperion collections. (C) 2014 Society of Photo-Optical Instrumentation Engineers (SPIE) C1 [Choi, Taeyoung] Sigma Space Corp, Lanham, MD 20706 USA. [Xiong, Xiaoxiong; Chander, Gyanesh] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Angal, Amit] Sci Syst & Applicat Inc, Lanham, MD 20706 USA. [Qu, John J.] George Mason Univ, Coll Sci, Dept GGS, Global Environm & Nat Resources Inst, Fairfax, VA 20151 USA. RP Choi, T (reprint author), Sigma Space Corp, 4801 Forbes Blvd, Lanham, MD 20706 USA. EM taeyoung.choi@noaa.gov RI Choi, Taeyoung/E-4437-2016 OI Choi, Taeyoung/0000-0002-4596-989X NR 16 TC 2 Z9 2 U1 0 U2 12 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 JUN 6 PY 2014 VL 8 AR 083618 DI 10.1117/1.JRS.8.083618 PG 14 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA AK5WI UT WOS:000338497000001 ER PT J AU Arens, EE Youngquist, RC Starr, SO AF Arens, Ellen E. Youngquist, Robert C. Starr, Stanley O. TI Intensity calibrated hydrogen flame spectrum SO INTERNATIONAL JOURNAL OF HYDROGEN ENERGY LA English DT Article DE Hydrogen flame spectroscopy; Flame spectroscopy; Hydrogen fire detection; Ultraviolet fire detection; Infrared fire detection; Fire detection AB The detection of hydrogen fires is important to the aerospace community. The National Aeronautics and Space Administration (NASA) has devoted significant effort to the development, testing, and installation of hydrogen fire detectors based on ultraviolet, near-infrared, mid-infrared, and/or far-infrared flame emission bands. Yet, there is no intensity calibrated hydrogen-air flame spectrum over this range in the literature and consequently, it can be difficult to compare the merits of different radiation-based hydrogen fire detectors. In this paper we present an intensity calibrated irradiance spectrum for a low pressure hydrogen flame burning in air from 200 nm to 13.5 microns that varies by more than six orders of magnitude. The results resolve relative intensity errors between spectral bands that appear within the literature. The impact of the measured spectrum on the choice of radiation-based hydrogen fire detectors is discussed. Copyright (C) 2014, Hydrogen Energy Publications, LLC. Published by Elsevier Ltd. All rights reserved. C1 [Arens, Ellen E.; Youngquist, Robert C.; Starr, Stanley O.] NASA, Kennedy Space Ctr, FL 32899 USA. RP Youngquist, RC (reprint author), NASA, Mail Stop NE-L5, Kennedy Space Ctr, FL 32899 USA. EM Robert.C.Youngquist@nasa.gov FU Ground Systems Development and Operations Program at the Kennedy Space Center, National Aeronautics and Space Administration FX This work received funding from the Ground Systems Development and Operations Program at the Kennedy Space Center, National Aeronautics and Space Administration. We acknowledge Damion M. Lucas, Teresa M. Lawhorn, and Robert B. Cox for providing aid in the performing the spectral measurements. NR 11 TC 2 Z9 2 U1 1 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0360-3199 EI 1879-3487 J9 INT J HYDROGEN ENERG JI Int. J. Hydrog. Energy PD JUN 5 PY 2014 VL 39 IS 17 BP 9545 EP 9551 DI 10.1016/j.ijhydene.2014.04.043 PG 7 WC Chemistry, Physical; Electrochemistry; Energy & Fuels SC Chemistry; Electrochemistry; Energy & Fuels GA AI5BN UT WOS:000336880500069 ER PT J AU Modest, HI Rath, C Banday, AJ Gorski, KM Morfill, GE AF Modest, H. I. Raeth, C. Banday, A. J. Gorski, K. M. Morfill, G. E. TI Correlating Fourier phase information with real-space higher order statistics in CMB data SO PHYSICAL REVIEW D LA English DT Article ID DEPENDENT NON-GAUSSIANITIES; PROBE WMAP OBSERVATIONS; SCALING INDEXES; MINKOWSKI FUNCTIONALS; INFLATIONARY UNIVERSE; BIANCHI-VIIH; MICROWAVE; MAPS; SKY; FLATNESS AB We present a heuristic study on the correlations between harmonic space phase information and higher-order statistics. Using the spherical full-sky maps of the cosmic microwave background as an example, we demonstrate that known phase correlations at large spatial scales can gradually be diminished when subtracting a suitable best-fit (Bianchi-) template map of a given strength. The weaker phase correlations are attended by a vanishing signature of anisotropy when measuring the Minkowski functionals and scaling indices in real space with the aid of surrogate maps being free of phase correlations. Those investigations can open a new road to a better understanding of signatures of non-Gaussianities in complex spatial structures, especially by elucidating the meaning of Fourier phase correlations and their influence on higher-order statistics. C1 [Modest, H. I.; Raeth, C.; Morfill, G. E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Banday, A. J.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Banday, A. J.] CNRS, IRAP, F-31028 Toulouse 4, France. [Gorski, K. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Modest, HI (reprint author), Max Planck Inst Extraterr Phys, POB 1312,Giessenbachstr 1, D-85748 Garching, Germany. EM hmodest@mpe.mpg.de FU Christiane Nusslein-Volhard (CNV) foundation; International Max Planck Research School FX We greatly thank Theresa Jaffe and Jason McEwen for providing us with the latest WMAP and Planck Bianchi templates, respectively. For the calculations, we employ the HEALPix software [48]. H. I. M. acknowledges the support of the Christiane Nusslein-Volhard (CNV) foundation and the International Max Planck Research School. NR 44 TC 1 Z9 1 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD JUN 5 PY 2014 VL 89 IS 12 AR 123004 DI 10.1103/PhysRevD.89.123004 PG 8 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AI5MX UT WOS:000336912800002 ER PT J AU Liu, YD Zhang, JS AF Liu, Yingdi Zhang, Jingsong TI Atmospheric Peroxy Radical Measurements Using Dual-Channel Chemical Amplification Cavity Ringdown Spectroscopy SO ANALYTICAL CHEMISTRY LA English DT Article ID LASER-INDUCED FLUORESCENCE; DOWN SPECTROSCOPY; TROPOSPHERIC OH; HO2; INSTRUMENT; AMPLIFIER; RO2; NO2; DEPLOYMENT; CHEMISTRY AB Peroxy (HO2 and RO2) radicals are important intermediates in tropospheric oxidation of hydrocarbons, and their accurate atmospheric measurements remain challenging. In this work, the peroxy radical chemical amplification (PERCA) method was combined with cavity ringdown spectroscopy (CRDS) to develop a dual-channel instrument for measurements of atmospheric peroxy radicals. In the amplification channel, the peroxy radicals were converted in an excess amount of NO and CO into a higher level of NO2 and measured along with the background NO2, while in the reference channel, only the background NO2 (ambient NO2 and NO2 converted from O-3 reaction with NO) was monitored. The NO2 levels from both channels were measured simultaneously at a high time resolution (similar to 1 s) using two identical CRDS systems with one 408.5-nm diode laser, and their difference gave the amplified NO2 from PERCA. The peroxy radical concentration was obtained from the amplified NO2 and the calibrated amplification factor or chain length (CL). The optimized CL was 190 +/- 20 (1 sigma) using laboratory-generated HO2 and CH3O2 radical sources. The detection sensitivity was 4 ppt/10 s (3 sigma). Ambient measurements in Riverside, CA were carried out. This dual-channel diode-laser PERCA-CRDS instrument was compact and capable of providing real-time, in situ, and sensitive measurements of atmospheric peroxy radicals with fast time response. C1 [Liu, Yingdi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, Jingsong] Univ Calif Riverside, Dept Chem, Riverside, CA 92521 USA. [Zhang, Jingsong] Univ Calif Riverside, Air Pollut Res Ctr, Riverside, CA 92521 USA. RP Zhang, JS (reprint author), Univ Calif Riverside, Dept Chem, Riverside, CA 92521 USA. EM jingsong.zhang@ucr.edu RI liu, yingdi/E-6410-2013 FU National Science Foundation [CHE-1214157]; W. M. Keck Foundation FX We thank Dr. David Medina for assistance during several of the experiments, and we thank Prof. Paul Ziemann for his chemiluminescence NOx analyzer. This work was supported by the National Science Foundation (No. CHE-1214157) and the W. M. Keck Foundation. NR 44 TC 3 Z9 3 U1 3 U2 42 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0003-2700 EI 1520-6882 J9 ANAL CHEM JI Anal. Chem. PD JUN 3 PY 2014 VL 86 IS 11 BP 5391 EP 5398 DI 10.1021/ac5004689 PG 8 WC Chemistry, Analytical SC Chemistry GA AI6AV UT WOS:000336953100029 PM 24798952 ER PT J AU Temi, P Marcum, PM Young, E Adams, JD Adams, S Andersson, BG Becklin, EE Boogert, A Brewster, R Burgh, E Cobleigh, BR Culp, S De Buizer, J Dunham, EW Engfer, C Ediss, G Fujieh, M Grashuis, R Gross, M Harmon, E Helton, A Hoffman, D Homan, J Hutwohl, M Jakob, H Jensen, SC Kaminski, C Kozarsky, D Krabbe, A Klein, R Lammen, Y Lampater, U Latter, WB Le, J McKown, N Melchiorri, R Meyer, AW Miles, J Miller, WE Miller, S Moore, E Nickison, DJ Opshaug, K Pfueller, E Radomski, J Rasmussen, J Reach, W Reinacher, A Roellig, TL Sandell, G Sankrit, R Savage, ML Shenoy, S Schonfeld, JE Shuping, RY Smith, EC Talebi, E Teufel, S Tseng, TC Vacca, WD Vaillancourt, J Van Cleve, JE Wiedemann, M Wolf, J Zavala, E Zeile, O Zell, PT Zinnecker, H AF Temi, Pasquale Marcum, Pamela M. Young, Erick Adams, Joseph D. Adams, Sybil Andersson, B. -G. Becklin, Eric E. Boogert, Adwin Brewster, Rick Burgh, Eric Cobleigh, Brent R. Culp, Steven De Buizer, Jim Dunham, Edward W. Engfer, Christian Ediss, Geoffrey Fujieh, Maura Grashuis, Randy Gross, Michael Harmon, Edward Helton, Andrew Hoffman, Douglas Homan, Jeff Huetwohl, Michael Jakob, Holger Jensen, Stephen C. Kaminski, Charles Kozarsky, Daniel Krabbe, Alfred Klein, Randolf Lammen, Yannick Lampater, Ulrich Latter, William B. Le, Jeanette McKown, Nancy Melchiorri, Riccardo Meyer, Allan W. Miles, John Miller, Walter E. Miller, Scott Moore, Elizabeth Nickison, Donald J. Opshaug, Kortney Pfueeller, Enrico Radomski, James Rasmussen, John Reach, William Reinacher, Andreas Roellig, Thomas L. Sandell, Goeran Sankrit, Ravi Savage, Maureen L. Shenoy, Sachindev Schonfeld, Julie E. Shuping, Ralph Y. Smith, Erin C. Talebi, Ehsan Teufel, Stefan Tseng, Ting C. Vacca, William D. Vaillancourt, John Van Cleve, Jeffrey E. Wiedemann, Manuel Wolf, Juergen Zavala, Eddie Zeile, Oliver Zell, Peter T. Zinnecker, Hans TI THE SOFIA OBSERVATORY AT THE START OF ROUTINE SCIENCE OPERATIONS: MISSION CAPABILITIES AND PERFORMANCE SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE instrumentation: detectors; instrumentation: interferometers; instrumentation: miscellaneous; instrumentation: photometers; instrumentation: spectrographs; telescopes ID POINTING CONTROL-SYSTEM; INFRARED ASTRONOMY; GREAT; SOFIA/FORCAST; TELESCOPE; INSTRUMENT; CAMERA AB The Stratospheric Observatory for Infrared Astronomy (SOFIA) has recently concluded a set of engineering flights for observatory performance evaluation. These in-flight opportunities are viewed as the first comprehensive assessment of the observatory's performance and are used to guide future development activities, as well as to identify additional observatory upgrades. Pointing stability was evaluated, including the image motion due to rigid-body and flexible-body telescope modes as well as possible aero-optical image motion. We report on recent improvements in pointing stability by using an active mass damper system installed on the telescope. Measurements and characterization of the shear layer and cavity seeing, as well as image quality evaluation as a function of wavelength have also been performed. Additional tests targeted basic observatory capabilities and requirements, including pointing accuracy, chopper evaluation, and imager sensitivity. This paper reports on the data collected during these flights and presents current SOFIA observatory performance and characterization. C1 [Temi, Pasquale; Marcum, Pamela M.; Fujieh, Maura; Harmon, Edward; Kozarsky, Daniel; Miller, Scott; Nickison, Donald J.; Roellig, Thomas L.; Schonfeld, Julie E.; Smith, Erin C.; Zell, Peter T.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. [Young, Erick; Adams, Joseph D.; Adams, Sybil; Andersson, B. -G.; Becklin, Eric E.; Boogert, Adwin; Burgh, Eric; De Buizer, Jim; Ediss, Geoffrey; Grashuis, Randy; Gross, Michael; Helton, Andrew; Kaminski, Charles; Klein, Randolf; Latter, William B.; McKown, Nancy; Melchiorri, Riccardo; Meyer, Allan W.; Miles, John; Moore, Elizabeth; Opshaug, Kortney; Radomski, James; Reach, William; Sandell, Goeran; Sankrit, Ravi; Savage, Maureen L.; Shenoy, Sachindev; Shuping, Ralph Y.; Vacca, William D.; Vaillancourt, John; Van Cleve, Jeffrey E.] NASA Ames Res Ctr, USRA SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Brewster, Rick; Culp, Steven; Hoffman, Douglas; Homan, Jeff; Miller, Walter E.; Talebi, Ehsan] Orbital Sci Corp, Moffett Field, CA 94035 USA. [Cobleigh, Brent R.; Jensen, Stephen C.; Le, Jeanette; Tseng, Ting C.; Zavala, Eddie] NASA Armstrong Flight Res Ctr, Edwards AFB, CA 93523 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Engfer, Christian; Huetwohl, Michael; Jakob, Holger; Lammen, Yannick; Lampater, Ulrich; Pfueeller, Enrico; Reinacher, Andreas; Teufel, Stefan; Wiedemann, Manuel; Wolf, Juergen; Zeile, Oliver; Zinnecker, Hans] NASA Ames Res Ctr, Deutsch SOFIA Inst, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Rasmussen, John] Crit Realm Corp, San Jose, CA 95135 USA. [Krabbe, Alfred] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany. RP Temi, P (reprint author), NASA Ames Res Ctr, Moffett Field, CA 94035 USA. OI Klein, Randolf/0000-0002-7187-9126; Andersson, B-G/0000-0001-6717-0686; Reach, William/0000-0001-8362-4094 NR 46 TC 8 Z9 8 U1 0 U2 4 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 JUN PY 2014 VL 212 IS 2 AR 24 DI 10.1088/0067-0049/212/2/24 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CD3PZ UT WOS:000350993000007 ER PT J AU Borges, M Filieri, A d'Amorim, M Pasareanu, CS Visser, W AF Borges, Mateus Filieri, Antonio d'Amorim, Marcelo Pasareanu, Corina S. Visser, Willem TI Compositional Solution Space Quantification for Probabilistic Software Analysis SO ACM SIGPLAN NOTICES LA English DT Article; Proceedings Paper CT 35th ACM SIGPLAN Conference on Programming Language Design and Implementation (PLDI) CY JUN 09-11, 2014 CL Edinburgh, SCOTLAND SP Assoc Comp Machinery Special Interest Grp Programming Languages, NSF DE Symbolic Execution; Monte Carlo Sampling; Probabilistic Analysis; Testing ID SYMBOLIC EXECUTION AB Probabilistic software analysis aims at quantifying how likely a target event is to occur during program execution. Current approaches rely on symbolic execution to identify the conditions to reach the target event and try to quantify the fraction of the input domain satisfying these conditions. Precise quantification is usually limited to linear constraints, while only approximate solutions can be provided in general through statistical approaches. However, statistical approaches may fail to converge to an acceptable accuracy within a reasonable time. We present a compositional statistical approach for the efficient quantification of solution spaces for arbitrarily complex constraints over bounded floating-point domains. The approach leverages interval constraint propagation to improve the accuracy of the estimation by focusing the sampling on the regions of the input domain containing the sought solutions. Preliminary experiments show significant improvement on previous approaches both in results accuracy and analysis time. C1 [Borges, Mateus; d'Amorim, Marcelo] Univ Fed Pernambuco, Recife, PE, Brazil. [Filieri, Antonio] Univ Stuttgart, Stuttgart, Germany. [Pasareanu, Corina S.] NASA, Ames Res Ctr, CMU SV, Washington, DC USA. [Visser, Willem] Univ Stellenbosch, ZA-7600 Stellenbosch, South Africa. RP Borges, M (reprint author), Univ Fed Pernambuco, Recife, PE, Brazil. OI Filieri, Antonio/0000-0001-9646-646X NR 30 TC 0 Z9 0 U1 0 U2 1 PU ASSOC COMPUTING MACHINERY PI NEW YORK PA 2 PENN PLAZA, STE 701, NEW YORK, NY 10121-0701 USA SN 0362-1340 EI 1558-1160 J9 ACM SIGPLAN NOTICES JI ACM Sigplan Not. PD JUN PY 2014 VL 49 IS 6 BP 123 EP 132 DI 10.1145/2594291.2594329 PG 10 WC Computer Science, Software Engineering SC Computer Science GA AS7ST UT WOS:000344455800015 ER PT J AU Blyakharchuk, TA Tchebakova, NM Parfenova, EI Soja, AJ AF Blyakharchuk, T. A. Tchebakova, N. M. Parfenova, E. I. Soja, A. J. TI Potential influence of the late Holocene climate on settled farming versus nomadic cattle herding in the Minusinsk Hollow, south-central Siberia SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE Holocene; human culture; economic strategies; Siberia ID POLLEN DATA; CENTRAL-ASIA; VEGETATION AB Prehistoric and early historic human cultures are known to be closely connected to and dependent on their natural environments. We test the hypothesis that climate change influenced the means of subsistence of ancient tribes and favored agricultural or cattle herding economic strategies. Our study area is the Khakass-Minusinsk Hollow, located in the foothills of the Sayan Mountains, south-central Siberia, which was, for a few millennia, a buffer zone for human migrations across the Great Eurasian Steppe. Three different methods (the Montane BioClimatic Model, MontBCliM; the biomization method; and the actualizm method) are employed to reconstruct vegetation taken from the fossil pollen of sediment cores in two mountain lakes at eleven time slices related to successive human cultures back to the mid-Holocene. MontBCliM model is used inversely to convert site paleo-vegetation into site paleo-climates. Climate-based regression models are developed and applied to reconstructed climates to evaluate possible pasture and grain crops for these time slices. Pollen-based reconstructions of the climate fluctuations uncovered several dry periods with steppe and forest-steppe and wetter periods with forests since 6000 BP. Grasslands increased by an order of magnitude during the dry periods and provided extensive open space suitable for pastoralism; however, both grain and pasture yields decreased during these dry periods. During wetter climates, both grain and pasture yields increased twofold and supported more fixed human settlements centered around farming and cattle herding. Thus, the dry periods favored pastoralist rather than farming activities. Conversely, tribes that practiced agriculture had some advantage in the wet periods. C1 [Blyakharchuk, T. A.] Russian Acad Sci, Siberian Branch, Inst Monitoring Climat & Ecol Syst, Tomsk 643055, Russia. [Tchebakova, N. M.; Parfenova, E. I.] Russian Acad Sci, Siberian Branch, VN Sukachev Inst Forests, Krasnoyarsk 660036, Russia. [Soja, A. J.] NASA, Langley Res Ctr, Natl Inst Aerosp, Hampton, VA 23681 USA. [Blyakharchuk, T. A.] Tomsk State Univ, Tomsk 634050, Russia. RP Blyakharchuk, TA (reprint author), Russian Acad Sci, Siberian Branch, Inst Monitoring Climat & Ecol Syst, Akad Prospekt 10-3, Tomsk 643055, Russia. EM tarun5@rambler.ru; ncheby@ksc.krasn.ru; lyeti@ksc.krasn.ru; Amber.J.Soja@nasa.gov FU Russian integration project [53]; NASA Interdisciplinary Science [NNH09ZDA001N-IDS program]; Russian Foundation of Basic Research [13-04-00984a]; Government of the Russian Federation [220]; Ministry of Education and Science of the Russian Federation [14.B25.31.0001] FX This study was supported by the Russian integration project #53, the NASA Interdisciplinary Science NNH09ZDA001N-IDS program, a grant from the Russian Foundation of Basic Research No 13-04-00984a, as well as a research grant carried out in accordance with the Resolution of the Government of the Russian Federation No 220 dated 09 April 2010, under Agreement No 14.B25.31.0001 with the Ministry of Education and Science of the Russian Federation dated 24 June 2013 (BIO-GEO-CLIM). The authors are grateful to Robert Monserud, Jerry Rehfeldt, Jane Bradford and Natalia Vygodskaya for invaluable help and to useful comments by three anonymous reviewers in preparation of this manuscript. NR 58 TC 0 Z9 0 U1 5 U2 23 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 JUN PY 2014 VL 9 IS 6 AR 065004 DI 10.1088/1748-9326/9/6/065004 PG 15 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AP1JM UT WOS:000341825200036 ER PT J AU Gatebe, CK Ichoku, CM Poudyal, R Roman, MO Wilcox, E AF Gatebe, C. K. Ichoku, C. M. Poudyal, R. Roman, M. O. Wilcox, E. TI Surface albedo darkening from wildfires in northern sub-Saharan Africa SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE surface albedo; wildfires; sub-Saharan Africa; MODIS; biomass burning; albedo recovery; albedo darkening ID BIDIRECTIONAL REFLECTANCE; SPECTRAL MEASUREMENTS; FIRE; MODIS; BIOMASS; SAHEL; DESERTIFICATION; ALGORITHM; DYNAMICS; AIRBORNE AB Northern sub-Saharan Africa (NSSA) has a wide variety of climate zones or biomes, where albedo dynamics are highly coupled with vegetation dynamics and fire disturbances. Quantifying surface albedo variations due to fire disturbances on time scales of several months to several years is complex and is made worse by lack of accurate and spatially consistent surface albedo data. Here, we estimate the surface albedo effect from wildfires in different land cover types in the NSSA region using Moderate Resolution Imaging Spectroradiometer (MODIS) multi-year observational data (2003-11). The average decrease in albedo after fires at the scale of 1 km MODIS footprint is -0.002 02 +/- 0.000 03 for woody savanna and -0.002 22 +/- 0.000 03 for savanna. These two land cover types together account for > 86% of the total MODIS fire count between 2003 and 2011. We found that only a small fraction of the pixels (<= 10%) burn in two successive years and about 47% had any fire recurrence in 9 years. The study also derived the trajectories of post-fire albedo dynamics from the percentages of pixels that recover to pre-fire albedo values each year. We found that the persistence of surface albedo darkening in most land cover types in the NSSA region is limited to about 6-7 years, after which at least 99% of the burnt pixels recover to their pre-fire albedo. Our results provide critical information for deriving necessary input to various models used in determining the effects of albedo change due to wild fires in the NSSA region. C1 [Gatebe, C. K.; Poudyal, R.] Univ Space Res Assoc, Columbia, MD 20146 USA. [Gatebe, C. K.; Ichoku, C. M.; Roman, M. O.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Poudyal, R.] Sci Syst & Applicat Inc, Lanham, MD USA. [Wilcox, E.] Desert Res Inst, Reno, NV 89512 USA. RP Gatebe, CK (reprint author), Univ Space Res Assoc, Columbia, MD 20146 USA. EM charles.k.gatebe@nasa.gov RI Gatebe, Charles/G-7094-2011; Roman, Miguel/D-4764-2012; Ichoku, Charles/E-1857-2012 OI Gatebe, Charles/0000-0001-9261-2239; Roman, Miguel/0000-0003-3953-319X; Ichoku, Charles/0000-0003-3244-4549 FU Science Mission Directorate of the National Aeronautics and Space Administration as part of the Interdisciplinary Studies (IDS) program; NASA's Terrestrial Ecology Program FX This research was supported by the Science Mission Directorate of the National Aeronautics and Space Administration as part of the Interdisciplinary Studies (IDS) program headed by Dr Jack Kaye, and conducted through the Radiation Sciences Program under Dr Hal B. Maring. We also acknowledge support from NASA's Terrestrial Ecology Program managed by Dr Diane Wickland. NR 31 TC 9 Z9 9 U1 1 U2 13 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 JUN PY 2014 VL 9 IS 6 AR 065003 DI 10.1088/1748-9326/9/6/065003 PG 12 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AP1JM UT WOS:000341825200035 ER PT J AU Yi, YH Kimball, JS Reichle, RH AF Yi, Yonghong Kimball, John S. Reichle, Rolf H. TI Spring hydrology determines summer net carbon uptake in northern ecosystems SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE boreal/arctic; net carbon uptake; spring hydrology; vegetation productivity; respiration; soil moisture ID DIOXIDE; BOREAL; FOREST; CO2; BALANCE; TEMPERATURE; SENSITIVITY; EXCHANGE; FIRE; RESPIRATION AB Increased photosynthetic activity and enhanced seasonal CO2 exchange of northern ecosystems have been observed from a variety of sources including satellite vegetation indices (such as the normalized difference vegetation index; NDVI) and atmospheric CO2 measurements. Most of these changes have been attributed to strong warming trends in the northern high latitudes (>= 50 degrees N). Here we analyze the interannual variation of summer net carbon uptake derived from atmospheric CO2 measurements and satellite NDVI in relation to surface meteorology from regional observational records. We find that increases in spring precipitation and snow pack promote summer net carbon uptake of northern ecosystems independent of air temperature effects. However, satellite NDVI measurements still show an overall benefit of summer photosynthetic activity from regional warming and limited impact of spring precipitation. This discrepancy is attributed to a similar response of photosynthesis and respiration to warming and thus reduced sensitivity of net ecosystem carbon uptake to temperature. Further analysis of boreal tower eddy covariance CO2 flux measurements indicates that summer net carbon uptake is positively correlated with early growing-season surface soil moisture, which is also strongly affected by spring precipitation and snow pack based on analysis of satellite soil moisture retrievals. This is attributed to strong regulation of spring hydrology on soil respiration in relatively wet boreal and arctic ecosystems. These results document the important role of spring hydrology in determining summer net carbon uptake and contrast with prevailing assumptions of dominant cold temperature limitations to high-latitude ecosystems. Our results indicate potentially stronger coupling of boreal/arctic water and carbon cycles with continued regional warming trends. C1 [Yi, Yonghong; Kimball, John S.] Univ Montana, Flathead Lake Biol Stn, Polson, MT 59860 USA. [Yi, Yonghong; Kimball, John S.] Univ Montana, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA. [Reichle, Rolf H.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. RP Yi, YH (reprint author), Univ Montana, Flathead Lake Biol Stn, 32125 Biostn Lane, Polson, MT 59860 USA. EM yonghong.yi@ntsg.umt.edu RI Reichle, Rolf/E-1419-2012; Yi, Yonghong/C-2395-2017 FU CarboEuropeIP; FAO-GTOS-TCO; iLEAPS; Max Planck Institute for Biogeochemistry; National Science Foundation; University of Tuscia; Universite Laval and Environment Canada; US Department of Energy; NOAA ESRL; NASA [NNX11AD46G] FX This study used tower eddy covariance data acquired by the FLUXNET community, which was supported by the CarboEuropeIP, FAO-GTOS-TCO, iLEAPS, Max Planck Institute for Biogeochemistry, National Science Foundation, University of Tuscia, Universite Laval and Environment Canada, US Department of Energy and NOAA ESRL, as well as many local funders. The authors thank Dr F Chevallier for providing the Bayesian model inversion results. Funding for this study was provided by the NASA Earth Science program (NNX11AD46G). NR 51 TC 7 Z9 7 U1 3 U2 35 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 JUN PY 2014 VL 9 IS 6 AR 064003 DI 10.1088/1748-9326/9/6/064003 PG 11 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AP1JM UT WOS:000341825200005 ER PT J AU Zhai, AR Jiang, JH AF Zhai, Alice R. Jiang, Jonathan H. TI Dependence of US hurricane economic loss on maximum wind speed and storm size SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE hurricane; economic loss; storm size; wind speed ID CLIMATE-CHANGE; DAMAGE AB Many empirical hurricane economic loss models consider only wind speed and neglect storm size. These models may be inadequate in accurately predicting the losses of super-sized storms, such as Hurricane Sandy in 2012. In this study, we examined the dependences of normalized US hurricane loss on both wind speed and storm size for 73 tropical cyclones that made landfall in the US from 1988 through 2012. A multi-variate least squares regression is used to construct a hurricane loss model using both wind speed and size as predictors. Using maximum wind speed and size together captures more variance of losses than using wind speed or size alone. It is found that normalized hurricane loss (L) approximately follows a power law relation with maximum wind speed (V-max) and size (R), L=10(c)V(max)(a)R(b), with c determining an overall scaling factor and the exponents a and b generally ranging between 4-12 and 2-4 respectively. Both a and b tend to increase with stronger wind speed. Hurricane Sandy's size was about three times of the average size of all hurricanes analyzed. Based on the bi-variate regression model that explains the most variance for hurricanes, Hurricane Sandy's loss would be approximately 20 times smaller if its size were of the average size with maximum wind speed unchanged. It is important to revise conventional empirical hurricane loss models that are only dependent on maximum wind speed to include both maximum wind speed and size as predictors. C1 [Zhai, Alice R.] La Canada High Sch, La Canada Flintridge, CA 91011 USA. [Jiang, Jonathan H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Zhai, AR (reprint author), La Canada High Sch, 4463 Oak Grove Dr, La Canada Flintridge, CA 91011 USA. EM Jonathan.H.Jiang@jpl.nasa.gov NR 28 TC 7 Z9 8 U1 2 U2 15 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 JUN PY 2014 VL 9 IS 6 AR 064019 DI 10.1088/1748-9326/9/6/064019 PG 9 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AP1JM UT WOS:000341825200021 ER PT J AU Zscheischler, J Michalak, AM Schwalm, C Mahecha, MD Huntzinger, DN Reichstein, M Berthier, G Ciais, P Cook, RB El-Masri, B Huang, MY Ito, A Jain, A King, A Lei, HM Lu, CQ Mao, JF Peng, SS Poulter, B Ricciuto, D Shi, XY Tao, B Tian, HQ Viovy, N Wang, WL Wei, YX Yang, J Zeng, N AF Zscheischler, Jakob Michalak, Anna M. Schwalm, Christopher Mahecha, Miguel D. Huntzinger, Deborah N. Reichstein, Markus Berthier, Gwenaelle Ciais, Philippe Cook, Robert B. El-Masri, Bassil Huang, Maoyi Ito, Akihiko Jain, Atul King, Anthony Lei, Huimin Lu, Chaoqun Mao, Jiafu Peng, Shushi Poulter, Benjamin Ricciuto, Daniel Shi, Xiaoying Tao, Bo Tian, Hanqin Viovy, Nicolas Wang, Weile Wei, Yaxing Yang, Jia Zeng, Ning TI Impact of large-scale climate extremes on biospheric carbon fluxes: An intercomparison based on MsTMIP data SO GLOBAL BIOGEOCHEMICAL CYCLES LA English DT Article ID NET PRIMARY PRODUCTION; TERRESTRIAL BIOSPHERE; TROPICAL FORESTS; FUTURE CLIMATE; RAIN-FORESTS; DROUGHT; MODEL; CYCLE; RESPIRATION; TEMPERATURE AB Understanding the role of climate extremes and their impact on the carbon (C) cycle is increasingly a focus of Earth system science. Climate extremes such as droughts, heat waves, or heavy precipitation events can cause substantial changes in terrestrial C fluxes. On the other hand, extreme changes in C fluxes are often, but not always, driven by extreme climate conditions. Here we present an analysis of how extremes in temperature and precipitation, and extreme changes in terrestrial C fluxes are related to each other in 10 state-of-the-art terrestrial carbon models, all driven by the same climate forcing. We use model outputs from the North American Carbon Program Multi-scale Synthesis and Terrestrial Model Intercomparison Project (MsTMIP). A global-scale analysis shows that both droughts and heat waves translate into anomalous net releases of CO2 from the land surface via different mechanisms: Droughts largely decrease gross primary production (GPP) and to a lower extent total respiration (TR), while heat waves slightly decrease GPP but increase TR. Cold and wet periods have a smaller opposite effect. Analyzing extremes in C fluxes reveals that extreme changes in GPP and TR are often caused by strong shifts in water availability, but for extremes in TR shifts in temperature are also important. Extremes in net CO2 exchange are equally strongly driven by deviations in temperature and precipitation. Models mostly agree on the sign of the C flux response to climate extremes, but model spread is large. In tropical forests, C cycle extremes are driven by water availability, whereas in boreal forests temperature plays a more important role. Models are particularly uncertain about the C flux response to extreme heat in boreal forests. C1 [Zscheischler, Jakob; Mahecha, Miguel D.; Reichstein, Markus] Max Planck Inst Biogeochem, D-07745 Jena, Germany. [Zscheischler, Jakob; Michalak, Anna M.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA USA. [Zscheischler, Jakob] Max Planck Inst Intelligent Syst, Tubingen, Germany. [Schwalm, Christopher; Huntzinger, Deborah N.] No Arizona Univ, Sch Earth Sci & Environm Sustainabil, Flagstaff, AZ 86011 USA. [Berthier, Gwenaelle; Ciais, Philippe; Peng, Shushi; Viovy, Nicolas] Lab Sci Climat & Environm, Gif Sur Yvette, France. [Cook, Robert B.; King, Anthony; Ricciuto, Daniel] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. [El-Masri, Bassil; Jain, Atul; Mao, Jiafu; Shi, Xiaoying; Wei, Yaxing] Univ Illinois, Dept Atmospher Sci, Urbana, IL USA. [Huang, Maoyi] Pacific NW Natl Lab, Atmospher & Global Change Div, Richland, WA 99352 USA. [Ito, Akihiko] Natl Inst Environm Studies, Tsukuba, Ibaraki, Japan. [Lei, Huimin] Tsinghua Univ, Dept Hydraul Engn, Beijing 100084, Peoples R China. [Lu, Chaoqun; Tao, Bo; Tian, Hanqin; Yang, Jia] Auburn Univ, Int Ctr Climate & Global Change Res, Auburn, AL 36849 USA. [Lu, Chaoqun; Tao, Bo; Tian, Hanqin; Yang, Jia] Auburn Univ, Sch Forestry & Wildlife Sci, Auburn, AL 36849 USA. [Peng, Shushi] CNRS, Lab Glaciol & Geophys Environm, Grenoble, France. [Peng, Shushi] Univ Grenoble Alpes, Grenoble, France. [Poulter, Benjamin] Montana State Univ, Dept Ecol, Bozeman, MT 59717 USA. [Wang, Weile] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Zeng, Ning] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. RP Zscheischler, J (reprint author), Max Planck Inst Biogeochem, D-07745 Jena, Germany. EM jzsch@bgc-jena.mpg.de RI Tian, Hanqin/A-6484-2012; Huang, Maoyi/I-8599-2012; Lei, Huimin/H-9596-2015; Mahecha, Miguel/F-2443-2010; Peng, Shushi/J-4779-2014; Ricciuto, Daniel/I-3659-2016; Yang, Jia/A-6483-2012; Jain, Atul/D-2851-2016; Mao, Jiafu/B-9689-2012 OI Cook, Robert/0000-0001-7393-7302; Poulter, Benjamin/0000-0002-9493-8600; Zscheischler, Jakob/0000-0001-6045-1629; Tian, Hanqin/0000-0002-1806-4091; Huang, Maoyi/0000-0001-9154-9485; Lei, Huimin/0000-0002-1175-2334; Mahecha, Miguel/0000-0003-3031-613X; Peng, Shushi/0000-0001-5098-726X; Ricciuto, Daniel/0000-0002-3668-3021; Yang, Jia/0000-0003-2019-9603; Jain, Atul/0000-0002-4051-3228; Mao, Jiafu/0000-0002-2050-7373 FU NASA ROSES [NNX10AG01A, NNH10AN681]; European Community [226701, 283080, 238366]; U.S. Department of Energy (DOE), Office of Science, Biological and Environmental Research; DOE [DE-AC05-00OR22725]; DOE's Office of Biological and Environmental Research; U.S. DOE [DE-AC05-76RLO1830] FX We thank Dominique Bachelet and Altaf Arain for helpful comments on the manuscript. Funding for the Multi-scale Synthesis and Terrestrial Model Intercomparison Project (MsTMIP; http://nacp.ornl.gov/MsTMIP.shtml) activity was provided through NASA ROSES grant NNX10AG01A. Data management support for preparing, documenting, and distributing model driver and output data was performed by the Modeling and Synthesis Thematic Data Center at Oak Ridge National Laboratory (ORNL; http://nacp.ornl.gov), with funding through NASA ROSES grant NNH10AN681. Finalized MsTMIP data products are archived at the ORNL DAAC (http://daac.ornl.gov). This is MsTMIP contribution 3. J.Z. is member of the International Max Planck Research School for Global Biogeochemical Cycles (IMPRS-gBGC) and acknowledges funding from the European Community's Seventh Framework Program (FP7 2007-2013) under the grant agreements 226701, 283080, and 238366. Acknowledgments for specific MsTMIP participating models is as follows. Biome-BGC code was provided by the Numerical Terradynamic Simulation Group at University of Montana. The computational facilities were provided by NASA Earth Exchange at NASA Ames Research Center. (CLM4 and GTEC) This research is supported in part by the U.S. Department of Energy (DOE), Office of Science, Biological and Environmental Research. Oak Ridge National Laboratory is managed by UT-BATTELLE for DOE under contract DE-AC05-00OR22725. (CLM4VIC) This research is supported in part by the U.S. Department of Energy (DOE), Office of Science, Biological and Environmental Research. CLM4VIC simulations were performed using the Environmental Molecular Sciences Laboratory (EMSL), a national scientific user facility sponsored by the DOE's Office of Biological and Environmental Research and located at Pacific Northwest National Laboratory. PNNL is operated for the U.S. DOE by BATTELLE Memorial Institute under contract DE-AC05-76RLO1830. The Dynamic Land Ecosystem Model (DLEM) developed in International Center for Climate and Global Change Research, Auburn University, has been supported by NASA Interdisciplinary Science Program (IDS), NASA Land Cover/ Land Use Change Program (LULUC), NASA Terrestrial Ecology Program, NASA Atmospheric Composition Modeling and Analysis Program (ACMAP), NSF Dynamics of Coupled Natural-Human System Program (CNH), Decadal and Regional Climate Prediction using Earth System Models (EaSM), DOE National Institute for Climate Change Research, USDA AFRI Program, and EPA STAR program. (LPJ-wsl) This work was conducted at LSCE, France, using a modified version of LPJ version 3.1 model, originally made available by the Potsdam Institute for Climate Impact Research. ORCHIDEE (Organizing Carbon and Hydrology In Dynamic Ecosystems) is a global land surface model developed at the IPSL (Institut Pierre Simon Laplace) in France. The simulations were performed with the support of the GhG Europe FP7 grant with computing facilities provided by LSCE (Laboratoire des Sciences du Climat et de l'Environnement) or TGCC (Tres Grand Centre de Calcul). VISIT was developed at the National Institute of Environmental Studies, Japan. This work was mostly conducted during a visiting stay at Oak Ridge National Laboratory. NR 80 TC 16 Z9 16 U1 4 U2 53 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 JUN PY 2014 VL 28 IS 6 BP 585 EP 600 DI 10.1002/2014GB004826 PG 16 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA AN5DI UT WOS:000340609400001 ER PT J AU Vasavada, AR Grotzinger, JP Arvidson, RE Calef, FJ Crisp, JA Gupta, S Hurowitz, J Mangold, N Maurice, S Schmidt, ME Wiens, RC Williams, RME Yingst, RA AF Vasavada, A. R. Grotzinger, J. P. Arvidson, R. E. Calef, F. J. Crisp, J. A. Gupta, S. Hurowitz, J. Mangold, N. Maurice, S. Schmidt, M. E. Wiens, R. C. Williams, R. M. E. Yingst, R. A. TI Overview of the Mars Science Laboratory mission: Bradbury Landing to Yellowknife Bay and beyond SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ROCKNEST AEOLIAN DEPOSIT; CHEMCAM INSTRUMENT SUITE; EVOLVED GAS-ANALYSIS; GALE CRATER; CURIOSITY ROVER; MARTIAN ATMOSPHERE; SPECTROMETER; CALIBRATION; ABUNDANCE; SYSTEM AB The Mars Science Laboratory mission reached Bradbury Landing in August 2012. In its first 500 sols, the rover Curiosity was commissioned and began its investigation of the habitability of past and present environments within Gale Crater. Curiosity traversed eastward toward Glenelg, investigating a boulder with a highly alkaline basaltic composition, encountering numerous exposures of outcropping pebble conglomerate, and sampling aeolian sediment at Rocknest and lacustrine mudstones at Yellowknife Bay. On sol 324, the mission turned its focus southwest, beginning a year-long journey to the lower reaches of Mt. Sharp, with brief stops at the Darwin and Cooperstown waypoints. The unprecedented complexity of the rover and payload systems posed challenges to science operations, as did a number of anomalies. Operational processes were revised to include additional opportunities for advance planning by the science and engineering teams. C1 [Vasavada, A. R.; Calef, F. J.; Crisp, J. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Grotzinger, J. P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Arvidson, R. E.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Gupta, S.] Univ London Imperial Coll Sci Technol & Med, Dept Earth Sci & Engn, London, England. [Hurowitz, J.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. [Mangold, N.] Lab Planetol & Geodynam Nantes, Nantes, France. [Maurice, S.] Univ Toulouse 3, CNRS, Obs, Inst Rech Astrophys & Planetol, F-31062 Toulouse, France. [Schmidt, M. E.] Brock Univ, Dept Earth Sci, St Catharines, ON L2S 3A1, Canada. [Wiens, R. C.] Los Alamos Natl Lab, Los Alamos, NM USA. [Williams, R. M. E.; Yingst, R. A.] Planetary Sci Inst, Tucson, AZ USA. RP Vasavada, AR (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM ashwin@jpl.nasa.gov RI Crisp, Joy/H-8287-2016 OI Crisp, Joy/0000-0002-3202-4416 FU National Aeronautics and Space Administration FX The MSL Science Team and all those who contributed to the design, development, testing, and operation of MSL are acknowledged for their roles in the mission's success. During early operations, the MSL Project Manager was Pete Theisinger, the Deputy Project Manager was Richard Cook, and the Mission Manager was Mike Watkins. Presently, the Project Manager is Jim Erickson and the Deputy Project Manager is Jennifer Trosper. Nicole Spanovich is the Science Operations Team Chief, and Andy Mishkin leads Integrated Planning and Execution. 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 53 TC 27 Z9 27 U1 5 U2 28 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 JUN PY 2014 VL 119 IS 6 BP 1134 EP 1161 DI 10.1002/2014JE004622 PG 28 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AN4CK UT WOS:000340535000003 ER PT J AU Jamieson, CS Dobrea, EZN Dalton, JB Pitman, KM Abbey, WJ AF Jamieson, C. S. Dobrea, E. Z. Noe Dalton, J. B., III Pitman, K. M. Abbey, W. J. TI The spectral variability of kieserite (MgSO4 center dot H2O) with temperature and grain size and its application to the Martian surface SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MAGNESIUM-SULFATE SALTS; REFLECTANCE SPECTRA; MU-M; PARTICLE-SIZE; WATER-CONTENT; MARS; MINERALS; SPECTROSCOPY; DEPENDENCE; STABILITY AB We spectrally characterize (lambda = 0.35-10 mu m) the low-humidity polymorph of kieserite (MgSO4 center dot H2O), which is abundant on Mars and likely present on Europa, at various grain sizes and temperatures (100-300 K) relevant to the surfaces of Mars and Europa. Compositional analysis of these surfaces often relies on remote sensing using imaging spectrometers such as Mars Reconnaissance Orbiter Compact Reconnaissance Imaging Spectrometer for Mars (CRISM), Mars Express Observatoire pour la Mineralogie, l'Eau, les Glaces et l'Activite, and Galileo Near-Infrared Mapping Spectrometer. To estimate surface abundances from these observations, well-characterized laboratory spectra are required for comparison. Several variables, including temperature and grain size, affect the observed spectra and must be quantified in the laboratory to more confidently evaluate the returned data. Certain spectral features of kieserite exhibit predictable variability with changes in temperature and grain size that may be exploited to better understand the nature of kieserite on the surface of Mars. For instance, trends in our spectral analysis suggest that absorption features centered at lambda < 3.0 mu m were primarily sensitive to temperature changes, while features at lambda > 3.0 mu m were additionally sensitive to grain size changes. We compare our laboratory spectra with selected CRISM data of suspected Martian kieserite and assess the inherent uncertainty that exists in using band center minima to determine surface composition. Incorporation of these temperature and grain size-specific spectra into linear mixture models of planetary surface spectra will improve the compositional interpretation and contribute to our understanding of surface geochemistry and chemical evolution. C1 [Jamieson, C. S.] SETI Inst, Mountain View, CA 94043 USA. [Jamieson, C. S.; Dalton, J. B., III; Abbey, W. J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Dobrea, E. Z. Noe; Pitman, K. M.] Planetary Sci Inst, Tucson, AZ USA. RP Jamieson, CS (reprint author), SETI Inst, Mountain View, CA 94043 USA. EM cjamieson@seti.org FU NASA's Mars Fundamental Research Program [NNX10AP78G]; National Aeronautics and Space Administration FX This work was supported by NASA's Mars Fundamental Research Program (NNX10AP78G; PI Pitman) and partly performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract to the National Aeronautics and Space Administration. Calibrated MRO CRISM data appear courtesy of the MRO CRISM team and the Planetary Data System. The authors would like to thank Robert Anderson of JPL for use of the X-ray diffractometer. This is PSI contribution No. 615. NR 72 TC 3 Z9 3 U1 0 U2 21 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 JUN PY 2014 VL 119 IS 6 BP 1218 EP 1237 DI 10.1002/2013JE004489 PG 20 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AN4CK UT WOS:000340535000006 ER PT J AU Litvak, ML Mitrofanov, IG Sanin, AB Lisov, D Behar, A Boynton, WV Deflores, L Fedosov, F Golovin, D Hardgrove, C Harshman, K Jun, I Kozyrev, AS Kuzmin, RO Malakhov, A Milliken, R Mischna, M Moersch, J Mokrousov, M Nikiforov, S Shvetsov, VN Stack, K Starr, R Tate, C Tret'yakov, VI Vostrukhin, A AF Litvak, M. L. Mitrofanov, I. G. Sanin, A. B. Lisov, D. Behar, A. Boynton, W. V. Deflores, L. Fedosov, F. Golovin, D. Hardgrove, C. Harshman, K. Jun, I. Kozyrev, A. S. Kuzmin, R. O. Malakhov, A. Milliken, R. Mischna, M. Moersch, J. Mokrousov, M. Nikiforov, S. Shvetsov, V. N. Stack, K. Starr, R. Tate, C. Tret'yakov, V. I. Vostrukhin, A. CA MSL Team TI Local variations of bulk hydrogen and chlorine-equivalent neutron absorption content measured at the contact between the Sheepbed and Gillespie Lake units in Yellowknife Bay, Gale Crater, using the DAN instrument onboard Curiosity SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID LABORATORYS DYNAMIC ALBEDO; MARS; CALIBRATION; ENVIRONMENT; SYSTEM AB Data gathered with the Dynamic Albedo of Neutron (DAN) instrument onboard rover Curiosity were analyzed for variations in subsurface neutron flux and tested for possible correlation with local geological context. A special DAN observation campaign was executed, in which 18 adjacent DAN active measurements were acquired every 0.75-1.0 m to search for the variations of subsurface hydrogen content along a 15 m traverse across geologic contacts between the Sheepbed and Gillespie Lake members of the Yellowknife Bay formation. It was found that several subunits in Sheepbed and Gillespie Lake could be characterized with different depth distributions of water-equivalent hydrogen (WEH) and different chlorine-equivalent abundance responsible for the distribution of neutron absorption elements. The variations of the average WEH at the top 60 cm of the subsurface are estimated at up to 2-3%. Chlorine-equivalent neutron absorption abundances ranged within 0.8-1.5%. The largest difference in WEH and chlorine-equivalent neutron absorption distribution is found between Sheepbed and Gillespie Lake. C1 [Litvak, M. L.; Mitrofanov, I. G.; Sanin, A. B.; Lisov, D.; Fedosov, F.; Golovin, D.; Kozyrev, A. S.; Kuzmin, R. O.; Malakhov, A.; Mokrousov, M.; Nikiforov, S.; Tret'yakov, V. I.; Vostrukhin, A.] RAS, Space Res Inst, Moscow 117901, Russia. [Behar, A.; Deflores, L.; Jun, I.; Mischna, M.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Boynton, W. V.; Harshman, K.] Univ Arizona, Tucson, AZ USA. [Hardgrove, C.; Moersch, J.; Tate, C.] Univ Tennessee, Knoxville, TN USA. [Kuzmin, R. O.] Vernadsky Inst Geochem & Analyt Chem, Moscow, Russia. [Milliken, R.] Brown Univ, Providence, RI 02912 USA. [Shvetsov, V. N.] Joint Inst Nucl Res, Dubna, Russia. [Stack, K.] CALTECH, Pasadena, CA 91125 USA. [Starr, R.] Catholic Univ Amer, Washington, DC 20064 USA. RP Litvak, ML (reprint author), RAS, Space Res Inst, Moscow 117901, Russia. EM litvak@mx.iki.rssi.ru RI Gonzalez, Rafael/D-1748-2009; Rodriguez-Manfredi, Jose/L-8001-2014; Ramos, Miguel/K-2230-2014 OI Rodriguez-Manfredi, Jose/0000-0003-0461-9815; Ramos, Miguel/0000-0003-3648-6818 NR 40 TC 8 Z9 8 U1 2 U2 11 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 JUN PY 2014 VL 119 IS 6 BP 1259 EP 1275 DI 10.1002/2013JE004556 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AN4CK UT WOS:000340535000008 ER PT J AU White, OL Schenk, PM Nimmo, F Hoogenboom, T AF White, Oliver L. Schenk, Paul M. Nimmo, Francis Hoogenboom, Trudi TI A new stereo topographic map of Io: Implications for geology from global to local scales SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID GALILEAN SATELLITES; HEAT-FLOW; INTERNAL STRUCTURE; TIDAL DISSIPATION; VOLCANIC ACTIVITY; ACTIVE VOLCANISM; MOUNTAINS; ERUPTION; SHAPE; LOKI AB We use Voyager and Galileo stereo pairs to construct the most complete stereo digital elevation model (DEM) of Io assembled to date, controlled using Galileo limb profiles. Given the difficulty of applying these two techniques to Io due to its anomalous surface albedo properties, we have experimented extensively with the relevant procedures in order to generate what we consider to be the most reliable DEMs. Our final stereo DEM covers similar to 75% of the globe, and we have identified a partial system of longitudinally arranged alternating basins and swells that correlates well to the distribution of mountain and volcano concentrations. We consider the correlation of swells to volcano concentrations and basins to mountain concentrations, to imply a heat flow distribution across Io that is consistent with the asthenospheric tidal heating model of Tackley et al. (2001). The stereo DEM reveals topographic signatures of regional-scale features including Loki Patera, Ra Patera, and the Tvashtar Paterae complex, in addition to previously unrecognized features including an similar to 1000 km diameter depression and a > 2000 km long topographic arc comprising mountainous and layered plains material. C1 [White, Oliver L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Schenk, Paul M.; Hoogenboom, Trudi] Lunar & Planetary Inst, Houston, TX 77058 USA. [Nimmo, Francis] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. RP White, OL (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM oliver.l.white@nasa.gov FU NASA Outer Planet Research Program; Lunar and Planetary Institute FX The supporting data included with this paper consist of a cube file of the Io DEM (which can be viewed by downloading ISIS3 from the USGS website: http://isis.astrogeology.usgs.gov/Installation/) and 18 tiff files of the limb and stereo topographic profiles and ground tracks for the Galileo limb profiles used to control the DEM. The authors wish to thank Michelle Kirchoff, Peter Thomas, David Williams, and Ashley Davies for their comments, which helped to improve this paper. This research was supported by funding from the NASA Outer Planet Research Program, as well as the Lunar and Planetary Institute. NR 58 TC 1 Z9 1 U1 2 U2 7 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 JUN PY 2014 VL 119 IS 6 BP 1276 EP 1301 DI 10.1002/2013JE004591 PG 26 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AN4CK UT WOS:000340535000009 ER PT J AU Kim, MHY Cucinotta, FA Nounu, HN Zeitlin, C Hassler, DM Rafkin, SCR Wimmer-Schweingruber, RF Ehresmann, B Brinza, DE Bottcher, S Bohm, E Burmeister, S Guo, JN Kohler, J Martin, C Reitz, G Posner, A Gomez-Elvira, J Harri, AM AF Kim, Myung-Hee Y. Cucinotta, Francis A. Nounu, Hatem N. Zeitlin, Cary Hassler, Donald M. Rafkin, Scot C. R. Wimmer-Schweingruber, Robert F. Ehresmann, Bent Brinza, David E. Boettcher, Stephan Boehm, Eckart Burmeister, Soenke Guo, Jingnan Koehler, Jan Martin, Cesar Reitz, Guenther Posner, Arik Gomez-Elvira, Javier Harri, Ari-Matti CA MSL Sci Team TI Comparison of Martian surface ionizing radiation measurements from MSL-RAD with Badhwar-O'Neill 2011/HZETRN model calculations SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID SPACE; TRANSPORT; MARS; CYCLE; CODE AB Dose rate measurements from Mars Science Laboratory-radiation assessment detector (MSL-RAD) for 300 sols on Mars are compared to simulation results using the Badhwar-O'Neill 2011 galactic cosmic ray (GCR) environment model and the high-charge and energy transport (HZETRN) code. For the nuclear interactions of primary GCR through Mars atmosphere and Curiosity rover, the quantum multiple scattering theory of nuclear fragmentation is used. Daily atmospheric pressure is measured at Gale Crater by the MSL Rover Environmental Monitoring Station. Particles impinging on top of the Martian atmosphere reach RAD after traversing varying depths of atmosphere that depend on the slant angles, and the model accounts for shielding of the RAD "E" detector (used for dosimetry) by the rest of the instrument. Simulation of average dose rate is in good agreement with RAD measurements for the first 200 sols and reproduces the observed variation of surface dose rate with changing heliospheric conditions and atmospheric pressure. Model results agree less well between sols 200 and 300 due to subtleties in the changing heliospheric conditions. It also suggests that the average contributions of albedo particles (charge number Z < 3) from Martian regolith comprise about 10% and 42% of the average daily point dose and dose equivalent, respectively. Neutron contributions to tissue-averaged effective doses will be reduced compared to point dose equivalent estimates because a large portion of the neutron point dose is due to low-energy neutrons with energies < 1 MeV, which do not penetrate efficiently to deep-seated tissues. However the exposures from neutrons to humans on Mars should become an important consideration in radiobiology research and risk assessment. C1 [Kim, Myung-Hee Y.; Nounu, Hatem N.] Wyle Sci Technol & Engn, Houston, TX 77058 USA. [Cucinotta, Francis A.] NASA Johnson Space Ctr, Houston, TX USA. [Cucinotta, Francis A.] Univ Nevada, Las Vegas, NV 89154 USA. [Zeitlin, Cary] SW Res Inst, Durham, NH USA. [Hassler, Donald M.; Rafkin, Scot C. R.; Ehresmann, Bent] SW Res Inst, Boulder, CO USA. [Wimmer-Schweingruber, Robert F.; Boettcher, Stephan; Boehm, Eckart; Burmeister, Soenke; Guo, Jingnan; Koehler, Jan; Martin, Cesar] Univ Kiel, Kiel, Germany. [Brinza, David E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Reitz, Guenther] German Aerosp Ctr DLR, Cologne, Germany. [Posner, Arik] NASA Headquarters, Washington, DC USA. [Gomez-Elvira, Javier] Ctr Astrobiol INTA CSIC, Madrid, Spain. [Harri, Ari-Matti] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. RP Kim, MHY (reprint author), Wyle Sci Technol & Engn, Houston, TX 77058 USA. EM myung-hee.y.kim@nasa.gov RI Gonzalez, Rafael/D-1748-2009; Rodriguez-Manfredi, Jose/L-8001-2014; Harri, Ari-Matti/C-7142-2012; Ramos, Miguel/K-2230-2014; OI Kim, Myung-Hee/0000-0001-5575-6858; Rodriguez-Manfredi, Jose/0000-0003-0461-9815; Harri, Ari-Matti/0000-0001-8541-2802; Ramos, Miguel/0000-0003-3648-6818; Posner, Arik/0000-0003-1572-8734 FU NASA (HEOMD) under Jet Propulsion Laboratory (JPL) [1273039]; Germany by the German Aerospace Center (DLR); DLR's Space Administration [50QM0501, 50QM1201]; NASA FX RAD is supported by NASA (HEOMD) under Jet Propulsion Laboratory (JPL) subcontract 1273039 to Southwest Research Institute and in Germany by the German Aerospace Center (DLR) and DLR's Space Administration grant 50QM0501 and 50QM1201 to the Christian-Albrechts-Universit at Kiel. Part of this research was carried out at JPL, California Institute of Technology, under a contract with NASA. We thank Jeff Simmonds, John Grotzinger, Joy Crisp, Ashwin Vasvada, and Helen Mortensen at JPL, Gale Allen, Michael Meyer, Chris Moore, Victoria Friedensen at NASA Headquarters, and Heiner Witte at DLR in Germany for their support of RAD. The data used in this paper are archived in the NASA Planetary Data System's Planetary Plasma Interactions Node at the University of California, Los Angeles. The archival volume includes the full binary raw data files, detailed descriptions of the structures therein, and higher-level data products in human-readable form. The PPI node is hosted at the following URL: http://ppi.pds.nasa.gov/. We appreciate helpful discussion in BO'11 with Dr. Patrick O'Neill at the NASA Johnson Space Center and in HZETRN with Dr. Francis Badavi at the NASA Langley Research Center. NR 34 TC 11 Z9 11 U1 2 U2 15 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 JUN PY 2014 VL 119 IS 6 BP 1311 EP 1321 DI 10.1002/2013JE004549 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AN4CK UT WOS:000340535000011 ER PT J AU Arvidson, RE Bellutta, P Calef, F Fraeman, AA Garvin, JB Gasnault, O Grant, JA Grotzinger, JP Hamilton, VE Heverly, M Iagnemma, KA Johnson, JR Lanza, N Le Mouelic, S Mangold, N Ming, DW Mehta, M Morris, RV Newsom, HE Renno, N Rubin, D Schieber, J Sletten, R Stein, NT Thuillier, F Vasavada, AR Vizcaino, J Wiens, RC AF Arvidson, R. E. Bellutta, P. Calef, F. Fraeman, A. A. Garvin, J. B. Gasnault, O. Grant, J. A. Grotzinger, J. P. Hamilton, V. E. Heverly, M. Iagnemma, K. A. Johnson, J. R. Lanza, N. Le Mouelic, S. Mangold, N. Ming, D. W. Mehta, M. Morris, R. V. Newsom, H. E. Renno, N. Rubin, D. Schieber, J. Sletten, R. Stein, N. T. Thuillier, F. Vasavada, A. R. Vizcaino, J. Wiens, R. C. TI Terrain physical properties derived from orbital data and the first 360 sols of Mars Science Laboratory Curiosity rover observations in Gale Crater SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID CHEMCAM INSTRUMENT SUITE; SURFACE-PROPERTIES; LASER-ABLATION; MISSION; UNIT AB Physical properties of terrains encountered by the Curiosity rover during the first 360 sols of operations have been inferred from analysis of the scour zones produced by Sky Crane Landing System engine plumes, wheel touch down dynamics, pits produced by Chemical Camera (ChemCam) laser shots, rover wheel traverses over rocks, the extent of sinkage into soils, and the magnitude and sign of rover-based slippage during drives. Results have been integrated with morphologic, mineralogic, and thermophysical properties derived from orbital data, and Curiosity-based measurements, to understand the nature and origin of physical properties of traversed terrains. The hummocky plains (HP) landing site and traverse locations consist of moderately to well-consolidated bedrock of alluvial origin variably covered by slightly cohesive, hard-packed basaltic sand and dust, with both embedded and surface-strewn rock clasts. Rock clasts have been added through local bedrock weathering and impact ejecta emplacement and form a pavement-like surface in which only small clasts (<5 to 10 cm wide) have been pressed into the soil during wheel passages. The bedded fractured (BF) unit, site of Curiosity's first drilling activity, exposes several alluvial-lacustrine bedrock units with little to no soil cover and varying degrees of lithification. Small wheel sinkage values (<1 cm) for both HP and BF surfaces demonstrate that compaction resistance countering driven-wheel thrust has been minimal and that rover slippage while traversing across horizontal surfaces or going uphill, and skid going downhill, have been dominated by terrain tilts and wheel-surface material shear modulus values. C1 [Arvidson, R. E.; Fraeman, A. A.; Stein, N. T.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Bellutta, P.; Calef, F.; Heverly, M.; Vasavada, A. R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Garvin, J. B.] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA. [Gasnault, O.] Univ Toulouse UPS OMP, CNRS, IRAP, Toulouse, France. [Grant, J. A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Grotzinger, J. P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Hamilton, V. E.] SW Res Inst, Boulder, CO USA. [Iagnemma, K. A.] MIT, Dept Mech Engn, Cambridge, MA 02139 USA. [Johnson, J. R.] Johns Hopkins Appl Phys Lab, Laurel, MD USA. [Lanza, N.; Wiens, R. C.] Los Alamos Natl Lab, Los Alamos, NM USA. [Le Mouelic, S.; Mangold, N.; Thuillier, F.] CNRS, UMR6112, LPGN, Nantes, France. [Le Mouelic, S.; Mangold, N.; Thuillier, F.] Univ Nantes, Nantes, France. [Ming, D. W.; Morris, R. V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Mehta, M.; Vizcaino, J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Newsom, H. E.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. [Renno, N.] Univ Michigan, Ann Arbor, MI 48109 USA. [Rubin, D.] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Schieber, J.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA. [Sletten, R.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA. RP Arvidson, RE (reprint author), Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. EM arvidson@wunder.wustl.edu RI Johnson, Jeffrey/F-3972-2015; OI Gasnault, Olivier/0000-0002-6979-9012 FU NASA FX We thank NASA for support for our work on MSL and CRISM, and we thank the science and engineering teams associated with the Mars Science Laboratory, HiRISE, CRISM, and THEMIS for planning and acquisition of the data used in this paper. Data are available from the NASA Planetary Data System Geosciences Node (http://pds-geosciences.wustl.edu/). NR 50 TC 11 Z9 11 U1 0 U2 16 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 JUN PY 2014 VL 119 IS 6 BP 1322 EP 1344 DI 10.1002/2013JE004605 PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AN4CK UT WOS:000340535000012 ER PT J AU Rafkin, SCR Zeitlin, C Ehresmann, B Hassler, D Guo, JN Kohler, J Wimmer-Schweingruber, R Gomez-Elvira, J Harri, AM Kahanpaa, H Brinza, DE Weigle, G Bottcher, S Bohm, E Burmeister, S Martin, C Reitz, G Cucinotta, FA Kim, MH Grinspoon, D Bullock, MA Posner, A AF Rafkin, Scot C. R. Zeitlin, Cary Ehresmann, Bent Hassler, Don Guo, Jingnan Koehler, Jan Wimmer-Schweingruber, Robert Gomez-Elvira, Javier Harri, Ari-Matti Kahanpaa, Henrik Brinza, David E. Weigle, Gerald Boettcher, Stephan Boehm, Eckart Burmeister, Soeenke Martin, Cesar Reitz, Gueenther Cucinotta, Francis A. Kim, Myung-Hee Grinspoon, David Bullock, Mark A. Posner, Arik CA MSL Sci Team TI Diurnal variations of energetic particle radiation at the surface of Mars as observed by the Mars Science Laboratory Radiation Assessment Detector SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MARTIAN ATMOSPHERE; CURIOSITY ROVER; COSMIC-RAYS; MODEL; ODYSSEY; ENVIRONMENT; NEUTRONS; FRAGMENTATION; VISUALIZATION; PRESSURE AB The Radiation Assessment Detector onboard the Mars Science Laboratory rover Curiosity is detecting the energetic particle radiation at the surface of Mars. Data collected over the first 350 Martian days of the nominal surface mission show a pronounced diurnal cycle in both the total dose rate and the neutral particle count rate. The diurnal variations detected by the Radiation Assessment Detector were neither anticipated nor previously considered in the literature. These cyclic variations in dose rate and count rate are shown to be the result of changes in atmospheric column mass driven by the atmospheric thermal tide that is characterized through pressure measurements obtained by the Rover Environmental Monitoring Station, also onboard the rover. In addition to bulk changes in the radiation environment, changes in atmospheric shielding forced by the thermal tide are shown to disproportionately affect heavy ions compared to H and He nuclei. C1 [Rafkin, Scot C. R.; Ehresmann, Bent; Hassler, Don; Bullock, Mark A.] SW Res Inst, Boulder, CO 80302 USA. [Zeitlin, Cary] SW Res Inst, Durham, NH USA. [Guo, Jingnan; Koehler, Jan; Wimmer-Schweingruber, Robert; Boettcher, Stephan; Boehm, Eckart; Burmeister, Soeenke; Martin, Cesar] Univ Kiel, Dept Extraterr Phys, Kiel, Germany. [Gomez-Elvira, Javier] Ctr Astrobiol CSIC INTA, Madrid, Spain. [Harri, Ari-Matti; Kahanpaa, Henrik] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. [Brinza, David E.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Weigle, Gerald] Big Head Endian, Burden, KS USA. [Reitz, Gueenther] German Aerosp Ctr, Cologne, Germany. [Cucinotta, Francis A.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Cucinotta, Francis A.] Univ Nevada, Las Vegas, NV 89154 USA. [Kim, Myung-Hee] Univ Space Res Assoc, Houston, TX USA. [Grinspoon, David] Lib Congress, Washington, DC 20540 USA. [Posner, Arik] NASA Headquarters, Washington, DC USA. RP Rafkin, SCR (reprint author), SW Res Inst, Boulder, CO 80302 USA. EM rafkin@boulder.swri.edu RI Ramos, Miguel/K-2230-2014; Gonzalez, Rafael/D-1748-2009; Rodriguez-Manfredi, Jose/L-8001-2014; Harri, Ari-Matti/C-7142-2012; OI Ramos, Miguel/0000-0003-3648-6818; Rodriguez-Manfredi, Jose/0000-0003-0461-9815; Harri, Ari-Matti/0000-0001-8541-2802; Kahanpaa, Henrik/0000-0001-9108-186X; Posner, Arik/0000-0003-1572-8734; Kim, Myung-Hee/0000-0001-5575-6858 FU NASA under JPL [1273039]; Germany by Deutsches Zentrum fur Luft-und Raumfahrt (DLR); DLR's Space Administration [50QM0501, 50QM1201]; National Aeronautics and Space Administration FX The authors are extremely grateful for the comments from the anonymous reviewers who greatly improved the manuscript. The data used in this paper may be retrieved from the NASA Planetary Data System. RAD is supported by NASA under JPL subcontract 1273039 to Southwest Research Institute and in Germany by Deutsches Zentrum fur Luft-und Raumfahrt (DLR) and DLR's Space Administration grants 50QM0501 and 50QM1201 to the Christian-Albrechts University, Kiel. A portion 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 43 TC 10 Z9 10 U1 2 U2 11 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 JUN PY 2014 VL 119 IS 6 BP 1345 EP 1358 DI 10.1002/2013JE004525 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AN4CK UT WOS:000340535000013 ER PT J AU Bridges, NT Calef, FJ Hallet, B Herkenhoff, KE Lanza, NL Le Mouelic, S Newman, CE Blaney, DL de Pablo, MA Kocurek, GA Langevin, Y Lewis, KW Mangold, N Maurice, S Meslin, PY Pinet, P Renno, NO Rice, MS Richardson, ME Sautter, V Sletten, RS Wiens, RC Yingst, RA AF Bridges, N. T. Calef, F. J. Hallet, B. Herkenhoff, K. E. Lanza, N. L. Le Mouelic, S. Newman, C. E. Blaney, D. L. de Pablo, M. A. Kocurek, G. A. Langevin, Y. Lewis, K. W. Mangold, N. Maurice, S. Meslin, P. -Y. Pinet, P. Renno, N. O. Rice, M. S. Richardson, M. E. Sautter, V. Sletten, R. S. Wiens, R. C. Yingst, R. A. TI The rock abrasion record at Gale Crater: Mars Science Laboratory results from Bradbury Landing to Rocknest SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID CHEMCAM INSTRUMENT SUITE; AEOLIAN PROCESSES; DESERT VARNISH; WIND EROSION; ORBITER DATA; SAND; VENTIFACTS; SITE; COATINGS; EARTH AB Ventifacts, rocks abraded by wind-borne particles, are found in Gale Crater, Mars. In the eastward drive from "Bradbury Landing" to "Rocknest," they account for about half of the float and outcrop seen by Curiosity's cameras. Many are faceted and exhibit abrasion textures found at a range of scales, from submillimeter lineations to centimeter-scale facets, scallops, flutes, and grooves. The drive path geometry in the first 100 sols of the mission emphasized the identification of abrasion facets and textures formed by westerly flow. This upwind direction is inconsistent with predictions based on models and the orientation of regional dunes, suggesting that these ventifact features formed from very rare high-speed winds. The absence of active sand and evidence for deflation in the area indicates that most of the ventifacts are fossil features experiencing little abrasion today. C1 [Bridges, N. T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Calef, F. J.; Blaney, D. L.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Hallet, B.; Sletten, R. S.] Univ Washington, Coll Environm, Dept Earth & Space Sci, Seattle, WA 98195 USA. [Herkenhoff, K. E.] US Geol Survey, Flagstaff, AZ 86001 USA. [Lanza, N. L.] Los Alamos Natl Lab, Los Alamos, NM USA. [Le Mouelic, S.; Mangold, N.; Wiens, R. C.] Univ Nantes, CNRS, UMR 6112, LPGNantes, Nantes, France. [Newman, C. E.; Richardson, M. E.] Ashima Res, Pasadena, CA USA. [de Pablo, M. A.] Univ Alcala de Henares, Madrid, Spain. [Kocurek, G. A.] Univ Texas Austin, Dept Geol Sci, Jackson Sch Geosci, Austin, TX USA. [Langevin, Y.] Univ Paris 11, Inst Astrophys Spatiale, Orsay, France. [Lewis, K. W.] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. [Maurice, S.; Meslin, P. -Y.; Pinet, P.] Univ Toulouse, CNRS, Inst Rech Astrophys & Planetol, Toulouse, France. [Renno, N. O.] Univ Michigan, Coll Engn, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Rice, M. S.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Sautter, V.] Lab Mineral & Cosmochim Museum, Paris, France. [Yingst, R. A.] Planetary Sci Inst, Tucson, AZ USA. RP Bridges, NT (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. EM nathan.bridges@jhuapl.edu RI Bridges, Nathan/D-6341-2016 FU Mars Exploration Program FX We are indebted to Hallie Gengl of JPL's OPGS Group for generating the Hottah orthorectified image. Reviews, comments, and suggestions from Lori Fenton and Laura Kerber significantly improved this paper and are gratefully acknowledged. Funding for this work in the U.S. was provided by the Mars Exploration Program to the MSL Project. NR 75 TC 11 Z9 11 U1 3 U2 15 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 JUN PY 2014 VL 119 IS 6 BP 1374 EP 1389 DI 10.1002/2013JE004579 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AN4CK UT WOS:000340535000015 ER PT J AU Pavlov, AA Pavlov, AK Ostryakov, VM Vasilyev, GI Mahaffy, P Steele, A AF Pavlov, A. A. Pavlov, A. K. Ostryakov, V. M. Vasilyev, G. I. Mahaffy, P. Steele, A. TI Alteration of the carbon and nitrogen isotopic composition in the Martian surface rocks due to cosmic ray exposure SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID METEORITE ALH84001; NOBLE-GASES; WEATHERING PRODUCTS; SNC METEORITES; MARS; EETA-79001; ATMOSPHERE; DIOXIDE; SPECTRA; HISTORY AB C-13/C-12 and N-15/N-14 isotopic ratios are pivotal for our understanding of the Martian carbon cycle, history of the Martian atmospheric escape, and origin of the organic compounds on Mars. Here we demonstrate that the carbon and nitrogen isotopic composition of the surface rocks on Mars can be significantly altered by the continuous exposure of Martian surface to cosmic rays. Cosmic rays can effectively produce C-13 and N-15 isotopes via spallation nuclear reactions on oxygen atoms in various Martian rocks. We calculate that in the top meter of the Martian rocks, the rates of production of both C-13 and N-15 due to galactic cosmic rays (GCRs) exposure can vary within 1.5-6 atoms/cm(3)/s depending on rocks' depth and chemical composition. We also find that the average solar cosmic rays can produce carbon and nitrogen isotopes at a rate comparable to GCRs in the top 5-10 cm of the Martian rocks. We demonstrate that if the total carbon content in a surface Martian rock is <10 ppm, then the "light," potentially "biological" C-13/C-12 ratio would be effectively erased by cosmic rays over 3.5 billion years of exposure. We found that for the rocks with relatively short exposure ages (e. g., 100 million years), cosmogenic changes in N-15/N-14 ratio are still very significant. We also show that a short exposure to cosmic rays of Allan Hills 84001 while on Mars can explain its high-temperature heavy nitrogen isotopic composition (N-15/N-14). Applications to Martian meteorites and the current Mars Science Laboratory mission are discussed. C1 [Pavlov, A. A.; Mahaffy, P.] NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Greenbelt, MD 20771 USA. [Pavlov, A. K.; Vasilyev, G. I.] Russian Acad Sci, AF Ioffe Physicotech Inst, St Petersburg 196140, Russia. [Pavlov, A. K.; Ostryakov, V. M.] St Petersburg State Polytech Univ, St Petersburg, Russia. [Steele, A.] Carnegie Inst Sci, Geophys Lab, Washington, DC USA. RP Pavlov, AA (reprint author), NASA, Goddard Space Flight Ctr, Planetary Environm Lab, Greenbelt, MD 20771 USA. EM Alexander.Pavlov@nasa.gov RI Vasilyev, Gennady/E-4843-2014 FU Program 22 "Fundamental problems in the studies and development of the Solar System" of the Russian Academy of Sciences FX Co-authors A. A. Pavlov and P. Mahaffy appreciate NASA's support to conduct this study. Contribution of co-authors A. K. Pavlov, V. M. Ostryakov, and G. I. Vasilyev was partially supported by Program 22 "Fundamental problems in the studies and development of the Solar System" of the Russian Academy of Sciences. NR 46 TC 1 Z9 1 U1 2 U2 20 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 JUN PY 2014 VL 119 IS 6 BP 1390 EP 1402 DI 10.1002/2014JE004615 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AN4CK UT WOS:000340535000016 ER PT J AU Viviano-Beck, CE Seelos, FP Murchie, SL Kahn, EG Seelos, KD Taylor, HW Taylor, K Ehlmann, BL Wisemann, SM Mustard, JF Morgan, MF AF Viviano-Beck, Christina E. Seelos, Frank P. Murchie, Scott L. Kahn, Eliezer G. Seelos, Kimberley D. Taylor, Howard W. Taylor, Kelly Ehlmann, Bethany L. Wisemann, Sandra M. Mustard, John F. Morgan, M. Frank TI Revised CRISM spectral parameters and summary products based on the currently detected mineral diversity on Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID RESOLUTION REFLECTANCE SPECTROSCOPY; REMOTE-SENSING IMPLICATIONS; OMEGA/MARS EXPRESS; SOUTHERN HIGHLANDS; USGS TETRACORDER; MAWRTH VALLIS; GLOBAL VIEW; ROCKS; DEPOSITS; SILICA AB The investigation of hyperspectral data from the Mars Reconnaissance Orbiter Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) and the Observatoire pour la Mineralogie, L'Eau, les Glaces et l'Activitie (OMEGA) on Mars Express has revealed an increasingly diverse suite of minerals present on the Martian surface. A revised set of 60 spectral parameters derived from corrected spectral reflectance at key wavelengths in CRISM targeted observations and designed to capture the known diversity of surface mineralogy on Mars is presented here as "summary products." Some of the summary products have strong heritage to OMEGA spectral parameter calculations; this paper also presents newly derived parameters that highlight locations with more recently discovered spectral signatures. Type locations for the diversity of currently identified mineral spectral signatures have been compiled into a library presented in this work. Our analysis indicates that the revised set of summary products captures the known spectral diversity of the surface, and successfully highlights and differentiates between locations with differing spectral signatures. The revised spectral parameter calculations and related products provide a useful tool for scientific interpretation and for future mission landing site selection and operations. C1 [Viviano-Beck, Christina E.; Seelos, Frank P.; Murchie, Scott L.; Kahn, Eliezer G.; Seelos, Kimberley D.; Taylor, Howard W.; Morgan, M. Frank] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Taylor, Kelly] Corning Inc, Corning, NY 14831 USA. [Ehlmann, Bethany L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Ehlmann, Bethany L.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Wisemann, Sandra M.; Mustard, John F.] Brown Univ, Providence, RI 02912 USA. RP Viviano-Beck, CE (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. EM Christina.Beck@jhuapl.edu RI Murchie, Scott/E-8030-2015; Viviano-Beck, Christina/F-3942-2015; Seelos, Kimberly/F-4647-2015; Morgan, Frank/C-5246-2016; Seelos, Frank/C-7875-2016 OI Murchie, Scott/0000-0002-1616-8751; Viviano-Beck, Christina/0000-0003-1601-2105; Seelos, Kimberly/0000-0001-7236-0580; Morgan, Frank/0000-0003-3166-7732; Seelos, Frank/0000-0001-9721-941X FU MRO Project FX The authors would like to thank the CRISM team for internal review of the updated summary products, particularly Janice Bishop, Jennifer Buz, Christopher Edwards, Tim Goudge, Laetitia Loncan, Mario Parente, Cedric Pilorget, and James Wray. John Carter provided pixel locations for the epidote observation, Richard Morris provided the hydroxyl ferric sulfate spectra, and David Humm provided guidance in the 1 m offset correction. Lastly, we would like to thank Stephane Le Mouelic and two anonymous reviewers for their thoughtful comments that improved this manuscript. This work was made possible through funding from the MRO Project to the CRISM team. NR 115 TC 27 Z9 27 U1 5 U2 23 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN PY 2014 VL 119 IS 6 BP 1403 EP 1431 DI 10.1002/2014JE004627 PG 29 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AN4CK UT WOS:000340535000017 ER PT J AU Li, F Choudhari, MM Duan, L Chang, CL AF Li, Fei Choudhari, Meelan M. Duan, Lian Chang, Chau-Lyan TI Nonlinear development and secondary instability of traveling crossflow vortices SO PHYSICS OF FLUIDS LA English DT Article ID 3-DIMENSIONAL BOUNDARY-LAYERS; DIRECT NUMERICAL-SIMULATION; TRANSITION; STABILITY; DISTURBANCES; MECHANISMS; TURBULENCE AB Building upon the prior research targeting the laminar breakdown mechanisms associated with stationary crossflow instability over a swept-wing configuration, this paper investigates the secondary instability of traveling crossflow modes as an alternate scenario for transition. For the parameter range investigated herein, this alternate scenario is shown to be viable unless the initial amplitudes of the traveling crossflow instability are lower than those of the stationary modes by considerably more than one order of magnitude. The linear growth predictions based on the secondary instability theory are found to agree well with both parabolized stability equations and direct numerical simulation, and the most significant discrepancies among the various predictions are limited to spatial regions of relatively weak secondary growth, i.e., regions where the primary disturbance amplitudes are smaller in comparison to their peak values. Nonlinear effects on secondary instability evolution are also investigated and found to be initially stabilizing when they first come into play. C1 [Li, Fei; Choudhari, Meelan M.; Chang, Chau-Lyan] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Duan, Lian] Missouri Univ Sci & Technol, Dept Mech & Aerosp Engn, Rolla, MO 65409 USA. RP Li, F (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM fei.li@nasa.gov; meelan.m.choudhari@nasa.gov; duanl@mst.edu; chau-lyan.chang@nasa.gov RI Choudhari, Meelan/F-6080-2017 OI Choudhari, Meelan/0000-0001-9120-7362 NR 37 TC 2 Z9 2 U1 0 U2 5 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-6631 EI 1089-7666 J9 PHYS FLUIDS JI Phys. Fluids PD JUN PY 2014 VL 26 IS 6 AR 064104 DI 10.1063/1.4883256 PG 19 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA AO2SG UT WOS:000341175200024 ER PT J AU Rame, E Zimmerli, GA AF Rame, Enrique Zimmerli, Gregory A. TI Analysis of capillary drainage from a flat solid strip SO PHYSICS OF FLUIDS LA English DT Article ID CHEMICALLY MICROPATTERNED SURFACES; WETTING LIQUID; FLOW; CORNERS AB A long and narrow solid strip coated with a thin liquid layer is used as a model of a generic fluid mass probe in a spacecraft propellant tank just after a small thruster firing. The drainage dynamics of the initial coating layer into the settled bulk fluid affects the interpretation of probe measurements as the sensors' signal depends strongly on whether a sensor is in contact with vapor or with liquid. We analyze the drainage under various conditions of zero-gravity (i.e., capillary drainage) and with gravity aligned with the strip length, corresponding to the thruster acceleration. Long-time analytical solutions are found for zero and non-zero gravity. In the case with gravity, an approximate solution is found using matched asymptotics. Estimates show that a thrust of 10(-3)g(0) significantly reduces drainage times. (C) 2014 AIP Publishing LLC. C1 [Rame, Enrique] NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. [Zimmerli, Gregory A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Rame, E (reprint author), NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. EM enrique.rame-1@nasa.gov FU National Aeronautics and Space Administration (NASA) Enabling Technology Development and Demonstration Program, through the Cryogenic Fluid Management Project Office FX This work was supported by the National Aeronautics and Space Administration (NASA) Enabling Technology Development and Demonstration Program, through the Cryogenic Fluid Management Project Office. We thank R. Balasubramaniam for probing discussions and paper review. NR 13 TC 0 Z9 0 U1 1 U2 3 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 JUN PY 2014 VL 26 IS 6 AR 062102 DI 10.1063/1.4879827 PG 14 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA AO2SG UT WOS:000341175200011 ER PT J AU Roth, ASG Bourdon, B Mojzsis, SJ Rudge, JF Guitreau, M Blichert-Toft, J AF Roth, Antoine S. G. Bourdon, Bernard Mojzsis, Stephen J. Rudge, John F. Guitreau, Martin Blichert-Toft, Janne TI Combined Sm-147,Sm-146-Nd-143,Nd-142 constraints on the longevity and residence time of early terrestrial crust SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS LA English DT Article ID NUVVUAGITTUQ SUPRACRUSTAL BELT; ACASTA GNEISS COMPLEX; 4.00-4.03 GA ORTHOGNEISSES; SOUTHERN WEST GREENLAND; NORTHWESTERN CANADA; CONTINENTAL-CRUST; ISOTOPE EVIDENCE; MAGMA-OCEAN; TRACE-ELEMENTS; EARLY EARTH AB Primordial silicate differentiation controlled the composition of Earth's oldest crust. Inherited Nd-142 anomalies in Archean rocks are vestiges of the mantle-crust differentiation before ca. 4300 Ma. Here we report new whole-rock Sm-147,Sm-146-Nd-143,Nd-142 data for the Acasta Gneiss Complex (AGC; Northwest Territories, Canada). Our Sm-147-Nd-143 data combined with literature data define an age of 3371 +/- 141 Ma (2 SD) and yield an initial epsilon Nd-143 of -5.6 +/- 2.1. These results are at odds with the Acasta zircon U-Pb record, which comprises emplacement ages of 3920-3960 Ma. Ten of our thirteen samples show Nd-142 deficits of -9.6 +/- 4.8 ppm (2 SD) relative to the modern Earth. The discrepancy between Nd-142 anomalies and a mid-Archean Sm-147-Nd-143 age can be reconciled with Nd isotope reequilibration of the AGC during metamorphic perturbations at ca. 3400 Ma. A model age of ca. 4310 Ma is derived for the early enrichment of the Acasta source. Two compositional end-members can be identified: a felsic component with Nd-142/Nd-144 identical to the modern Earth and a mafic component with Nd-142/Nd-144 as low as -14.1 ppm. The ca. 4310 Ma AGC source is similar to 200 Myr younger than those estimated for Nuvvuagittuq (northern Quebec) and Isua (Itsaq Gneiss Complex, West Greenland). The AGC does not have the same decoupled Nd-Hf isotope systematics as these other two terranes, which have been attributed to the crystallization of an early magma ocean. The Acasta signature rather is ascribed to the formation of Hadean crust that was preserved for several hundred Myr. Its longevity can be linked to Nd-142 evolution in the mantle and does not require slow mantle stirring times nor modification of its convective mode. C1 [Roth, Antoine S. G.] Swiss Fed Inst Technol, Inst Geochem & Petr, Zurich, Switzerland. [Bourdon, Bernard; Mojzsis, Stephen J.; Guitreau, Martin; Blichert-Toft, Janne] ENS Lyon, Lab Geol Lyon, Lyon, France. [Bourdon, Bernard; Mojzsis, Stephen J.; Guitreau, Martin; Blichert-Toft, Janne] UCBL, CNRS, UMR 5276, Lyon, France. [Mojzsis, Stephen J.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. [Mojzsis, Stephen J.] NASA, Lunar Sci Inst, Ctr Lunar Origin & Evolut, Washington, DC USA. [Mojzsis, Stephen J.] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Inst Geol & Geochem Res, Budapest, Hungary. [Rudge, John F.] Univ Cambridge, Dept Earth Sci, Bullard Labs, Cambridge CB2 3EQ, England. [Guitreau, Martin] Univ New Hampshire, Dept Earth Sci, CEPS, Durham, NH 03824 USA. RP Roth, ASG (reprint author), Univ Bern, Inst Phys, Bern, Switzerland. EM antoine.roth@space.unibe.ch RI Blichert-Toft, Janne/C-8280-2012; Rudge, John/A-2653-2012 OI Roth, Antoine/0000-0001-9772-4643; Blichert-Toft, Janne/0000-0002-4932-4079; Rudge, John/0000-0002-9399-7166 FU ETH; NASA Exobiology and Evolutionary Biology Program (Investigating the Hadean Earth); NASA Lunar Science Institute (Center for Lunar Origin and Evolution, CLOE); Laboratoire de Geologie de Lyon, Universite Claude Bernard Lyon 1; Hungarian Academy of Sciences; French Agence Nationale de la Recherche [ANR-10-BLAN-0603] FX We are indebted to W. Bleeker (Geological Survey of Canada) for discussions of the geological context of the Acasta rocks and advice in the course of field studies. N.L. Cates (University of Colorado) provided valuable data to unravel the geochemical relations of the samples. Insightful discussions with S. Labrosse, S. Jacobsen, and Y. Ueno helped to forge the ideas presented herein. This project was funded by an ETH internal grant to B. B. We thank C. Maden for maintenance of the mass spectrometer. S.J.M. acknowledges support from the NASA Exobiology and Evolutionary Biology Program (Investigating the Hadean Earth) and the NASA Lunar Science Institute (Center for Lunar Origin and Evolution, CLOE). Additional support to S.J.M. came from the Laboratoire de Geologie de Lyon, Universite Claude Bernard Lyon 1, and a Distinguished Professorship awarded by the Hungarian Academy of Sciences. J.B.T. received support from the French Agence Nationale de la Recherche (grant ANR-10-BLAN-0603 M&Ms-Mantle Melting-Measurements, Models, Mechanisms). We are especially grateful for the invaluable logistical assistance for work in the Acasta Gneiss Complex provided by the Geological Survey of Canada and the Northwest Territories Geoscience Field Office in Yellowknife by J. Ketchum and D. Irwin. We also thank an anonymous reviewer for providing a constructive review. NR 65 TC 19 Z9 19 U1 6 U2 38 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1525-2027 J9 GEOCHEM GEOPHY GEOSY JI Geochem. Geophys. Geosyst. PD JUN PY 2014 VL 15 IS 6 BP 2329 EP 2345 DI 10.1002/2014GC005313 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AN1RY UT WOS:000340362500016 ER PT J AU Tzortziou, M Herman, JR Ahmad, Z Loughner, CP Abuhassan, N Cede, A AF Tzortziou, Maria Herman, Jay R. Ahmad, Ziauddin Loughner, Christopher P. Abuhassan, Nader Cede, Alexander TI Atmospheric NO2 dynamics and impact on ocean color retrievals in urban nearshore regions SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID DISSOLVED ORGANIC-MATTER; OZONE MONITORING INSTRUMENT; CHESAPEAKE BAY; CHLOROPHYLL-A; AIR-QUALITY; SATELLITE-OBSERVATIONS; LIGHTNING NOX; DISCOVER-AQ; WATERS; ABSORPTION AB Urban nearshore regions are characterized by strong variability in atmospheric composition, associated with anthropogenic emissions and meteorological processes that influence the circulation and accumulation of atmospheric pollutants at the land-water interface. If not adequately corrected in satellite retrievals of ocean color, this atmospheric variability can impose a false impression of diurnal and seasonal changes in nearshore water quality and biogeochemical processes. Consideration of these errors is important for measurements from polar orbiting ocean color sensors but becomes critical for geostationary satellite missions having the capability for higher frequency and higher spatial resolution observations of coastal ocean dynamics. We examined variability in atmospheric NO2 over urban nearshore environments in the Eastern US, Europe, and Korea, using a new network of ground-based Pandora spectrometers and Aura-OMI satellite observations. Our measurements in the US and in Europe revealed clear diurnal and day-of-the-week patterns in total column NO2 (TCNO2), temporal changes as large as 0.8 DU within 4 h, and spatial variability as large as 0.7 DU within an area often covered by just a single OMI pixel. TCNO2 gradients were considerably stronger over the coastal cities of Korea. With a coarse resolution and an overpass at around 13: 30 local time, OMI cannot detect this strong variability in NO2, missing pollution peaks from industrial and rush hour activities. Observations were combined with air quality model simulations and radiative transfer calculations to estimate the impact of atmospheric NO2 variability on satellite retrievals of coastal ocean remote sensing reflectance and biogeochemical variables (i.e., chlorophyll and CDOM). C1 [Tzortziou, Maria; Loughner, Christopher P.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Herman, Jay R.; Abuhassan, Nader] Univ Maryland, Joint Ctr Earth Syst Technol, College Pk, MD 20742 USA. [Herman, Jay R.; Ahmad, Ziauddin; Abuhassan, Nader; Cede, Alexander] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ahmad, Ziauddin] Sci & Data Syst Inc, Silver Spring, MD USA. [Cede, Alexander] LuftBlick, Kreith, Austria. RP Tzortziou, M (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. EM martz@umd.edu OI Herman, Jay/0000-0002-9146-1632; Loughner, Christopher/0000-0002-3833-2014 FU National Aeronautics and Space Administration (NASA) DISCOVER-AQ project [NNX10AR39G]; NASA CBODAQ; [NASA.NNX10AQ79G]; [NASA.NNX11AP07G] FX This work was supported under the National Aeronautics and Space Administration (NASA) DISCOVER-AQ project (grant NNX10AR39G) and the NASA CBODAQ field campaign, with additional support from grants NASA.NNX10AQ79G and NASA.NNX11AP07G. The authors would like to thank Christian Retscher, James H. Crawford, Kenneth E. Pickering, Antonio Mannino, Jhoon Kim, Jae Kim, Jari Hovila, Johanna Tamminen, and two anonymous reviewers for their constructive comments and suggestions for improvement of the manuscript. The Pandora data are publically available on NASA's AVDC (Aura Validation Data Center) site (http://avdc.gsfc.nasa.gov/). NR 81 TC 3 Z9 3 U1 1 U2 12 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 JUN PY 2014 VL 119 IS 6 BP 3834 EP 3854 DI 10.1002/2014JC009803 PG 21 WC Oceanography SC Oceanography GA AN2KT UT WOS:000340414800034 ER PT J AU Hasson, A Delcroix, T Boutin, J Dussin, R Ballabrera-Poy, J AF Hasson, Audrey Delcroix, Thierry Boutin, Jacqueline Dussin, Raphael Ballabrera-Poy, Joaquim TI Analyzing the 2010-2011 La Nina signature in the tropical Pacific sea surface salinity using in situ data, SMOS observations, and a numerical simulation SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID EL-NINO; SOUTHERN-OSCILLATION; BARRIER-LAYER; TOGA DECADE; MIXED-LAYER; FRESH POOL; WARM POOL; PART II; OCEAN; VARIABILITY AB The tropical Pacific Ocean remained in a La Nina phase from mid-2010 to mid-2012. In this study, the 2010-2011 near-surface salinity signature of ENSO (El Nino-Southern Oscillation) is described and analyzed using a combination of numerical model output, in situ data, and SMOS satellite salinity products. Comparisons of all salinity products show a good agreement between them, with a RMS error of 0.2-0.3 between the thermosalinograph (TSG) and SMOS data and between the TSG and model data. The last 6 months of 2010 are characterized by an unusually strong tripolar anomaly captured by the three salinity products in the western half of the tropical Pacific. A positive SSS anomaly sits north of 10 degrees S (>0.5), a negative tilted anomaly lies between 10 degrees S and 20 degrees S and a positive one south of 20 degrees S. In 2011, anomalies shift south and amplify up to 0.8, except for the one south of 20 degrees S. Equatorial SSS changes are mainly the result of anomalous zonal advection, resulting in negative anomalies during El Nino (early 2010), and positive ones thereafter during La Nina. The mean seasonal and interannual poleward drift exports those anomalies toward the south in the southern hemisphere, resulting in the aforementioned tripolar anomaly. The vertical salinity flux at the bottom of the mixed layer tends to resist the surface salinity changes. The observed basin-scale La Nina SSS signal is then compared with the historical 1998-1999 La Nina event using both observations and modeling. C1 [Hasson, Audrey; Delcroix, Thierry] Univ Toulouse, LEGOS, CNRS, CNES,IRD,UMR 5566, Toulouse, France. [Boutin, Jacqueline] UPMC, CNRS, LOCEAN, IRD,MNHN,UMR 7159, Paris, France. [Dussin, Raphael] LEGI, Grenoble, France. [Ballabrera-Poy, Joaquim] ICM CSIC, Barcelona, Spain. RP Hasson, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Audrey.Hasson@legos.obs-mip.fr RI Delcroix, Thierry/I-6103-2016; Boutin, Jacqueline/M-2253-2016; OI Delcroix, Thierry/0000-0002-8850-4865; Ballabrera-Poy, Joaquim/0000-0002-1753-221X FU CNES/TOSCA SMOS-Ocean; ESA SMOS+SOS; [AYA2012-39356-C05-03] FX This work is a contribution to the ESA GLOSCAL SMOS Cal/Val project. It is supported by CNES/TOSCA SMOS-Ocean, by ESA SMOS+SOS projects, and by the Spanish project AYA2012-39356-C05-03. We benefited from numerous data sets made freely available, including those from the French SSS Observation Service (www.legos.obsmip.fr/observations/sss) and from the DRAKKAR model group (www.drakkarocean.eu). The in situ Analysis System (ISAS) was developed by LPO (CNRS/IFREMER/IRD/UBO) and products were made available by F. Gaillard (wwz.ifremer.fr/lpo/La-recherche/Projetsen-cours/GLOSCAL). The LOCEAN_v2013 SSS maps have been produced by LOCEAN/IPSL (UMR CNRS/UPMC/IRD/MNHN) laboratory which participates in the Ocean Salinity Expertise Center (CECOS) of Centre Aval de Traitement des Donnees SMOS (CATDS) at IFREMER, Plouzane, France (http://www.catds.fr/Products). NOAA_OI_SST_V2 data were provided by the NOAA/OAR/ERSL PSD, Boulder, Colordao, USA (http://www.esrl.noaa.gov/psd/). The programming support of N. Martin and O. Hernandez from LOCEAN in Paris regarding the SMOS data was deeply appreciated. We are thankful to the reviewers for their thoughtful comments, which greatly increased the quality of the present paper. NR 42 TC 12 Z9 12 U1 1 U2 8 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 JUN PY 2014 VL 119 IS 6 BP 3855 EP 3867 DI 10.1002/2013JC009388 PG 13 WC Oceanography SC Oceanography GA AN2KT UT WOS:000340414800035 ER PT J AU Preston, A Merkowitz, S AF Preston, Alix Merkowitz, Stephen TI Comparison of fabrication techniques for hollow retroreflectors SO OPTICAL ENGINEERING LA English DT Article DE optics; hollow retroreflectors; fabrication techniques; hydroxide-catalysis bonding; epoxy ID SPACE AB Despite the wide usage of hollow retroreflectors, there is limited literature involving their fabrication techniques and only two documented construction methods could be found. One consists of an adjustable fixture that allows for the independent alignment of each mirror, while the other consists of a modified solid retroreflector that is used as a mandrel. Although both methods were shown to produce hollow retroreflectors with arc second dihedral angle errors, a comparison and analysis of each method could not be found, which makes it difficult to ascertain which method would be better suited to use for precision-aligned retroreflectors. Although epoxy bonding is generally the preferred method to adhere the three mirrors, a relatively new method known as hydroxidecatalysis bonding (HCB) presents several potential advantages over epoxy bonding. HCB has been used to bond several optical components for space-based missions, but has never been applied for construction of hollow retroreflectors. We examine the benefits and limitations of each bonding fixture as well as the present results and analysis of hollow retroreflectors made using both epoxy and HCB techniques. (c) 2014 Society of Photo-Optical Instrumentation Engineers (SPIE) C1 [Preston, Alix; Merkowitz, Stephen] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Merkowitz, S (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM stephen.m.merkowitz@nasa.gov NR 19 TC 0 Z9 0 U1 1 U2 4 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 JUN PY 2014 VL 53 IS 6 AR 065107 DI 10.1117/1.OE.53.6.065107 PG 6 WC Optics SC Optics GA AN5ZR UT WOS:000340672800035 ER PT J AU Behrangi, A Tian, YD Lambrigtsen, BH Stephens, GL AF Behrangi, Ali Tian, Yudong Lambrigtsen, Bjorn H. Stephens, Graeme L. TI What does CloudSat reveal about global land precipitation detection by other spaceborne sensors? SO WATER RESOURCES RESEARCH LA English DT Article ID MICROWAVE SOUNDING UNIT; PASSIVE MICROWAVE; CLASSIFICATION-SYSTEM; TROPICAL RAINFALL; SATELLITE; RADAR; ALGORITHM; STATES; WATER; INFORMATION AB Current orbital land precipitation products have serious shortcomings in detecting light rain and snowfall, the most frequent types of global precipitation. The missed precipitation is then propagated into the merged precipitation products that are widely used. Precipitation characteristics such as frequency and intensity and their regional distribution are expected to change in a warming climate. It is important to accurately capture those characteristics to understand and model the current state of the Earth's climate and predict future changes. In this work, the precipitation detection performance of a suite of precipitation sensors, commonly used in generating the merged precipitation products, are investigated. The high sensitivity of CloudSat Cloud Profiling Radar (CPR) to liquid and frozen hydrometeors enables superior estimates of light rainfall and snowfall within 80 degrees S-80 degrees N. Three years (2007-2009) of CloudSat precipitation data were collected to construct a climatology reference for guiding our analysis. In addition, auxiliary data such as infrared brightness temperature, surface air temperature, and cloud types were used for a more detailed assessment. The analysis shows that no more than 50% of the tropical (40 degrees S-40 degrees N) precipitation occurrence is captured by the current suite of precipitation measuring sensors. Poleward of 50 degrees latitude, a combination of various factors such as an abundance of light rainfall, snowfall, shallow precipitation-bearing clouds, and frozen surfaces reduces the space-based precipitation detection rate to less than 20%. This shows that for a better understanding of precipitation from space, especially at higher latitudes, there is a critical need to improve current precipitation retrieval techniques and sensors. C1 [Behrangi, Ali; Lambrigtsen, Bjorn H.; Stephens, Graeme L.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Tian, Yudong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Tian, Yudong] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA. RP Behrangi, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Ali.Behrangi@jpl.nasa.gov RI Measurement, Global/C-4698-2015 FU NASA's Weather program FX We acknowledge support from NASA's Weather program through Dr. Ramesh Kakar. 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 67 TC 13 Z9 13 U1 3 U2 20 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 JUN PY 2014 VL 50 IS 6 BP 4893 EP 4905 DI 10.1002/2013WR014566 PG 13 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA AN2QM UT WOS:000340430400020 ER PT J AU Gong, W Yang, DW Gupta, HV Nearing, G AF Gong, Wei Yang, Dawen Gupta, Hoshin V. Nearing, Grey TI Estimating information entropy for hydrological data: One-dimensional case SO WATER RESOURCES RESEARCH LA English DT Article ID RAINFALL PROBABILISTIC FORECASTS; WATER-SUPPLY MANAGEMENT; PARTIAL MUTUAL INFORMATION; PREDICTOR IDENTIFICATION; PARAMETER-ESTIMATION; RUNOFF MODELS; UNCERTAINTY; OPTIMIZATION; HISTOGRAMS; RESOURCES AB There has been a recent resurgence of interest in the application of Information Theory to problems of system identification in the Earth and Environmental Sciences. While the concept of entropy has found increased application, little attention has yet been given to the practical problems of estimating entropy when dealing with the unique characteristics of two commonly used kinds of hydrologic data: rainfall and runoff. In this paper, we discuss four important issues of practical relevance that can bias the computation of entropy if not properly handled. The first (zero effect) arises when precipitation and ephemeral streamflow data must be viewed as arising from a discrete-continuous hybrid distribution due to the occurrence of many zero values (e. g., days with no rain/no runoff). Second, in the widely used bin-counting method for estimation of PDF's, significant error can be introduced if the bin width is not carefully selected. The third (measurement effect) arises due to the fact that continuously varying hydrologic variables can typically only be observed discretely to some degree of precision. The Fourth (skewness effect) arises when the distribution of a variable is significantly skewed. Here we present an approach that can deal with all four of these issues, and test them with artificially generated and real hydrological data. The results indicate that the method is accurate and robust. C1 [Gong, Wei] Beijing Normal Univ, Coll Global Change & Earth Syst Sci, Beijing 100875, Peoples R China. [Gong, Wei; Yang, Dawen] Tsinghua Univ, State Key Lab Hydrosci & Engn, Beijing 100084, Peoples R China. [Gupta, Hoshin V.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. [Nearing, Grey] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Sci Applicat Int Corp, Greenbelt, MD 20771 USA. RP Gong, W (reprint author), Beijing Normal Univ, Coll Global Change & Earth Syst Sci, Beijing 100875, Peoples R China. EM gongwei2012@bnu.edu.cn RI Gupta, Hoshin/D-1642-2010; OI Gupta, Hoshin/0000-0001-9855-2839; Gong, Wei/0000-0003-3622-7090 FU National Science Foundation of China [51025931, 50939004, 51309011] FX Support for this study was provided by the National Science Foundation of China (contracts 51025931, 50939004, and 51309011). We would like to acknowledge the thorough and constructive suggestions from Steven Weijs, Nick van de Giesen, and another anonymous referee. Their comments significantly improved the quality of this paper. NR 40 TC 7 Z9 7 U1 3 U2 39 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 JUN PY 2014 VL 50 IS 6 BP 5003 EP 5018 DI 10.1002/2014WR015874 PG 16 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA AN2QM UT WOS:000340430400025 ER PT J AU Gupta, HV Nearing, GS AF Gupta, Hoshin V. Nearing, Grey S. TI Debates-The future of hydrological sciences: A (common) path forward? Using models and data to learn: A systems theoretic perspective on the future of hydrological science SO WATER RESOURCES RESEARCH LA English DT Editorial Material ID INFORMATION; CALIBRATION; UNCERTAINTY; SURFACE C1 [Gupta, Hoshin V.] Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. [Nearing, Grey S.] NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD USA. [Nearing, Grey S.] Sci Applicat Int Corp, Mclean, VA 22102 USA. RP Gupta, HV (reprint author), Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. EM hoshin.gupta@hwr.arizona.edu RI Gupta, Hoshin/D-1642-2010 OI Gupta, Hoshin/0000-0001-9855-2839 NR 27 TC 27 Z9 27 U1 4 U2 28 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 JUN PY 2014 VL 50 IS 6 BP 5351 EP 5359 DI 10.1002/2013WR015096 PG 9 WC Environmental Sciences; Limnology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA AN2QM UT WOS:000340430400050 ER PT J AU Miller, RL Schmidt, GA Nazarenko, LS Tausnev, N Bauer, SE DelGenio, AD Kelley, M Lo, KK Ruedy, R Shindell, DT Aleinov, I Bauer, M Bleck, R Canuto, V Chen, YH Cheng, Y Clune, TL Faluvegi, G Hansen, JE Healy, RJ Kiang, NY Koch, D Lacis, AA LeGrande, AN Lerner, J Menon, S Oinas, V Garcia-Pando, CP Perlwitz, JP Puma, MJ Rind, D Romanou, A Russell, GL Sato, M Sun, S Tsigaridis, K Unger, N Voulgarakis, A Yao, MS Zhang, JL AF Miller, Ron L. Schmidt, Gavin A. Nazarenko, Larissa S. Tausnev, Nick Bauer, Susanne E. DelGenio, Anthony D. Kelley, Max Lo, Ken K. Ruedy, Reto Shindell, Drew T. Aleinov, Igor Bauer, Mike Bleck, Rainer Canuto, Vittorio Chen, Yonghua Cheng, Ye Clune, Thomas L. Faluvegi, Greg Hansen, James E. Healy, Richard J. Kiang, Nancy Y. Koch, Dorothy Lacis, Andy A. LeGrande, Allegra N. Lerner, Jean Menon, Surabi Oinas, Valdar Garcia-Pando, Carlos Perez Perlwitz, Jan P. Puma, Michael J. Rind, David Romanou, Anastasia Russell, Gary L. Sato, Makiko Sun, Shan Tsigaridis, Kostas Unger, Nadine Voulgarakis, Apostolos Yao, Mao-Sung Zhang, Jinlun TI CMIP5 historical simulations (1850-2012) with GISS ModelE2 SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS LA English DT Article ID CLIMATE FORCING RECONSTRUCTIONS; GENERAL-CIRCULATION MODEL; TROPOSPHERIC OZONE; CLOUD MICROPHYSICS; TEMPERATURE TRENDS; GLOBAL TEMPERATURE; RELATIVE-HUMIDITY; PMIP SIMULATIONS; WATER-VAPOR; UPPER-OCEAN AB Observations of climate change during the CMIP5 extended historical period (1850-2012) are compared to trends simulated by six versions of the NASA Goddard Institute for Space Studies ModelE2 Earth System Model. The six models are constructed from three versions of the ModelE2 atmospheric general circulation model, distinguished by their treatment of atmospheric composition and the aerosol indirect effect, combined with two ocean general circulation models, HYCOM and Russell. Forcings that perturb the model climate during the historical period are described. Five-member ensemble averages from each of the six versions of ModelE2 simulate trends of surface air temperature, atmospheric temperature, sea ice and ocean heat content that are in general agreement with observed trends, although simulated warming is slightly excessive within the past decade. Only simulations that include increasing concentrations of long-lived greenhouse gases match the warming observed during the twentieth century. Differences in twentieth-century warming among the six model versions can be attributed to differences in climate sensitivity, aerosol and ozone forcing, and heat uptake by the deep ocean. Coupled models with HYCOM export less heat to the deep ocean, associated with reduced surface warming in regions of deepwater formation, but greater warming elsewhere at high latitudes along with reduced sea ice. All ensembles show twentieth-century annular trends toward reduced surface pressure at southern high latitudes and a poleward shift of the midlatitude westerlies, consistent with observations. C1 [Miller, Ron L.; Schmidt, Gavin A.; Nazarenko, Larissa S.; Tausnev, Nick; Bauer, Susanne E.; DelGenio, Anthony D.; Kelley, Max; Lo, Ken K.; Ruedy, Reto; Shindell, Drew T.; Aleinov, Igor; Bauer, Mike; Bleck, Rainer; Canuto, Vittorio; Chen, Yonghua; Cheng, Ye; Clune, Thomas L.; Faluvegi, Greg; Hansen, James E.; Healy, Richard J.; Kiang, Nancy Y.; Koch, Dorothy; Lacis, Andy A.; LeGrande, Allegra N.; Lerner, Jean; Oinas, Valdar; Garcia-Pando, Carlos Perez; Perlwitz, Jan P.; Puma, Michael J.; Rind, David; Romanou, Anastasia; Russell, Gary L.; Sato, Makiko; Sun, Shan; Tsigaridis, Kostas; Unger, Nadine; Voulgarakis, Apostolos; Yao, Mao-Sung] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Miller, Ron L.; Bauer, Mike; Bleck, Rainer; Garcia-Pando, Carlos Perez; Perlwitz, Jan P.; Romanou, Anastasia] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA. [Schmidt, Gavin A.; Nazarenko, Larissa S.; Bauer, Susanne E.; Shindell, Drew T.; Aleinov, Igor; Cheng, Ye; Faluvegi, Greg; Healy, Richard J.; Puma, Michael J.; Tsigaridis, Kostas] Columbia Univ, Ctr Climate Syst Res, New York, NY USA. [Tausnev, Nick; Kelley, Max; Lo, Ken K.; Ruedy, Reto; Chen, Yonghua; Oinas, Valdar; Yao, Mao-Sung] Trinnovim LLC, New York, NY USA. [Clune, Thomas L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Menon, Surabi] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Sun, Shan] MIT, Cambridge, MA 02139 USA. [Zhang, Jinlun] Univ Washington, Polar Sci Ctr, Appl Phys Lab, Seattle, WA 98195 USA. RP Miller, RL (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM RonL.Miller@nasa.gov RI Miller, Ron/E-1902-2012; Schmidt, Gavin/D-4427-2012; Bauer, Susanne/P-3082-2014; Healy, Richard/J-9214-2015; Sun, Shan/H-2318-2015; Shindell, Drew/D-4636-2012; Unger, Nadine/M-9360-2015; OI Schmidt, Gavin/0000-0002-2258-0486; Healy, Richard/0000-0002-5098-8921; Perez Garcia-Pando, Carlos/0000-0002-4456-0697 FU NASA Modeling, Analysis, and Prediction (MAP) Program; National Oceanic and Atmospheric Administration; Department of Energy; NOAA Climate and Global Change Program; NASA Earth Science Division FX We thank two anonymous reviewers for their substantial effort to improve this article. CMIP5 simulations with the GISS ModelE2 were made possible by the NASA High-End Computing (HEC) Program through the NASA Center for Climate Simulation (NCCS) at Goddard Space Flight Center. Development of ModelE2 was supported by the NASA Modeling, Analysis, and Prediction (MAP) Program with additional support from the National Science Foundation, the National Oceanic and Atmospheric Administration, and the Department of Energy. We thank Ellen Salmon and the NCCS staff for hosting and providing convenient access to the model output. MSU data are made available by Remote Sensing Systems and supported by the NOAA Climate and Global Change Program and the NASA Earth Science Division. Sea-ice area is provided by the National Snow and Ice Data Center. The Division of Marine and Atmospheric Research within the Commonwealth Scientific and Industrial Research Organisation provides analyses of ocean heat content and thermosteric sea level, while the NOAA Pacific Marine Environmental Laboratory makes available additional ocean heat content data. NCEP Reanalysis sea-level pressure is provided by the Physical Science Division of the NOAA Earth Science Research Laboratory. Model output analyzed in this study is available from the Earth System Grid Federation. NR 117 TC 25 Z9 25 U1 4 U2 34 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 JUN PY 2014 VL 6 IS 2 BP 441 EP 477 DI 10.1002/2013MS000266 PG 37 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AM7TR UT WOS:000340072100009 ER PT J AU Ofman, L Vinas, AF Maneva, Y AF Ofman, L. Vinas, A. F. Maneva, Y. TI Two-dimensional hybrid models of H+-He++ expanding solar wind plasma heating SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ION-CYCLOTRON WAVES; ULTRAVIOLET CORONAGRAPH SPECTROMETER; PROTON; SIMULATIONS; TURBULENCE; ACCELERATION; DRIVEN; ANISOTROPY; INSTABILITIES; CONSTRAINTS AB Preferential heating and acceleration of the solar wind He++ ions compared to protons in fast solar wind streams have been known for decades, thanks to in situ spacecraft measurements at 0.29-5 AU. Turbulent magnetic field fluctuations with approximate power law spectra have been observed as well. However, the exact causes of these processes are still not known due to the lack of detailed information on the magnetic field fluctuations and ion velocity distributions in the acceleration region of the solar wind. Here the collisionless heating processes in expanding solar wind plasma are investigated using 2-D hybrid modeling with parameters appropriate to the heliocentric distance of 10 R-S. In this study the ion dynamics is described kinetically, while electrons are treated as a background massless fluid in an expanding solar wind model. The source of free energy for the heating is introduced through an initial nonequilibrium state of the plasma with large He++ ion temperature anisotropy or with super-Alfvenic relative ion drift. We also employ an externally imposed spectrum of magnetic fluctuations in the frequency range below the proton gyroresonant frequency to heat the He++ ions. We investigate the effects of solar wind radial expansion by modeling several values of the expansion rate in a parametric study. We find that the preferential ion heating is attained in both nonexpanding and expanding solar wind models. Thus, the expansion has little effect on the preferential He++ ion heating by the processes considered here. Moreover, the expansion leads to faster evolution of the magnetosonic drift instability, reducing the drift velocity to lower values sooner, and the corresponding generation of the magnetic fluctuations that heat the ions, compared to the nonexpanding case. This is due to the reduction of the perpendicular particle velocities in the expanding (inflated) frame. For cases with little proton perpendicular heating, the solar wind expansion leads to the reduction of the proton temperature anisotropy to values less than one in the low-beta(p parallel to). solar wind acceleration region consistent with some observed values. However, this effect must be offset by perpendicular proton heating-likely by the same process that heats the He++ ions to be consistent with the full range of observed proton perpendicular temperature values. C1 [Ofman, L.; Maneva, Y.] CUA, Greenbelt, MD 20771 USA. [Ofman, L.; Vinas, A. F.; Maneva, Y.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ofman, L.] Tel Aviv Univ, Dept Geophys, Ramat Aviv, Israel. RP Ofman, L (reprint author), CUA, Greenbelt, MD 20771 USA. EM Leon.Ofman@nasa.gov FU NASA [NNX10AC56G] FX The authors would like to acknowledge support by NASA grant NNX10AC56G. NR 75 TC 11 Z9 11 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 JUN PY 2014 VL 119 IS 6 BP 4223 EP 4238 DI 10.1002/2013JA019590 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2VZ UT WOS:000339710300006 ER PT J AU Ngwira, CM Pulkkinen, A Kuznetsova, MM Glocer, A AF Ngwira, Chigomezyo M. Pulkkinen, Antti Kuznetsova, Maria M. Glocer, Alex TI Modeling extreme "Carrington-type" space weather events using three-dimensional global MHD simulations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID FIELD-ALIGNED CURRENTS; CORONAL MASS EJECTION; GROUND MAGNETIC-FIELD; RING CURRENT; HILL MODEL; SOLAR-WIND; ART.; MAGNETOSPHERE; IONOSPHERE; EARTH AB There is a growing concern over possible severe societal consequences related to adverse space weather impacts on man-made technological infrastructure. In the last two decades, significant progress has been made toward the first-principles modeling of space weather events, and three-dimensional (3-D) global magnetohydrodynamics (MHD) models have been at the forefront of this transition, thereby playing a critical role in advancing our understanding of space weather. However, the modeling of extreme space weather events is still a major challenge even for the modern global MHD models. In this study, we introduce a specially adapted University of Michigan 3-D global MHD model for simulating extreme space weather events with a Dst footprint comparable to the Carrington superstorm of September 1859 based on the estimate by Tsurutani et. al., (2003). Results are presented for a simulation run with "very extreme" constructed/idealized solar wind boundary conditions driving the magnetosphere. In particular, we describe the reaction of the magnetosphere-ionosphere system and the associated induced geoelectric field on the ground to such extreme driving conditions. The model setup is further tested using input data for an observed space weather event of Halloween storm October 2003 to verify the MHD model consistence and to draw additional guidance for future work. This extreme space weather MHD model setup is designed specifically for practical application to the modeling of extreme geomagnetically induced electric fields, which can drive large currents in ground-based conductor systems such as power transmission grids. Therefore, our ultimate goal is to explore the level of geoelectric fields that can be induced from an assumed storm of the reported magnitude, i.e., Dst similar to= -1600 nT. C1 [Ngwira, Chigomezyo M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Ngwira, Chigomezyo M.; Pulkkinen, Antti; Kuznetsova, Maria M.; Glocer, Alex] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. RP Ngwira, CM (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. EM chigongwira@yahoo.co.uk RI Glocer, Alex/C-9512-2012; ngwira, chigomezyo/D-7310-2012 OI Glocer, Alex/0000-0001-9843-9094; FU EPRI [EPRI-18403] FX The authors acknowledge colleagues Rebekah Evans, Lutz Rastatter, Mei-Ching Fok, and Anne Michelle Mandoza for their support toward this project. We also thank our EURISGIC partners (European Risk from Geomagnetically Induced Currents), an EU/FP7 Space Research project, for useful discussions on this work. The MHD results were processed for visualization at the Community Coordinated Modeling Center (CCMC) through the runs-on-request system. The CCMC is a multiagency partnership between NASA, AFMC, AFOSR, AFRL, AFWA, NOAA, NSF, and ONR. The SMWF/BATSRUS Models were developed at the University of Michigan. The first author C. M. Ngwira is supported through EPRI under contract EPRI-18403 administered by The Catholic University of America. The authors thank the reviewers for their invaluable contribution to this paper. NR 64 TC 12 Z9 12 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2014 VL 119 IS 6 BP 4456 EP 4474 DI 10.1002/2013JA019661 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2VZ UT WOS:000339710300022 ER PT J AU Hoilijoki, S Souza, VM Walsh, BM Janhunen, P Palmroth, M AF Hoilijoki, Sanni Souza, Vitor M. Walsh, Brian M. Janhunen, Pekka Palmroth, Minna TI Magnetopause reconnection and energy conversion as influenced by the dipole tilt and the IMF B-X SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID INTERPLANETARY MAGNETIC-FIELD; DAYSIDE MAGNETOPAUSE; DEPENDENCE; SIMULATIONS; INSTRUMENT AB We study the effect of Earth's dipole tilt angle and interplanetary magnetic field (IMF) B-x and By components on the location of reconnection and the energy conversion at the magnetopause. We simulate southward IMF satisfying both inward-and outward-type Parker spiral conditions during three different dipole tilt angles using a global magnetohydrodynamic model GUMICS-4. We find that positive (negative) B-x contributes to the magnetopause reconnection line location by moving northward (southward) and positive (negative) dipole tilt angle by moving it southward (northward). The tilt shifts the dayside load region toward the winter hemisphere and the summer cusp toward the equatorial plane. Magnetic flux hence piles effectively in the summer hemisphere leading to increased magnetopause currents that enhance the Poynting flux through the magnetopause. We find that the intensity of the energy conversion in the generators is strongly affected by the dipole tilt angle, whereas intensity in the load region is mainly affected by IMF B-x C1 [Hoilijoki, Sanni; Janhunen, Pekka; Palmroth, Minna] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. [Hoilijoki, Sanni] Univ Helsinki, Dept Phys, Helsinki, Finland. [Souza, Vitor M.] Natl Inst Space Res, INPE, Sao Jose Dos Campos, Brazil. [Souza, Vitor M.; Walsh, Brian M.] NASA, Goddard Space Flight Ctr, Heliospher Div, Greenbelt, MD 20771 USA. [Walsh, Brian M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Hoilijoki, S (reprint author), Finnish Meteorol Inst, FIN-00101 Helsinki, Finland. EM sanni.hoilijoki@fmi.fi RI Walsh, Brian/C-4899-2016 OI Walsh, Brian/0000-0001-7426-5413 FU Academy of Finland [138599]; ERC [200141-QuESpace] FX The research was supported by project 138599 of the Academy of Finland and ERC Starting grant agreement 200141-QuESpace. We thank Andrew Fazekerley for providing PEACE electron data for Double Star TC1 and Vassilis Angelopoulos for the use of THEMIS data. We also acknowledge use of NASA/GSFC's Space Physics Data Facility's OMNIWeb service, and OMNI data. NR 29 TC 5 Z9 5 U1 0 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 JUN PY 2014 VL 119 IS 6 BP 4484 EP 4494 DI 10.1002/2013JA019693 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2VZ UT WOS:000339710300024 ER PT J AU Holappa, L Mursula, K Asikainen, T Richardson, IG AF Holappa, L. Mursula, K. Asikainen, T. Richardson, I. G. TI Annual fractions of high-speed streams from principal component analysis of local geomagnetic activity SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SOLAR-CYCLE; MAGNETIC ACTIVITY; INDEX; WIND; SUBSTORMS; STORMS AB We study the latitudinal distribution of geomagnetic activity in 1966-2009 with local geomagnetic activity indices at 26 magnetic observatories. Using the principal component analysis method we find that more than 97% of the variance in annually averaged geomagnetic activity can be described by the two first principal components. The first component describes the evolution of the global geomagnetic activity, and has excellent correlation with, e. g., the Kp/Ap index. The second component describes the leading pattern by which the latitudinal distribution of geomagnetic activity deviates from the global average. We show that the second component is highly correlated with the relative (annual) fraction of high-speed streams (HSS) in solar wind. The latitudinal distribution of the second mode has a high maximum at auroral latitudes, a local minimum at subauroral latitudes and a low maximum at midlatitudes. We show that this distribution is related to the difference in the average location and intensity between substorms related to coronal mass ejections (CMEs) and HSSs. This paper demonstrates a new way to extract useful, quantitative information about the solar wind from local indices of geomagnetic activity over a latitudinally extensive network. C1 [Holappa, L.; Mursula, K.; Asikainen, T.] Univ Oulu, Dept Phys, ReSoLVE Ctr Excellence, FIN-90570 Oulu, Finland. [Richardson, I. G.] Univ Maryland, CRESST Dept Astron, College Pk, MD 20742 USA. [Richardson, I. G.] NASA GSFC, Explorat Univ Div, Greenbelt, MD USA. RP Holappa, L (reprint author), Univ Oulu, Dept Phys, ReSoLVE Ctr Excellence, FIN-90570 Oulu, Finland. EM lauri.holappa@oulu.fi RI Mursula, Kalevi/L-8952-2014; OI Mursula, Kalevi/0000-0003-4892-5056; Richardson, Ian/0000-0002-3855-3634; Holappa, Lauri/0000-0002-7394-6003 FU Academy of Finland [272157, 264994]; COST ES1005 (TOSCA) Network Action (especially Working Group 2) FX We acknowledge the financial support by the Academy of Finland to the ReSoLVE Center of Excellence (project 272157) and to project 264994. This work has benefited for collaborations and contacts within the COST ES1005 (TOSCA) Network Action (especially Working Group 2). The hourly magnetometer data were obtained from the World Data Center for Geomagnetism, Edinburgh (http://www.wdc.bgs.ac.uk/). The Ap index was obtained from World Data Center for Geomagnetism, Kyoto (http://http://wdc.kugi.kyoto-u.ac.jp/). The sunspot data were obtained from WDC-SILSO, Royal Observatory of Belgium, Brussels (http://sidc.be/silso/). The hourly values of the solar wind speed were obtained from the OMNI database (http://omniweb.gsfc.nasa.gov/). We thank Jesper W. Gjerloev for the SuperMAG-based list of substorms which is available at the SuperMAG website http://supermag.uib.no/. The list of the solar wind structures can be obtained by contacting Ian G. Richardson. NR 31 TC 8 Z9 8 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 JUN PY 2014 VL 119 IS 6 BP 4544 EP 4555 DI 10.1002/2014JA019958 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2VZ UT WOS:000339710300029 ER PT J AU Farrugia, CJ Gratton, FT Gnavi, G Torbert, RB Wilson, LB AF Farrugia, C. J. Gratton, F. T. Gnavi, G. Torbert, R. B. Wilson, Lynn B., III TI A vortical dawn flank boundary layer for near-radial IMF: Wind observations on 24 October 2001 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID KELVIN-HELMHOLTZ INSTABILITY; SOLAR-WIND; EARTHS MAGNETOSPHERE; MAGNETOPAUSE; STABILITY; TRANSPORT; SURFACE; PLASMA AB We present an example of a boundary layer tailward of the dawn terminator which is entirely populated by rolled-up flow vortices. Observations were made by Wind on 24 October 2001 as the spacecraft moved across the region at X similar to-13 R-E. Interplanetary conditions were steady with a near-radial interplanetary magnetic field (IMF). Approximately 15 vortices were observed over the 1.5 h duration of Wind's crossing, each lasting similar to 5 min. The rolling up is inferred from the presence of a hot tenuous plasma being accelerated to speeds higher than in the adjoining magnetosheath, a circumstance which has been shown to be a reliable signature of this in single-spacecraft observations. A blob of cold dense plasma was entrained in each vortex, at whose leading edge abrupt polarity changes of field and velocity components at current sheets were regularly observed. In the frame of the average boundary layer velocity, the dense blobs were moving predominantly sunward and their scale size along X was similar to 7.4 R-E. Inquiring into the generation mechanism of the vortices, we analyze the stability of the boundary layer to sheared flows using compressible magnetohydrodynamic Kelvin-Helmholtz theory with continuous profiles for the physical quantities. We input parameters from (i) the exact theory of magnetosheath flow under aligned solar wind field and flow vectors near the terminator and (ii) the Wind data. It is shown that the configuration is indeed Kelvin-Helmholtz (KH) unstable. This is the first reported example of KH-unstable waves at the magnetopause under a radial IMF. C1 [Farrugia, C. J.; Torbert, R. B.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Farrugia, C. J.; Torbert, R. B.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Gratton, F. T.; Gnavi, G.] Univ Buenos Aires, Inst Fis Plasma, Consejo Nacl Invest Cient & Tecn, Buenos Aires, DF, Argentina. [Gratton, F. T.] Pontificia Univ Catolica Argentina, Dept Fis, Fac Ciencias Fisicomatemat & Ingn, Buenos Aires, DF, Argentina. [Torbert, R. B.; Wilson, Lynn B., III] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. RP Farrugia, CJ (reprint author), Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. EM charlie.farrugia@unh.edu RI Wilson III, Lynn/D-4425-2012 OI Wilson III, Lynn/0000-0002-4313-1970 FU Argentine CONICET [11220090100608 PIP 2010-2012]; NASA [NNX10AQ29G, NNX13AP39G]; International Space Science Institute (ISSI), Switzerland FX We thank the referees for their many helpful comments. We thank all the providers of the data used here: Adam Szabo for the Wind magnetic field data and Dave McComas and Charles Smith for the ACE plasma and field data through NASA's cdaweb site. F.T.G. and G. G. are grateful for the support of the Argentine CONICET, grant 11220090100608 PIP 2010-2012. This work is supported by NASA grants NNX10AQ29G and NNX13AP39G. CJF and FTG acknowledge the support by the International Space Science Institute (ISSI), Switzerland and discussions within the ISSI team 214 on Flow-Driven Instabilities of the Sun-Earth System. NR 35 TC 2 Z9 2 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2014 VL 119 IS 6 BP 4572 EP 4590 DI 10.1002/2013JA019578 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2VZ UT WOS:000339710300031 ER PT J AU Gjerloev, JW Hoffman, RA AF Gjerloev, J. W. Hoffman, R. A. TI The large-scale current system during auroral substorms SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID FIELD-ALIGNED CURRENTS; MAGNETOSPHERIC SUBSTORMS; EXPANSIVE PHASE; IONOSPHERE; TIME; ELECTROJETS; EXCITATION; PHYSICS; MODEL; FLOW AB We present an empiricalmodel of the equivalent current systemin the ionosphere during the peak of a classical bulge-type auroral substorm. This model is derived from measurements made by similar to 110 ground magnetometer stations during 116 substorms. The data are temporally and spatially organized using global auroral images obtained by the Polar Visible Imaging System Earth Camera. The empirical equivalent current system displays three key features: a poleward shift of the westward electrojet connecting the postmidnight and premidnight components; a polar cap swirl; and significantly different magnitudes of the postmidnight and premidnight westward electrojets. This leads us to propose a two-wedge current system linking the ionosphere to the magnetosphere. The bulge current wedge is located in the premidnight region just equatorward of the open-closed field line boundary while another three-dimensional current system is located in the postmidnight region well within the auroral oval. We use Biot and Savart calculations and Tsyganenko mapping and show that this new model is a likely solution for the large-scale current system. C1 [Gjerloev, J. W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Gjerloev, J. W.] Univ Bergen, Birkeland Ctr, N-5020 Bergen, Norway. [Hoffman, R. A.] NASA, Goddard Space Flight Ctr, Heliophys Div, Greenbelt, MD 20771 USA. RP Gjerloev, JW (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. EM Jesper.Gjerloev@jhuapl.edu NR 44 TC 8 Z9 8 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 JUN PY 2014 VL 119 IS 6 BP 4591 EP 4606 DI 10.1002/2013JA019176 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2VZ UT WOS:000339710300032 ER PT J AU Li, W Thorne, RM Ma, Q Ni, B Bortnik, J Baker, DN Spence, HE Reeves, GD Kanekal, SG Green, JC Kletzing, CA Kurth, WS Hospodarsky, GB Blake, JB Fennell, JF Claudepierre, SG AF Li, W. Thorne, R. M. Ma, Q. Ni, B. Bortnik, J. Baker, D. N. Spence, H. E. Reeves, G. D. Kanekal, S. G. Green, J. C. Kletzing, C. A. Kurth, W. S. Hospodarsky, G. B. Blake, J. B. Fennell, J. F. Claudepierre, S. G. TI Radiation belt electron acceleration by chorus waves during the 17 March 2013 storm SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID VAN ALLEN PROBES; PHASE-SPACE DENSITY; RELATIVISTIC ELECTRONS; GEOMAGNETIC STORMS; INNER MAGNETOSPHERE; ENERGETIC PARTICLE; PLASMASPHERIC HISS; PC5 WAVES; PRECIPITATION; SCATTERING AB Local acceleration driven by whistler-mode chorus waves is fundamentally important for accelerating seed electron populations to highly relativistic energies in the outer radiation belt. In this study, we quantitatively evaluate chorus-driven electron acceleration during the 17 March 2013 storm, when the Van Allen Probes observed very rapid electron acceleration up to several MeVwithin similar to 12 hours. A clear radial peak in electron phase space density (PSD) observed near L*similar to 4 indicates that an internal local acceleration process was operating. We construct the global distribution of chorus wave intensity from the low-altitude electron measurements made by multiple Polar Orbiting Environmental Satellites (POES) satellites over a broad region, which is ultimately used to simulate the radiation belt electron dynamics driven by chorus waves. Our simulation results show remarkable agreement in magnitude, timing, energy dependence, and pitch angle distribution with the observed electron PSD near its peak location. However, radial diffusion and other loss processes may be required to explain the differences between the observation and simulation at other locations away from the PSD peak. Our simulation results, together with previous studies, suggest that local acceleration by chorus waves is a robust and ubiquitous process and plays a critical role in accelerating injected seed electrons with convective energies (similar to 100 keV) to highly relativistic energies (several MeV). C1 [Li, W.; Thorne, R. M.; Ma, Q.; Ni, B.; Bortnik, J.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA. [Baker, D. N.] Univ Colorado, Lab Atmospher & Space Res, Boulder, CO 80309 USA. [Spence, H. E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Reeves, G. D.] Los Alamos Natl Lab, Space Sci & Applicat Grp, Los Alamos, NM USA. [Kanekal, S. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Green, J. C.] Natl Ocean & Atmospher Adm, Natl Geophys Data Ctr, Boulder, CO USA. [Kletzing, C. A.; Kurth, W. S.; Hospodarsky, G. B.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Blake, J. B.; Fennell, J. F.; Claudepierre, S. G.] Aerosp Corp, Los Angeles, CA 90009 USA. RP Li, W (reprint author), Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA. EM moonli@atmos.ucla.edu RI Reeves, Geoffrey/E-8101-2011; OI Reeves, Geoffrey/0000-0002-7985-8098; Kletzing, Craig/0000-0002-4136-3348; Hospodarsky, George/0000-0001-9200-9878; Kurth, William/0000-0002-5471-6202 FU JHU/APL under NASA [967399, 921647, NAS5-01072]; EMFISIS [001057397: 01]; ECT [13-041]; NASA [NNX11AD75G, NNX11AR64G, NNX12AD12G, NNX13AI61G] FX This work was supported by JHU/APL contracts 967399 and 921647 under NASA's prime contract NAS5-01072. The analysis at UCLA was supported by the EMFISIS sub-award 1001057397: 01, ECT sub-award 13-041, NASA grants NNX11AD75G, NNX11AR64G, NNX12AD12G, and NNX13AI61G. We acknowledge the Van Allen Probes data from the EMFISIS instrument obtained from https://emfisis.physics.uiowa.edu/data/index and from the REPT and MagEIS instrument obtained from http://www.rbsp-ect.lanl.gov/data_pub/. We greatly appreciate the NOAA POES data obtained from http://satdat.ngdc.noaa.gov/sem/poes/data/. We also thank the World Data Center for Geomagnetism, Kyoto for providing SYM-H, AU and AL index (http://wdc.kugi.kyoto-u.ac.jp/aeasy/index.html), and the Space Physics Data Facility at the NASA Goddard Space Flight Center for providing the OMNI2 data (ftp://spdf.gsfc.nasa.gov/pub/data/omni/omni_cdaweb/). NR 60 TC 44 Z9 44 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 JUN PY 2014 VL 119 IS 6 BP 4681 EP 4693 DI 10.1002/2014JA019945 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2VZ UT WOS:000339710300038 ER PT J AU Weygand, JM Zesta, E Troshichev, O AF Weygand, J. M. Zesta, E. Troshichev, O. TI Auroral electrojet indices in the Northern and Southern Hemispheres: A statistical comparison SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CONJUGACY; SUBSTORM; ONSET; ARCS; AE AB The auroral electrojet (AE) index is traditionally derived from about 12 ground magnetometer observatories located around the average northern auroral oval location. The AE index calculation has only been performed with Northern Hemisphere data, because similar coverage in the Southern Hemisphere does not exist. In this study, eight southern auroral ground magnetometers and their near conjugate Northern Hemisphere counterparts are used to calculate conjugate AE indices for 274 days covering all four seasons from 2005 to 2010. The correlation coefficient between the northern and southern AE indices for many of the intervals is 0.65 indicating strong asymmetries between the two hemispheres. We compare our conjugate AE indices with the standard AE index and find a number of asymmetries because of station coverage gaps in the southern and northern arrays. The mean difference between the southern and northern AE indices is largest during northern summer season, and the smallest mean difference occurs in the spring. The mean differences between the southern and conjugate northern AE indices are about 31 nT with the largest differences occurring in the midnight magnetic local time (MLT) sector. We suggest that these differences may be a function of seasonal, MLT, and ionospheric effects. We also find a difference in the southern and northern AE related to UT and believe that this pertains to the distribution of the magnetometers. The fact that a difference between the southern and northern AE indices exists indicates the importance of examining geomagnetic activity in both hemispheres when considering magnetospheric phenomena. C1 [Weygand, J. M.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. [Zesta, E.] NASA GSFC, Greenbelt, MD USA. [Troshichev, O.] Arctic & Antarctica Res Inst, St Petersburg, Russia. RP Weygand, JM (reprint author), Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA. EM jweygand@igpp.ucla.edu FU NSF Antarctic Aeronomy and Astrophysics, Office of Polar Programs [ANT-1043621] FX This work was supported by NSF Antarctic Aeronomy and Astrophysics, Office of Polar Programs grant ANT-1043621. We would also like to thank: GIMA = Geophysical Institute Magnetometer Array for the data from the BET station; the THEMIS team for the data from SNKQ and KIAN. DMI = the Danish Meteorological Institute for data from AMK, NAQ, and SCO; BAS = British Antarctic Survey for data from the HBA and M78-337 stations; Science Institute, University of Iceland for the data from LVR; Geoscience Australia for data from MCQ and MAW; INTERMAGNET = International Real-time Magnetic Observatory for data from PBQ; Pieter Stoker for data from the SNA magnetometer; IMAGE = International Monitor for Auroral Geomagnetic Effects for the data from SOR and BJN; the WDC for Aurora in National Institute of Polar Research in Japan for data from the HLL and SYO stations; and the WDC for geomagnetism, Kyoto for the standard AE index data. Finally, we want to give special thanks to Masahito Nose for providing us with some detailed plots of the magnetometer data that contributed to the standard AE index we used. NR 26 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 JUN PY 2014 VL 119 IS 6 BP 4819 EP 4840 DI 10.1002/2013JA019377 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2VZ UT WOS:000339710300048 ER PT J AU Jiang, GY Wang, WB Xu, JY Yue, J Burns, AG Lei, JH Mlynczak, MG Rusell, JM AF Jiang, Guoying Wang, Wenbin Xu, Jiyao Yue, Jia Burns, Alan G. Lei, Jiuhou Mlynczak, Martin G. Rusell, James M., III TI Responses of the lower thermospheric temperature to the 9 day and 13.5 day oscillations of recurrent geomagnetic activity SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID GENERAL-CIRCULATION MODEL; LONGITUDINAL VARIATION; INTERACTION REGIONS; FIELD VARIABILITY; SOLAR-CYCLE; IONOSPHERE; ELECTRODYNAMICS; MINIMUM; AU AB Responses of the lower thermospheric temperature to the 9 day and 13.5 day oscillations of recurrent geomagnetic activity and solar EUV radiation have been investigated using neutral temperature data observed by the TIMED/SABER (Thermosphere Ionosphere Mesosphere Energetics and Dynamics/Sounding of the Atmosphere using Broadband Emission Radiometry) instrument and numerical experiments by the NCAR-TIME-GCM (National Center for Atmospheric Research-thermosphere-ionosphere-mesosphere electrodynamics-general circulation model). The TIMED/SABER data analyzed were for the period from 2002 to 2007 during the declining phase of solar cycle 23. The observations show that the zonal mean temperature in the lower thermosphere oscillated with periods of near 9 and 13.5 days in the height range of 100-120 km. These oscillations were more strongly correlated with the recurrent geomagnetic activity than with the solar EUV variability of the same periods. The 9 day and 13.5 day oscillations of lower thermospheric temperature had greater amplitudes at high latitudes than at low latitudes; they also had larger amplitudes at higher altitudes, and the oscillations could penetrate down to similar to 105 km, depending on the strength of the recurrent geomagnetic activity for a particular time period. The data further show that the periodic responses of the lower thermospheric temperature to recurrent geomagnetic activity were different in the two hemispheres. In addition, numerical experiments have been carried out using the NCAR-TIME-GCM to investigate the causal relationship between the temperature oscillations and the geomagnetic activity and solar EUV variations of the same periods. Model simulations showed the same periodic oscillations as those seen in the observations when the real geomagnetic activity index, Kp, was used to drive the model. These numerical results show that recurrent geomagnetic activity is the main cause of the 9 day and 13.5 day variations in the lower thermosphere temperature, and the contribution from solar EUV variations is minor. Furthermore, we also found that consecutive coronal mass ejection events could cause long-duration enhancements in the lower thermospheric temperature that strengthen the 9 day and 13.5 day signals, and this kind of phenomenon mostly occurred between 2002 and 2005 during the declining phase of solar cycle 23. C1 [Jiang, Guoying; Xu, Jiyao] Chinese Acad Sci, State Key Lab Space Weather, Ctr Space Sci & Appl Res, Beijing, Peoples R China. [Wang, Wenbin; Burns, Alan G.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Yue, Jia; Rusell, James M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. [Lei, Jiuhou] Univ Sci & Technol China, CAS Key Lab Geospace Environm, Sch Earth & Space Sci, Hefei 230026, Peoples R China. [Mlynczak, Martin G.] NASA Langley Res Ctr, Hampton, VA USA. RP Jiang, GY (reprint author), Chinese Acad Sci, State Key Lab Space Weather, Ctr Space Sci & Appl Res, Beijing, Peoples R China. EM gyjiang@spaceweather.ac.cn RI Yue, Jia/D-8177-2011; Wang, Wenbin/G-2596-2013; Burns, Alan/L-1547-2013; Lei, Jiuhou/A-3015-2012 OI Wang, Wenbin/0000-0002-6287-4542; Lei, Jiuhou/0000-0002-4374-5083 FU National Science Foundation of China [41229001, 41274145, 41331069]; Chinese Academy of Sciences [KZZD-EW-01-2]; National Important basic Research Project of China [2011CB811405]; Specialized Research Fund for State Key Laboratories; National Science Foundation FX This work was supported by the National Science Foundation of China (41229001, 41274145, and 41331069), the Chinese Academy of Sciences (KZZD-EW-01-2), and the National Important basic Research Project of China (2011CB811405). This project is also supported by the Specialized Research Fund for State Key Laboratories. The National Center for Atmospheric Research is sponsored by the National Science Foundation. Special thanks for Yanhong Chen's helpful discussions. The SABER neutral temperature data can be downloaded from saber.gats-inc.com/Version_07/Level2A. NR 50 TC 2 Z9 2 U1 0 U2 13 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 JUN PY 2014 VL 119 IS 6 BP 4841 EP 4859 DI 10.1002/2013JA019406 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2VZ UT WOS:000339710300049 ER PT J AU Shi, Y Zesta, E AF Shi, Yong Zesta, Eftyhia TI Global-scale ionospheric flow and aurora precursors of auroral substorms: Coordinated SuperDARN and IMAGE/WIC observations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID PLASMA SHEET; MAGNETOTAIL; CONVECTION; SPACECRAFT; RECONNECTION; DYNAMICS; BURSTS; SYSTEM; ONSET; FUV AB We use global-scale polar cap flow vector measurements from the Super Dual Auroral Radar Network (SuperDARN) with the concurrent auroral observations from the Wideband Imaging Camera on board Imager for Magnetopause-to-Aurora Global Exploration (IMAGE/WIC) to study the polar cap flow and auroral precursors during a substorm onset on 26 December 2000. We show, for the first time, close connection between the dayside and nightside polar cap flow enhancements (with the enhanced dayside flow preceding the nightside one by several minutes) and the ensuing poleward boundary intensification (PBI)/streamer, and the later onset, forming a complete preonset sequence for a substorm onset. Our results supplement our previous study by providing further evidence that the dayside polar cap flow disturbance may be the key to initiate the whole process of a certain type of substorm by triggering reconnection somewhere in the tail via applied field (or flow) perturbations on the nightside plasma sheet boundary layer. Our results also indicate that a preexisting double oval structure is likely a favorable precondition for a certain type of substorm to be triggered by polar cap flow disturbance and the associated PBIs/streamers. On the other hand, not all our global-scale preonset auroral sequences support the recent revised onset scenario proposed by Nishimura et al. (2010a) using the all-sky imagers of the Time History of Events and Macroscale Interactions during Substorms mission. This suggests that the preceding PBI/streamer is not a sufficient condition to trigger a substorm. It may not even be a necessary condition considering the existence of various types of substorm onsets. C1 [Shi, Yong] US Air Force, Res Lab, NRC Res Associateship, Albuquerque, NM 87116 USA. [Shi, Yong] Univ New Mexico, Dept Elect & Comp Engn, Albuquerque, NM 87131 USA. [Zesta, Eftyhia] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. RP Shi, Y (reprint author), US Air Force, Res Lab, NRC Res Associateship, Albuquerque, NM 87116 USA. EM yongshi999@gmail.com FU NRC Research Associateship at AFRL; NASA [NNH09AL23I, NNX10AL30G] FX This work was supported in part by the NRC Research Associateship at AFRL and NASA grants NNH09AL23I and NNX10AL30G. The authors are grateful to the PIs of the SuperDARN radars and for the support of their national funding agencies. The authors acknowledge the PIs of the IMAGE FUV and the IMAGE magnetometer stations for the use of the global auroral images and magnetometer data. The authors also would like to thank the INTERMAGNET for providing related magnetometer data. NR 33 TC 4 Z9 4 U1 0 U2 12 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUN PY 2014 VL 119 IS 6 BP 4860 EP 4871 DI 10.1002/2013JA019175 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2VZ UT WOS:000339710300050 ER PT J AU Mierkiewicz, EJ Oliversen, RJ Roesler, FL Lupie, OL AF Mierkiewicz, E. J. Oliversen, R. J. Roesler, F. L. Lupie, O. L. TI High-resolution spectroscopy of the lunar sodium exosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ATMOSPHERE; MOON; LINES AB We have applied high-resolution Fabry-Perot spectroscopy to the study of the lunar sodium exosphere for the study of exospheric effective temperature and velocity variations. Observing from the National Solar Observatory McMath-Pierce Telescope, we used a dual-etalon Fabry-Perot spectrometer with a resolving power of 180,000 to measure line widths and Doppler shifts of the sodium D2 (5889.95 angstrom) emission line. Our field of view was 360 km, and measurements were made in equatorial and polar regions from 500 km to 3500 km off the limb. Data were obtained from full moon to 3 days following full moon (waning phase) in March 2009. Measured Doppler line widths within 1100 km of the sunlit east and south lunar limbs for observations between 5 and 40 degrees lunar phase imply effective temperatures ranging between 3260 +/- 190 and 1000 +/- 135 K. Preliminary line center analysis indicates velocity displacements between different locations off the lunar limb ranging between 100 and 600 m/s from the lunar rest velocity with a precision of +/- 20 to +/- 50 m/s depending on brightness. Based on the success of these exploratory observations, an extensive program has been initiated that is expected to constrain lunar atmospheric and surface-process modeling and help quantify source and escape mechanisms. C1 [Mierkiewicz, E. J.] Embry Riddle Aeronaut Univ, Dept Phys Sci, Daytona Beach, FL 32114 USA. [Oliversen, R. J.; Lupie, O. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Roesler, F. L.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. RP Mierkiewicz, EJ (reprint author), Embry Riddle Aeronaut Univ, Dept Phys Sci, Daytona Beach, FL 32114 USA. EM mierkiee@erau.edu RI Mierkiewicz, Edwin/N-7926-2016 OI Mierkiewicz, Edwin/0000-0002-4283-3751 FU NASA Planetary Astronomy award [NNX11AE38G, NNX13AL30G] FX The authors thank the National Solar Observatory and the Kitt Peak mountain staff for their efforts in making this engineering run so successful. We also thank K. Jaehnig for his invaluable engineering support and undergraduate students S. A. Sans, NASA summer internship program, and S. C. McKillop for their participation in data analysis. This work was supported by NASA Planetary Astronomy award NNX11AE38G and NNX13AL30G. NR 18 TC 0 Z9 0 U1 1 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 JUN PY 2014 VL 119 IS 6 BP 4950 EP 4956 DI 10.1002/2014JA019801 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2VZ UT WOS:000339710300058 ER PT J AU Chan, OW Bugler-Lacap, DC Biddle, JF Lim, DS McKay, CP Pointing, SB AF Chan, Olivia W. Bugler-Lacap, Donnabella C. Biddle, Jennifer F. Lim, Darlene S. McKay, Christopher P. Pointing, Stephen B. TI Phylogenetic diversity of a microbialite reef in a cold alkaline freshwater lake SO CANADIAN JOURNAL OF MICROBIOLOGY LA English DT Article DE biomineralization; cyanobacteria; microbialite; Pavilion Lake; reefs ID PAVILION LAKE; HIGHBORNE CAY; SHARK BAY; STROMATOLITES; CYANOBACTERIA; FUNGI; COLONIZATION; POPULATIONS; ENVIRONMENT; BAHAMAS AB A culture-independent multidomain survey of biodiversity in microbialite structures within the cold alkaline Pavilion Lake (British Columbia, Canada) revealed a largely homogenous community at depths from 10 to 30 m. Real-time quantitative PCR was used to demonstrate that bacteria comprised approximately 80%-95% of recoverable phylotypes. Archaeal phylotypes accounted for <5% of the community in microbialites exposed to the water column, while structures in sediment contact supported 4- to 5-fold higher archaeal abundance. Eukaryal phylotypes were rare and indicated common aquatic diatoms that were concluded not to be part of the microbialite community. Phylogenetic analysis of rRNA genes from clone libraries (N = 491) revealed that alphaproteobacterial phylotypes were most abundant. Cyanobacterial phylotypes were highly diverse but resolved into 4 dominant genera: Acaryochloris, Leptolyngbya, Microcoleus, and Pseudanabaena. Interestingly, microbialite cyanobacteria generally affiliated phylogenetically with aquatic and coral cyanobacterial groups rather than those from stromatolites. Other commonly encountered bacterial phylotypes were from members of the Acidobacteria, with relatively low abundance of the Betaproteobacteria, Chloroflexi, Nitrospirae, and Planctomycetes. Archaeal diversity (N = 53) was largely accounted for by Euryarchaeota, with most phylotypes affiliated with freshwater methanogenic taxa. C1 [Chan, Olivia W.; Bugler-Lacap, Donnabella C.; Pointing, Stephen B.] Auckland Univ Technol, Sch Appl Sci, Inst Appl Ecol New Zealand, Auckland, New Zealand. [Biddle, Jennifer F.] Univ Delaware, Coll Earth Ocean & Environm, Lewes, DE 19958 USA. [Lim, Darlene S.] SETI Inst, Mountain View, CA USA. [McKay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Pointing, SB (reprint author), Auckland Univ Technol, Sch Appl Sci, Inst Appl Ecol New Zealand, Auckland, New Zealand. EM steve.pointing@aut.ac.nz RI Biddle, Jennifer/F-8323-2010 OI Biddle, Jennifer/0000-0002-4344-8724 FU NASA Planetary Biology Internship program FX Many members of the Pavilion Lake Research Project research team generously gave their time during fieldwork for this investigation. Olivia Chan acknowledges support from the NASA Planetary Biology Internship program. NR 43 TC 2 Z9 2 U1 3 U2 21 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA SN 0008-4166 EI 1480-3275 J9 CAN J MICROBIOL JI Can. J. Microbiol. PD JUN PY 2014 VL 60 IS 6 BP 391 EP 398 DI 10.1139/cjm-2014-0024 PG 8 WC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Immunology; Microbiology SC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Immunology; Microbiology GA AL6QT UT WOS:000339258400006 PM 24861562 ER PT J AU Martin-Neira, M LeVine, DM Kerr, Y Skou, N Peichl, M Camps, A Corbella, I Hallikainen, M Font, J Wu, J Mecklenburg, S Drusch, M AF Martin-Neira, M. LeVine, D. M. Kerr, Y. Skou, N. Peichl, M. Camps, A. Corbella, I. Hallikainen, M. Font, J. Wu, J. Mecklenburg, S. Drusch, M. TI Microwave interferometric radiometry in remote sensing: An invited historical review SO RADIO SCIENCE LA English DT Review ID SYNTHETIC-APERTURE RADIOMETER; SURFACE SOIL-MOISTURE; OCEAN SALINITY; L-BAND; SEMIARID AREAS; SMOS; EMISSION; CALIBRATION; SPACE; ESTAR AB The launch of the Soil Moisture and Ocean Salinity (SMOS) mission on 2 November 2009 marked a milestone in remote sensing for it was the first time a radiometer capable of acquiring wide field of view images at every single snapshot, a unique feature of the synthetic aperture technique, made it to space. The technology behind such an achievement was developed, thanks to the effort of a community of researchers and engineers in different groups around the world. It was only because of their joint work that SMOS finally became a reality. The fact that the European Space Agency, together with CNES (Centre National d'Etudes Spatiales) and CDTI (Centro para el Desarrollo Tecnologico e Industrial), managed to get the project through should be considered a merit and a reward for that entire community. This paper is an invited historical review that, within a very limited number of pages, tries to provide insight into some of the developments which, one way or another, are imprinted in the name of SMOS. C1 [Martin-Neira, M.; Drusch, M.] European Space Agcy, Estec, NL-2200 AG Noordwijk, Netherlands. [LeVine, D. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kerr, Y.] Ctr Etud Spatiales Biosphere, Toulouse, France. [Skou, N.] Tech Univ Denmark, DTU Space, Copenhagen, Denmark. [Peichl, M.] Microwaves & Radar Inst, DLR, Oberpfaffenhofen, Germany. [Camps, A.; Corbella, I.] Polythecn Univ Catalonia, Dept Signal Theory & Commun, Barcelona, Spain. [Hallikainen, M.] Aalto Univ, Dept Radio Sci & Engn, Espoo, Finland. [Font, J.] Inst Ciencies Mar CSIC, Barcelona, Spain. [Font, J.] SMOS Barcelona Expert Ctr, Barcelona, Spain. [Wu, J.] Natl Space Sci Ctr, Beijing, Peoples R China. [Mecklenburg, S.] European Space Agcy, ESRIN, Rome, Italy. RP Martin-Neira, M (reprint author), European Space Agcy, Estec, NL-2200 AG Noordwijk, Netherlands. EM manuel.martin-neira@esa.int RI Hallikainen, Martti/A-4201-2011; Font, Jordi/E-5355-2013 OI Font, Jordi/0000-0003-2590-1457 NR 105 TC 8 Z9 8 U1 2 U2 30 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 JUN PY 2014 VL 49 IS 6 BP 415 EP 449 DI 10.1002/2013RS005230 PG 35 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA AL9BT UT WOS:000339435300005 ER PT J AU Arora, HS Mridha, S Grewal, HS Singh, H Hofmann, DC Mukherjee, S AF Arora, Harpreet Singh Mridha, Sanghita Grewal, Harpreet Singh Singh, Harpreet Hofmann, Douglas C. Mukherjee, Sundeep TI Controlling the length scale and distribution of the ductile phase in metallic glass composites through friction stir processing SO SCIENCE AND TECHNOLOGY OF ADVANCED MATERIALS LA English DT Article DE bulk amorphous alloys; thermomechanical processing; nanoindentation; shear bands ID MECHANICAL-PROPERTIES; MATRIX COMPOSITES; FLOW VISUALIZATION; TENSILE DUCTILITY; ALUMINUM; NANOINDENTATION; PLASTICITY; SIMULATION; ALLOYS AB We demonstrate the refinement and uniform distribution of the crystalline dendritic phase by friction stir processing (FSP) of titanium based in situ ductile-phase reinforced metallic glass composite. The average size of the dendrites was reduced by almost a factor of five (from 24 m to 5 m) for the highest tool rotational speed of 900 rpm. The large inter-connected dendrites become more fragmented with increased circularity after processing. The changes in thermal characteristics were measured by differential scanning calorimetry. The reduction in crystallization enthalpy after processing suggests partial devitrification due to the high strain plastic deformation. FSP resulted in increased hardness and modulus for both the amorphous matrix and the crystalline phase. This is explained by interaction of shear bands in amorphous matrix with the strain-hardened dendritic phase. Our approach offers a new strategy for microstructural design in metallic glass composites. C1 [Arora, Harpreet Singh; Mridha, Sanghita; Mukherjee, Sundeep] Univ N Texas, Dept Mat Sci & Engn, Denton, TX 76203 USA. [Grewal, Harpreet Singh; Singh, Harpreet] Indian Inst Technol Ropar, Sch Mech Mat & Energy Engn, Rupnagar 140001, Punjab, India. [Hofmann, Douglas C.] CALTECH, Jet Prop Lab, Engn & Sci Directorate, Pasadena, CA 91109 USA. RP Arora, HS (reprint author), Univ N Texas, Dept Mat Sci & Engn, Denton, TX 76203 USA. EM sundeep.mukherjee@unt.edu RI Mukherjee, Sundeep/N-5247-2014; OI Singh, Harpreet /0000-0002-6812-2667 NR 22 TC 0 Z9 0 U1 1 U2 25 PU NATL INST MATERIALS SCIENCE PI IBARAKI PA NATL INST MATERIALS SCIENCE, 1-2-1 SENGEN, TSUKUBA-CITY, IBARAKI, 305-0047, JAPAN SN 1468-6996 J9 SCI TECHNOL ADV MAT JI Sci. Technol. Adv. Mater. PD JUN PY 2014 VL 15 IS 3 AR 035011 DI 10.1088/1468-6996/15/3/035011 PG 7 WC Materials Science, Multidisciplinary SC Materials Science GA AL8IC UT WOS:000339380700019 PM 27877687 ER PT J AU Schwadron, NA Gorby, M Torok, T Downs, C Linker, J Lionello, R Mikic, Z Riley, P Giacalone, J Chandran, B Germaschewski, K Isenberg, PA Lee, MA Lugaz, N Smith, S Spence, HE Desai, M Kasper, J Kozarev, K Korreck, K Stevens, M Cooper, J MacNeice, P AF Schwadron, Nathan A. Gorby, Matt Torok, Tibor Downs, Cooper Linker, Jon Lionello, Roberto Mikic, Zoran Riley, Pete Giacalone, Joe Chandran, Ben Germaschewski, Kai Isenberg, Phil A. Lee, Martin A. Lugaz, Noe Smith, Sonya Spence, Harlan E. Desai, Mihir Kasper, Justin Kozarev, Kamen Korreck, Kelly Stevens, Mike Cooper, John MacNeice, Peter TI Synthesis of 3-D Coronal-Solar Wind Energetic Particle Acceleration Modules SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID WHOLE SUN MONTH; MAGNETIC-FIELD; MASS EJECTION; 1 AU; FLARES C1 [Schwadron, Nathan A.; Chandran, Ben; Germaschewski, Kai; Isenberg, Phil A.; Lee, Martin A.; Lugaz, Noe; Smith, Sonya; Spence, Harlan E.] Univ New Hampshire, Durham, NH 03824 USA. [Gorby, Matt] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Torok, Tibor; Downs, Cooper; Lionello, Roberto; Mikic, Zoran] Predict Sci Inc, San Diego, CA USA. [Linker, Jon; Riley, Pete] Predict Sci Inc, Morristown, NJ USA. [Giacalone, Joe] Univ Arizona, Tucson, AZ 85721 USA. [Spence, Harlan E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Desai, Mihir] Southwest Res Inst, San Antonio, TX USA. [Kasper, Justin] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Kozarev, Kamen; Korreck, Kelly; Stevens, Mike] Smithsonian Astrophys Observ, Washington, DC USA. [Cooper, John] NASA, Space Phys Data Facil, Washington, DC USA. [Cooper, John] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Heliophys Sci Div, Washington, DC USA. [MacNeice, Peter] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Washington, DC USA. RP Schwadron, NA (reprint author), Univ New Hampshire, Durham, NH 03824 USA. RI Lugaz, Noe/C-1284-2008; Kasper, Justin/D-1152-2010; OI Lugaz, Noe/0000-0002-1890-6156; Kasper, Justin/0000-0002-7077-930X; Riley, Pete/0000-0002-1859-456X FU C-SWEPA (NASA) [NNX13AI75G]; EMMREM [NNX07AC14G]; Sun-2-Ice (NSF) projects [AGS1135432]; DREAM (NASA) [NNX10AB17A]; DREAM2 (NASA) [NNX14AG13A] FX We thank all those who made C-SWEPA (NASA grant NNX13AI75G) possible. This work was also funded EMMREM (grant NNX07AC14G), Sun-2-Ice (NSF grant AGS1135432) projects, DREAM (NASA grant NNX10AB17A), and DREAM2 (NASA grant NNX14AG13A). NR 27 TC 3 Z9 3 U1 0 U2 4 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 JUN PY 2014 VL 12 IS 6 BP 323 EP 328 DI 10.1002/2014SW001086 PG 6 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AM0CG UT WOS:000339509900001 ER PT J AU Walsh, BM Kuntz, KD Collier, MR Sibeck, DG Snowden, SL Thomas, NE AF Walsh, B. M. Kuntz, K. D. Collier, M. R. Sibeck, D. G. Snowden, S. L. Thomas, N. E. TI Energetic particle impact on X-ray imaging with XMM-Newton SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID EARTHS BOW SHOCK; INTERPLANETARY SHOCKS; DAYSIDE MAGNETOPAUSE; MAGNETOSPHERIC IONS; EVENT FILES; ELECTRONS; CHANDRA; ANOMALIES; ACCELERATION; DEGRADATION AB Since energetic protons (similar to 100 keV) hinder space-based X-ray imaging, there is a need to characterize the proton environments encountered by a soft X-ray mission when planning missions and operations in the near-Earth environment. Impacts range from enhanced noise in the images to damage to CCD detectors. The high-apogee (17.9 R-E), inclined (40 degrees), and elliptical orbit of European Space Agency's XMM-Newton mission frequently passes through the Earth's Van Allen radiation belts on closed magnetospheric magnetic field lines, the magnetotail lobes on open magnetic field lines, and into the magnetosheath and solar wind on open solar magnetic field lines, four regions with very different energetic proton environments. We use XMM-Newton measurements from 2000 to 2010 to survey the occurrence of proton strikes or "soft proton flares" on the European Photon Imaging Camera pn-junction CCD detector. Proton flares affect similar to 55% of all measurements. Rates vary from 50% at large radial distances in the solar wind and magnetosheath to 25% in the high-latitude magnetotail lobes and increase to 66% of the measurements on closed low-latitude magnetospheric magnetic field lines. C1 [Walsh, B. M.; Collier, M. R.; Sibeck, D. G.; Thomas, N. E.] NASA, Goddard Space Flight Ctr, Heliosphys Div, Greenbelt, MD 20771 USA. [Walsh, B. M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Kuntz, K. D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. RP Walsh, BM (reprint author), NASA, Goddard Space Flight Ctr, Heliosphys Div, Greenbelt, MD 20771 USA. EM bwalsh@ssl.berkeley.edu RI Walsh, Brian/C-4899-2016; Collier, Michael/I-4864-2013 OI Walsh, Brian/0000-0001-7426-5413; Collier, Michael/0000-0001-9658-6605 FU National Science Foundation [AGS-1136827] FX Partial support was given by the National Science Foundation through grant AGS-1136827. We would like to thank Matthias Ehle of the XMM Science Operations Center for his help with the radiation monitor data. We acknowledge NASA HEASARC for producing the XMM-Newton trend data. The authors thank Y. Collado-Vega, F. S. Porter, and J. S. Hendrickson for useful discussions. We would also like to express our gratitude to the International Space Science Institute which hosted the "Solar Wind Charge Exchange Soft X-ray Imaging in the Solar System" group. NR 40 TC 0 Z9 0 U1 0 U2 4 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 JUN PY 2014 VL 12 IS 6 BP 387 EP 394 DI 10.1002/2014SW001046 PG 8 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AM0CG UT WOS:000339509900007 ER PT J AU Owens, MJ Horbury, TS Wicks, RT McGregor, SL Savani, NP Xiong, M AF Owens, M. J. Horbury, T. S. Wicks, R. T. McGregor, S. L. Savani, N. P. Xiong, M. TI Ensemble downscaling in coupled solar wind-magnetosphere modeling for space weather forecasting SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article ID EVENT; PREDICTIONS; SIMULATION; SKILL AB Advanced forecasting of space weather requires simulation of the whole Sun-to-Earth system, which necessitates driving magnetospheric models with the outputs from solar wind models. This presents a fundamental difficulty, as the magnetosphere is sensitive to both large-scale solar wind structures, which can be captured by solar wind models, and small-scale solar wind "noise," which is far below typical solar wind model resolution and results primarily from stochastic processes. Following similar approaches in terrestrial climate modeling, we propose statistical "downscaling" of solar wind model results prior to their use as input to a magnetospheric model. As magnetospheric response can be highly nonlinear, this is preferable to downscaling the results of magnetospheric modeling. To demonstrate the benefit of this approach, we first approximate solar wind model output by smoothing solar wind observations with an 8 h filter, then add small-scale structure back in through the addition of random noise with the observed spectral characteristics. Here we use a very simple parameterization of noise based upon the observed probability distribution functions of solar wind parameters, but more sophisticated methods will be developed in the future. An ensemble of results from the simple downscaling scheme are tested using a model-independent method and shown to add value to the magnetospheric forecast, both improving the best estimate and quantifying the uncertainty. We suggest a number of features desirable in an operational solar wind downscaling scheme. C1 [Owens, M. J.] Univ Reading, Dept Meteorol, Space Environm Phys Grp, Reading, Berks, England. [Horbury, T. S.] Univ London Imperial Coll Sci Technol & Med, London, England. [Wicks, R. T.; Savani, N. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wicks, R. T.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [McGregor, S. L.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Savani, N. P.] George Mason Univ, Sch Phys, Fairfax, VA 22030 USA. [Xiong, M.] Chinese Acad Sci, Ctr Space Sci & Appl Res, State Key Lab SpaceWeather, Beijing, Peoples R China. RP Owens, MJ (reprint author), Univ Reading, Dept Meteorol, Space Environm Phys Grp, Reading, Berks, England. EM m.j.owens@reading.ac.uk RI Wicks, Robert/A-1180-2009; Owens, Mathew/B-3006-2010 OI Wicks, Robert/0000-0002-0622-5302; Owens, Mathew/0000-0003-2061-2453 FU Natural Environment Research Council (NERC) [NE/J024678/1] FX M.O. is partially funded by the Natural Environment Research Council (NERC) under grant NE/J024678/1. We are grateful to the ACE Science Center (ASC) for magnetic field and solar wind plasma data. Simulation results have been provided by the Community Coordinated Modeling Center at Goddard Space Flight Center through their public Runs on Request system (http://ccmc.gsfc.nasa.gov). The CCMC is a multiagency partnership between NASA, AFMC, AFOSR, AFRL, AFWA, NOAA, NSF, and ONR. The LFM Model was developed by John Lyon, Wenbin Wang, Slava Merkin, Mike Wiltberger, Pete Schmitt, and Ben Foster at Dartmouth College/NCAR-HAO/JHU-APL/CISM. NR 33 TC 5 Z9 5 U1 0 U2 7 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 JUN PY 2014 VL 12 IS 6 BP 395 EP 405 DI 10.1002/2014SW001064 PG 11 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA AM0CG UT WOS:000339509900008 ER PT J AU Begault, DR Bittner, RM Anderson, MR AF Begault, Durand R. Bittner, Rachel M. Anderson, Mark R. TI Multimodal Information Management: Evaluation of Auditory and Haptic Cues for NextGen Communication Displays SO JOURNAL OF THE AUDIO ENGINEERING SOCIETY LA English DT Article ID DATA LINK; PERFORMANCE; MODALITY AB Auditory communication displays within the NextGen data link system may use synthetic speech messages to replace voice communications. An interface design for selecting among multiple incoming messages can impact both user performance and preference. Two design factors were evaluated: physical pressure-sensitive switches versus flat panel "virtual switches," and auditory feedback from switch contact. Performance with stimuli using physical switches was 1.2 s faster than virtual switches (2.0 s vs. 3.2 s); auditory feedback provided a 0.6 s performance advantage (2.3 s vs. 2.9 s). There was no interaction between these variables. Preference data were highly correlated with performance. C1 [Begault, Durand R.] NASA, Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA. [Bittner, Rachel M.] NYU, Courant Inst Math Sci, New York, NY 10012 USA. [Anderson, Mark R.] NASA, Ames Res Ctr, ASRC, Moffett Field, CA 94035 USA. RP Begault, DR (reprint author), NASA, Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA. EM Durand.R.Begault@nasa.gov; rmb456@nyu.edu; Mark.R.Anderson@nasa.gov FU NASA FX This work was supported by NASA's System-wide Safety Assurance Technologies (SSAT) Project. We appreciate the assistance of our colleagues in the Advanced Controls and Displays Laboratory at NASA Ames' Human Systems Integration Division. NR 13 TC 0 Z9 0 U1 1 U2 5 PU AUDIO ENGINEERING SOC PI NEW YORK PA 60 E 42ND ST, NEW YORK, NY 10165-2520 USA SN 1549-4950 J9 J AUDIO ENG SOC JI J. Audio Eng. Soc. PD JUN PY 2014 VL 62 IS 6 BP 375 EP 385 PG 11 WC Acoustics; Engineering, Multidisciplinary SC Acoustics; Engineering GA AL6GB UT WOS:000339229500001 ER PT J AU Che, H AF Che, H. TI Two-fluid description of wave-particle interactions in strong Buneman turbulence SO PHYSICS OF PLASMAS LA English DT Article ID HYBRID-DRIFT INSTABILITY; MAGNETIC RECONNECTION; ANOMALOUS RESISTIVITY; MAGNETOPAUSE; PLASMA AB To understand the nature of anomalous resistivity in magnetic reconnection, we investigate turbulence-induced momentum transport and energy dissipation while a plasma is unstable to the Buneman instability in force-free current sheets. Using 3D particle-in-cell simulations, we find that the macroscopic effects generated by wave-particle interactions in Buneman instability can be approximately described by a set of electron fluid equations. We show that both energy dissipation and momentum transport along electric current in the current layer are locally quasi-static, but globally dynamic and irreversible. Turbulent drag dissipates both the streaming energy of the current sheet and the associated magnetic energy. The net loss of streaming energy is converted into the electron component heat conduction parallel to the magnetic field and increases the electron Boltzmann entropy. The growth of self-sustained Buneman waves satisfies a Bernoulli-like equation that relates the turbulence-induced convective momentum transport and thermal momentum transport. Electron trapping and de-trapping drive local momentum transports, while phase mixing converts convective momentum into thermal momentum. The drag acts like a micro-macro link in the anomalous heating processes. The decrease of magnetic field maintains an inductive electric field that re-accelerates electrons, but most of the magnetic energy is dissipated and converted into the component heat of electrons perpendicular to the magnetic field. This heating process is decoupled from the heating of Buneman instability in the current sheets. Ion heating is weak but ions play an important role in assisting energy exchanges between waves and electrons. Cold ion fluid equations together with our electron fluid equations form a complete set of equations that describes the occurrence, growth, saturation and decay of the Buneman instability. (C) 2014 AIP Publishing LLC. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Che, H (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. FU NASA Postdoctoral Program at NASA/GSFC; NASA [NNH11ZDA001N] FX This research was supported by the NASA Postdoctoral Program at NASA/GSFC administered by Oak Ridge Associated Universities through a contract with NASA and NASA Grant No. NNH11ZDA001N. The simulations and analysis were partially carried out at the National Energy Research Scientific Computing Center and at NASA/Ames High-End Computing Capacity. NR 32 TC 2 Z9 2 U1 0 U2 4 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD JUN PY 2014 VL 21 IS 6 AR 062305 DI 10.1063/1.4882677 PG 10 WC Physics, Fluids & Plasmas SC Physics GA AL2ZT UT WOS:000338995300046 ER PT J AU Karimabadi, H Roytershteyn, V Vu, HX Omelchenko, YA Scudder, J Daughton, W Dimmock, A Nykyri, K Wan, M Sibeck, D Tatineni, M Majumdar, A Loring, B Geveci, B AF Karimabadi, H. Roytershteyn, V. Vu, H. X. Omelchenko, Y. A. Scudder, J. Daughton, W. Dimmock, A. Nykyri, K. Wan, M. Sibeck, D. Tatineni, M. Majumdar, A. Loring, B. Geveci, B. TI The link between shocks, turbulence, and magnetic reconnection in collisionless plasmas SO PHYSICS OF PLASMAS LA English DT Article ID QUASI-PARALLEL SHOCK; EARTHS BOW SHOCK; HIGH-SPEED JETS; SOLAR-WIND; HYBRID SIMULATIONS; MAGNETOSHEATH; MAGNETOPAUSE; MAGNETOSPHERE; ACCELERATION; ENHANCEMENTS AB Global hybrid (electron fluid, kinetic ions) and fully kinetic simulations of the magnetosphere have been used to show surprising interconnection between shocks, turbulence, and magnetic reconnection. In particular, collisionless shocks with their reflected ions that can get upstream before retransmission can generate previously unforeseen phenomena in the post shocked flows: (i) formation of reconnecting current sheets and magnetic islands with sizes up to tens of ion inertial length. (ii) Generation of large scale low frequency electromagnetic waves that are compressed and amplified as they cross the shock. These "wavefronts" maintain their integrity for tens of ion cyclotron times but eventually disrupt and dissipate their energy. (iii) Rippling of the shock front, which can in turn lead to formation of fast collimated jets extending to hundreds of ion inertial lengths downstream of the shock. The jets, which have high dynamical pressure, "stir" the downstream region, creating large scale disturbances such as vortices, sunward flows, and can trigger flux ropes along the magnetopause. This phenomenology closes the loop between shocks, turbulence, and magnetic reconnection in ways previously unrealized. These interconnections appear generic for the collisionless plasmas typical of space and are expected even at planar shocks, although they will also occur at curved shocks as occur at planets or around ejecta. (C) 2014 AIP Publishing LLC. C1 [Karimabadi, H.; Omelchenko, Y. A.] Univ Calif San Diego, La Jolla, CA 92093 USA. [Karimabadi, H.; Roytershteyn, V.; Vu, H. X.; Omelchenko, Y. A.] SciberQuest Inc, Del Mar, CA 92014 USA. [Scudder, J.] Univ Iowa, Iowa City, IA 52242 USA. [Daughton, W.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Dimmock, A.; Nykyri, K.] Aalto Univ, Espoo, Finland. [Dimmock, A.; Nykyri, K.] Embry Riddle Aeronaut Univ, Daytona Beach, FL 32114 USA. [Wan, M.] Univ Delaware, Newark, DE 19716 USA. [Sibeck, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tatineni, M.; Majumdar, A.] San Diego Supercomp Ctr, La Jolla, CA 92093 USA. [Loring, B.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Geveci, B.] Kitware, New York, NY 12065 USA. RP Karimabadi, H (reprint author), Univ Calif San Diego, La Jolla, CA 92093 USA. RI Daughton, William/L-9661-2013; Wan, Minping/A-1344-2011; OI Roytershteyn, Vadim/0000-0003-1745-7587; Nykyri, Katariina/0000-0002-6905-9487 FU NASA [NNX12AD30G, NNX11AJ44G, NNX07AF40G]; NSF [0904734, 1104815, AGS-1063439, AGS-1156094, ATM 0802380, OCI 07-25070]; DOE [DE-SC0004662]; state of Illinois FX This work was partially supported by NASA (NNX12AD30G, Heliophysics Theory), NSF (0904734, 1104815), and DOE (DE-SC0004662). M. W. acknowledges support from NSF Grants No. AGS-1063439 and No. AGS-1156094 (SHINE), and from NASA Grant No. NNX11AJ44G. JS acknowledges support from NSF ATM 0802380 and NASA NNX07AF40G. Simulations were performed on Pleiades provided by NASA's HEC Program, and Blue Waters sustained-petascale computing project, which is supported by the NSF (OCI 07-25070) and the state of Illinois. We gratefully acknowledge useful discussions with J. Giacalone, J. Borovsky, and A. Retino. We also thank the referee for making useful suggestions that improved the paper. NR 52 TC 39 Z9 40 U1 1 U2 20 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 JUN PY 2014 VL 21 IS 6 AR 062308 DI 10.1063/1.4882875 PG 21 WC Physics, Fluids & Plasmas SC Physics GA AL2ZT UT WOS:000338995300049 ER PT J AU Chuss, DT Eimer, JR Fixsen, DJ Hinderks, J Kogut, AJ Lazear, J Mirel, P Switzer, E Voellmer, GM Wollack, EJ AF Chuss, D. T. Eimer, J. R. Fixsen, D. J. Hinderks, J. Kogut, A. J. Lazear, J. Mirel, P. Switzer, E. Voellmer, G. M. Wollack, E. J. TI Variable-delay polarization modulators for cryogenic millimeter-wave applications SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID GRIDS AB We describe the design, construction, and initial validation of the variable-delay polarization modulator (VPM) designed for the PIPER cosmic microwave background polarimeter. The VPM modulates between linear and circular polarization by introducing a variable phase delay between orthogonal linear polarizations. Each VPM has a diameter of 39 cm and is engineered to operate in a cryogenic environment (1.5 K). We describe the mechanical design and performance of the kinematic double-blade flexure and drive mechanism along with the construction of the high precision wire grid polarizers. (C) 2014 AIP Publishing LLC. C1 [Chuss, D. T.; Fixsen, D. J.; Hinderks, J.; Kogut, A. J.; Mirel, P.; Switzer, E.; Voellmer, G. M.; Wollack, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Eimer, J. R.; Lazear, J.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Chuss, DT (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM David.T.Chuss@nasa.gov RI Wollack, Edward/D-4467-2012 OI Wollack, Edward/0000-0002-7567-4451 FU NASA APRA suborbital grant FX We thank Alyssa Barlis, Adam Blake, Matheus Teixeira, and Vien Ha for work in the initial testing of the fabrication process and Paul Cursey for machining support. We thank Mackenzie Turvey for assistance with the electromagnetic testing. In addition, we would like to thank Mike Jackson for modeling and finite element analysis for the flexure and drive system. This work was funded by a NASA APRA suborbital grant. NR 18 TC 1 Z9 1 U1 0 U2 7 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0034-6748 EI 1089-7623 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD JUN PY 2014 VL 85 IS 6 AR 064501 DI 10.1063/1.4879499 PG 6 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA AL3FB UT WOS:000339010500039 PM 24985830 ER PT J AU Jahromi, AE Sullivan, DF AF Jahromi, Amir E. Sullivan, Dan F. TI A piezoelectric cryogenic heat switch SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article AB We have measured the thermal conductance of a mechanical heat switch actuated by a piezoelectric positioner, the PZHS (PieZo electric Heat Switch), at cryogenic temperatures. The thermal conductance of the PZHS was measured between 4 K and 10 K, and on/off conductance ratios of about 100-200 at lowest and highest measures temperature were achieved when the positioner applied its maximum force of 8 N, respectively. We discuss the advantages of using this system in cryogenic applications, and estimate the ultimate performance of an ideal PZHS. (C) 2014 AIP Publishing LLC. C1 [Jahromi, Amir E.; Sullivan, Dan F.] NASA, Goddard Space Flight Ctr, Cryogen & Fluids Branch Code 552, Greenbelt, MD 20771 USA. RP Jahromi, AE (reprint author), NASA, Goddard Space Flight Ctr, Cryogen & Fluids Branch Code 552, Greenbelt, MD 20771 USA. EM amir.e.jahromi@nasa.gov; dan.f.sullivan@nasa.gov NR 7 TC 1 Z9 1 U1 1 U2 6 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0034-6748 EI 1089-7623 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD JUN PY 2014 VL 85 IS 6 AR 065118 DI 10.1063/1.4876483 PG 3 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA AL3FB UT WOS:000339010500072 PM 24985863 ER PT J AU Martinache, F Guyon, O Jovanovic, N Clergeon, C Singh, G Kudo, T Currie, T Thalmann, C McElwain, M Tamura, M AF Martinache, Frantz Guyon, Olivier Jovanovic, Nemanja Clergeon, Christophe Singh, Garima Kudo, Tomoyuki Currie, Thayne Thalmann, Christian McElwain, Michael Tamura, Motohide TI On-Sky Speckle Nulling Demonstration at Small Angular Separation with SCExAO SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID INDUCED AMPLITUDE APODIZATION; KERNEL PHASE; CORONAGRAPH; INTERFEROMETRY; PRINCIPLE; LIMITS; SEEDS AB This paper presents the first on-sky demonstration of speckle nulling, which was achieved at the Subaru Telescope in the context of the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) Project. Despite the absence of a high-order high-bandwidth closed-loop AO system, observations conducted with SCExAO show that even in poor-to-moderate observing conditions, speckle nulling can be used to suppress static and slow speckles even in the presence of a brighter dynamic speckle halo, suggesting that more advanced high-contrast imaging algorithms developed in the laboratory can be applied to ground-based systems. C1 [Martinache, Frantz; Guyon, Olivier; Jovanovic, Nemanja; Clergeon, Christophe; Singh, Garima; Kudo, Tomoyuki] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Martinache, Frantz] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR7293, Nice, France. [Guyon, Olivier] Univ Arizona, Stewart Observ, Tucson, AZ 85721 USA. [Currie, Thayne] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 1A1, Canada. [Thalmann, Christian] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Thalmann, Christian] ETH, Dept Astron, CH-8093 Zurich, Switzerland. [McElwain, Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tamura, Motohide] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. RP Martinache, F (reprint author), Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Pl, Hilo, HI 96720 USA. EM frantz@naoj.org NR 28 TC 21 Z9 21 U1 0 U2 4 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUN PY 2014 VL 126 IS 940 BP 565 EP 572 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL0OB UT WOS:000338825100006 ER PT J AU Dibarboure, G Ubelmann, C AF Dibarboure, Gerald Ubelmann, Clement TI Investigating the Performance of Four Empirical Cross-Calibration Methods for the Proposed SWOT Mission SO REMOTE SENSING LA English DT Article DE SWOT; empirical calibration; roll; error budget; interferometry; topography ID RADAR INTERFEROMETRY; OCEAN; TOPOGRAPHY; SEA AB The proposed surface water and ocean topography (SWOT) mission aims at observing short scale ocean topography with an unprecedented resolution and accuracy. Its main proposed sensor is a radar interferometer, so a major source of topography error is the roll angle: the relative positions of SWOT's antennas must be known within a few micrometers. Because reaching SWOT's stringent requirements with onboard roll values is challenging, we carried out simulations as a contingency strategy (i.e., to be ready if roll is larger than anticipated) that could be used with ground-based data. We revisit the empirical calibration algorithms with additional solving methods (e. g., based on orbit sub-cycle) and more sophisticated performance assessments with spectral decompositions. We also explore the link between the performance of four calibration methods and the attributes of their respective calibration zones: size and geometry (e. g., crossover diamonds), temporal variability (e. g., how many days between overlapping SWOT images). In general, the so-called direct method (using a single SWOT image) yields better coverage and smaller calibrated roll residuals because the full extent of the swath can be used for calibration, but this method makes an extensive use of the external nadir constellation to separate roll from oceanic variability, and it is more prone to leakages from oceanic variability on roll (i.e., true topography signal is more likely to be corrupted if it is misinterpreted as roll) and inaccurate modeling of the true topography spectrum. For SWOT's baseline orbit (21 days repeat and 10.9 days sub-cycle), three other methods are found to be complementary with the direct method: swath crossovers, external nadir crossovers, and sub-cycle overlaps are shown to provide an additional calibration capability, albeit with complex latitude-varying coverage and performance. The main asset of using three or four methods concurrently is to minimize systematic leakages from oceanic variability or measurement errors, by maximizing overlap zones and by minimizing the temporal variability with one-day to three-day image differences. To that extent, SWOT's proposed "contingency orbit" is an attractive risk reduction asset: the one-day sub-cycle overlaps of adjoining swaths would provide a good, continuous, and self-sufficient (no need for external nadirs) calibration scheme. The benefit is however essentially located at mid to high-latitudes and it is substantial only for wavelengths longer than 100 km. C1 [Dibarboure, Gerald] CLS, F-31520 Ramonville St Agne, France. [Ubelmann, Clement] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Dibarboure, G (reprint author), CLS, 8-10 Rue Hermes, F-31520 Ramonville St Agne, France. EM gerald.dibarboure@cls.fr; Clement.Ubelmann@jpl.nasa.gov FU Centre National d'Etudes Spatiales (CNES) in the frame of their TOSCA contracts (SWOT mission development); Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA) FX This work was carried in part at Collecte Localisation Satellites (CLS) with support from the Centre National d'Etudes Spatiales (CNES) in the frame of their TOSCA contracts (SWOT mission development) and in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). NR 15 TC 0 Z9 1 U1 4 U2 9 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD JUN PY 2014 VL 6 IS 6 BP 4831 EP 4869 DI 10.3390/rs6064831 PG 39 WC Remote Sensing SC Remote Sensing GA AK9RB UT WOS:000338763300010 ER PT J AU Negron-Juarez, RI Chambers, JQ Hurtt, GC Annane, B Cocke, S Powell, M Stott, M Goosem, S Metcalfe, DJ Saatchi, SS AF Negron-Juarez, Robinson I. Chambers, Jeffrey Q. Hurtt, George C. Annane, Bachir Cocke, Stephen Powell, Mark Stott, Michael Goosem, Stephen Metcalfe, Daniel J. Saatchi, Sassan S. TI Remote Sensing Assessment of Forest Disturbance across Complex Mountainous Terrain: The Pattern and Severity of Impacts of Tropical Cyclone Yasi on Australian Rainforests SO REMOTE SENSING LA English DT Article DE multispectral data; complex mountainous terrain; tropical rainforests; tropical cyclones; forest disturbance ID NORTHEAST AUSTRALIA; CATASTROPHIC WIND; LANDSAT DATA; WET TROPICS; MODIS; DAMAGE; REFLECTANCE; LANDSCAPE; LARRY; HURRICANES AB Topography affects the patterns of forest disturbance produced by tropical cyclones. It determines the degree of exposure of a surface and can alter wind characteristics. Whether multispectral remote sensing data can sense the effect of topography on disturbance is a question that deserves attention given the multi-scale spatial coverage of these data and the projected increase in intensity of the strongest cyclones. Here, multispectral satellite data, topographic maps and cyclone surface wind data were used to study the patterns of disturbance in an Australian rainforest with complex mountainous terrain produced by tropical cyclone Yasi (2011). The cyclone surface wind data (H*wind) was produced by the Hurricane Research Division of the National Oceanic and Atmospheric Administration (HRD/NOAA), and this was the first time that this data was produced for a cyclone outside of United States territory. A disturbance map was obtained by applying spectral mixture analyses on satellite data and presented a significant correlation with field-measured tree mortality. Our results showed that, consistent with cyclones in the southern hemisphere, multispectral data revealed that forest disturbance was higher on the left side of the cyclone track. The highest level of forest disturbance occurred in forests along the path of the cyclone track (+/- 30 degrees). Levels of forest disturbance decreased with decreasing slope and with an aspect facing off the track of the cyclone or away from the dominant surface winds. An increase in disturbance with surface elevation was also observed. However, areas affected by the same wind intensity presented increased levels of disturbance with increasing elevation suggesting that complex terrain interactions act to speed up wind at higher elevations. Yasi produced an important offset to Australia's forest carbon sink in 2010. We concluded that multispectral data was sensitive to the main effects of complex topography on disturbance patterns. High resolution cyclone wind surface data are needed in order to quantify the effects of topographic accelerations on cyclone related forest disturbances. C1 [Negron-Juarez, Robinson I.; Chambers, Jeffrey Q.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Climate Sci Dept, Div Earth Sci, Berkeley, CA 94720 USA. [Negron-Juarez, Robinson I.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Hurtt, George C.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [Annane, Bachir] Univ Miami, CIMAS, Coral Gables, FL 33149 USA. [Cocke, Stephen] Florida State Univ, COAPS, Tallahassee, FL 32306 USA. [Powell, Mark] NOAA, Hurricane Res Div, Miami, FL 33149 USA. [Stott, Michael; Goosem, Stephen] Wet Trop Management Author, Cairns, Qld 4870, Australia. [Metcalfe, Daniel J.] CSIRO Ecosyst Sci EcoSci Precinct, Dutton Pk, Qld 4102, Australia. [Saatchi, Sassan S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Negron-Juarez, RI (reprint author), Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Climate Sci Dept, Div Earth Sci, 1 Cyclotron Rd,MS 50-4037, Berkeley, CA 94720 USA. EM robinson.inj@lbl.gov; jchambers@lbl.gov; gchurtt@umd.edu; Bachir.Annane@noaa.gov; scocke@fsu.edu; Mark.Powell@noaa.gov; mike.stott@wtma.qld.gov.au; steve.goosem@wtma.qld.gov.au; dan.metcalfe@csiro.au; Sasan.S.Saatchi@jpl.nasa.gov RI Metcalfe, Daniel/G-3305-2010; Chambers, Jeffrey/J-9021-2014; Powell, Mark/I-4963-2013; Annane, Bachir/A-3399-2017; Negron-Juarez, Robinson/I-6289-2016 OI Metcalfe, Daniel/0000-0001-6853-7072; Chambers, Jeffrey/0000-0003-3983-7847; Powell, Mark/0000-0002-4890-8945; FU NASA-IDS [NNX10AP11G]; DOE's Office of Biological and Environmental Research [DE-AC02- 05CH11231] FX We thank the four anonymous reviewers and one External editor for their valuable comments on our manuscript. Funding from a NASA-IDS (NNX10AP11G) grant to the University of Maryland with a subcontract to Tulane University, and DOE's Office of Biological and Environmental Research (Contract No. DE-AC02- 05CH11231), under the Climate and Earth System Modeling Program, supported the work presented here. The authors also thank to Sonya Jeffrey, Douglas Jeffrey and Ernie Grant (INGAN Pty Ltd, http://www.ingan.com.au) and to Mr. Noel and Mrs. Dot Barrow (A Tropical Scape B&B, http://www.atropicalescape.com/) for all the logistic support. RINJ thank the Office of Biological and Environmental Research of the U.S. Department of Energy as part of their Regional and Global Climate Modeling (RGCM) Program. NR 50 TC 3 Z9 3 U1 4 U2 25 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD JUN PY 2014 VL 6 IS 6 BP 5633 EP 5649 DI 10.3390/rs6065633 PG 17 WC Remote Sensing SC Remote Sensing GA AK9RB UT WOS:000338763300043 ER PT J AU Mueller, T Dressler, G Tucker, CJ Pinzon, JE Leimgruber, P Dubayah, RO Hurtt, GC Bohning-Gaese, K Fagan, WF AF Mueller, Thomas Dressler, Gunnar Tucker, Compton J. Pinzon, Jorge E. Leimgruber, Peter Dubayah, Ralph O. Hurtt, George C. Boehning-Gaese, Katrin Fagan, William F. TI Human Land-Use Practices Lead to Global Long-Term Increases in Photosynthetic Capacity SO REMOTE SENSING LA English DT Article DE NDVI; land-use; anthropogenic biomes; anthromes; global change; GIMMS3g ID NDVI DATA SETS; TIME-SERIES; VEGETATION INDEX; SATELLITE DATA; SOUTH-AMERICA; TRENDS; MODIS; CLIMATE; COVER; PRODUCTIVITY AB Long-term trends in photosynthetic capacity measured with the satellite-derived Normalized Difference Vegetation Index (NDVI) are usually associated with climate change. Human impacts on the global land surface are typically not accounted for. Here, we provide the first global analysis quantifying the effect of the earth's human footprint on NDVI trends. Globally, more than 20% of the variability in NDVI trends was explained by anthropogenic factors such as land use, nitrogen fertilization, and irrigation. Intensely used land classes, such as villages, showed the greatest rates of increase in NDVI, more than twice than those of forests. These findings reveal that factors beyond climate influence global long-term trends in NDVI and suggest that global climate change models and analyses of primary productivity should incorporate land use effects. C1 [Mueller, Thomas; Fagan, William F.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Mueller, Thomas; Boehning-Gaese, Katrin] Senckenberg Gesell Nat Forsch, Biodivers & Climate Res Ctr, D-60325 Frankfurt, Germany. [Mueller, Thomas; Boehning-Gaese, Katrin] Goethe Univ Frankfurt, Dept Biol Sci, D-60438 Frankfurt, Germany. [Mueller, Thomas; Leimgruber, Peter] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Dressler, Gunnar] UFZ Helmholtz Ctr Environm Res, Dept Ecol Modeling, D-04318 Leipzig, Germany. [Tucker, Compton J.; Pinzon, Jorge E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dubayah, Ralph O.; Hurtt, George C.] Univ Maryland, Dept Geog Sci, College Pk, MD 20771 USA. [Hurtt, George C.; Fagan, William F.] Natl Socioenvironm Synth Ctr SESYNC, Annapolis, MD 21401 USA. RP Mueller, T (reprint author), Univ Maryland, Dept Biol, College Pk, MD 20742 USA. EM muellert@gmail.com; gunnar.dressler@gmail.com; compton.j.tucker@nasa.gov; jorge.e.pinzon@nasa.gov; leimgruberp@si.edu; dubayah@umd.edu; gchurtt@umd.edu; katrin.boehning-gaese@senckenberg.de; bfagan@umd.edu RI Leimgruber, Peter/O-1304-2015 OI Leimgruber, Peter/0000-0002-3682-0153 FU NSF ABI [1062411]; Robert Bosch Foundation; National Socio-Environmental Synthesis Center (SESYNC) - National Science Foundation [DBI-1052875] FX WFF and TM were supported by NSF ABI award 1062411 and TM was supported by the Robert Bosch Foundation. This work was also supported by the National Socio-Environmental Synthesis Center (SESYNC) under funding received from the National Science Foundation DBI-1052875. NR 45 TC 8 Z9 8 U1 1 U2 13 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD JUN PY 2014 VL 6 IS 6 BP 5717 EP 5731 DI 10.3390/rs6065717 PG 15 WC Remote Sensing SC Remote Sensing GA AK9RB UT WOS:000338763300048 ER PT J AU Abergel, A Ade, PAR Aghanim, N Alves, MIR Aniano, G Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartett, JG Battaner, E Benabed, K Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bonaldi, A Bond, JR Bouchet, FR Boulanger, F Burigana, C Cardoso, JF Catalano, A Chamballu, A Chiang, HC Christensen, PR Clements, DL Colombi, S Colombo, LPL Couchot, F Crill, BP Cuttaia, F Danese, L 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 Efstathiou, G Ensslin, TA Eriksen, HK Falgarone, E Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Ganga, K Ghosh, T Giard, M Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gregorio, A Gruppuso, A Guillet, V Hansen, FK Harrison, D Helou, G Henrot-Versille, S Hernandez-Monteagudo, C Herranz, D Hildebrandt, SR Hivon, E Hobson, M Holmes, WA Hornstrup, A Hovest, W Huffenberger, KM Jaffe, AH Jaffe, TR Joncas, G Jones, A Jones, WC Juvela, M Kalberla, P Kaihanen, E Kerp, J Keskitalo, R Kisner, TS Kneissl, R Knoche, J Kunz, M Kurki-Suonio, H Lagache, G Lahteenmaki, A Lamarre, JM Lasenby, A Lawrence, CR Leonardi, R 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 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 Noviello, F Novikov, D Novikov, I Oxborrow, CA Pagano, L Pajot, F Paoletti, D Pasian, F Perdereau, O Perotto, L 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 Reach, WT Rebolo, R Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Roudier, G Rusholme, B Sandri, M Savini, G Spencer, LD Starck, JL Sureau, F Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Umana, G Valenziano, L Valiviita, J Van Tent, B Verstraete, L Vielva, P Villa, F Wade, LA Wandelt, BD Winkel, B Yvon, D Zacchei, A Zonca, A AF Abergel, A. Ade, P. A. R. Aghanim, N. Alves, M. I. R. Aniano, G. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartett, J. G. Battaner, E. Benabed, K. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bonaldi, A. Bond, J. R. Bouchet, F. R. Boulanger, F. Burigana, C. Cardoso, J. -F. Catalano, A. Chamballu, A. Chiang, H. C. Christensen, P. R. Clements, D. L. Colombi, S. Colombo, L. P. L. Couchot, F. Crill, B. P. Cuttaia, F. Danese, L. 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. Efstathiou, G. Ensslin, T. A. Eriksen, H. K. Falgarone, E. 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. Gregorio, A. Gruppuso, A. Guillet, V. Hansen, F. K. Harrison, D. Helou, G. Henrot-Versille, S. Hernandez-Monteagudo, C. Herranz, D. Hildebrandt, S. R. Hivon, E. Hobson, M. Holmes, W. A. Hornstrup, A. Hovest, W. Huffenberger, K. M. Jaffe, A. H. Jaffe, T. R. Joncas, G. Jones, A. Jones, W. C. Juvela, M. Kalberla, P. Kaihanen, E. Kerp, J. Keskitalo, R. Kisner, T. S. Kneissl, R. Knoche, J. Kunz, M. Kurki-Suonio, H. Lagache, G. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Lawrence, C. R. Leonardi, R. 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. 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. Noviello, F. Novikov, D. Novikov, I. Oxborrow, C. A. Pagano, L. Pajot, F. Paoletti, D. Pasian, F. Perdereau, O. Perotto, L. 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. Reach, W. T. Rebolo, R. Reinecke, M. Remazeilles, M. Renault, C. Ricciardi, S. Riller, T. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rusholme, B. Sandri, M. Savini, G. Spencer, L. D. Starck, J. -L. Sureau, F. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Tucci, M. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Verstraete, L. Vielva, P. Villa, F. Wade, L. A. Wandelt, B. D. Winkel, B. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck intermediate results XVII. Emission of dust in the diffuse interstellar medium from the far-infrared to microwave frequencies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE dust, extinction; submillimeter: ISM; local insterstellar matter; infrared: diffuse background; cosmic background radiation ID BACKGROUND EXPERIMENT SEARCH; ANISOTROPY-PROBE; MILKY-WAY; MAGNETIC NANOPARTICLES; SOLAR NEIGHBORHOOD; MOLECULAR-HYDROGEN; CENTIMETER EXCESS; GALACTIC EMISSION; MAGELLANIC STREAM; DATA RELEASE AB The dust-HI correlation is used to characterize the emission properties of dust in the diffuse interstellar medium (ISM) from far infrared wavelengths to microwave frequencies. The field of this investigation encompasses the part of the southern sky best suited to study the cosmic infrared and microwave backgrounds. We cross-correlate sky maps from Planck, the Wilkinson Microwave Anisotropy Probe (WMAP), and the diffuse infrared background experiment (DIRBE), at 17 frequencies from 23 to 3000 GHz, with the Parkes survey of the 21 cm line emission of neutral atomic hydrogen, over a contiguous area of 7500 deg(2) centred on the southern Galactic pole. We present a general methodology to study the dust-H I correlation over the sky, including simulations to quantify uncertainties. Our analysis yields four specific results. (1) We map the temperature, submillimetre emissivity, and opacity of the dust per H-atom. The dust temperature is observed to be anti-correlated with the dust emissivity and opacity. We interpret this result as evidence of dust evolution within the diffuse ISM. The mean dust opacity is measured to be (7.1 +/- 0.6) x 10(-27) cm(2) H-1 x (nu/353 GHz)(1.53 +/- 0.03) for 100 <= nu <= 353 GHz. This is a reference value to estimate hydrogen column densities from dust emission at submillimetre and millimetre wavelengths. (2) We map the spectral index beta(mm) of dust emission at millimetre wavelengths (defined here as nu <= 353GHz), and find it to be remarkably constant at beta(mm) = 1.51 +/- 0.13. We compare it with the far infrared spectral index beta(FIR) derived from greybody fits at higher frequencies, and find a systematic difference, beta(mm) - beta(FIR) = -0.15, which suggests that the dust spectral energy distribution (SED) flattens at nu <= 353 GHz. (3) We present spectral fits of the microwave emission correlated with Hi from 23 to 353 GHz, which separate dust and anomalous microwave emission (AME). We show that the flattening of the dust SED can be accounted for with an additional component with a blackbody spectrum. This additional component, which accounts for (26 +/- 6)% of the dust emission at 100GHz, could represent magnetic dipole emission. Alternatively, it could account for an increasing contribution of carbon dust, or a flattening of the emissivity of amorphous silicates, at millimetre wavelengths. These interpretations make different predictions for the dust polarization SED. (4) We analyse the residuals of the dust-Hi correlation. We identify a Galactic contribution to these residuals, which we model with variations of the dust emissivity on angular scales smaller than that of our correlation analysis. This model of the residuals is used to quantify uncertainties of the CIB power spectrum in a companion Planck paper. C1 [Bartett, J. G.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Piat, M.; Remazeilles, M.; Rosset, C.; Roudier, G.] Univ Paris Diderot, Sorbonne Paris Cite, Observ Paris, APC,CNRS,IN2P3,CEA Irfu, F-75205 Paris 13, France. [Lahteenmaki, A.] Aalto Univ, Metsahovi Radio Observ, Aalto 00076, Finland. [Lahteenmaki, A.] Aalto Univ, 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. [Kalberla, P.; Kerp, J.; Winkel, B.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Ashdown, M.; Hobson, M.; Lasenby, A.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Chiang, H. C.] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Math Stat & Comp Sci, ZA-4000 Durban, South Africa. [Kneissl, R.] ALMA Santiago Cent Off, Atacama Large Millimeter Submillimeter Array, Santiago, Chile. [Bond, J. R.; 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.] IRAP, CNRS, F-31028 Toulouse 4, France. [Dore, O.; Helou, G.; Hildebrandt, S. R.; Rocha, G.] CALTECH, Pasadena, CA 91125 USA. [Hernandez-Monteagudo, C.] CEFCA, Teruel 44001, Spain. [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.; Oxborrow, C. A.] Tech Univ Denmark, DTU Space, Natl Space Inst, DK-2800 Lyngby, Denmark. [Kunz, M.; Tucci, M.] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland. [Joncas, G.] Univ Laval, Dept Phys Genie Phys & Opt, Quebec City, PQ, Canada. [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. [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.; Kaihanen, E.; Kurki-Suonio, H.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Dept Phys, Helsinki 00014, Finland. [Chiang, H. C.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Lubin, P. M.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Wandelt, B. D.] Univ Illinois, Dept Phys, 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.; Maino, D.; Mennella, A.] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy. [Gregorio, A.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Mazzotta, P.] 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, San Cristobal la Laguna 38206, Tenerife, Spain. [Kneissl, R.] ESO Vitacura, European So Observ, Santiago, Chile. [Dupac, X.; Leonardi, R.; Mendes, L.] European Space Agcy, ESAC, Planck Sci Off, Madrid 28692, Spain. [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. [Umana, G.] INAF Osservatorio Astrofis Catania, I-95123 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. [Frailis, M.; Galeotta, S.; Gregorio, A.; Maris, M.; Pasian, F.; Zacchei, A.] INAF Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Massardi, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Burigana, C.; Cuttaia, F.; de Rosa, 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.] INAF IASF Bologna, I-40129 Bologna, Italy. [Bersanelli, M.; Donzelli, S.; Maino, D.; 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.; 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, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Rusholme, B.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Dole, H.] Inst Univ France, F-75005 Paris, France. [Abergel, A.; Aghanim, N.; Alves, M. I. R.; Aniano, G.; Aumont, J.; Boulanger, F.; Chamballu, A.; Dole, H.; Douspis, M.; Ghosh, T.; Guillet, V.; Jones, A.; Kunz, M.; Lagache, G.; Miville-Deschenes, M. -A.; Pajot, F.; Ponthieu, N.; Puget, J. -L.; Remazeilles, M.; Verstraete, L.] Univ Paris 11, CNRS, UMR8617, Inst Astrophys Spatiale, 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, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Popa, L.] Inst Space Sci, Bucharest, Romania. [Efstathiou, G.; 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, San Cristobal la Laguna 38205, Tenerife, Spain. [Barreiro, R. B.; 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. [Bartett, J. G.; Colombo, L. P. L.; Crill, B. P.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Lawrence, C. R.; Mitra, S.; Pietrobon, D.; Rocha, G.; Roudier, G.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Bonaldi, A.; Davis, R. J.; Dickinson, C.; Maffei, B.; Noviello, F.; Remazeilles, M.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Harrison, D.; Lasenby, A.; Migliaccio, M.; 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-91405 Orsay, France. [Catalano, A.; Falgarone, E.; Lamarre, J. -M.; Levrier, F.; 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, Lab AIM, IRFU Serv Astrophys, CEA DSM,CNRS,CEA Saclay, F-91191 Gif Sur Yvette, France. [Cardoso, J. -F.] CNRS, UMR 5141, Lab Traitement & Commun Informat, F-75634 Paris 13, France. [Cardoso, J. -F.] Telecom ParisTech, F-75634 Paris 13, France. [Catalano, A.; Macias-Perez, J. F.; Perotto, L.; Renault, C.] 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.; Rachen, J. P.; Reinecke, M.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth 12, Kildare, Ireland. [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 WC1E 6BT, England. [Baccigalupi, C.; Bielewicz, P.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Ade, P. A. R.; Munshi, D.; Spencer, L. D.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [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. [Reach, W. T.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, Moffett Field, CA 94035 USA. [Battaner, E.] Univ Granada, Dept Fis Teor & Cosmos, Fac Ciencias, Granada 411007, Spain. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Boulanger, F (reprint author), Univ Paris 11, CNRS, UMR8617, Inst Astrophys Spatiale, Batiment 121, F-91405 Orsay, France. EM francois.boulanger@ias.u-psud.fr RI 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; 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; Lahteenmaki, Anne/L-5987-2013; Martinez-Gonzalez, Enrique/E-9534-2015; Toffolatti, Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Gruppuso, Alessandro/N-5592-2015; Novikov, Dmitry/P-1807-2015; Lopez-Caniego, Marcos/M-4695-2013; Bobin, Jerome/P-3729-2014; Battaner, Eduardo/P-7019-2014; Vielva, Patricio/F-6745-2014; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; Remazeilles, Mathieu/N-1793-2015; OI 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; De Zotti, Gianfranco/0000-0003-2868-2595; Lopez-Caniego, Marcos/0000-0003-1016-9283; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Gruppuso, Alessandro/0000-0001-9272-5292; Bobin, Jerome/0000-0003-1457-7890; Vielva, Patricio/0000-0003-0051-272X; Barreiro, Rita Belen/0000-0002-6139-4272; Pierpaoli, Elena/0000-0002-7957-8993; Reach, William/0000-0001-8362-4094; 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; 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; WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Frailis, Marco/0000-0002-7400-2135; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; 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; Pasian, Fabio/0000-0002-4869-3227 FU Commonwealth of Australia; European Research Council under the European Union [267934] 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); ECT/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 he found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collabora tion. The Parkes Radio Telescope is part of the Australia Telescope, which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. 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. NR 91 TC 37 Z9 37 U1 3 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 JUN PY 2014 VL 566 AR A55 DI 10.1051/0004-6361/201323270 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500074 ER PT J AU Ade, PAR Aghanim, N Arnaud, M Ashdown, M Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartlett, JG Battaner, E Benabed, K Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bobin, J Bonaldi, A Bond, JR Bouchet, FR Burigana, C Cardoso, JF Catalano, A Chamballu, A Chiang, HC Christensen, PR Clements, DL Colombi, S Colombo, LPL Couchot, F 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 Ensslin, TA Eriksen, HK Finelli, F Forni, O Frailis, M Franceschi, E Galeotta, S Galli, S Ganga, K Giard, M Giraud-Heraud, Y Gonzalez-Nuevo, J Gorski, KM Gregorio, A Gruppuso, A Hansen, FK 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 Lawrence, CR Leonardi, R Liddle, A Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Maris, M Martin, PG Martinez-Gonzalez, E Masi, S Massardi, M Matarrese, S Mazzotta, P Melchiorri, A Mendes, L Mennella, A Migliaccio, M Mitra, S Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Munshi, D Murphy, JA Naselsky, P Nati, F Natoli, P Noviello, F Novikov, D Novikov, I Oxborrow, CA Pagano, L Pajot, F Paoletti, D Pasian, F Perdereau, O Perotto, L Perrotta, F Pettorino, V Piacentini, F Piat, M Pierpaoli, E Pietrobon, D Plaszczynski, S Pointecouteau, E Polenta, G Popa, L Pratt, GW Puget, JL Rachen, JP Rebolo, R Reinecke, M Remazeilles, M Renault, C Ricciardi, S Riller, T Ristorcelli, I Rocha, G Rosset, C Roudier, G d'Orfeuil, BR Rubino-Martin, JA Rusholme, B Sandri, M Savelainen, M Savini, G Spencer, LD Spinelli, M Starck, JL Sureau, F Sutton, D Suur-Uski, AS Sygnet, JF Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Tristram, M Tucci, M Umana, G Valenziano, L Valiviita, J Van Tent, B Vielva, P Villa, F Wade, LA Wandelt, BD White, M Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Arnaud, M. Ashdown, M. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartlett, J. G. Battaner, E. Benabed, K. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bobin, J. Bonaldi, A. Bond, J. R. Bouchet, F. R. Burigana, C. Cardoso, J. -F. Catalano, A. Chamballu, A. Chiang, H. C. Christensen, P. R. Clements, D. L. Colombi, S. Colombo, L. P. L. Couchot, F. 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. Ensslin, T. A. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Franceschi, E. Galeotta, S. Galli, S. Ganga, K. Giard, M. Giraud-Heraud, Y. Gonzalez-Nuevo, J. Gorski, K. M. Gregorio, A. Gruppuso, A. Hansen, F. K. 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. Lawrence, C. R. Leonardi, R. 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. Maris, M. Martin, P. G. Martinez-Gonzalez, E. Masi, S. Massardi, M. Matarrese, S. Mazzotta, P. Melchiorri, A. Mendes, L. Mennella, A. Migliaccio, M. Mitra, S. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Munshi, D. Murphy, J. A. Naselsky, P. Nati, F. Natoli, P. Noviello, F. Novikov, D. Novikov, I. Oxborrow, C. A. Pagano, L. Pajot, F. Paoletti, D. Pasian, F. Perdereau, O. Perotto, L. Perrotta, F. Pettorino, V. Piacentini, F. Piat, M. Pierpaoli, E. Pietrobon, D. Plaszczynski, S. Pointecouteau, E. Polenta, G. Popa, L. Pratt, G. W. 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. d'Orfeuil, B. Rouille Rubino-Martin, J. A. Rusholme, B. Sandri, M. Savelainen, M. Savini, G. Spencer, L. D. Spinelli, M. Starck, J. -L. Sureau, F. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Tristram, M. Tucci, M. Umana, G. Valenziano, L. Valiviita, J. Van Tent, B. Vielva, P. Villa, F. Wade, L. A. Wandelt, B. D. White, M. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck intermediate results XVI. Profile likelihoods for cosmological parameters SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmic background radiation; cosmology: observations; cosmology: theory; cosmological parameters; methods: statistical ID BARYON ACOUSTIC-OSCILLATIONS; DARK ENERGY AB We explore the 2013 Planck likelihood function with a high-precision multi-dimensional minimizer (Minuit). This allows a refinement of the ACDM best-fit solution with respect to previously-released results, and the construction of frequentist confidence intervals using profile likelihoods. The agreement with the cosmological results from the Bayesian framework is excellent, demonstrating the robustness of the Planck results to the statistical methodology. We investigate the inclusion of neutrino masses, where more significant differences may appear due to the non-Gaussian nature of the posterior mass distribution. By applying the Feldman-Cousins prescription, we again obtain results very similar to those of the Bayesian methodology. However, the profile-likelihood analysis of the cosmic microwave background (CMB) combination (Planck+WP+highL) reveals a minimum well within the unphysical negative-mass region. We show that inclusion of the Planck CMB-lensing information regularizes this issue, and provide a robust frequentist upper limit Sigma m(v) <= 0.26 eV (95% confidence) from the CMB+lensing+BAO data combination. C1 [Bartlett, J. G.; Cardoso, J. -F.; Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Piat, M.; Remazeilles, M.; Rosset, C.; Roudier, G.] Univ Paris Diderot, APC, CEA Irfu, Sorbonne Paris Cite,Observ Paris,CNRS,IN2PE, F-75205 Paris 13, France. [Lahteenmaki, A.] Aalto Univ, Metsahovi Radio Observ, Aalto 00076, Finland. [Lahteenmaki, A.] 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, I-00133 Rome, Italy. [Ashdown, M.; Hobson, M.; Lasenby, A.] Univ Cambridge, Astrophys Grp, Cavendish Lab, Cambridge CB3 0HE, England. [Chiang, H. C.] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Math Stat & Comp Sci, ZA-4000 Durban, South Africa. [Kneissl, R.] ALMA Santiago Cent Off, Atacama Large Millimeter Submillimeter Array, Santiago, Chile. [Bond, J. R.; Martin, P. G.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, Toronto, ON M55 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] IRAP, CNRS, F-31028 Toulouse 4, France. [Dore, O.; Hildebrandt, S. R.; Rocha, G.] CALTECH, Pasadena, CA 91125 USA. [Hernandez-Monteagudo, C.] CEFCA, Teruel 44001, Spain. [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, DSM Irfu SPP, F-91191 Gif Sur Yvette, France. [Hornstrup, A.; Linden-Vornle, M.; Oxborrow, C. A.] Tech Univ Denmark, DTU Space, Natl Space Inst, DK-2800 Lyngby, Denmark. [Kunz, M.; Pettorino, V.; Tucci, M.] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland. [Toffolatti, L.] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain. [Rachen, J. P.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [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. [Liddle, 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.; Savelainen, M.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Dept Phys, 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 94720 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.; Masi, S.; Melchiorri, A.; Nati, F.; Pagano, L.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Bersanelli, M.; Maino, D.; Mennella, A.; Tomasi, M.] Univ Milan, Dipartimento Fis, Milan, Italy. [Gregorio, A.] Univ Trieste, Dipartimento Fis, Trieste, Italy. [Mazzotta, P.] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy. [Christensen, P. R.; Naselsky, P.] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark. [Rebolo, R.; Rubino-Martin, J. A.] Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38206, Tenerife, Spain. 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[Burigana, C.; Cuttaia, F.; de Rosa, 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.] INAF IASF Bologna, Bologna, Italy. [Bersanelli, M.; Donzelli, S.; Maino, D.; Mennella, A.; 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, Ist Nazl Fis Nucl, Sez Roma 1, I-00185 Rome, Italy. [Gregorio, A.] Ist Nazl Fis Nucl, I-34127 Trieste, Italy. [Mitra, S.] IUCAA, Pune 411007, Maharashtra, India. [Clements, D. L.; Jaffe, A. H.; 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. [Dole, H.] Inst Univ France, F-75005 Paris, France. [Aghanim, N.; Aumont, J.; Chamballu, A.; Dole, H.; Douspis, M.; Kunz, M.; Lagache, G.; Miville-Deschenes, M. -A.; Pajot, F.; Puget, J. -L.; Remazeilles, M.] Univ Paris 11, CNRS, UMR 8617, Inst Astrophys Spatiale, F-91405 Orsay, France. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Cardoso, J. -F.; Colombi, S.; Galli, S.; Hivon, E.; Moneti, A.; Sygnet, J. -F.; Wandelt, B. D.] CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Popa, L.] Inst Space Sci, Bucharest, Romania. [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, Oslo, Norway. [Rebolo, R.; Rubino-Martin, J. A.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Barreiro, R. B.; 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.; Colombo, L. P. L.; Dore, O.; Gorski, K. M.; Holmes, W. A.; Lawrence, C. R.; Mitra, S.; Pietrobon, D.; Rocha, G.; Roudier, G.; Wade, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Bonaldi, A.; Davies, R. D.; Davis, R. J.; Dickinson, C.; Maffei, B.; Noviello, F.; Remazeilles, M.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Ashdown, M.; Harrison, D. L.; Lasenby, A.; Migliaccio, M.; Sutton, D.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Couchot, F.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; d'Orfeuil, B. Rouille; Spinelli, M.; Tristram, M.; Tucci, M.] Univ Paris 11, CNRS, IN2P3, LAL, F-91405 Orsay, France. [Catalano, A.; Lamarre, J. -M.; Roudier, G.] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Arnaud, M.; Bobin, J.; Chamballu, A.; Pratt, G. W.; Starck, J. -L.; Sureau, F.] Univ Paris Diderot, IRFU Serv Astrophys, Lab AIM, 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.] 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.; Rachen, J. P.; Reinecke, M.; Riller, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [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. [Savini, G.] UCL, Opt Sci Lab, London WC1E 6BT, England. [Baccigalupi, C.; Bielewicz, P.; Danese, L.; de Zotti, G.; Gonzalez-Nuevo, J.; Perrotta, F.] SISSA, Astrophys Sect, I-34136 Trieste, Italy. [Liddle, A.] Univ Edinburgh, SUPA, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ade, P. A. R.; Munshi, D.; Spencer, L. D.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Colombi, S.; Hivon, E.; 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. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teor & Cosmos, Granada, Spain. [Battaner, E.] Univ Granada, Inst Carlos Fis Teor & Computac 1, Granada, Spain. [Gorski, K. M.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Plaszczynski, S (reprint author), Univ Paris 11, CNRS, IN2P3, LAL, F-91405 Orsay, France. EM plaszczy@lal.in2p3.fr RI Gonzalez-Nuevo, Joaquin/I-3562-2014; White, Martin/I-3880-2015; Gruppuso, Alessandro/N-5592-2015; Lahteenmaki, Anne/L-5987-2013; Toffolatti, Luigi/K-5070-2014; Herranz, Diego/K-9143-2014; Lopez-Caniego, Marcos/M-4695-2013; Bobin, Jerome/P-3729-2014; Battaner, Eduardo/P-7019-2014; Vielva, Patricio/F-6745-2014; Barreiro, Rita Belen/N-5442-2014; Yvon, Dominique/D-2280-2015; Martinez-Gonzalez, Enrique/E-9534-2015; Remazeilles, Mathieu/N-1793-2015; 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; 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; OI Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; White, Martin/0000-0001-9912-5070; Gruppuso, Alessandro/0000-0001-9272-5292; Toffolatti, Luigi/0000-0003-2645-7386; Herranz, Diego/0000-0003-4540-1417; Bobin, Jerome/0000-0003-1457-7890; Vielva, Patricio/0000-0003-0051-272X; Barreiro, Rita Belen/0000-0002-6139-4272; Martinez-Gonzalez, Enrique/0000-0002-0179-8590; Pierpaoli, Elena/0000-0002-7957-8993; TERENZI, LUCA/0000-0001-9915-6379; Starck, Jean-Luc/0000-0003-2177-7794; Zacchei, Andrea/0000-0003-0396-1192; Hivon, Eric/0000-0003-1880-2733; Lilje, Per/0000-0003-4324-7794; Paoletti, Daniela/0000-0003-4761-6147; Savini, Giorgio/0000-0003-4449-9416; Sandri, Maura/0000-0003-4806-5375; Cuttaia, Francesco/0000-0001-6608-5017; Huffenberger, Kevin/0000-0001-7109-0099; Burigana, Carlo/0000-0002-3005-5796; Bouchet, Francois/0000-0002-8051-2924; Ricciardi, Sara/0000-0002-3807-4043; Villa, Fabrizio/0000-0003-1798-861X; Galeotta, Samuele/0000-0002-3748-5115; Pasian, Fabio/0000-0002-4869-3227; WANDELT, Benjamin/0000-0002-5854-8269; Finelli, Fabio/0000-0002-6694-3269; Umana, Grazia/0000-0002-6972-8388; Frailis, Marco/0000-0002-7400-2135; Lopez-Caniego, Marcos/0000-0003-1016-9283; Gregorio, Anna/0000-0003-4028-8785; Polenta, Gianluca/0000-0003-4067-9196; De Zotti, Gianfranco/0000-0003-2868-2595; Matarrese, Sabino/0000-0002-2573-1243; 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; Rubino-Martin, Jose Alberto/0000-0001-5289-3021 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 We thank F. Le Diberder for discussions about the Feldman-Cousins method. We gratefully acknowledge IN2P3 Computer Center (http://cc.in2p3.fr) for providing the computing resources and services needed to this work. 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, 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. NR 30 TC 28 Z9 28 U1 2 U2 18 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 JUN PY 2014 VL 566 AR A54 DI 10.1051/0004-6361/201323003 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500054 ER PT J AU Aleman, I Ueta, T Ladjal, D Exter, KM Kastner, JH Montez, R Tielens, AGGM Chu, YH Izumiura, H McDonald, I Sahai, R Siodmiak, N Szczerba, R van Hoof, PAM Villaver, E Vlemmings, W Wittkowski, M Zijlstra, AA AF Aleman, I. Ueta, T. Ladjal, D. Exter, K. M. Kastner, J. H. Montez, R., Jr. Tielens, A. G. G. M. Chu, Y. -H. Izumiura, H. McDonald, I. Sahai, R. Siodmiak, N. Szczerba, R. van Hoof, P. A. M. Villaver, E. Vlemmings, W. Wittkowski, M. Zijlstra, A. A. TI Herschel Planetary Nebula Survey (HerPlaNS) First detection of OH+ in planetary nebulae SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; circumstellar matter; planetary nebulae: general; planetary nebulae: individual: NGC 6445; planetary nebulae: individual: NGC 6720; planetary nebulae: individual: NGC 6781 ID INTERSTELLAR OH+; STAR-FORMATION; ORION-KL; MOLECULAR FRACTION; DIPOLE-MOMENT; H-2 EMISSION; HELIX-NEBULA; NGC 6781; ARP 220; SUBMILLIMETER AB Aims. We report the first detections of OH+ emission in planetary nebulae (PNe). Methods. As part of an imaging and spectroscopy survey of 11 PNe in the far-IR using the PACS and SPIRE instruments aboard the Herschel Space Observatory, we performed a line survey in these PNe over the entire spectral range between 51 mu m and 672 mu m to look for new detections. Results. The rotational emission lines of OH+ at 152.99, 290.20, 308.48, and 329.77 mu m were detected in the spectra of three planetary nebulae: NGC 6445, NGC6720, and NGC 6781. Excitation temperatures and column densities derived from these lines are in the range of 27-47 K and 2 x 10(10)-4 x 10(11) cm(-2), respectively. Conclusions. In PNe, the OH+ rotational line emission appears to be produced in the photodissociation region (PDR) in these objects. The emission of OH+ is observed only in PNe with hot central stars (T-eff > 100 000 K), suggesting that high-energy photons may play a role in OH+ formation and its line excitation in these objects, as seems to be the case for ultraluminous galaxies. C1 [Aleman, I.; Tielens, A. G. G. M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Ueta, T.; Ladjal, D.] Univ Denver, Dept Phys & Astron, Denver, CO 80210 USA. [Ueta, T.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Exter, K. M.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Leuven, Belgium. [Kastner, J. H.] Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. [Kastner, J. H.] Rochester Inst Technol, Lab Multiwavelength Astrophys, Rochester, NY 14623 USA. [Montez, R., Jr.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Chu, Y. -H.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Izumiura, H.] Natl Astron Observ Japan, Okayama Astrophys Observ, Asakuchi, Okayama 7190232, Japan. [McDonald, I.; Zijlstra, A. A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Sahai, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Siodmiak, N.; Szczerba, R.] N Copernicus Astron Ctr, PL-87100 Torun, Poland. [van Hoof, P. A. M.] Royal Observ Belgium, B-1180 Brussels, Belgium. [Villaver, E.] Univ Autonoma Madrid, Dept Fis Teor, Fac Ciencias, E-28049 Madrid, Spain. [Vlemmings, W.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Wittkowski, M.] ESO, D-85748 Garching, Germany. RP Aleman, I (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM aleman@strw.leidenuniv.nl RI Aleman, Isabel/F-3251-2012; OI /0000-0002-2700-9916 FU advanced-ERC grant from the European Research Council [246976]; Dutch Science Agency, NWO, as part of the Dutch Astrochemistry Network; NASA by JPL/Caltech; Japan Society of the Promotion of Science; Belgian Science Policy Office through the ESA/PRODEX program; Polish NUN [2011/01/B/ST9/02031]; Chandra X-ray Observatory Center [GO3-14019A, GO3-14019B]; NASA [NAS803060] FX We thank the anonymous referee for the invaluable suggestions to improve this paper Studies of interstellar chemistry at Leiden Observatory are supported through the advanced-ERC grant 246976 from the European Research Council; through a grant by the Dutch Science Agency, NWO, as part of the Dutch Astrochemistry Network, and through the Spinoza prize from the Dutch Science Agency, NWO. LA. is thankful for useful discussions with F. S. Cambiazo; M. Kama; and R. Meijerink. Support for this work was provided by NASA through an award issued by JPL/Caltech in support of Herschel Guest Observer programs (Ueta, Ladjal, Kastner, Sahai), by the Japan Society of the Promotion of Science through a FY2013 long-term invitation fellowship program (Ueta). K.M.E. and P.v.H, acknowledges support from the Belgian Science Policy Office through the ESA/PRODEX program. R.Sz. and N.S. acknowledge support from the Polish NUN grant 2011/01/B/ST9/02031. J.H.K.'s and R.M.'s research on planetary nebulae is supported via award numbers GO3-14019A to RIT and GO3-14019B to Vanderbilt University (respectively) issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS803060. This work is based on observations made with the Herschel Space Observatory, a European Space Agency (ESA) Cornerstone Mission with significant participation by NASA. NR 62 TC 9 Z9 9 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2014 VL 566 AR A79 DI 10.1051/0004-6361/201322940 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500045 ER PT J AU Drouart, G De Breuck, C Vernet, J Seymour, N Lehnert, M Barthel, P Bauer, FE Ibar, E Galametz, A Haas, M Hatch, N Mullaney, JR Nesvadba, N Rocca-Volmerange, B Rottgering, HJA Stern, D Wylezalek, D AF Drouart, G. De Breuck, C. Vernet, J. Seymour, N. Lehnert, M. Barthel, P. Bauer, F. E. Ibar, E. Galametz, A. Haas, M. Hatch, N. Mullaney, J. R. Nesvadba, N. Rocca-Volmerange, B. Rottgering, H. J. A. Stern, D. Wylezalek, D. TI Rapidly growing black holes and host galaxies in the distant Universe from the Herschel Radio Galaxy Evolution Project SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; quasars: general; galaxies: high-redshift; galaxies: evolution; quasars: supermassive black holes; infrared: galaxies ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMING GALAXIES; DEEP-FIELD-SOUTH; FAR-INFRARED PROPERTIES; LYMAN BREAK GALAXIES; Z-ALPHA CORRELATION; DIGITAL SKY SURVEY; GREATER-THAN 5; SIMILAR-TO 2.5 AB We present results from a comprehensive survey of 70 radio galaxies at redshifts 1 < z < 5 : 2 using the PACS and SPIRE instruments on board the Herschel Space Observatory. Combined with existing mid-IR photometry from the Spitzer Space Telescope, published 870 mu m photometry, and new observations obtained with LABOCA on the APEX telescope, the spectral energy distributions (SEDs) of galaxies in our sample are continuously covered across 3.6-870 mu m. The total 8-1000 mu m restframe infrared luminosities of these radio galaxies are such that almost all of them are either ultra-(L-tot(IR) > 10(12) L-circle dot) or hyper-luminous (L-tot(IR) > 10(13) L-circle dot) infrared galaxies. We fit the infrared SEDs with a set of empirical templates which represent dust heated by a variety of starbursts (SB) and by an active galactic nucleus (AGN). We find that the SEDs of radio galaxies require the dust to be heated by both AGN and SB, but the luminosities of these two components are not strongly correlated. Assuming empirical relations and simple physical assumptions, we calculate the star formation rate (SFR), the black hole mass accretion rate ((M) over dot(BH)), and the black hole mass (M-BH) for each radio galaxy. We find that the host galaxies and their black holes are growing extremely rapidly, having SFR approximate to 100-5000 M-circle dot yr(-1) and. (M) over dot(BH) approximate to 1-100 M(circle dot)yr(-1). The mean specific SFRs (sSFR) of radio galaxies at z > 2 : 5 are higher than the sSFR of typical star forming galaxies over the same redshift range, but are similar or perhaps lower than the galaxy population for radio galaxies at z < 2.5. By comparing the sSFR and the specific. (M) over dot(BH) (s(M) over dot(BH)), we conclude that black holes in radio loud AGN are already, or soon will be, overly massive compared to their host galaxies in terms of expectations from the local M-BH-M-Gal relation. In order to catch up with the black hole, the galaxies require about an order of magnitude more time to grow in mass at the observed SFRs compared to the time the black hole is actively accreting. However, during the current cycle of activity, we argue that this catching up is likely to be difficult because of the short gas depletion times. Finally, we speculate on how the host galaxies might grow sufficiently in stellar mass to ultimately fall onto the local MBH-MGal relation. C1 [Drouart, G.; De Breuck, C.; Vernet, J.; Wylezalek, D.] European So Observ, D-85748 Garching, Germany. [Drouart, G.; Lehnert, M.; Rocca-Volmerange, B.] Inst Astrophys, F-75014 Paris, France. [Drouart, G.; Seymour, N.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Drouart, G.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden. [Barthel, P.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. [Bauer, F. E.; Ibar, E.] Pontificia Univ Catlica Chile, Inst Astrofis, Fac Fis, Santiago 22, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Ibar, E.] Univ Valparaiso, Inst Fis & Astron, Valparaiso, Chile. [Galametz, A.] INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy. [Haas, M.] Ruhr Univ Bochum, Astron Inst, D-44801 Bochum, Germany. [Hatch, N.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Mullaney, J. R.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Nesvadba, N.] Univ Paris 11, Inst Astrophys Spatiale, CNRS, F-91405 Orsay, France. [Rottgering, H. J. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Drouart, G (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM guidro@chalmers.se RI Drouart, Guillaume/C-6049-2016; OI Drouart, Guillaume/0000-0003-2275-5466; Hatch, Nina/0000-0001-5600-0534; Vernet, Joel/0000-0002-8639-8560; Seymour, Nicholas/0000-0003-3506-5536; De Breuck, Carlos/0000-0002-6637-3315 FU Australian Research Council Future Fellowship; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT 1101024, Anillo ACT1101]; CONICYT/FONDECYT [3130504]; NASA FX G.D. warmly thanks Clive Tadhunter and Rob Ivison for their comments allowing a significative improvement of this paper. G.D. also thanks the referee for his comments that helped to clarify this paper. N.S. is the recipient of an Australian Research Council Future Fellowship. F.E.B. acknowledges support from Basal-CATA PFB-06/2007 and CONICYT-Chile grants FONDECYT 1101024 and Anillo ACT1101. E.I. acknowledges funding from CONICYT/FONDECYT postdoctoral project No: 3130504. The work of D.S. was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This work is based in part on observations made with the Spitzer Space Telescope. This work is based on observations made with the APEX Telescope, based on the Chajnantor Plateau in Chile. 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. Facilities: Spitzer, Herschel, APEX NR 192 TC 30 Z9 30 U1 1 U2 12 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2014 VL 566 AR A53 DI 10.1051/0004-6361/201323310 PG 36 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500081 ER PT J AU Krauss, F Kadler, M Mannheim, K Schulz, R Trustedt, J Wilms, J Ojha, R Ros, E Anton, G Baumgartner, W Beuchert, T Blanchard, J Burkel, C Carpenter, B Eberl, T Edwards, PG Eisenacher, D Elsasser, D Fehn, K Fritsch, U Gehrels, N Grafe, C Grossberger, C Hase, H Horiuchi, S James, C Kappes, A Katz, U Kreikenbohm, A Kreykenbohm, I Langejahn, M Leiter, K Litzinger, E Lovell, JEJ Muller, C Phillips, C Plotz, C Quick, J Steinbring, T Stevens, J Thompson, DJ Tzioumis, AK AF Krauss, F. Kadler, M. Mannheim, K. Schulz, R. Truestedt, J. Wilms, J. Ojha, R. Ros, E. Anton, G. Baumgartner, W. Beuchert, T. Blanchard, J. Buerkel, C. Carpenter, B. Eberl, T. Edwards, P. G. Eisenacher, D. Elsaesser, D. Fehn, K. Fritsch, U. Gehrels, N. Graefe, C. Grossberger, C. Hase, H. Horiuchi, S. James, C. Kappes, A. Katz, U. Kreikenbohm, A. Kreykenbohm, I. Langejahn, M. Leiter, K. Litzinger, E. Lovell, J. E. J. Mueller, C. Phillips, C. Ploetz, C. Quick, J. Steinbring, T. Stevens, J. Thompson, D. J. Tzioumis, A. K. TI TANAMI blazars in the IceCube PeV-neutrino fields SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE neutrinos; galaxies: active; quasars: general ID LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; VLBA CALIBRATOR SURVEY; HIGH-ENERGY NEUTRINOS; ALL-SKY SURVEY; SOFTWARE CORRELATOR; MISSION; CATALOG; ACCELERATION; ASTROPHYSICS AB The IceCube Collaboration has announced the discovery of a neutrino flux in excess of the atmospheric background. Owing to the steeply falling atmospheric background spectrum, events at PeV energies most likely have an extraterrestrial origin. We present the multiwavelength properties of the six radio-brightest blazars that are positionally coincident with these events using contemporaneous data of the TANAMI blazar sample, including high-resolution images and spectral energy distributions. Assuming the X-ray to gamma-ray emission originates in the photoproduction of pions by accelerated protons, the integrated predicted neutrino luminosity of these sources is high enough to explain the two detected PeV events. C1 [Krauss, F.; Schulz, R.; Truestedt, J.; Wilms, J.; Beuchert, T.; Buerkel, C.; Graefe, C.; Kreikenbohm, A.; Kreykenbohm, I.; Langejahn, M.; Leiter, K.; Litzinger, E.; Mueller, C.; Steinbring, T.] Univ Erlangen Nurnberg, Dr Remeis Sternwarte & ECAP, D-96049 Bamberg, Germany. [Krauss, F.; Kadler, M.; Mannheim, K.; Schulz, R.; Truestedt, J.; Beuchert, T.; Buerkel, C.; Eisenacher, D.; Elsaesser, D.; Graefe, C.; Kappes, A.; Kreikenbohm, A.; Langejahn, M.; Leiter, K.; Litzinger, E.; Mueller, C.; Steinbring, T.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [Ojha, R.; Baumgartner, W.; Gehrels, N.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ojha, R.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Ojha, R.; Carpenter, B.] Catholic Univ Amer, Washington, DC 20064 USA. [Ros, E.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Ros, E.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain. [Ros, E.] Astron Observ, Valencia 46980, Spain. [Anton, G.; Eberl, T.; Fehn, K.; Fritsch, U.; James, C.; Katz, U.] Univ Erlangen Nurnberg, ECAP, D-91058 Erlangen, Germany. [Blanchard, J.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Edwards, P. G.; Phillips, C.; Stevens, J.; Tzioumis, A. K.] CSIRO Astron & Space Sci, ATNF, Epping, NSW 1710, Australia. [Grossberger, C.] Max Planck Inst Extraterr Phys, D-85741 Bonn, Germany. [Hase, H.; Ploetz, C.] Bundesamt Kartog & Geodasie, D-93444 Bad Kotzting, Germany. [Horiuchi, S.] CSIRO Astron & Space Sci, Tuggeranong, ACT 2901, Australia. [Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Quick, J.] Hartebeesthoek Radio Astron Observ, Krugersdorp, South Africa. RP Krauss, F (reprint author), Univ Erlangen Nurnberg, Dr Remeis Sternwarte & ECAP, Sternwartstr 7, D-96049 Bamberg, Germany. EM Felicia.Krauss@fau.de RI Wilms, Joern/C-8116-2013; James, Clancy/G-9178-2015; Anton, Gisela/C-4840-2013; Eberl, Thomas/J-4826-2016; OI Wilms, Joern/0000-0003-2065-5410; Kadler, Matthias/0000-0001-5606-6154; James, Clancy/0000-0002-6437-6176; Anton, Gisela/0000-0003-2039-4724; Eberl, Thomas/0000-0002-5301-9106; Krauss, Felicia/0000-0001-6191-1244; Ros, Eduardo/0000-0001-9503-4892 FU Deutsche Forschungsgemeinschaft [WI 1860-10/1, GRK 1147]; Deutsches Zentrum fur Luft-und Raumfahrt grant [50 OR 1311/50 OR 1103]; Helmholtz Alliance for Astroparticle Physics (HAP); Spanish MINECO [AYA2009-13036-C02-02, AYA2012-38491-C02-01]; Generalitat Valenciana project [PROMETEO/2009/104]; COST [MP0905]; Commonwealth of Australia FX We thank the referee for the helpful comments. We acknowledge support and partial funding by the Deutsche Forschungsgemeinschaft grant WI 1860-10/1 (TANAMI) and GRK 1147, Deutsches Zentrum fur Luft-und Raumfahrt grant 50 OR 1311/50 OR 1103, and the Helmholtz Alliance for Astroparticle Physics (HAP). E.R. was partially supported by the Spanish MINECO projects AYA2009-13036-C02-02, and AYA2012-38491-C02-01 and by the Generalitat Valenciana project PROMETEO/2009/104, as well as by the COST MP0905 action "Black Holes in a Violent Universe". We thank J. E. Davis and T. Johnson for the development of the slxfig module and the SED scripts that have been used to prepare the figures in this work. This research has made use of a collection of ISIS scripts provided by the Dr. Karl Remeis-Observatory, Bamberg, Germany at http://www.sternwarte.uni-erlangen.de/isis/. The Long Baseline Array and Australia Telescope Compact Array are 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 Fermi-LAT Collaboration acknowledges support for LAT development, operation and data analysis from NASA and DOE (United States), CEA/Irfu and IN2P3/CNRS (France), ASI and INFN (Italy), MEXT, KEK, and JAXA (Japan), and the K.A. Wallenberg Foundation, the Swedish Research Council, and the National Space Board (Sweden). Science analysis support in the operations phase from INAF (Italy) and CNES (France) is also gratefully acknowledged. NR 51 TC 18 Z9 18 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2014 VL 566 AR L7 DI 10.1051/0004-6361/201424219 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500160 ER PT J AU Mookerjea, B Vastel, C Hassel, GE Gerin, M Pety, J Goldsmith, PF Black, JH Giesen, T Harrison, T Persson, CM Stutzki, J AF Mookerjea, B. Vastel, C. Hassel, G. E. Gerin, M. Pety, J. Goldsmith, P. F. Black, J. H. Giesen, T. Harrison, T. Persson, C. M. Stutzki, J. TI Detection of a dense clump in a filament interacting with W51e2 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: molecules; submillimeter: ISM; ISM: lines and bands; line: formation; line: identification; molecular data ID LOW-MASS PROTOSTAR; HERSCHEL/HIFI OBSERVATIONS; DEUTERIUM FRACTIONATION; NITROGEN HYDRIDES; DEUTERATED WATER; MOLECULAR CLOUD; STAR-FORMATION; GAS-PHASE; INTERSTELLAR AMMONIA; TRANSLUCENT CLOUDS AB In the framework of the Herschel/PRISMAS guaranteed time key program, the line of sight to the distant ultracompact H II region W51e2 has been observed using several selected molecular species. Most of the detected absorption features are not associated with the background high-mass star-forming region and probe the diffuse matter along the line of sight. We present here the detection of an additional narrow absorption feature at similar to 70 km s(-1) in the observed spectra of HDO, NH3 and C-3. The 70 km s(-1) feature is not uniquely identifiable with the dynamic components (the main cloud and the large-scale foreground filament) so-far identified toward this region. The narrow absorption feature is similar to the one found toward low-mass protostars, which is characteristic of the presence of a cold external envelope. The far-infrared spectroscopic data were combined with existing ground-based observations of (CO)-C-12, (CO)-C-13, CCH, CN, and C3H2 to characterize the 70 km s(-1) component. Using a non-LTE analysis of multiple transitions of NH3 and CN, we estimated the density (n(H-2) similar to (1-5) x 10(5) cm(-3)) and temperature (10-30 K) for this narrow feature. We used a gas-grain warm-up based chemical model with physical parameters derived from the NH3 data to explain the observed abundances of the different chemical species. We propose that the 70 km s(-1) narrow feature arises in a dense and cold clump that probably undergoes collapse to form a low-mass protostar, formed on the trailing side of the high-velocity filament, which is thought to be interacting with the W51 main cloud. While the fortuitous coincidence of the dense clump along the line of sight with the continuum-bright W51e2 compact HII region has contributed to its nondetection in the continuum images, this same attribute makes it an appropriate source for absorption studies and in particular for ice studies of star-forming regions. C1 [Mookerjea, B.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. [Vastel, C.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Vastel, C.] CNRS, IRAP, F-31028 Toulouse 4, France. [Hassel, G. E.; Harrison, T.] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. [Gerin, M.; Pety, J.] Observ Paris ENS, LERMA, F-75231 Paris 05, France. [Gerin, M.; Pety, J.] CNRS, UMR8112, F-75231 Paris 05, France. [Pety, J.] IRAM, F-38406 St Martin Dheres, France. [Goldsmith, P. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Black, J. H.; Persson, C. M.] Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden. [Giesen, T.] Univ Kassel, Inst Phys, D-34132 Kassel, Germany. [Stutzki, J.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. RP Mookerjea, B (reprint author), Tata Inst Fundamental Res, Homi Bhabha Rd, Bombay 400005, Maharashtra, India. EM bhaswati@tifr.res.in RI Giesen, Thomas /B-9476-2015; Goldsmith, Paul/H-3159-2016; OI Giesen, Thomas /0000-0002-2401-0049; PETY, Jerome/0000-0003-3061-6546; Black, John/0000-0001-7221-7207 FU Center for Undergraduate Research and Creative Activity (CURCA), Siena College; National Science Foundation [AST-9800334, AST-0098562, AST-0100793, AST-0228993, AST-0507657]; INSU/CNRS (France); MPG (Germany); IGN (Spain); National Aeronautics and Space Administration FX We thank the anonymous referee for the suggestions that helped improve the clarity of the paper significantly. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany. France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON; TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologa (CSIC-INTA). Sweden: Chalmers University of Technology - MC2; RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. G. Hassel gratefully acknowledges helpful discussions and rate information provided by Yuri Aikawa, C. Vastel is grateful to F. Lique for providing the CN collisional rates in the LAMDA database format. T. Harrison thanks the Summer Scholars grant from the Center for Undergraduate Research and Creative Activity (CURCA), Siena College. This paper has made extensive use of the SIMBAD database, operated at CDS, Strasbourg, France. This publication makes use of molecular line data from the Boston University-FCRAO Galactic Ring Survey (GRS). The GRS is a joint project of Boston University and Five College Radio Astronomy Observatory, funded by the National Science Foundation under grants AST-9800334, AST-0098562, AST-0100793, AST-0228993, & AST-0507657. This paper is partly based on observations obtained with the TRAM Plateau de Bure interferometer and 30 m telescope. We are grateful to the IRAM staff at Plateau de Bure, Grenoble for their support during the observations and data reductions. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 72 TC 6 Z9 6 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2014 VL 566 AR A61 DI 10.1051/0004-6361/201323131 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500064 ER PT J AU Nucita, AA Kuulkers, E De Paolis, F Mukai, K Ingrosso, G Maiolo, BMT AF Nucita, A. A. Kuulkers, E. De Paolis, F. Mukai, K. Ingrosso, G. Maiolo, B. M. T. TI XMM-Newton and Swift observations of WZ Sagittae: spectral and timing analysis SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE binaries: general; white dwarfs; X-rays: binaries ID HUBBLE-SPACE-TELESCOPE; RAY POWER SPECTRA; X-RAY; CATACLYSMIC VARIABLES; ACCRETION DISKS; 2001 OUTBURST; LIGHT CURVES; GW-LIBRAE; OSCILLATIONS; GALAXIES AB Context. WZ Sagittae is the prototype object of a subclass of dwarf novae with rare and long (super) outbursts, in which a white dwarf primary accretes matter from a low mass companion. High-energy observations offer the possibility of a better understanding of the disk-accretion mechanism in WZ Sge-like binaries. Aims. We used archival XMM-Newton and Swift data to characterize the X-ray spectral and temporal properties of WZ Sge in quiescence. Methods. We performed a detailed timing analysis of the simultaneous X-ray and UV light curves obtained with the EPIC and OM instruments on board XMM-Newton in 2003. We employed several techniques in this study, including a correlation study between the two curves. We also performed an X-ray spectral analysis using the EPIC data and Swift/XRT data obtained in 2011. Results. We find that the X-ray intensity is clearly modulated at a period of similar or equal to 28.96 s, confirming previously published preliminary results. We find that the X-ray spectral shape of WZ Sge remains practically unchanged between the XMM-Newton and Swift observations. However, after correcting for interstellar absorption, the intrinsic luminosity is estimated to be L-X(Una) = (2.65 +/- 0.06) x10(30) erg s(-1) and L-X(Una) = (1.57 +/- 0.03) x10(30) erg s(-1) in 2003 and 2011, respectively. During the Swift/XRT observation, the observed flux is a factor similar or equal to 2 lower than that observed by XMM-Newton but is similar to the quiescent levels that are observed various times before the 2001 outburst. C1 [Nucita, A. A.; De Paolis, F.; Ingrosso, G.; Maiolo, B. M. T.] Univ Salento, Dept Math & Phys E De Giorgi, I-73100 Lecce, Italy. [Nucita, A. A.; De Paolis, F.; Ingrosso, G.; Maiolo, B. M. T.] Ist Nazl Fis Nucl, Sez Lecce, I-73100 Lecce, Italy. [Kuulkers, E.] European Space Astron Ctr, SRE O, Villanueva De La Canada 28691, Madrid, Spain. [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. RP Nucita, AA (reprint author), Univ Salento, Dept Math & Phys E De Giorgi, Via Arnesano,CP 193, I-73100 Lecce, Italy. EM nucita@le.infn.it FU ESA Member States; NASA FX K.M. thanks Paula Szkody for informative discussion on the latest results of pulsations in low accretion rate CVs. This paper is based on observations from XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. Part of this work is based on archival data, software or online services provided by the AS! Science Data Center (ASDC), Italy. We are also in debt with the anonymous referee for pointing us a problem in the Swift analysis. NR 59 TC 1 Z9 1 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2014 VL 566 AR A121 DI 10.1051/0004-6361/201322875 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500040 ER PT J AU Puspitarini, L Lallement, R Vergely, JL Snowden, SL AF Puspitarini, L. Lallement, R. Vergely, J. -L. Snowden, S. L. TI Local ISM 3D distribution and soft X-ray background Inferences on nearby hot gas and the North Polar Spur SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: bubbles; ISM: structure; X-rays: diffuse background; local insterstellar matter; solar neighborhood; ISM: general ID CHARGE-EXCHANGE EMISSION; SOLAR-WIND; SPATIAL-DISTRIBUTION; INTERSTELLAR-MEDIUM; GALACTIC-CENTER; ROSAT SURVEY; BUBBLE; MAPS; MODEL; HI AB Three-dimensional (3D) interstellar medium (ISM) maps can be used to locate not only interstellar (IS) clouds, but also IS bubbles between the clouds that are blown by stellar winds and supernovae, and that are filled by hot gas. To demonstrate this and to derive a clearer picture of the local ISM, we compare our recent 3D maps of the IS dust distribution to the ROSAT diffuse X-ray background maps after removing heliospheric emission. In the Galactic plane, there is a good correspondence between the locations and extents of the mapped nearby cavities and the soft (0.25 keV) background emission distribution, showing that most of these nearby cavities contribute to this soft X-ray emission. Assuming a constant dust-to-gas ratio and homogeneous 106 K hot gas filling the cavities, we modeled the 0.25 keV surface brightness in a simple way along the Galactic plane as seen from the Sun, taking the absorption by the mapped clouds into account. The data-model comparison favors the existence of hot gas in the solar neighborhood, the so-called Local Bubble (LB). The inferred average mean pressure in the local cavities is found to be on the order of 10 000 cm(-3) K, in agreement with previous studies, providing a validation test for the method. On the other hand, the model overestimates the emission from the huge cavities located in the third quadrant. Using CaII absorption data, we show that the dust-to-CaII ratio is very low in this region, implying there is a large quantity of lower temperature (non-X-ray emitting) ionized gas and, as a consequence, a reduction in the volume filled by hot gas, explaining at least part of the discrepancy. In the meridian plane, the main two brightness enhancements coincide well with the LB's most elongated parts and chimneys connecting the LB to the halo, but no particular nearby cavity is found towards the enhancement in the direction of the bright North Polar Spur (NPS) at high latitude. We searched in the 3D maps for the source regions of the higher energy (0.75 keV) enhancements in the fourth and first quadrants. Tunnels and cavities are found to coincide with the main bright areas; however, no tunnel or cavity is found to match the low-latitude b greater than or similar to 8 degrees, brightest part of the NPS. In addition, the comparison between the 3D maps and published spectral data do not favor the nearby cavities being located within similar to 200 pc as potential source regions for the NPS. Those examples illustrate the potential use of more detailed 3D distributions of the nearby ISM for interpreting the diffuse soft X-ray background. C1 [Puspitarini, L.; Lallement, R.] Univ Paris Diderot, CNRS, GEPI Observ Paris, F-92190 Meudon, France. [Vergely, J. -L.] ACRI ST, F-06904 Sophia Antipolis, France. [Snowden, S. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Puspitarini, L (reprint author), Univ Paris Diderot, CNRS, GEPI Observ Paris, Pl Jules Janssen, F-92190 Meudon, France. EM lucky.puspitarini@obspm.fr; rosine.lallement@obspm.fr; jeanluc.vergely@latmos.ipsl.fr; steven.l.snowden@nasa.gov FU French Research Agency (ANR) as part of the STILISM project FX We thank our anonymous referee for the numerous constructive comments on the manuscript. They resulted in a significant improvement of the article. J.L.V., R.L., and L.P. acknowledge funding by the French Research Agency (ANR) as part of the STILISM project. NR 44 TC 16 Z9 16 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2014 VL 566 AR A13 DI 10.1051/0004-6361/201322942 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500047 ER PT J AU Rauch, T Werner, K Quinet, P Kruk, JW AF Rauch, T. Werner, K. Quinet, P. Kruk, J. W. TI Stellar laboratories III. New Ba V, Ba VI, and Ba VII oscillator strengths and the barium abundance in the hot white dwarfs G191-B2B and RE 0503-289 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE atomic data; line: identification; stars: abundances; stars: individual: G191-B2B; stars: individual: RE 0503-289; virtual observatory tools ID NUCLEOSYNTHESIS; VALIDATION AB Context. For the spectral analysis of high-resolution and high-signal-to-noise (S/N) spectra of hot stars, state-of-the-art non-local thermodynamic equilibrium (NLTE) model atmospheres are mandatory. These are strongly dependent on the reliability of the atomic data that is used for their calculation. Aims. Reliable Ba V-VII oscillator strengths are used to identify Ba lines in the spectra of the DA-type white dwarf G191-B2B and the DO-type white dwarf RE 0503-289 and to determine their photospheric Ba abundances. Methods. We newly calculated Ba V-VII oscillator strengths to consider their radiative and collisional bound-bound transitions in detail in our NLTE stellar-atmosphere models for the analysis of Ba lines exhibited in high-resolution and high-S/N UV observations of G191-B2B and RE 0503-289. Results. For the first time, we identified highly ionized Ba in the spectra of hot white dwarfs. We detected Ba VI and Ba VII lines in the Far Ultraviolet Spectroscopic Explorer (FUSE) spectrum of RE 0503-289. The Ba VI/Ba VII ionization equilibrium is well reproduced with the previously determined effective temperature of 70 000 K and surface gravity of log g = 7.5. The Ba abundance is 3.5 +/- 0.5 x 10(-4) (mass fraction, about 23 000 times the solar value). In the FUSE spectrum of G191-B2B, we identified the strongest Ba NTH line (at 993.41 angstrom) only, and determined a Ba abundance of 4.0 +/- 0.5 x 10(-6) (about 265 times solar). Conclusions. Reliable measurements and calculations of atomic data are a pre-requisite for stellar-atmosphere modeling. Observed Ba VI-VII line profiles in two white dwarfs' (G191-B2B and RE 0503-289) far-ultraviolet spectra were well reproduced with our newly calculated oscillator strengths. This allowed to determine the photospheric Ba abundance of these two stars precisely. C1 [Rauch, T.; Werner, K.] Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Quinet, P.] Univ Mons UMONS, B-7000 Mons, Belgium. [Quinet, P.] Univ Liege, IPNAS, B-4000 Liege, Belgium. [Kruk, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Rauch, T (reprint author), Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany. EM rauch@astro.uni-tuebingen.de FU German Aerospace Center (DLR) [05 OR 1301]; Belgian FRS-FNRS; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G] FX T.R. is supported by the German Aerospace Center (DLR, grant 05 OR 1301). Financial support from the Belgian FRS-FNRS is also acknowledged. P.Q. is research director of this organization. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. NR 17 TC 11 Z9 11 U1 2 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 JUN PY 2014 VL 566 AR A10 DI 10.1051/0004-6361/201423878 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500148 ER PT J AU Rauch, T Rudkowski, A Kampka, D Werner, K Kruk, JW Moehler, S AF Rauch, T. Rudkowski, A. Kampka, D. Werner, K. Kruk, J. W. Moehler, S. TI The virtual observatory service TheoSSA: Establishing a database of synthetic stellar flux standards II. NLTE spectral analysis of the OB-type subdwarf Feige 110 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE standards; stars: abundances; stars: atmospheres; stars: individual: Feige 110; subdwarfs; virtual observatory tools ID ACCELERATED LAMBDA-ITERATION; HUBBLE SPACE TELESCOPE; NON-LTE ANALYSIS; TO-OXYGEN RATIO; MODEL ATMOSPHERES; HOT STARS; INTERSTELLAR-MEDIUM; WHITE-DWARFS; SDOB PRIMARY; LB 3459 AB Context. In the framework of the Virtual Observatory (VO), the German Astrophysical VO (GAVO) developed the registered service TheoSSA (Theoretical Stellar Spectra Access). It provides easy access to stellar spectral energy distributions (SEDs) and is intended to ingest SEDs calculated by any model-atmosphere code, generally for all effective temperatures, surface gravities, and elemental compositions. We will establish a database of SEDs of flux standards that are easily accessible via TheoSSA's web interface. Aims. The OB-type subdwarf Feige 110 is a standard star for flux calibration. State-of-the-art non-local thermodynamic equilibrium stellar-atmosphere models that consider opacities of species up to trans-iron elements will be used to provide a reliable synthetic spectrum to compare with observations. Methods. In case of Feige 110, we demonstrate that the model reproduces not only its overall continuum shape from the far-ultraviolet (FUV) to the optical wavelength range but also the numerous metal lines exhibited in its FUV spectrum. Results. We present a state-of-the-art spectral analysis of Feige 110. We determined T-eff = 47 250 +/- 2000 K, log g=6.00 +/- 0.20, and the abundances of He, N, P, S, Ti, V, Cr, Mn, Fe, Co, Ni, Zn, and Ge. Ti, V, Mn, Co, Zn, and Ge were identified for the first time in this star. Upper abundance limits were derived for C, O, Si, Ca, and Sc. Conclusions. The TheoSSA database of theoretical SEDs of stellar flux standards guarantees that the flux calibration of astronomical data and cross-calibration between different instruments can be based on models and SEDs calculated with state-of-the-art model-atmosphere codes. C1 [Rauch, T.; Rudkowski, A.; Kampka, D.; Werner, K.] Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Kruk, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Moehler, S.] European So Observ, D-85748 Garching, Germany. RP Rauch, T (reprint author), Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany. EM rauch@astro.uni-tuebingen.de FU German Aerospace Center (DLR) [05 OR 1301]; Federal Ministry of Education and Research (BMBF) [05 AC 6 VTB, 05 AC 11 VTB]; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G] FX T.R. is supported by the German Aerospace Center (DLR, grant 05 OR 1301). The GAVO project at Tubingen has been supported by the Federal Ministry of Education and Research (BMBF, grants 05 AC 6 VTB, 05 AC 11 VTB). This work used the profile-fitting procedure OWENS developed by M. Lemoine and the FUSE French Team. This research has made use of the SIMBAD database, operated at the CDS, Strasbourg, France. This research has made use of NASA's Astrophysics Data System. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-FIST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. The TIRO service (http : //astro-uni - tuebingen. de/similar to TIRO) used to calculate opacities for this paper was constructed as part of the activities of the German Astrophysical Virtual Observatory. The TMAW service (http : //astro-uni - tuebingen. de/similar to TMAW) used to calculate theoretical spectra for this paper was constructed as part of the activities of the German Astrophysical Virtual Observatory. NR 43 TC 6 Z9 6 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2014 VL 566 AR A3 DI 10.1051/0004-6361/201423711 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500129 ER PT J AU Reindl, N Rauch, T Werner, K Kruk, JW Todt, H AF Reindl, N. Rauch, T. Werner, K. Kruk, J. W. Todt, H. TI On helium-dominated stellar evolution: the mysterious role of the O(He)-type stars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: AGB and post-AGB; stars: evolution; stars: fundamental parameters; stars: abundances ID DIGITAL-SKY-SURVEY; SUBDWARF-O-STARS; COMMON ENVELOPE EVOLUTION; DEFICIENT CENTRAL STAR; SUBLUMINOUS B-STARS; PRE-WHITE-DWARFS; POST-AGB STARS; PLANETARY-NEBULA; SPECTRAL-ANALYSIS; ATMOSPHERIC PARAMETERS AB Context. About a quarter of all post-asymptotic giant branch (AGB) stars are hydrogen-deficient. Stellar evolutionary models explain the carbon-dominated H-deficient stars by a (very) late thermal pulse scenario where the hydrogen-rich envelope is mixed with the helium-rich intershell layer. Depending on the particular time at which the final flash occurs, the entire hydrogen envelope may be burned. In contrast, helium-dominated post-AGB stars and their evolution are not yet understood. Aims. A small group of very hot, helium-dominated stars is formed by O(He)-type stars. A precise analysis of their photospheric abundances will establish constraints to their evolution. Methods. We performed a detailed spectral analysis of ultraviolet and optical spectra of four O(He) stars by means of state-of-the-art non-LTE model-atmosphere techniques. Results. We determined effective temperatures, surface gravities, and the abundances of H, He, C, N, O, F, Ne, Si, P, S, Ar, and Fe. By deriving upper limits for the mass-loss rates of the O(He) stars, we found that they do not exhibit enhanced mass-loss. The comparison with evolutionary models shows that the status of the O(He) stars remains uncertain. Their abundances match predictions of a double helium white dwarf (WD) merger scenario, suggesting that they might be the progeny of the compact and of the luminous helium-rich sdO-type stars. The existence of planetary nebulae that do not show helium enrichment around every other O(He) star precludes a merger origin for these stars. These stars must have formed in a different way, for instance via enhanced mass-loss during their post-AGB evolution or a merger within a common-envelope (CE) of a CO-WD and a red giant or AGB star. Conclusions. A helium-dominated stellar evolutionary sequence exists that may be fed by different types of mergers or CE scenarios. It appears likely that all these pass through the O(He) phase just before they become WDs. C1 [Reindl, N.; Rauch, T.; Werner, K.] Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, D-72076 Tubingen, Germany. [Kruk, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Todt, H.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. RP Reindl, N (reprint author), Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, Sand 1, D-72076 Tubingen, Germany. EM reindl@astro.uni-tuebingen.de FU German Research Foundation (DFG) [WE 1312/41-1]; German Aerospace Center (DLR) [05 OR 1301]; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G] FX N.R. is supported by the German Research Foundation (DFG, grant WE 1312/41-1), T.R. by the German Aerospace Center (DLR, grant 05 OR 1301). We thank Marcelo Miguel Miller Bertolami, Simon Jeffery, Stephan Geier, and Geoffrey Clayton for helpful discussions and comments. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This research has made use of NASA's Astrophysics Data System. This work used the profile-fitting procedure OWENS developed by M. Lemoine and the FUSE French Team. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScl is operated by the Association of Universities for Research in Astronomy. Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. NR 60 TC 12 Z9 12 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2014 VL 566 AR A116 DI 10.1051/0004-6361/201423498 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500106 ER PT J AU Rosenberg, MJF Berne, O Boersma, C AF Rosenberg, Marissa J. F. Berne, Olivier Boersma, Christiaan TI Random mixtures of polycyclic aromatic hydrocarbon spectra match interstellar infrared emission SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: general; ISM: lines and bands; infrared: ISM; astrochemistry ID SPITZER-SPACE-TELESCOPE; SPECTROSCOPIC DATABASE; PAH MOLECULES; RED-RECTANGLE; BANDS; FEATURES; CARRIERS; CATIONS; MODEL; DUST AB The mid-infrared (mid-IR; 5-15 mu m) spectrum of a wide variety of astronomical objects exhibits a set of broad emission features at 6.2, 7.7, 8.6, 11.3, and 12.7 mu m. About 30 years ago it was proposed that these signatures are due to emission from a family of UV heated nanometer-sized carbonaceous molecules known as polycyclic aromatic hydrocarbons (PAHs), causing them to be referred to as aromatic IR bands (AIBs). Today, the acceptance of the PAH model is far from settled, as the identification of a single PAH in space has not yet been successful, and physically relevant theoretical models involving true PAH cross sections do not reproduce the AIBs in detail. In this paper, we use the NASA Ames PAH IR Spectroscopic Database, which contains over 500 quantum-computed spectra, in conjunction with a simple emission model, to show that the spectrum produced by any random mixture of at least 30 PAHs converges to the same kernel-spectrum. This kernel-spectrum captures the essence of the PAH emission spectrum and is highly correlated with observations of AIBs, strongly supporting PAHs as their source. Furthermore, the fact that a large number of molecules are required implies that spectroscopic signatures of the individual PAHs contributing to the AIBs spanning the visible, near-IR, and far-IR spectral regions are weak, explaining why they have not yet been detected. An improved effort, joining laboratory, theoretical, and observational studies of the PAH emission process, will support the use of PAH features as a probe of physical and chemical conditions in the near and distant Universe. C1 [Rosenberg, Marissa J. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Berne, Olivier] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Berne, Olivier] CNRS, IRAP, F-31028 Toulouse 4, France. [Boersma, Christiaan] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Rosenberg, MJF (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM rosenberg@strw.leidenuniv.nl RI Boersma, Christiaan/L-7696-2014 OI Boersma, Christiaan/0000-0002-4836-217X FU NASA's Laboratory Astrophysics, "Carbon in the Galaxy" consortium grant [NNH10ZDA001N] FX C. Boersma acknowledges support from NASA's Laboratory Astrophysics, "Carbon in the Galaxy" consortium grant (NNH10ZDA001N) and is grateful for an appointment at NASA's Ames Research Center through San Jose State University Research Foundation (NNX11AJ33A). We thank K. Dasyra for providing her stacked IRS spectra of luminous galaxies. NR 43 TC 4 Z9 4 U1 3 U2 13 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2014 VL 566 AR L4 DI 10.1051/0004-6361/201423953 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500157 ER PT J AU Schilke, P Neufeld, DA Muller, HSP Comito, C Bergin, EA Lis, DC Gerin, M Black, JH Wolfire, M Indriolo, N Pearson, JC Menten, KM Winkel, B Sanchez-Monge, A Moller, T Godard, B Falgarone, E AF Schilke, P. Neufeld, D. A. Mueller, H. S. P. Comito, C. Bergin, E. A. Lis, D. C. Gerin, M. Black, J. H. Wolfire, M. Indriolo, N. Pearson, J. C. Menten, K. M. Winkel, B. Sanchez-Monge, A. Moeller, T. Godard, B. Falgarone, E. TI Ubiquitous argonium (ArH+) in the diffuse interstellar medium: molecular tracer of almost purely atomic gas SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; line: identification; molecular processes; ISM: abundances; ISM: molecules; ISM: structure ID COSMIC-RAY IONIZATION; STAR-FORMING REGIONS; EXTRAORDINARY SOURCES HEXOS; ROTATIONAL SPECTRUM; DISSOCIATIVE RECOMBINATION; HERSCHEL/HIFI DISCOVERY; ABSORPTION-SPECTROSCOPY; HETERODYNE INSTRUMENT; COLOGNE DATABASE; GROUND-STATE AB Aims. We describe the assignment of a previously unidentified interstellar absorption line to ArH+ and discuss its relevance in the context of hydride absorption in diffuse gas with a low H-2 fraction. The confidence of the assignment to ArH+ is discussed, and the column densities are determined toward several lines of sight. The results are then discussed in the framework of chemical models, with the aim of explaining the observed column densities. Methods. We fitted the spectral lines with multiple velocity components, and determined column densities from the line-to-continuum ratio. The column densities of ArH+ were compared to those of other species, tracing interstellar medium (ISM) components with different H-2 abundances. We constructed chemical models that take UV radiation and cosmic ray ionization into account. Results. Thanks to the detection of two isotopologues, (ArH+)-Ar-36 and (ArH+)-Ar-38, we are confident about the carrier assignment to NeH+. is not detected with a limit of [NeH+]/[ArH+] <= 0.1. The derived column densities agree well with the predictions of chemical models. ArH+ is a unique tracer of gas with a fractional H-2 abundance of 10(-4)-10(-3) and shows little correlation to H2O+, which traces gas with a fractional H2 abundance of Conclusions. A careful analysis of variations in the ArH+, OH, H2O+, and HF column densities promises to be a faithful tracer of the distribution of the H-2 fractional abundance by providing unique information on a poorly known phase in the cycle of interstellar matter and on its transition from atomic diffuse gas to dense molecular gas traced by CO emission. Abundances of these species put strong observational constraints upon magnetohydrodynamical (MHD) simulations of the interstellar medium, and potentially could evolve into a tool characterizing the ISM. Paradoxically, the ArH+ molecule is a better tracer of almost purely atomic hydrogen gas than Hi itself. since Hi can also be present in gas with a significant molecular content, but ArH+ singles out gas that is >99.9% atomic. C1 [Schilke, P.; Mueller, H. S. P.; Comito, C.; Sanchez-Monge, A.; Moeller, T.] Univ Cologne, Inst Phys, D-50937 Cologne, Germany. [Neufeld, D. A.; Indriolo, N.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Lis, D. C.] CALTECH, Pasadena, CA 91125 USA. [Lis, D. C.] Univ Paris 06, Sorbonne Univ, CNRS, Observ Paris,LERMA,UMR 8112, Paris, France. [Gerin, M.; Godard, B.; Falgarone, E.] CNRS, LERMA, UMR 8112, Observ Paris, F-75005 Paris, France. [Gerin, M.; Godard, B.; Falgarone, E.] Ecole Normale Super, F-75005 Paris, France. [Black, J. H.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden. [Wolfire, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Menten, K. M.; Winkel, B.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Schilke, P (reprint author), Univ Cologne, Inst Phys, Zulpicher Str 77, D-50937 Cologne, Germany. EM schilke@ph1.uni-koeln.de OI Indriolo, Nick/0000-0001-8533-6440; Black, John/0000-0001-7221-7207 FU German Deutsche Forschungsgemeinschaft in the Collaborative Research Center [SFB956]; German Ministry of Science (BMBF) [05A11PK3]; NASA; Bundesministerium fur Bildung und Forschung (BMBF) [FKZ 50OF0901] FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U.Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUT 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 & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. H.S.P.M. is very grateful to the Bundesministerium fur Bildung und Forschung (BMBF) for initial support through project FKZ 50OF0901 (ICC HIFI Herschel) aimed at maintaining the Cologne Database for Molecular Spectroscopy, CDMS. This support has been administered by the Deutsches Zentrum fur Luft- und Raumfahrt (DLR). Part of this work was supported by the German Deutsche Forschungsgemeinschaft in the Collaborative Research Center SFB956, and by the German Ministry of Science (BMBF) trough contract 05A11PK3. This work also has been supported by NASA through an award issued by JPL/Caltech. We thank Christian Endres for tireless work on the molecular line catalog implementation. NR 87 TC 33 Z9 33 U1 1 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 JUN PY 2014 VL 566 AR A29 DI 10.1051/0004-6361/201423727 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500135 ER PT J AU Schulze, S Malesani, D Cucchiara, A Tanvir, NR Kruhler, T Postigo, AD Leloudas, G Lyman, J Bersier, D Wiersema, K Perley, DA Schady, P Gorosabel, J Anderson, JP Castro-Tirado, AJ Cenko, SB De Cia, A Ellerbroek, LE Fynbo, JPU Greiner, J Hjorth, J Kann, DA Kaper, L Klose, S Levan, AJ Martin, S O'Brien, PT Page, KL Pignata, G Rapaport, S Sanchez-Ramirez, R Sollerman, J Smith, IA Sparre, M Thone, CC Watson, DJ Xu, D Bauer, EE Bayliss, M Bjornsson, G Bremer, M Cano, Z Covino, S D'Elia, V Frail, DA Geier, S Goldoni, P Hartoog, OE Jakobsson, P Korhonen, H Lee, KY Milvang-Jensen, B Nardini, M Guelbenzu, AN Oguri, M Pandey, SB Petitpas, G Rossi, A Sandberg, A Schmidl, S Tagliaferri, G Tilanus, RPJ Winters, JM Wright, D Wuyts, E AF Schulze, S. Malesani, D. Cucchiara, A. Tanvir, N. R. Kruhler, T. de Ugarte Postigo, A. Leloudas, G. Lyman, J. Bersier, D. Wiersema, K. Perley, D. A. Schady, P. Gorosabel, J. Anderson, J. P. Castro-Tirado, A. J. Cenko, S. B. De Cia, A. Ellerbroek, L. E. Fynbo, J. P. U. Greiner, J. Hjorth, J. Kann, D. A. Kaper, L. Klose, S. Levan, A. J. Martin, S. O'Brien, P. T. Page, K. L. Pignata, G. Rapaport, S. Sanchez-Ramirez, R. Sollerman, J. Smith, I. A. Sparre, M. Thoene, C. C. Watson, D. J. Xu, D. Bauer, E. E. Bayliss, M. Bjornsson, G. Bremer, M. Cano, Z. Covino, S. D'Elia, V. Frail, D. A. Geier, S. Goldoni, P. Hartoog, O. E. Jakobsson, P. Korhonen, H. Lee, K. Y. Milvang-Jensen, B. Nardini, M. Guelbenzu, A. Nicuesa Oguri, M. Pandey, S. B. Petitpas, G. Rossi, A. Sandberg, A. Schmidl, S. Tagliaferri, G. Tilanus, R. P. J. Winters, J. M. Wright, D. Wuyts, E. TI GRB 120422A/SN 2012bz: Bridging the gap between low- and high-luminosity gamma-ray bursts SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray burst: individual: GRB 120422A; supernovae: individual: SN 2012bz; dust, extinction; galaxies: ISM; galaxies: individual: GRB 120422A ID MASS-METALLICITY RELATION; CORE-COLLAPSE SUPERNOVAE; COSMIC STAR-FORMATION; DIGITAL SKY SURVEY; 25 APRIL 1998; HOST GALAXIES; LIGHT CURVES; 980425/SN 1998BW; LY-ALPHA; PHOTOMETRIC REDSHIFTS AB Context. At low redshift, a handful of gamma-ray bursts (GRBs) have been discovered with luminosities that are substantially lower (L-iso less than or similar to 10(48.5) erg s(-1)) than the average of more distant ones (L-iso greater than or similar to 10(49.5) erg s(-1)). It has been suggested that the properties of several low-luminosity (low-L) GRBs are due to shock break-out, as opposed to the emission from ultrarelativistic jets. This has led to much debate about how the populations are connected. Aims. The burst at redshift z = 0.283 from 2012 April 22 is one of the very few examples of intermediate-L GRBs with a gamma-ray luminosity of L-iso similar to 10(49.6-49.9) erg s(-1) that have been detected up to now. With the robust detection of its accompanying supernova SN 2012bz, it has the potential to answer important questions on the origin of low-and high-L GRBs and the GRB-SN connection. Methods. We carried out a spectroscopy campaign using medium-and low-resolution spectrographs with 6-10-m class telescopes, which covered a time span of 37.3 days, and a multi-wavelength imaging campaign, which ranged from radio to X-ray energies over a duration of similar to 270 days. Furthermore, we used a tuneable filter that is centred at H alpha to map star-formation in the host and the surrounding galaxies. We used these data to extract and model the properties of different radiation components and fitted the spectral energy distribution to extract the properties of the host galaxy. Results. Modelling the light curve and spectral energy distribution from the radio to the X-rays revealed that the blast wave expanded with an initial Lorentz factor of Gamma(0) similar to 50, which is a low value in comparison to high-L GRBs, and that the afterglow had an exceptionally low peak luminosity density of less than or similar to 2 x 10(30) erg s(-1) Hz(-1) in the sub-mm. Because of the weak afterglow component, we were able to recover the signature of a shock break-out in an event that was not a genuine low-L GRB for the first time. At 1.4 hr after the burst, the stellar envelope had a blackbody temperature of k(B)T similar to 16 eV and a radius of similar to 7 x 10(13) cm (both in the observer frame). The accompanying SN 2012bz reached a peak luminosity of M-V = -19.7 mag, which is 0.3 mag more luminous than SN 1998bw. The synthesised nickel mass of 0.58 M-circle dot, ejecta mass of 5.87 M-circle dot, and kinetic energy of 4.10x10(52) erg were among the highest for GRB-SNe, which makes it the most luminous spectroscopically confirmed SN to date. Nebular emission lines at the GRB location were visible, which extend from the galaxy nucleus to the explosion site. The host and the explosion site had close-to-solar metallicity. The burst occurred in an isolated star-forming region with an SFR that is 1/10 of that in the galaxy's nucleus. Conclusions. While the prompt gamma-ray emission points to a high-L GRB, the weak afterglow and the low Gamma(0) were very atypical for such a burst. Moreover, the detection of the shock break-out signature is a new quality for high-L GRBs. So far, shock break-outs were exclusively detected for low-L GRBs, while GRB 120422A had an intermediate L-iso of similar to 10(49.6-49.9) erg s(-1). Therefore, we conclude that GRB 120422A was a transition object between low-and high-L GRBs, which supports the failed-jet model that connects low-L GRBs that are driven by shock break-outs and high-L GRBs that are powered by ultra-relativistic jets. C1 [Schulze, S.; Bauer, E. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago, Chile. [Schulze, S.; Bjornsson, G.; Cano, Z.; Jakobsson, P.] Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland. [Schulze, S.; Bjornsson, G.; Cano, Z.; Jakobsson, P.] Univ Iceland, IS-107 Reykjavik, Iceland. [Malesani, D.; Kruhler, T.; de Ugarte Postigo, A.; Leloudas, G.; Fynbo, J. P. U.; Hjorth, J.; Sparre, M.; Watson, D. J.; Xu, D.; Geier, S.; Milvang-Jensen, B.] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Cucchiara, A.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Tanvir, N. R.; Wiersema, K.; O'Brien, P. T.; Page, K. L.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [de Ugarte Postigo, A.; Gorosabel, J.; Castro-Tirado, A. J.; Sanchez-Ramirez, R.; Thoene, C. C.] CSIC, IAA, E-18008 Granada, Spain. [Leloudas, G.] Stockholm Univ, Oskar Klein Ctr, Dept Phys, AlbaNova Univ Ctr, S-10691 Stockholm, Sweden. [Lyman, J.; Bersier, D.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Perley, D. A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Schady, P.; Greiner, J.; Kann, D. A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Anderson, J. P.] Univ Chile, Dept Astron, Santiago, Chile. [Cenko, S. B.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Cenko, S. B.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [De Cia, A.; Xu, D.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, Fac Phys, IL-76100 Rehovot, Israel. [Ellerbroek, L. E.; Kaper, L.; Hartoog, O. E.] Univ Amsterdam, NL-1098 XH Amsterdam, Netherlands. [Kann, D. A.; Klose, S.; Guelbenzu, A. Nicuesa; Rossi, A.; Schmidl, S.] Thuringer Landessternwarte Tautenburg, Tautenburg, Germany. [Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Kruhler, T.; Anderson, J. P.; Martin, S.] European So Observ, Santiago 19, Chile. [Pignata, G.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. [Rapaport, S.] Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Sollerman, J.; Lee, K. Y.; Sandberg, A.] Stockholm Univ, Oskar Klein Ctr, Dept Astron, AlbaNova Univ Ctr, S-10691 Stockholm, Sweden. [Smith, I. A.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. [Bayliss, M.; Petitpas, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bayliss, M.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Covino, S.; Tagliaferri, G.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Bremer, M.; Winters, J. M.] Inst Radioastron Millimetr IRAM, F-38406 St Martin Dheres, France. [D'Elia, V.] ASI Sci Data Ctr, I-00133 Rome, Italy. [Frail, D. A.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Geier, S.] Nord Opt Telescope, Santa Cruz De La Palma 38700, Spain. [Goldoni, P.] Univ Paris Diderot, APC, CNRS IN2P3, CEA Irfu,Observ Paris,Sorbonne Paris Cite, F-75205 Paris 13, France. [Korhonen, H.] Univ Turku, Finnish Ctr Astron ESO FINCA, Piikkio 21500, Finland. [Nardini, M.] Univ Milano Bicocca, I-20126 Milan, Italy. [Oguri, M.] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Oguri, M.] Univ Tokyo, Kavli IPMU, WPI, Chiba 2778583, Japan. [Pandey, S. B.] Aryabhatta Res & Observat Sci, Naini Tal 263129, India. [Tilanus, R. P. J.] Joint Astron Ctr, James Clerk Maxwell Telescope, Hilo, HI 96720 USA. [Tilanus, R. P. J.] Netherlands Org Sci Res, NL-2509 AC The Hague, Netherlands. [Wright, D.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Wuyts, E.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Wuyts, E.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Bauer, E. E.] Space Sci Inst, Boulder, CO 80301 USA. [Gorosabel, J.] Univ Pais Vasco UPV EHU, Unidad Asociada Grp Ciencia Planetarias UPV EHU I, Dept Fis Aplicada 1, Bilbao 48013, Spain. [Gorosabel, J.] Basque Fdn Sci, Ikerbasque, Bilbao 48008, Spain. [D'Elia, V.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. RP Schulze, S (reprint author), Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Av Vicuna Mackenna 4860, Santiago, Chile. EM sschulze@astro.puc.cl RI Oguri, Masamune/C-6230-2011; Hjorth, Jens/M-5787-2014; Sparre, Martin/C-2424-2015; Watson, Darach/E-4521-2015; Jakobsson, Pall/L-9950-2015; Korhonen, Heidi/E-3065-2016; Rossi, Andrea/N-4674-2015; OI Schulze, Steve/0000-0001-6797-1889; de Ugarte Postigo, Antonio/0000-0001-7717-5085; Covino, Stefano/0000-0001-9078-5507; Sanchez-Ramirez, Ruben/0000-0002-7158-5099; Kruehler, Thomas/0000-0002-8682-2384; Tagliaferri, Gianpiero/0000-0003-0121-0723; D'Elia, Valerio/0000-0002-7320-5862; Sollerman, Jesper/0000-0003-1546-6615; Castro-Tirado, A. J./0000-0003-2999-3563; Hjorth, Jens/0000-0002-4571-2306; Sparre, Martin/0000-0002-9735-3851; Watson, Darach/0000-0002-4465-8264; Jakobsson, Pall/0000-0002-9404-5650; Korhonen, Heidi/0000-0003-0529-1161; Rossi, Andrea/0000-0002-8860-6538; Thone, Christina/0000-0002-7978-7648 FU Icelandic Research Fund; University of Iceland Research Fund; Dark Cosmology Centre; CONICYT through FONDECYT [3140534, 3110142]; Basal-CATA [PFB-06/2007]; Iniciativa Cientifica Milenio grant (Millennium Center for Supernova Science) [P10-064-F]; "Millennium Institute of Astrophysics (MAS)" of Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo de Chile [IC120009]; "Fondo de Innovacion para la Competitividad, del Ministerio de Economia, Foment y Turismo de Chile"; CONICYT-Chile FONDECYT [1101024]; Instrument Center for Danish Astrophysics; European Commission under the Marie Curie Intra-European Fellowship Programme; ERC-StG [EGGS-278202]; UK Space Agency; Swedish Research Council [623-2011-7117]; UK Science and Technology Facilities Council; Spanish research project [AYA2012-39362-C02-02, AYA2009-14000-C03-01, AYA2012-39727-C03-01]; European Commission under the Marie Curie Career Integration Grant programme [FP7-PEOPLE-2012-CIG 322307]; DFG cluster of excellence "Origin and Structure of the Universe" - Thuringer Landessternwarte Tautenburg; Thuringer Landessternwarte Tautenburg; Alexander von Humboldt Foundation of Germany; DFG [KL 766/16-1, HA 1850/28-1]; Thuringer Ministerium fur Bildung, Wissenschaft und Kultur [FKZ 12010-514]; Danish National Research Foundation; Spitzer/NASA grant RSA [1287913]; NSF [GN-2012A-Q-9, GN-2012A-Q-39, GN-2012B-Q-5, GS-2012A-Q-30, GS-2012A-Q-38]; Nordic Optical Telescope (NOT); Instituto de Astrofisica de Canarias [P45-002, ITP10-04]; Gran Telescopio Canarias (GTC) in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias in the island of La Palma; Magellan [CN2012A-059]; TRAM Plateau de Bure Interferometer; James Clerk Maxwell Telescope [M12AI12]; XMM-Newton, an ESA science mission; ESA Member States; NASA; W.M. Keck Foundation; Science and Technology Facilities Council of the United Kingdom; National Research Council of Canada; Netherlands Organisation for Scientific Research; Canada Foundation for Innovation; Smithsonian Institution; Academia Sinica; INSU/CNRS (France); MPG (Germany); IGN (Spain); Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris Foundation; James S. McDonnell Foundation; Associates of the California Institute of Technology; University of Chicago; state of California, Illinois; state of California, Maryland; National Science Foundation; Alfred P. Sloan Foundation; US Department of Energy Office of Science FX We thank Shri Kulkarni (Caltech) for obtaining the Keck spectrum. S.S. thanks Tsvi Piran (The Hebrew University, Israel), Nir Sapir, Eli Waxman (Weizmann Institute of Science, Israel), Milena Butane (Universidad Andres Bello, Chile), Maryam Modjaz (New York University, USA), and the anonymous referee for many productive and valuable discussions. S.S. acknowledges support by a Grant of Excellence from the Icelandic Research Fund, from the University of Iceland Research Fund, from the Dark Cosmology Centre, where part of this study was performed, and from CONICYT through FONDECYT grant 3140534. We acknowledge support from Basal-CATA PFB-06/2007 (FEB, SS), Iniciativa Cientifica Milenio grant P10-064-F (Millennium Center for Supernova Science), by Project IC120009 "Millennium Institute of Astrophysics (MAS)" of Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo de Chile, with input from "Fondo de Innovacion para la Competitividad, del Ministerio de Economia, Foment y Turismo de Chile" (F.E.B., G.P., J.A.R., S.S.), CONICYT-Chile FONDECYT 1101024 (FEB). J.A.P. acknowledges support by CONICYT through FONDECYT grant 3110142. D.M. acknowledges the Instrument Center for Danish Astrophysics for support. T.K. and H.K. acknowledge support by the European Commission under the Marie Curie Intra-European Fellowship Programme in FP7. J.P.U.F., B.M.J., and D.X. acknowledge support from the ERC-StG grant EGGS-278202. K.L.P. acknowledges financial support by the UK Space Agency for the Swift project. G.L. is supported by the Swedish Research Council through grant No. 623-2011-7117. J.L. acknowledges the UK Science and Technology Facilities Council for research studentship support. The research activity of AdUP, C.T., and J.G. is supported by Spanish research project AYA2012-39362-C02-02. A.d.U.P. acknowledges support by the European Commission under the Marie Curie Career Integration Grant programme (FP7-PEOPLE-2012-CIG 322307). A.J.C.T. acknowledges support front the Spanish research project AYA2009-14000-C03-01 and AYA2012-39727-C03-01 D.A.K. acknowledges support by the DFG cluster of excellence "Origin and Structure of the Universe" and funding by the Thuringer Landessternwarte Tautenburg. A. R. acknowledges support by the Thuringer Landessternwarte Tautenburg. P.S. acknowledges support through the Sofja Kovalevskaja Award from the Alexander von Humboldt Foundation of Germany. A.N.G. and S.K. acknowledge support by DFG KL 766/16-1. S. Schmidl acknowledges support by the Thuringer Ministerium fur Bildung, Wissenschaft und Kultur under FKZ 12010-514. The Dark Cosmology Centre is funded by the Danish National Research Foundation. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. This research has made use of the GHostS database (www.grbhosts.org), which is partly funded by Spitzer/NASA grant RSA Agreement No. 1287913. Based in part on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, as part of the program 089.A-0067, the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc.; , under a co-operative agreement with the NSF on behalf of the Gemini partnership, as part of the programs GN-2012A-Q-9, GN-2012A-Q-39, GN-2012B-Q-5, GS-2012A-Q-30, GS-2012A-Q-38, GS-2012A-Q-30, and GN-2012B-Q-5, the Nordic Optical Telescope (NOT), operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias, as part of the program P45-002 (PI: Jakobsson) and ITP10-04 (PI: Kotak, QUB), the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, in the island of La Palma, with Magellan as part of CN2012A-059, with the TRAM Plateau de Bure Interferometer, the James Clerk Maxwell Telescope, as part of the program M12AI12, with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and 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 the National Aeronautics and Space Administration. The observatory was made possible by the generous financial support of the W.M. Keck Foundation, The United Kingdom Infrared Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK The lames 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 the Netherlands Organisation for Scientific Research. Additional funds for the construction of SCUBA-2 were provided by the Canada Foundation for Innovation. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of California, Illinois, and Maryland, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. Part of the funding for GROND (both hardware as well as personnel) was generously granted from the Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo. University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 216 TC 23 Z9 23 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 JUN PY 2014 VL 566 AR A102 DI 10.1051/0004-6361/201423387 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500092 ER PT J AU Thalmann, C Mulders, GD Hodapp, K Janson, M Grady, CA Min, M Ovelar, MD Carson, J Brandt, T Bonnefoy, M McElwain, MW Leisenring, J Dominik, C Henning, T Tamura, M AF Thalmann, C. Mulders, G. D. Hodapp, K. Janson, M. Grady, C. A. Min, M. Ovelar, M. de Juan Carson, J. Brandt, T. Bonnefoy, M. McElwain, M. W. Leisenring, J. Dominik, C. Henning, T. Tamura, M. TI The architecture of the LkCa 15 transitional disk revealed by high-contrast imaging SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: individual: LkCa 15; stars: pre-main sequence; planetary systems; planets and satellites: formation; protoplanetary disks ID INTERSTELLAR SILICATE MINERALOGY; POLARIZED SCATTERED-LIGHT; T TAURI STARS; PROTOPLANETARY DISKS; HD 100546; PRETRANSITIONAL DISKS; CIRCUMSTELLAR DISKS; RADIATIVE-TRANSFER; MULTIPLE PLANETS; FORMING REGION AB We present four new epochs of K-s-band images of the young pre-transitional disk around LkCa 15 and perform extensive forward modeling to derive the physical parameters of the disk. We find indications of strongly anisotropic scattering (Henyey-Greenstein g = 0.67(-0.11)(+0.18)) and a significantly tapered gap edge ("round wall") but see no evidence that the inner disk, whose existence is predicted by the spectral energy distribution, shadows the outer regions of the disk visible in our images. We marginally confirm the existence of an offset between the disk center and the star along the line of nodes; however, the magnitude of this offset (x = 27(-20)(+19) mas) is notably lower than that found in our earlier H-band images. Intriguingly, we also find an offset of y = 69(-25)(+49) mas perpendicular to the line of nodes at high significance. If confirmed by future observations, this would imply a highly elliptical - or otherwise asymmetric - disk gap with an effective eccentricity of e approximate to 0.3. Such asymmetry would most likely be the result of dynamical sculpting by one or more unseen planets in the system. Finally, we find that the bright arc of scattered light we see in direct imaging observations originates from the near side of the disk and appears brighter than the far side because of strong forward scattering. C1 [Thalmann, C.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Thalmann, C.; Mulders, G. D.; Min, M.; Ovelar, M. de Juan; Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Mulders, G. D.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Hodapp, K.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Janson, M.] Queens Univ Belfast, Astrophys Res Ctr, Belfast, Antrim, North Ireland. [Grady, C. A.] Eureka Sci, Oakland, CA 96002 USA. [Grady, C. A.; McElwain, M. W.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Grady, C. A.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [Ovelar, M. de Juan] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Carson, J.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA. [Brandt, T.] Inst Adv Study, Dept Astrophys, Princeton, NJ 08540 USA. [Bonnefoy, M.; Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Leisenring, J.] Dept Astron, Tucson, AZ 85721 USA. [Leisenring, J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Tamura, M.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Tamura, M.] Grad Univ Adv Studies Sokendai, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan. RP Thalmann, C (reprint author), ETH, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. EM thalmann@phys.ethz.ch FU European Commission [329875]; US National Science Foundation [1008440, 1009203]; NASA Origins of Solar Systems program [NNG13PB64P]; EU [284405] FX We thank F. Meru and S. Quanz for useful discussions, and the anonymous referee for helpful comments that improved the quality of the manuscript. C.Th. is supported by the European Commission under the Marie Curie ID, grant No. 329875. C.A.G. is supported by the US National Science Foundation under Award No. 1008440 and through the NASA Origins of Solar Systems program on NNG13PB64P. M.M. acknowledges funding from the EU FP7-2011 under Grant Agreement No. 284405. J.C. is supported by the US National Science Foundation under Award No. 1009203. This work is based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia:), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 79 TC 17 Z9 17 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2014 VL 566 AR A51 DI 10.1051/0004-6361/201322915 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AK8MI UT WOS:000338681500043 ER PT J AU Wiesner, V AF Wiesner, Valerie TI Internship-A pathway to employment SO AMERICAN CERAMIC SOCIETY BULLETIN LA English DT Article C1 [Wiesner, Valerie] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA. [Wiesner, Valerie] Purdue Univ, W Lafayette, IN 47907 USA. RP Wiesner, V (reprint author), NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA. NR 0 TC 0 Z9 0 U1 1 U2 3 PU AMER CERAMIC SOC PI WESTERVILLE PA 600 N CLEVELAND AVE, WESTERVILLE, OH 43082 USA SN 0002-7812 EI 1945-2705 J9 AM CERAM SOC BULL JI Am. Ceram. Soc. Bull. PD JUN-JUL PY 2014 VL 93 IS 5 BP 29 EP 29 PG 1 WC Materials Science, Ceramics SC Materials Science GA AK1OF UT WOS:000338183700004 ER PT J AU Daigle, MJ Bregon, A Roychoudhury, I AF Daigle, Matthew J. Bregon, Anibal Roychoudhury, Indranil TI Distributed Prognostics Based on Structural Model Decomposition SO IEEE TRANSACTIONS ON RELIABILITY LA English DT Article DE Model-based prognostics; distributed prognostics; structural model decomposition ID KALMAN FILTER; PARAMETER; DIAGNOSIS AB Within systems health management, prognostics focuses on predicting the remaining useful life of a system. In the model-based prognostics paradigm, physics-based models are constructed that describe the operation of a system, and how it fails. Such approaches consist of an estimation phase, in which the health state of the system is first identified, and a prediction phase, in which the health state is projected forward in time to determine the end of life. Centralized solutions to these problems are often computationally expensive, do not scale well as the size of the system grows, and introduce a single point of failure. In this paper, we propose a novel distributed model-based prognostics scheme that formally describes how to decompose both the estimation and prediction problems into computationally-independent local subproblems whose solutions may be easily composed into a global solution. The decomposition of the prognostics problem is achieved through structural decomposition of the underlying models. The decomposition algorithm creates from the global system model a set of local submodels suitable for prognostics. Computationally independent local estimation and prediction problems are formed based on these local submodels, resulting in a scalable distributed prognostics approach that allows the local subproblems to be solved in parallel, thus offering increases in computational efficiency. Using a centrifugal pump as a case study, we perform a number of simulation-based experiments to demonstrate the distributed approach, compare the performance with a centralized approach, and establish its scalability. C1 [Daigle, Matthew J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Bregon, Anibal] Univ Valladolid, Dept Comp Sci, Intelligent Syst Grp, Valladolid, Spain. [Roychoudhury, Indranil] NASA, Stinger Ghaffarian Technol, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Daigle, MJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM matthew.j.daigle@nasa.gov; anibal@infor.uva.es; indranil.roychoudhury@nasa.gov OI Daigle, Matthew/0000-0002-4616-3302 FU NASA; NASA Autonomous Cryogenic Loading Operations (ACLO) Project under the Office of the Chief Technologies (OCT); Spanish MCI [TIN2009-11326] FX The work of M. Daigle and I. Roychoudhury was supported in part by the NASA System-wide Safety Assurance (SSAT) Project within the Aviation Safety Program (ASP) under the Aeronautics Mission Directorate (ARMD), and the NASA Autonomous Cryogenic Loading Operations (ACLO) Project under the Office of the Chief Technologies (OCT). The work of A. Bregon was supported in part by a Spanish MCI TIN2009-11326 Grant. Associate Editor: J. Rupe. NR 40 TC 6 Z9 6 U1 1 U2 11 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 JUN PY 2014 VL 63 IS 2 BP 495 EP 510 DI 10.1109/TR.2014.2313791 PG 16 WC Computer Science, Hardware & Architecture; Computer Science, Software Engineering; Engineering, Electrical & Electronic SC Computer Science; Engineering GA AK0NW UT WOS:000338111400009 ER PT J AU Sankararaman, S Daigle, MJ Goebel, K AF Sankararaman, Shankar Daigle, Matthew J. Goebel, Kai TI Uncertainty Quantification in Remaining Useful Life Prediction Using First-Order Reliability Methods SO IEEE TRANSACTIONS ON RELIABILITY LA English DT Article DE Analytical algorithms; first-order reliability method; ithium-ion battery; model-based prognostics; probability distribution; remaining useful life; uncertainty ID STRUCTURAL RELIABILITY; HEALTH; APPROXIMATION; FRAMEWORK; SYSTEM AB In this paper, we investigate the use of first-order reliability methods to quantify the uncertainty in the remaining useful life (RUL) estimate of components used in engineering applications. The prediction of RUL is affected by several sources of uncertainty, and it is important to systematically quantify their combined effect on the RUL prediction in order to aid risk assessment, risk mitigation, and decision-making. While sampling-based algorithms have been conventionally used for quantifying the uncertainty in RUL, analytical approaches are computationally cheaper, and sometimes they are better suited for online decision-making. Exact analytical algorithms may not be available for practical engineering applications, but effective approximations can be made using first-order reliability methods. This paper describes three first-order reliability-based methods for RUL uncertainty quantification: first-order second moment method (FOSM), the first-order reliability method (FORM), and the inverse first-order reliability method (inverse-FORM). The inverse-FORM methodology is particularly useful in the context of online health monitoring, and this method is illustrated using the power system of an unmanned aerial vehicle, where the goal is to predict the end of discharge of a lithium-ion battery. C1 [Sankararaman, Shankar] NASA, SGT Inc, Ames Res Ctr, Moffett Field, CA 94035 USA. [Daigle, Matthew J.; Goebel, Kai] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Sankararaman, S (reprint author), NASA, SGT Inc, Ames Res Ctr, Moffett Field, CA 94035 USA. EM shankar.sankararaman@nasa.gov OI Daigle, Matthew/0000-0002-4616-3302 FU NASA System-wide Satefy Assurance Technologies (SSAT) project under the Aviation Safety (AvSafe) Program of the Aeronautics Research Mission Directorate (ARMD); NASA Automated Cryogenic Loading Operations (ACLO) project under the Office of the Chief Technologist (OCT) of Advanced Exploration Systems (AES) FX This work was supported in part by the NASA System-wide Satefy Assurance Technologies (SSAT) project under the Aviation Safety (AvSafe) Program of the Aeronautics Research Mission Directorate (ARMD), and by the NASA Automated Cryogenic Loading Operations (ACLO) project under the Office of the Chief Technologist (OCT) of Advanced Exploration Systems (AES). Associate Editor: M. Xie. NR 54 TC 9 Z9 9 U1 4 U2 47 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 JUN PY 2014 VL 63 IS 2 BP 603 EP 619 DI 10.1109/TR.2014.2313801 PG 17 WC Computer Science, Hardware & Architecture; Computer Science, Software Engineering; Engineering, Electrical & Electronic SC Computer Science; Engineering GA AK0NW UT WOS:000338111400018 ER PT J AU Walker, JJ Koepke, ME Zimmerman, MI Farrell, WM Demidov, VI AF Walker, Jeffrey J. Koepke, M. E. Zimmerman, M. I. Farrell, W. M. Demidov, V. I. TI Analytical model for gyro-phase drift arising from abrupt inhomogeneity SO JOURNAL OF PLASMA PHYSICS LA English DT Article ID PARTICLES; MOTION AB If a magnetized-orbit-charged grain encounters any abrupt inhomogeneity in plasma conditions during a gyro-orbit, such that the resulting in-situ equilibrium charge is significantly different between these regions (q(1)/q(2) similar to 2, where q(1) is the in-situ equilibrium charge on one side of the inhomogeneity, q(2) is the in-situ equilibrium charge on the other side, and q(1) < q(2) < 0), then the capacitive effects of charging and discharging of the dust grain can result in a modification to the orbit-averaged grain trajectory, i.e. gyro-phase drift. The special case of q(1)/q(2) is notioned for the purpose of illustrating the utility of the method. An analytical expression is derived for the grain velocity, assuming a capacitor approximation to the OML charging model. For cases in which a strong electric field suddenly appears in the wake or at the space-plasma-to-crater interface from solar wind and/or ultraviolet illumination and in which a magnetic field permeates an asteroid, comet, or moon, this model could contribute to the interpretation of the distribution of fields and particles. C1 [Walker, Jeffrey J.; Koepke, M. E.; Demidov, V. I.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. [Zimmerman, M. I.; Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Demidov, V. I.] Univ ITMO, St Petersburg 197101, Russia. RP Walker, JJ (reprint author), W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. EM jwalke17@mix.wvu.edu RI Demidov, Vladimir/A-4247-2013; Farrell, William/I-4865-2013 OI Demidov, Vladimir/0000-0002-2672-7684; FU US Department of Energy, Office of Fusion Energy Science [DE-SC0001939] FX Funding through the US Department of Energy, Office of Fusion Energy Science grant DE-SC0001939 and useful discussions with Dr. Marlene Rosenberg are gratefully acknowledged. NR 8 TC 1 Z9 1 U1 1 U2 5 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-3778 EI 1469-7807 J9 J PLASMA PHYS JI J. Plasma Phys. PD JUN PY 2014 VL 80 BP 395 EP 404 DI 10.1017/S0022377813001359 PN 3 PG 10 WC Physics, Fluids & Plasmas SC Physics GA AK2ZW UT WOS:000338291900005 ER PT J AU Aydinoglu, AU Suomela, T Malone, J AF Aydinoglu, Arsev Umur Suomela, Todd Malone, Jim TI Data Management in Astrobiology: Challenges and Opportunities for an Interdisciplinary Community SO ASTROBIOLOGY LA English DT Editorial Material DE Data management; Data sharing; Data preservation ID ECOLOGY; SCIENCE AB Data management and sharing are growing concerns for scientists and funding organizations throughout the world. Funding organizations are implementing requirements for data management plans, while scientists are establishing new infrastructures for data sharing. One of the difficulties is sharing data among a diverse set of research disciplines. Astrobiology is a unique community of researchers, containing over 110 different disciplines. The current study reports the results of a survey of data management practices among scientists involved in the astrobiology community and the NASA Astrobiology Institute (NAI) in particular. The survey was administered over a 2-month period in the first half of 2013. Fifteen percent of the NAI community responded (n = 114), and additional (n = 80) responses were collected from members of an astrobiology Listserv. The results of the survey show that the astrobiology community shares many of the same concerns for data sharing as other groups. The benefits of data sharing are acknowledged by many respondents, but barriers to data sharing remain, including lack of acknowledgement, citation, time, and institutional rewards. Overcoming technical, institutional, and social barriers to data sharing will be a challenge into the future. C1 [Aydinoglu, Arsev Umur] NASA, Ames Res Ctr, Astrobiol Inst, Mountain View, CA 94043 USA. [Suomela, Todd; Malone, Jim] Univ Tennessee, Sch Informat Sci, Knoxville, TN USA. RP Aydinoglu, AU (reprint author), NASA, Ames Res Ctr, Astrobiol Inst, MS 247-6, Mountain View, CA 94043 USA. EM arsevu@gmail.com OI AYDINOGLU, ARSEV UMUR/0000-0001-8857-6001; Suomela, Todd/0000-0002-4549-0782 NR 35 TC 2 Z9 2 U1 1 U2 12 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 JUN PY 2014 VL 14 IS 6 BP 451 EP 461 DI 10.1089/ast.2013.1127 PG 11 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AJ7WF UT WOS:000337910400001 PM 24840364 ER PT J AU Bekker, DL Thompson, DR Abbey, WJ Cabrol, NA Francis, R Manatt, KS Ortega, KF Wagstaff, KL AF Bekker, Dmitriy L. Thompson, David R. Abbey, William J. Cabrol, Nathalie A. Francis, Raymond Manatt, Ken S. Ortega, Kevin F. Wagstaff, Kiri L. TI Field Demonstration of an Instrument Performing Automatic Classification of Geologic Surfaces SO ASTROBIOLOGY LA English DT Article DE Interpretation of planetary mission data ID CIMA VOLCANIC FIELD; LANDSCAPE EVOLUTION; AUTONOMOUS SCIENCE; MOJAVE-DESERT; MARS; RECOGNITION; CALIFORNIA; PAVEMENTS; MISSION AB This work presents a method with which to automate simple aspects of geologic image analysis during space exploration. Automated image analysis on board the spacecraft can make operations more efficient by generating compressed maps of long traverses for summary downlink. It can also enable immediate automatic responses to science targets of opportunity, improving the quality of targeted measurements collected with each command cycle. In addition, automated analyses on Earth can process large image catalogs, such as the growing database of Mars surface images, permitting more timely and quantitative summaries that inform tactical mission operations. We present TextureCam, a new instrument that incorporates real-time image analysis to produce texture-sensitive classifications of geologic surfaces in mesoscale scenes. A series of tests at the Cima Volcanic Field in the Mojave Desert, California, demonstrated mesoscale surficial mapping at two distinct sites of geologic interest. C1 [Bekker, Dmitriy L.; Thompson, David R.; Abbey, William J.; Manatt, Ken S.; Ortega, Kevin F.; Wagstaff, Kiri L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cabrol, Nathalie A.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Francis, Raymond] Western Univ, Ctr Planetary Sci & Explorat CPSX, London, ON, Canada. RP Thompson, DR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 306-463, Pasadena, CA 91109 USA. EM david.r.thompson@jpl.nasa.gov OI Wagstaff, Kiri/0000-0003-4401-5506 FU NASA Astrobiology Science and Technology Instrument Development program [NNH10ZDA001N-ASTID]; National Park Service [MOJA-2013-SCI-0011] FX The TextureCam project is supported by the NASA Astrobiology Science and Technology Instrument Development program (NNH10ZDA001N-ASTID) and National Park Service permit MOJA-2013-SCI-0011. Accommodations for the field experiment were provided by the Desert Studies Center, Zzyzx, CA, a field station of the California State University (CSU). NR 32 TC 4 Z9 4 U1 0 U2 4 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 JUN PY 2014 VL 14 IS 6 BP 486 EP 501 DI 10.1089/ast.2014.1172 PG 16 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AJ7WF UT WOS:000337910400004 PM 24886217 ER PT J AU Parenteau, MN Jahnke, LL Farmer, JD Cady, SL AF Parenteau, Mary N. Jahnke, Linda L. Farmer, Jack D. Cady, Sherry L. TI Production and Early Preservation of Lipid Biomarkers in Iron Hot Springs SO ASTROBIOLOGY LA English DT Article DE Lipid biomarkers; Photosynthesis; Iron; Hot springs; Mars ID YELLOWSTONE-NATIONAL-PARK; FATTY-ACID-COMPOSITION; BLUE-GREEN-ALGAE; MOUNT BRUCE SUPERGROUP; MICROBIAL MATS; CYANOBACTERIAL MAT; BACILLUS-SUBTILIS; WESTERN-AUSTRALIA; BRANCHED ALKANES; NEW-ZEALAND AB The bicarbonate-buffered anoxic vent waters at Chocolate Pots hot springs in Yellowstone National Park are 51-54 degrees C, pH 5.5-6.0, and are very high in dissolved Fe(II) at 5.8-5.9 mg/L. The aqueous Fe(II) is oxidized by a combination of biotic and abiotic mechanisms and precipitated as primary siliceous nanophase iron oxyhydroxides (ferrihydrite). Four distinct prokaryotic photosynthetic microbial mat types grow on top of these iron deposits. Lipids were used to characterize the community composition of the microbial mats, link source organisms to geologically significant biomarkers, and investigate how iron mineralization degrades the lipid signature of the community. The phospholipid and glycolipid fatty acid profiles of the highest-temperature mats indicate that they are dominated by cyanobacteria and green nonsulfur filamentous anoxygenic phototrophs (FAPs). Diagnostic lipid biomarkers of the cyanobacteria include midchain branched mono- and dimethylalkanes and, most notably, 2-methylbacteriohopanepolyol. Diagnostic lipid biomarkers of the FAPs (Chloroflexus and Roseiflexus spp.) include wax esters and a long-chain tri-unsaturated alkene. Surprisingly, the lipid biomarkers resisted the earliest stages of microbial degradation and diagenesis to survive in the iron oxides beneath the mats. Understanding the potential of particular sedimentary environments to capture and preserve fossil biosignatures is of vital importance in the selection of the best landing sites for future astrobiological missions to Mars. This study explores the nature of organic degradation processes in moderately thermal Fe(II)-rich groundwater springs-environmental conditions that have been previously identified as highly relevant for Mars exploration. C1 [Parenteau, Mary N.] SETI Inst, Mountain View, CA USA. [Parenteau, Mary N.; Jahnke, Linda L.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. [Farmer, Jack D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Cady, Sherry L.] Portland State Univ, Dept Geol, Portland, OR 97207 USA. [Cady, Sherry L.] Pacific NW Natl Lab, Richland, WA 99352 USA. RP Parenteau, MN (reprint author), NASA, Ames Res Ctr, Exobiol Branch, M-S 239-4, Moffett Field, CA 94035 USA. EM Mary.N.Parenteau@nasa.gov FU NASA [NAG5-12328, NNX08AZ47A, NNH08ZDA001N, NNX11AR81G]; Environmental and Molecular Sciences Laboratory (EMSL), a national scientific user facility; Department of Energy's Office of Biological and Environmental Research FX This work was supported by NASA Exobiology Grant NAG5-12328. Additional support was generously provided by a NASA Oregon Space Grant Graduate Fellowship, a NASA Planetary Biology Internship, and a NASA Post-doctoral Program Fellowship to M.N. Parenteau. Part of this work was supported by grants from the NASA Exobiology Program (NNX08AZ47A) to L. Jahnke and the NASA Mars Fundamental Research Program (NNH08ZDA001N) to J.D. Farmer. S.L. Cady acknowledges financial support from the Environmental and Molecular Sciences Laboratory (EMSL), a national scientific user facility sponsored by the Department of Energy's Office of Biological and Environmental Research and located at Pacific Northwest National Laboratory, and from the NASA Exobiology Program (NNX11AR81G). We thank the National Park Service for allowing us to conduct research in Yellowstone National Park and thank Mike Kubo and Tsegereda Embaye, SETI Institute; Kendra Turk, University of California Santa Cruz; and Georg Grathoff, Portland State University for technical assistance. We thank Dave Des Marais and Beverly Pierson for helpful discussions and two anonymous reviewers, who helped strengthen the manuscript. NR 134 TC 1 Z9 1 U1 3 U2 31 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 JUN PY 2014 VL 14 IS 6 BP 502 EP 521 DI 10.1089/ast.2013.1122 PG 20 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AJ7WF UT WOS:000337910400005 PM 24886100 ER PT J AU Davila, AF McKay, CP AF Davila, Alfonso F. McKay, Christopher P. TI Chance and Necessity in Biochemistry: Implications for the Search for Extraterrestrial Biomarkers in Earth-like Environments SO ASTROBIOLOGY LA English DT Article DE Origin of life; Biomarkers; Exobiology; Extraterrestrial life; Prebiotic chemistry ID MURCHISON CARBONACEOUS CHONDRITE; AMINO-ACIDS; PREBIOTIC SYNTHESIS; LIQUID WATER; GENETIC-CODE; ALIEN LIFE; METEORITES; URACIL; NUCLEOBASES; COMPONENTS AB In this paper, we examine a restricted subset of the question of possible alien biochemistries. That is, we look into how different life might be if it emerged in environments similar to that required for life on Earth. We advocate a principle of chance and necessity in biochemistry. According to this principle, biochemistry is in some fundamental way the sum of two processes: there is an aspect of biochemistry that is an endowment from prebiotic processes, which represents the necessity, plus an aspect that is invented by the process of evolution, which represents the chance. As a result, we predict that life originating in extraterrestrial Earth-like environments will share biochemical motifs that can be traced back to the prebiotic world but will also have intrinsic biochemical traits that are unlikely to be duplicated elsewhere as they are combinatorially path-dependent. Effective and objective strategies to search for biomarkers, and evidence for a second genesis, on planets with Earth-like environments can be built based on this principle. C1 [Davila, Alfonso F.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Davila, Alfonso F.; McKay, Christopher P.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. RP Davila, AF (reprint author), SETI Inst, Carl Sagan Ctr, 189 Bernardo Ave Suite 100, Mountain View, CA 94043 USA. EM adavila@seti.org RI Davila, Alfonso/A-2198-2013 OI Davila, Alfonso/0000-0002-0977-9909 FU NASA Astrobiology Program [NNX12AD61G] FX We wish to thank Norman Sleep and an anonymous reviewer for their useful and constructive comments, and Susan O'Connor for early revisions of the manuscript. A.F.D. acknowledges funding from the NASA Astrobiology Program (Grant Number NNX12AD61G). NR 50 TC 9 Z9 9 U1 5 U2 40 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 JUN PY 2014 VL 14 IS 6 BP 534 EP 540 DI 10.1089/ast.2014.1150 PG 7 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AJ7WF UT WOS:000337910400007 PM 24867145 ER PT J AU Adell, PC Yager, J Pannell, Z Shelton, J Mojarradi, MM Blalock, B Allen, G Some, R AF Adell, Philippe C. Yager, Jeremy Pannell, Zack Shelton, Jacob Mojarradi, Mohammad M. Blalock, Benjamin Allen, Greg Some, Raphael TI Radiation Hardening of an SiGe BiCMOS Wilkinson ADC for Distributed Motor Controller Application SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article DE Distributed motor controller (DMC); impedance; radiation hardening; single-event effects; total dose; Wilkinson analog-to-digital converter (ADC) ID EXTREME ENVIRONMENT ELECTRONICS; TO-DIGITAL CONVERTER; TECHNOLOGY AB The radiation robustness of a newly designed Wilkinson analog-to-digital converter (ADC) is being investigated. The ADC is a front-end design block within a cold capable, analog sense, application-specific integrated circuit (ASIC) manufactured using the IBM 0.5 mu m silicon germanium (SiGe) BiCMOS 5HP process. The ASIC is part of a next-generation, cold capable, distributed motor controller architecture, which is a candidate for the next generation of Mars rovers. Its main function is to interface with various sensor types to monitor motor health (i.e., temperature, mechanical stress, pressure). While relatively well-hardened against total ionizing dose and destructive single-event latchup, the ADC showed some SEU (SET) sensitivity that is heavily dependent on its input channel configuration. For this study, we used a combination of experiments (pulsed-laser) and Cadence mixed-mode SEE simulations to explain the heavy ion irradiation results. We concluded that ADC input impedance configuration should be carefully controlled in the design of radiation-hardened systems for space. C1 [Adell, Philippe C.; Yager, Jeremy; Pannell, Zack; Shelton, Jacob; Mojarradi, Mohammad M.; Allen, Greg; Some, Raphael] CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA. [Blalock, Benjamin] Univ Tennessee, Dept Elect Engn, Knoxville, TN 37996 USA. RP Adell, PC (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA. EM Philippe.c.adell@jpl.nasa.gov FU Mars Technology Research and Development Program at the Jet Propulsion Laboratory, California Institute of Technology; NASA Electronic Parts and Packaging Program FX The authors would like to thank the Mars Technology Research and Development Program at the Jet Propulsion Laboratory, California Institute of Technology, and the NASA Electronic Parts and Packaging Program for supporting this work. NR 14 TC 2 Z9 2 U1 1 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD JUN PY 2014 VL 61 IS 3 BP 1236 EP 1242 DI 10.1109/TNS.2014.2323975 PN 2 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA AJ7VC UT WOS:000337905900006 ER PT J AU Kumar, A Chen, F Barlage, M Ek, MB Niyogi, D AF Kumar, Anil Chen, Fei Barlage, Michael Ek, Michael B. Niyogi, Dev TI Assessing Impacts of Integrating MODIS Vegetation Data in the Weather Research and Forecasting (WRF) Model Coupled to Two Different Canopy-Resistance Approaches SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID LAND-SURFACE PARAMETERIZATION; INTERNATIONAL H2O PROJECT; CONVECTIVE ADJUSTMENT SCHEME; MESOSCALE ETA-MODEL; LAYER PARAMETERIZATIONS; ATMOSPHERE INTERACTIONS; STOMATAL CONDUCTANCE; PHOTOSYNTHESIS MODEL; BIOCHEMICAL-MODEL; FIFE OBSERVATIONS AB The impact of 8-day-averaged data from the Moderate Resolution Imaging Spectroradiometer (MODIS) sensor-namely, the 1-km leaf area index, absorbed photosynthetic radiation, and land-use data-is investigated for use in the Weather Research and Forecasting (WRF) model for regional weather prediction. These high-resolution, near-real-time MODIS data are hypothesized to enhance the representation of land-atmosphere interactions and to potentially improve the WRF model forecast skill for temperature, surface moisture, surface fluxes, and soil temperature. To test this hypothesis, the impact of using MODIS-based land surface data on surface energy and water budgets was assessed within the "Noah" land surface model with two different canopy-resistance schemes. An ensemble of six model experiments was conducted using the WRF model for a typical summertime episode over the U.S. southern Great Plains that occurred during the International H2O Project (IHOP_2002) field experiment. The six model experiments were statistically analyzed and showed some degree of improvement in surface latent heat flux and sensible heat flux, as well as surface temperature and moisture, after land use, leaf area index, and green vegetation fraction data were replaced by remotely sensed data. There was also an improvement in the WRF-simulated temperature and boundary layer moisture with MODIS data in comparison with the default U.S. Geological Survey land-use and leaf area index inputs. Overall, analysis suggests that recalibration and improvements to both the input data and the land model help to improve estimation of surface and soil parameters and boundary layer moisture and led to improvement in simulating convection in WRF runs. Incorporating updated land conditions provided the most notable improvements, and the mesoscale model performance could be further enhanced when improved land surface schemes become available. C1 [Kumar, Anil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kumar, Anil] Earth Syst Sci Interdisciplinary Ctr, College Pk, MD USA. [Kumar, Anil; Niyogi, Dev] Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA. [Chen, Fei; Barlage, Michael] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Ek, Michael B.] Natl Ctr Environm Predict, Camp Springs, MD USA. RP Kumar, A (reprint author), NASA, Hydrol Sci Branch, GSFC, Code 614-3, Greenbelt, MD 20771 USA. EM anil.kumar@nasa.gov RI Chen, Fei/B-1747-2009 FU National Environmental Satellite, Data, and Information Service (NESDIS); NOAA/JCSDA; DOE ARM [08ER64674]; NASA/GWEC-Terrestrial Hydrology Program; NCAR Water Cycle Program FX This work. was supported in part by the National Environmental Satellite, Data, and Information Service (NESDIS), NOAA/JCSDA (Research Area: Land Surface), DOE ARM (08ER64674; Dr. Rick Petty), NASA/GWEC-Terrestrial Hydrology Program (Dr. Jared Entin), and the NCAR Water Cycle Program. We also thank K. Manning (NCAR) and M. Duda (NCAR) for helping us with using satellite data in the model. NR 75 TC 11 Z9 11 U1 2 U2 29 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 JUN PY 2014 VL 53 IS 6 BP 1362 EP 1380 DI 10.1175/JAMC-D-13-0247.1 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ5YT UT WOS:000337767400003 ER PT J AU Adirosi, E Gorgucci, E Baldini, L Tokay, A AF Adirosi, Elisa Gorgucci, Eugenio Baldini, Luca Tokay, Ali TI Evaluation of Gamma Raindrop Size Distribution Assumption through Comparison of Rain Rates of Measured and Radar-Equivalent Gamma DSD SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY LA English DT Article ID POLARIMETRIC RADAR; MOMENT ESTIMATORS; CONVECTIVE CLOUDS; VIDEO DISDROMETER; PARAMETERS; SHAPE; BIAS; SPECTRA; ERROR; PRECIPITATION AB To date, one of the most widely used parametric forms for modeling raindrop size distribution (DSD) is the three-parameter gamma. The aim of this paper is to analyze the error of assuming such parametric form to model the natural DSDs. To achieve this goal, a methodology is set up to compare the rain rate obtained from a disdrometer-measured drop size distribution with the rain rate of a gamma drop size distribution that produces the same triplets of dual-polarization radar measurements, namely reflectivity factor, differential reflectivity, and specific differential phase shift. In such a way, any differences between the values of the two rain rates will provide information about how well the gamma distribution fits the measured precipitation. The difference between rain rates is analyzed in terms of normalized standard error and normalized bias using different radar frequencies, drop shape size relations, and disdrometer integration time. The study is performed using four datasets of DSDs collected by two-dimensional video disdrometers deployed in Huntsville (Alabama) and in three different prelaunch campaigns of the NASA-Japan Aerospace Exploration Agency (JAXA) Global Precipitation Measurement (GPM) ground validation program including the Hydrological Cycle in Mediterranean Experiment (HyMeX) special observation period (SOP) 1 field campaign in Rome. The results show that differences in rain rates of the disdrometer DSD and the gamma DSD determining the same dual-polarization radar measurements exist and exceed those related to the methodology itself and to the disdrometer sampling error, supporting the finding that there is an error associated with the gamma DSD assumption. C1 [Adirosi, Elisa; Gorgucci, Eugenio; Baldini, Luca] Italian Natl Res Council CNR, Inst Atmospher Sci & Climate, Rome, Italy. [Adirosi, Elisa] Univ Roma La Sapienza, Dept Civil Bldg & Environm Engn, I-00185 Rome, Italy. [Tokay, Ali] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Catonsville, MD USA. [Tokay, Ali] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Baldini, L (reprint author), CNR, Ist Sci Atmosfera & Clima, Area Ric Roma Tor Vergata 2, Via Fosso del Cavaliere, I-00133 Rome, Italy. EM l.baldini@isac.cnr.it RI Measurement, Global/C-4698-2015 OI Baldini, Luca/0000-0001-5217-1205; FU Italian Department of Civil Protection; NASA Precipitation Measurement Mission (PMM) [NNX10AJ12G] FX This research was partially supported by the Italian Department of Civil Protection and NASA Precipitation Measurement Mission (PMM) NNX10AJ12G under Ramesh Kakar, program scientist, NASA Headquarters. The authors acknowledge the anonymous reviewers for their detailed and helpful comments to the manuscript. The 2DVD measurements used in this study were collected during a 6-month-long field campaign in Huntsville, Alabama; LPVEx in Finland; MC3E in Oklahoma; and finally during the HyMeX SOP 1 in Rome, Italy, when the NASA 2DVD was set up at the Laboratory of Radio Meteorology of Sapienza University of Rome (Prof. F. S. Marzano). The authors acknowledge the NASA GPM mission ground validation program under Matthew Schwaller, GPM ground validation manager, and Walter A. Petersen, GPM ground validation science manager, for providing 2DVD data and contributions to the HyMeX field campaign. Acknowledgments extend to Arthur Hou (deceased), former GPM project scientist, for his vision throughout the GPM core-satellite prelaunch activities. NR 46 TC 12 Z9 12 U1 3 U2 8 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1558-8424 EI 1558-8432 J9 J APPL METEOROL CLIM JI J. Appl. Meteorol. Climatol. PD JUN PY 2014 VL 53 IS 6 BP 1618 EP 1635 DI 10.1175/JAMC-D-13-0150.1 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AJ5YT UT WOS:000337767400018 ER PT J AU Feldman, A de Kleer, J Kurtoglu, T Narasimhan, S Poll, S Garcia, D Kuhn, L van Gemund, AJC AF Feldman, Alexander de Kleer, Johan Kurtoglu, Tolga Narasimhan, Sriram Poll, Scott Garcia, David Kuhn, Lukas van Gemund, Arjan J. C. TI The Diagnostic Competitions SO AI MAGAZINE LA English DT Article AB The international diagnostic competitions provide a set of diagnostic benchmarks to evaluate diagnostic algorithms. This article describes a common diagnostic framework used to evaluate these algorithms. These competitions, started in 2009, have significantly helped shape subsequent diagnostic algorithms. C1 [Feldman, Alexander] AI Lab, Delft, Netherlands. [de Kleer, Johan] Xeroxs Palo Alto Res Ctr, Palo Alto, CA USA. [Kurtoglu, Tolga] PARCs Design & Digital Mfg Program, Palo Alto, CA USA. [Narasimhan, Sriram] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Narasimhan, Sriram] NASA, Ames Res Ctr, Mountain View, CA USA. [Poll, Scott] Univ Michigan, Ann Arbor, MI 48109 USA. [Garcia, David] Palo Alto Res Ctr, Palo Alto, CA USA. RP Feldman, A (reprint author), AI Lab, Delft, Netherlands. NR 12 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 SUM PY 2014 VL 35 IS 2 BP 49 EP 53 PG 5 WC Computer Science, Artificial Intelligence SC Computer Science GA AJ5ZH UT WOS:000337768900005 ER PT J AU Takahashi, Y Scheeres, DJ AF Takahashi, Yu Scheeres, D. J. TI Small body surface gravity fields via spherical harmonic expansions SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY LA English DT Article DE Asteroid; Gravity field; Spherical harmonics; Spherical Bessel function; Proximity operation; Laplace's equation; Poisson's equation; Brillouin sphere; Bennu; Castalia ID RADAR IMAGES; SHAPE MODEL AB Conventional gravity field expressions are derived from Laplace's equation, the result being the spherical harmonic gravity field. This gravity field is said to be the exterior spherical harmonic gravity field, as its convergence region is outside the Brillouin (i.e., circumscribing) sphere of the body. In contrast, there exists its counterpart called the interior spherical harmonic gravity field for which the convergence region lies within the interior Brillouin sphere that is not the same as the exterior Brillouin sphere. Thus, the exterior spherical harmonic gravity field cannot model the gravitation within the exterior Brillouin sphere except in some special cases, and the interior spherical harmonic gravity field cannot model the gravitation outside the interior Brillouin sphere. In this paper, we will discuss two types of other spherical harmonic gravity fields that bridge the null space of the exterior/interior gravity field expressions by solving Poisson's equation. These two gravity fields are obtained by assuming the form of Helmholtz's equation to Poisson's equation. This method renders the gravitational potentials as functions of spherical Bessel functions and spherical harmonic coefficients. We refer to these gravity fields as the interior/exterior spherical Bessel gravity fields and study their characteristics. The interior spherical Bessel gravity field is investigated in detail for proximity operation purposes around small primitive bodies. Particularly, we apply the theory to asteroids Bennu (formerly 1999 RQ36) and Castalia to quantify its performance around both nearly spheroidal and contact-binary asteroids, respectively. Furthermore, comparisons between the exterior gravity field, interior gravity field, interior spherical Bessel gravity field, and polyhedral gravity field are made and recommendations are given in order to aid planning of proximity operations for future small body missions. C1 [Takahashi, Yu; Scheeres, D. J.] Univ Colorado, Boulder, CO 80309 USA. RP Takahashi, Y (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM yu.takahashi@colorado.edu; scheeres@colorado.edu FU NASA's OSIRIS-REx New Frontiers mission [NNM10AA11C] FX This research was supported by NASA's OSIRIS-REx New Frontiers mission through grant NNM10AA11C. NR 35 TC 4 Z9 4 U1 1 U2 6 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0923-2958 EI 1572-9478 J9 CELEST MECH DYN ASTR JI Celest. Mech. Dyn. Astron. PD JUN PY 2014 VL 119 IS 2 BP 169 EP 206 DI 10.1007/s10569-014-9552-9 PG 38 WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications SC Astronomy & Astrophysics; Mathematics GA AJ6GE UT WOS:000337787900003 ER PT J AU Cumbers, J Rothschild, LJ AF Cumbers, John Rothschild, Lynn J. TI Salt tolerance and polyphyly in the cyanobacterium Chroococcidiopsis (Pleurocapsales) SO JOURNAL OF PHYCOLOGY LA English DT Article DE Chroococcidiopsis; Cyanobacteria; extremophile; halophile; halophyly; halotolerance; moderate halophile; phylogenetics; Pleurocapsales; salt tolerance ID BLUE-GREEN-ALGAE; PHYLOGENETIC TREES; LIFE; INFERENCE; PROGRAM; ECOLOGY; MODEL; MARS; ARB AB Chroococcidiopsis Geitler (Geitler 1933) is a genus of cyanobacteria containing desiccation and radiation resistant strains. Members of the genus live in habitats ranging from hot and cold deserts to fresh and saltwater environments. Morphology and cell division pattern have historically been used to define the genus. To better understand the evolution and ability of the Chroococcidiopsis genus to survive in diverse environments we investigated how salt tolerance varies among 15 strains previously isolated from different locations, and if salt tolerant strains are monophyletic to those isolated from freshwater and land environments. Four markers were sequenced from these 15 strains, the 16S rRNA, rbcL, desC1, and gltX genes. Phylogenetic trees were generated which identified a distinct clade of salt-tolerant strains. This study demonstrates that the genus is polyphyletic based on saltwater and freshwater phenotypes. To understand the resistance to salt in more details, the strains were grown on a range of sea salt concentrations which demonstrated that the freshwater strains were salt-intolerant whilst the saltwater strains required salt for growth. This study shows an increased resolution of the phylogeny of Chroococcidiopsis and provides further evidence that the genus is polyphyletic and should be reclassified to improve clarity in the literature. C1 [Cumbers, John] NASA, Ames Res Ctr, NASA Ames Space Portal SynBioBeta, Moffett Field, CA 94035 USA. [Cumbers, John; Rothschild, Lynn J.] Brown Univ, Dept Mol Biol Cell Biol & Biochem, Providence, RI 02912 USA. [Rothschild, Lynn J.] NASA, Ames Res Ctr, Biospher Sci Branch, Moffett Field, CA 94035 USA. RP Rothschild, LJ (reprint author), Brown Univ, Dept Mol Biol Cell Biol & Biochem, Box G-W, Providence, RI 02912 USA. EM lynn.j.rothschild@nasa.gov FU Brown University; NASA Ames Research Center, NASA [NNX08AZ52A] FX Thanks to J. M. Grace for technical assistance and thanks to R. Castenholz, A. Coleman, C. Dunn, M. Tatar, D. Weinreich, and G. Wessel for commenting on the manuscript. Thanks to R. Castenholz for the kind gift of strains from the Culture Collection of Microorganisms from Extreme Environments (CCMEE), to R. Anderson for the kind gift of strains from the Center for Culture of Marine Phytoplankton, to C. Kerfeld for sequence data from Chroococcidiopsis PCC 7203 (Germany) which aided primer design and to two anonymous reviewers whose comments greatly improved the manuscript. Special thanks to S. P. Worden and the NASA Synthetic Biology Program. JC was funded as part of a cooperative agreement between Brown University and NASA Ames Research Center, NASA Award Number NNX08AZ52A. NR 47 TC 4 Z9 4 U1 1 U2 22 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-3646 EI 1529-8817 J9 J PHYCOL JI J. Phycol. PD JUN PY 2014 VL 50 IS 3 BP 472 EP 482 DI 10.1111/jpy.12169 PG 11 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA AJ3IN UT WOS:000337559800006 PM 26988320 ER PT J AU Jacobson, NS AF Jacobson, Nathan S. TI Silica Activity Measurements in the Y2O3-SiO2 System and Applications to Modeling of Coating Volatility SO JOURNAL OF THE AMERICAN CERAMIC SOCIETY LA English DT Article ID TEMPERATURE MASS-SPECTROMETRY; IONIZATION CROSS-SECTIONS; PHASE-EQUILIBRIA; KNUDSEN CELL; WATER-VAPOR; THERMODYNAMICS; CONSTRAINTS; CERAMICS; PRESSURE; Y2SIO5 AB Rare-earth silicate compounds, such as those in the Y2O3-SiO2 system, are promising candidates for coatings of SiC-based ceramics and ceramic matrix composites in combustion environments. The predicted lower activity of silica in these silicates will lead to less reactivity with the water vapor combustion products. A procedure for measuring silica activities in this system is discussed. Knudsen effusion mass spectrometry is used and the measured vapor pressure of SiO(g) is correlated to activity. Due to the low vapor pressure of SiO(g) in the temperature range of interest, a reducing agent is utilized to boost this vapor pressure without altering the solid-state composition. In addition, corrections are made for nonequilibrium vaporization. The measured silica activities are: Y2O3+Y2O3 center dot SiO2 two phase field: log[a(SiO2)]=-5200.26(1/T)+0.0567 (15322 calibration gas, and R.H. Becker and R.O. Pepin for insightful discussions during preparation of this manuscript. NR 33 TC 5 Z9 5 U1 1 U2 32 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 JUN PY 2014 VL 96 BP 99 EP 113 DI 10.1016/j.pss.2014.03.005 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI4GV UT WOS:000336824600010 ER PT J AU Strapazzon, G Pilo, L Bessone, L Barratt, MR AF Strapazzon, Giacomo Pilo, Luca Bessone, Loredana Barratt, Michael R. TI CAVES as an Environment for Astronaut Training SO WILDERNESS & ENVIRONMENTAL MEDICINE LA English DT Letter C1 [Strapazzon, Giacomo] EURAC Inst Mt Emergency Med, Bolzano, Italy. [Strapazzon, Giacomo; Pilo, Luca] CNSAS Italian Mt & Cave Rescue Serv, Milan, Italy. [Bessone, Loredana] European Space Agcy, Directorate Human Space Flight & Operat, Cologne, Germany. [Barratt, Michael R.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Strapazzon, G (reprint author), EURAC Inst Mt Emergency Med, Bolzano, Italy. NR 5 TC 1 Z9 1 U1 0 U2 1 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 1080-6032 EI 1545-1534 J9 WILD ENVIRON MED JI Wildern. Environ. Med. PD SUM PY 2014 VL 25 IS 2 BP 244 EP 245 PG 2 WC Public, Environmental & Occupational Health; Sport Sciences SC Public, Environmental & Occupational Health; Sport Sciences GA AI5YL UT WOS:000336946800017 PM 24631231 ER PT J AU Ladd, SL Toscano, WB Cowings, PS Gabrieli, JDE AF Ladd, Sandra L. Toscano, William B. Cowings, Patricia S. Gabrieli, John D. E. TI Cardiovascular Change During Encoding Predicts the Nonconscious Mere Exposure Effect SO AMERICAN JOURNAL OF PSYCHOLOGY LA English DT Article ID FEEDBACK TRAINING EXERCISE; RATE-ORIENTING RESPONSE; IMPLICIT MEMORY; RELAXATION RESPONSE; INDIVIDUAL-DIFFERENCES; SELECTIVE ATTENTION; PERCEPTUAL FLUENCY; EXPLICIT MEMORY; RECOGNITION; PREFERENCE AB These studies examined memory encoding to determine whether the mere exposure effect could be categorized as a form of conceptual or perceptual implicit priming and, if it was not conceptual or perceptual, whether cardiovascular psychophysiology could reveal its nature. Experiment 1 examined the effects of study phase level of processing on recognition, the mere exposure effect, and word identification implicit priming. Deep relative to shallow processing improved recognition but did not influence the mere exposure effect for nonwords or word identification implicit priming for words. Experiments 2 and 3 examined the effect of study test changes in font and orientation, respectively, on the mere exposure effect and word identification implicit priming. Different study test font and orientation reduced word identification implicit priming but had no influence on the mere exposure effect. Experiments 4 and 5 developed and used, respectively, a cardiovascular psychophysiological implicit priming paradigm to examine whether stimulus-specific cardiovascular reactivity at study predicted the mere exposure effect at test. Blood volume pulse change at study was significantly greater for nonwords that were later preferred than for nonwords that were not preferred at test. There was no difference in blood volume pulse change for words at study that were later either identified or not identified at test. Fluency effects, at encoding or retrieval, are an unlikely explanation for these behavioral and cardiovascular findings. The relation of blood volume pulse to affect suggests that an affective process that is not conceptual or perceptual contributes to the mere exposure effect. C1 [Ladd, Sandra L.] Boston Univ, Sch Med, Boston, MA 02118 USA. [Toscano, William B.; Cowings, Patricia S.] NASA, Ames Res Ctr, Pasadena, CA USA. [Gabrieli, John D. E.] MIT, Cambridge, MA 02139 USA. RP Ladd, SL (reprint author), Boston Univ, Sch Med, Div Grad Med Sci, L-815,715 Albany St, Boston, MA 02118 USA. EM laddsl@bu.edu NR 75 TC 2 Z9 2 U1 1 U2 20 PU UNIV ILLINOIS PRESS PI CHAMPAIGN PA 1325 S OAK ST, CHAMPAIGN, IL 61820-6903 USA SN 0002-9556 EI 1939-8298 J9 AM J PSYCHOL JI Am. J. Psychol. PD SUM PY 2014 VL 127 IS 2 BP 157 EP 182 PG 26 WC Psychology, Multidisciplinary SC Psychology GA AH7XV UT WOS:000336349600003 PM 24934008 ER PT J AU Kopparapu, RK Ramirez, RM SchottelKotte, J Kasting, JF Domagal-Goldman, S Eymet, V AF Kopparapu, Ravi Kumar Ramirez, Ramses M. SchottelKotte, James Kasting, James F. Domagal-Goldman, Shawn Eymet, Vincent TI HABITABLE ZONES AROUND MAIN-SEQUENCE STARS: DEPENDENCE ON PLANETARY MASS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planets and satellites: atmospheres ID EXTRA-SOLAR PLANETS; EARTH-LIKE PLANETS; M-CIRCLE-PLUS; HARPS SEARCH; SUPER-EARTHS; RUNAWAY GREENHOUSE; EARLY MARS; SYSTEM; ATMOSPHERE; INSOLATION AB The ongoing discoveries of extra-solar planets are unveiling a wide range of terrestrial mass (size) planets around their host stars. In this Letter, we present estimates of habitable zones (HZs) around stars with stellar effective temperatures in the range 2600 K-7200 K, for planetary masses between 0.1 M-circle plus and 5 M-circle plus. Assuming H2O-(inner HZ) and CO2-(outer HZ) dominated atmospheres, and scaling the background N-2 atmospheric pressure with the radius of the planet, our results indicate that larger planets have wider HZs than do smaller ones. Specifically, with the assumption that smaller planets will have less dense atmospheres, the inner edge of the HZ (runaway greenhouse limit) moves outward (similar to 10% lower than Earth flux) for low mass planets due to larger greenhouse effect arising from the increased H2O column depth. For larger planets, the H2O column depth is smaller, and higher temperatures are needed before water vapor completely dominates the outgoing longwave radiation. Hence the inner edge moves inward (similar to 7% higher than Earth's flux). The outer HZ changes little due to the competing effects of the greenhouse effect and an increase in albedo. New, three-dimensional climate model results from other groups are also summarized, and we argue that further, independent studies are needed to verify their predictions. Combined with our previous work, the results presented here provide refined estimates of HZs around main-sequence stars and provide a step toward a more comprehensive analysis of HZs. C1 [Kopparapu, Ravi Kumar; Ramirez, Ramses M.; Kasting, James F.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Kopparapu, Ravi Kumar; Ramirez, Ramses M.; Kasting, James F.; Domagal-Goldman, Shawn] NASA, Astrobiol Inst, Virtual Planetary Lab, Seattle, WA 98195 USA. [Kopparapu, Ravi Kumar; Ramirez, Ramses M.; Kasting, James F.] Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA. [Kopparapu, Ravi Kumar; Ramirez, Ramses M.; Kasting, James F.] Penn State Univ, Dept Geosci, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Kopparapu, Ravi Kumar] Blue Marble Space Inst Sci, Seattle, WA 98145 USA. [SchottelKotte, James] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Domagal-Goldman, Shawn] NASA, Planetary Environm Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Eymet, Vincent] Univ Bordeaux 1, Lab Astrophys Bordeaux, UMR 5804, F-33270 Floirac, France. RP Kopparapu, RK (reprint author), Penn State Univ, Dept Geosci, 443 Deike Bldg, University Pk, PA 16802 USA. EM ruk15@psu.edu OI Domagal-Goldman, Shawn/0000-0003-0354-9325 FU NASA Astrobiology Institute's Virtual Planetary Laboratory; NASA [NNH05ZDA001C]; Penn State Astrobiology Research Center; European Research Council [209622: E3ARTHs]; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium FX The authors thank an anonymous reviewer whose comments greatly improved the manuscript. R.K., R.R., J.F.K, and S.D.G. gratefully acknowledge funding from NASA Astrobiology Institute's Virtual Planetary Laboratory lead team, supported by NASA under cooperative agreement NNH05ZDA001C, and the Penn State Astrobiology Research Center. V.E. acknowledges the support of the European Research Council (Starting Grant 209622: E3ARTHs). 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. R.K. and R.R. contributed equally to this work. NR 41 TC 70 Z9 71 U1 5 U2 27 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 JUN 1 PY 2014 VL 787 IS 2 AR L29 DI 10.1088/2041-8205/787/2/L29 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI3XB UT WOS:000336797700014 ER PT J AU Tricarico, P Samarasinha, NH Sykes, MV Li, JY Farnham, TL Kelley, MSP Farnocchia, D Stevenson, R Bauer, JM Lock, RE AF Tricarico, Pasquale Samarasinha, Nalin H. Sykes, Mark V. Li, Jian-Yang Farnham, Tony L. Kelley, Michael S. P. Farnocchia, Davide Stevenson, Rachel Bauer, James M. Lock, Robert E. TI DELIVERY OF DUST GRAINS FROM COMET C/2013 A1 (SIDING SPRING) TO MARS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE comets: individual (C/2013 A1 (Siding Spring)); meteorites, meteors, meteoroids ID 103P/HARTLEY 2 AB Comet C/2013 A1 (Siding Spring) will have a close encounter with Mars on 2014 October 19. We model the dynamical evolution of dust grains from the time of their ejection from the comet nucleus to the close encounter with Mars, and determine the flux at Mars. Constraints on the ejection velocity from Hubble Space Telescope observations indicate that the bulk of the grains will likely miss Mars, although it is possible that a few percent of the grains with higher velocities will reach Mars, peaking approximately 90-100 minutes after the close approach of the nucleus, and consisting mostly of millimeter-radius grains ejected from the comet nucleus at a heliocentric distance of approximately 9 AU or larger. At higher velocities, younger grains from submillimeter to several millimeters can also reach Mars, although an even smaller fraction of grains is expected have these velocities, with negligible effect on the peak timing. Using NEOWISE observations of the comet, we can estimate that the maximum fluence will be of the order of 10(-7) grains m(-2). We include a detailed analysis of how the expected fluence depends on the grain density, ejection velocity, and size frequency distribution, to account for current model uncertainties and in preparation of possible refined model values in the near future. C1 [Tricarico, Pasquale; Samarasinha, Nalin H.; Sykes, Mark V.; Li, Jian-Yang] Planetary Sci Inst, Tucson, AZ 85719 USA. [Farnham, Tony L.; Kelley, Michael S. P.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Farnocchia, Davide; Stevenson, Rachel; Bauer, James M.; Lock, Robert E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Tricarico, P (reprint author), Planetary Sci Inst, 1700 E Ft Lowell 106, Tucson, AZ 85719 USA. EM tricaric@psi.edu OI Kelley, Michael/0000-0002-6702-7676 FU NASA JPL Mars Critical Data Products Program; NASA Planetary Atmospheres Program [NNX11AD91G]; Planetary Science Division of NASA; NASA; NASA Postdoctoral Program FX This research was supported by a contract to the Planetary Science Institute by the NASA JPL Mars Critical Data Products Program and by NASA Planetary Atmospheres Program grant NNX11AD91G to the Planetary Science Institute. HST data and funding were provided through GO-13610. NEOWISE is a project of JPL/Caltech funded by the Planetary Science Division of NASA. The work of D. Farnocchia was conducted at JPL/Caltech under a contract with NASA. R. Stevenson is funded by the NASA Postdoctoral Program. NR 18 TC 19 Z9 19 U1 0 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 JUN 1 PY 2014 VL 787 IS 2 AR L35 DI 10.1088/2041-8205/787/2/L35 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AI3XB UT WOS:000336797700020 ER PT J AU Drewry, DT Kumar, P Long, SP AF Drewry, Darren T. Kumar, Praveen Long, Stephen P. TI Simultaneous improvement in productivity, water use, and albedo through crop structural modification SO GLOBAL CHANGE BIOLOGY LA English DT Article DE agriculture; albedo; carbon uptake; climate change; crop breeding; crop ideotype; evapotranspiration; plant optimization; sustainability; water use efficiency ID NITROGEN USE EFFICIENCY; CO2 ENRICHMENT FACE; GREEN-REVOLUTION; LEAF NITROGEN; ELEVATED CO2; BIOMASS PRODUCTION; PLANT CANOPIES; GAS-EXCHANGE; PHOTOSYNTHESIS; YIELD AB Spanning 15% of the global ice-free terrestrial surface, agricultural lands provide an immense and near-term opportunity to address climate change, food, and water security challenges. Through the computationally informed breeding of canopy structural traits away from those of modern cultivars, we show that solutions exist that increase productivity and water use efficiency, while increasing land-surface reflectivity to offset greenhouse gas warming. Plants have evolved to maximize capture of radiation in the upper leaves, thus shading competitors. While important for survival in the wild, this is suboptimal in monoculture crop fields for maximizing productivity and other biogeophysical services. Crop progenitors evolved over the last 25 million years in an atmosphere with less than half the [CO2] projected for 2050. By altering leaf photosynthetic rates, rising [CO2] and temperature may also alter the optimal canopy form. Here using soybean, the world's most important protein crop, as an example we show by applying optimization routines to a micrometeorological leaf canopy model linked to a steady-state model of photosynthesis, that significant gains in production, water use, and reflectivity are possible with no additional demand on resources. By modifying total canopy leaf area, its vertical profile and angular distribution, and shortwave radiation reflectivity, all traits available in most major crop germplasm collections, increases in productivity (7%) are possible with no change in water use or albedo. Alternatively, improvements in water use (13%) or albedo (34%) can likewise be made with no loss of productivity, under Corn Belt climate conditions. C1 [Drewry, Darren T.] CALTECH, Jet Prop Lab, Climate Phys Grp, Pasadena, CA 91109 USA. [Drewry, Darren T.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA. [Kumar, Praveen] Univ Illinois, Dept Civil & Environm Engn, Hydrosyst Lab 2527B, Urbana, IL 61801 USA. [Kumar, Praveen] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA. [Long, Stephen P.] Univ Illinois, Dept Crop Sci, Urbana, IL 61801 USA. [Long, Stephen P.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. RP Drewry, DT (reprint author), CALTECH, Jet Prop Lab, Climate Phys Grp, M-S 233-300, Pasadena, CA 91109 USA. EM ddrewry@jpl.nasa.gov; kumar1@illinois.edu RI Kumar, Praveen/D-2036-2010; Long, Stephen/A-2488-2008 OI Kumar, Praveen/0000-0002-4787-0308; Long, Stephen/0000-0002-8501-7164 FU NSF [ATM 06-28687, CBET 12-09402, EAR 13-31906]; National Science Foundation International Research Fellowship Program (IRFP) [OISE-0900556]; Bill and Melinda Gates Foundation [OPP1060461]; Civil and Environmental Engineering Department, University of Illinois; Jet Propulsion Laboratory; California Institute of Technology; National Aeronautics and Space Administration FX This study was initiated under NSF Grant ATM 06-28687 when the first author was at the University of Illinois. This support is gratefully acknowledged. DTD further acknowledges support by the National Science Foundation International Research Fellowship Program (IRFP), award OISE-0900556. DTD also acknowledges support of the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. SPL and PK acknowledge support from the Bill and Melinda Gates Foundation (OPP1060461) titled 'RIPE - Realizing Increased Photosynthetic Efficiency for Sustainable Increases in Crop Yield'. PK also acknowledges NSF awards CBET 12-09402 and EAR 13-31906, as well as support from the Civil and Environmental Engineering Department, University of Illinois, to support research on Water Security and Emergent Risks. NR 75 TC 25 Z9 26 U1 5 U2 75 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 JUN PY 2014 VL 20 IS 6 BP 1955 EP 1967 DI 10.1111/gcb.12567 PG 13 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AH9SP UT WOS:000336482700021 PM 24700722 ER PT J AU Banik, A Gabb, T AF Banik, Anthony Gabb, Timothy TI International Symposium on Superalloy 718 and Derivatives Offers Technical Breadth SO JOM LA English DT Editorial Material C1 [Banik, Anthony] ATI Allvac Allegheny Technol, Monroe, NC 28110 USA. [Gabb, Timothy] NASA, Glenn Res Ctr, Washington, DC USA. RP Banik, A (reprint author), ATI Allvac Allegheny Technol, Monroe, NC 28110 USA. EM anthony.banik@atimetals.com; timothy.p.gabb@nasa.gov NR 0 TC 0 Z9 0 U1 1 U2 2 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 JUN PY 2014 VL 66 IS 6 BP 855 EP 855 DI 10.1007/s11837-014-0992-1 PG 1 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering; Mineralogy; Mining & Mineral Processing SC Materials Science; Metallurgy & Metallurgical Engineering; Mineralogy; Mining & Mineral Processing GA AI2ZM UT WOS:000336727700002 ER PT J AU Le Borgne, JF Poretti, E Klotz, A Denoux, E Smith, HA Kolenberg, K Szabo, R Bryson, S Audejean, M Buil, C Caron, J Conseil, E Corp, L Drillaud, C de France, T Graham, K Hirosawa, K Klotz, AN Kugel, F Loughney, D Menzies, K Rodriguez, M Ruscitti, PM AF Le Borgne, J. F. Poretti, E. Klotz, A. Denoux, E. Smith, H. A. Kolenberg, K. Szabo, R. Bryson, S. Audejean, M. Buil, C. Caron, J. Conseil, E. Corp, L. Drillaud, C. de France, T. Graham, K. Hirosawa, K. Klotz, A. N. Kugel, F. Loughney, D. Menzies, K. Rodriguez, M. Ruscitti, P. M. TI Historical vanishing of the Blazhko effect of RR Lyr from the GEOS and Kepler surveys SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; stars: individual: RR Lyrae; stars: oscillations; stars: variables: RR Lyrae ID TAROT TELESCOPES; STARS; PERIOD; LIGHT; BEHAVIOR; CYCLE AB RR Lyr is one of the most studied variable stars. Its light curve has been regularly monitored since the discovery of its periodic variability in 1899. The analysis of all observed maxima allows us to identify two primary pulsation states, defined as pulsation over a long (P-0 longer than 0.56684 d) and a short (P-0 shorter than 0.56682 d) primary pulsation period. These states alternate with intervals of 13-16 yr, and are well defined after 1943. The 40.8-d periodical modulations of the amplitude and the period (i.e. the Blazhko effect) were noticed in 1916. We provide homogeneous determinations of the Blazhko period in the different primary pulsation states. The Blazhko period does not follow the variations of P-0 and suddenly diminished from 40.8 d to around 39.0 d in 1975. The monitoring of these periodicities deserved, and still deserves, a continuous and intensive observational effort. For this purpose, we have built dedicated, transportable and autonomous small instruments, Very Tiny Telescopes (VTTs), to observe the times of maximum brightness of RR Lyr. As immediate results, the VTTs recorded the last change of the P-0 state in mid-2009 and extended the time coverage of the Kepler observations, thus recording a maximum O - C amplitude of the Blazhko effect at the end of 2008, followed by the historically smallest O - C amplitude in late 2013. This decrease is still ongoing and the VTTs are ready to monitor the expected increase in the next few years. C1 [Le Borgne, J. F.; Poretti, E.; Klotz, A.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Le Borgne, J. F.; Poretti, E.; Klotz, A.] CNRS, IRAP, F-31400 Toulouse, France. [Le Borgne, J. F.; Poretti, E.; Klotz, A.; Denoux, E.; Corp, L.; Klotz, A. N.] GEOS, F-28300 Bailleau Leveque, France. [Poretti, E.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Smith, H. A.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Kolenberg, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kolenberg, K.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium. [Szabo, R.] MTA CSFK, Konkoly Observ, H-1121 Budapest, Hungary. [Bryson, S.] NASA Ames Res Ctr, Mountain View, CA 94035 USA. [Audejean, M.] Observ Chinon, F-37500 Chinon, France. [Buil, C.] Observ Castanet Tolosan, F-31320 Castanet Tolosan, France. [Caron, J.; Kugel, F.] Observ Chante Perdrix, F-04150 Banon, France. [Conseil, E.; Drillaud, C.] Observ Strasbourg, AFOEV, F-67000 Strasbourg, France. [Corp, L.; de France, T.; Graham, K.; Menzies, K.] AAVSO, Cambridge, MA 02138 USA. [Hirosawa, K.] VSOLJ, Tsukuba, Ibaraki 3050035, Japan. [Loughney, D.] British Astron Assoc, Variable Star Sect BAA VSS, London W1J 0DU, England. [Ruscitti, P. M.] Osservatorio Astron B Occhialini, I-67041 Aielli, AQ, Italy. RP Le Borgne, JF (reprint author), Univ Toulouse, UPS OMP, IRAP, Toulouse, France. EM jleborgne@irap.omp.eu OI Poretti, Ennio/0000-0003-1200-0473; Szabo, Robert/0000-0002-3258-1909 FU NASA's Science Mission Directorate; Hungarian Academy of Science; Hungarian OTKA grant [K83790]; KTIA [URKUT_10-1-2011-0019]; European Community [269194]; Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences FX Funding for the Kepler Discovery Mission is provided by NASA's Science Mission Directorate. The Kepler Team and the Kepler Guest Observer Office are recognized for helping to make this mission and these data possible. EP acknowledges Observatoire Midi-Pyrenees for the two-month grant allocated in 2013 October and November, which allowed him to work at the Institut de Recherche en Astrophysique et Planetologie in Toulouse, France. The present study has used the SIMBAD data base operated at the Centre de Donnees Astronomiques (Strasbourg, France) and the GEOS RR Lyr data base hosted by IRAP (OMP-UPS, Toulouse, France). This study has been supported by the Lendulet-2009 Young Researchers Programme of the Hungarian Academy of Science, the Hungarian OTKA grant K83790 and the KTIA URKUT_10-1-2011-0019 grant. The research leading to these results has received funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 269194 (IRSES/ASK). RSz was supported by the Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences. The basic ideas of the VTT project have been sketched during several GEOS meetings, and fruitful discussions with R. Boninsegna, M. Dumont, J. Fabregat, F. Fumagalli, D. Husar, J. Remis, J. Vandenbroere and J. M. Vilalta are gratefully acknowledged. NR 39 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 JUN PY 2014 VL 441 IS 2 BP 1435 EP 1443 DI 10.1093/mnras/stu671 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH9WC UT WOS:000336494800039 ER PT J AU Graff, P Feroz, F Hobson, MP Lasenby, A AF Graff, Philip Feroz, Farhan Hobson, Michael P. Lasenby, Anthony TI SkyNet: an efficient and robust neural network training tool for machine learning in astronomy SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; methods: statistical ID COSMOLOGICAL PARAMETER-ESTIMATION; DEEP; CLASSIFICATION; RECOGNITION; NETS AB We present the first public release of our generic neural network training algorithm, called SkyNet. This efficient and robust machine learning tool is able to train large and deep feed-forward neural networks, including autoencoders, for use in a wide range of supervised and unsupervised learning applications, such as regression, classification, density estimation, clustering and dimensionality reduction. SkyNet uses a 'pre-training' method to obtain a set of network parameters that has empirically been shown to be close to a good solution, followed by further optimization using a regularized variant of Newton's method, where the level of regularization is determined and adjusted automatically; the latter uses second-order derivative information to improve convergence, but without the need to evaluate or store the full Hessian matrix, by using a fast approximate method to calculate Hessian-vector products. This combination of methods allows for the training of complicated networks that are difficult to optimize using standard backpropagation techniques. SkyNet employs convergence criteria that naturally prevent overfitting, and also includes a fast algorithm for estimating the accuracy of network outputs. The utility and flexibility of SkyNet are demonstrated by application to a number of toy problems, and to astronomical problems focusing on the recovery of structure from blurred and noisy images, the identification of gamma-ray bursters, and the compression and denoising of galaxy images. The SkyNet software, which is implemented in standard ANSI c and fully parallelized using MPI, is available at http://www.mrao.cam.ac.uk/software/skynet/. C1 [Graff, Philip] NASA, Gravitat Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Feroz, Farhan; Hobson, Michael P.; Lasenby, Anthony] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Lasenby, Anthony] Kavli Inst Cosmol, Cambridge CB3 0HA, England. RP Graff, P (reprint author), NASA, Gravitat Astrophys Lab, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM philip.b.graff@nasa.gov FU SGI/Intel; HEFCE; PPARC; Higher Education Funding Council for England; NASA Postdoctoral Fellowship from the Oak Ridge Associated Universities; Gates Cambridge Scholarship at the University of Cambridge; Leverhulme Trust; Newton Trust FX The authors thank John Skilling for providing very useful advice in the early stages of algorithm development. We also thank Amy Lien for providing the data used in Section 5.2. This work utilized three different high-performance computing facilities at different times: initial work was performed on COSMOS VIII, an SGI Altix UV1000 supercomputer, funded by SGI/Intel, HEFCE and PPARC, and the authors thank Andrey Kaliazin for assistance; early work also utilized 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; later work utilized the Discover system of the NASA Center for Climate Simulation at NASA Goddard Space Flight Center. PG is currently supported by a NASA Postdoctoral Fellowship from the Oak Ridge Associated Universities and completed a portion of this work while funded by a Gates Cambridge Scholarship at the University of Cambridge. FF is supported by a Research Fellowship from the Leverhulme and Newton Trusts. NR 53 TC 21 Z9 21 U1 2 U2 12 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 JUN PY 2014 VL 441 IS 2 BP 1741 EP 1759 DI 10.1093/mnras/stu642 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH9WC UT WOS:000336494800061 ER PT J AU Potter, C Melack, J Engle, D AF Potter, Christopher Melack, John M. Engle, Diana TI Modeling Methane Emissions from Amazon Floodplain Ecosystems SO WETLANDS LA English DT Article DE Methane; Amazon; Floodplain; Modeling; Wetlands ID COMPARISON PROJECT WETCHIMP; GLOBAL WETLAND EXTENT; MACROPHYTE COVER; NATURAL WETLANDS; CARBON-DIOXIDE; PRESENT STATE; LAKE; PRODUCTIVITY; VARIABILITY; SEDIMENTS AB A new process-based simulation model to estimate methane emissions from Amazon floodplain ecosystems is described and evaluated in comparison to independent measurements of methane fluxes. The model's three major components are 1) types of wetland vegetation and the changes in water level, temperature and dissolved oxygen of flooded areas, 2) plant production, biomass accumulation, and litterfall decay in soils and sediments, and 3) methane production and transport pathways through the water column and into the atmosphere. Ecological and limnological data from Lake Calado, a well-studied site in the central Amazon basin, were used to develop the model. One set of model simulations were generated for floating macrophytes. Predicted rates of CH4 emission to the atmosphere by all simulated transfer pathways were typically in the range of 0.25 to 0.33 g C m(-2) day(-1). Simulated CH4 emissions from flooded forests were predicted to be around 0.25 g m(-2) day(-1), nearly all by ebullition. These rates compare favorably to rates measured in Amazon floodplain habitats. C1 [Potter, Christopher] NASA Ames Res Ctr, Biospher Sci Branch, Moffett Field, CA USA. [Melack, John M.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. [Melack, John M.] Univ Calif Santa Barbara, Bren Sch Environm Sci andManagement, Santa Barbara, CA 93106 USA. [Engle, Diana] Univ Calif Santa Barbara, Earth Res Inst, Santa Barbara, CA 93106 USA. RP Melack, J (reprint author), Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. EM Chris.Potter@nasa.gov; melack@bren.ucsb.edu; DianaE@lwa.com FU NASA LBA ECO; NASA Terrestrial Ecology grants FX Funding for modeling and manuscript preparation was provided by NASA LBA ECO and NASA Terrestrial Ecology grants. NR 70 TC 2 Z9 2 U1 2 U2 53 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0277-5212 EI 1943-6246 J9 WETLANDS JI Wetlands PD JUN PY 2014 VL 34 IS 3 BP 501 EP 511 DI 10.1007/s13157-014-0516-3 PG 11 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA AH7CA UT WOS:000336288800009 ER PT J AU Vander Wal, RL Gaddam, CK Kulis, MJ AF Vander Wal, Randy L. Gaddam, Chethan K. Kulis, Michael J. TI An Investigation of Micro-Hollow Cathode Glow Discharge Generated Optical Emission Spectroscopy for Hydrocarbon Detection and Differentiation SO APPLIED SPECTROSCOPY LA English DT Article DE Micro-hollow cathode glow discharge; MHGD; Optical emission spectroscopy; OES; Micro-plasma; Spectral simulation; Plasma temperature ID ATMOSPHERIC-PRESSURE; GAS-CHROMATOGRAPHY; PLASMA; MICROPLASMA; EXPLOSIVES; AIR AB The analytical utility of a micro-hollow cathode glow discharge plasma for detection of varied hydrocarbons was tested using acetone, ethanol, heptane, nitrobenzene, and toluene. Differences in fragmentation pathways, reflecting parent compound molecular structure, led to differences in optical emission patterns that can then potentially serve as signatures for the species of interest. Spectral simulations were performed emphasizing the CH (A(2)Delta-X-2 Pi), CH (C-2 Sigma-X-2 Pi), and OH (A(2)Sigma-X-2 Pi) electronic systems. The analytical utility of selected emission lines is demonstrated by a linear relationship between optical emission spectroscopy and parent compound concentration over a wide range, with detection limits extending down to parts per billion (ppb) levels. C1 [Vander Wal, Randy L.; Gaddam, Chethan K.] Penn State Univ, John & Willie Leone Family Dept Energy & Mineral, University Pk, PA 16802 USA. [Vander Wal, Randy L.; Gaddam, Chethan K.] Penn State Univ, EMS Energy Inst, University Pk, PA 16802 USA. [Kulis, Michael J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Vander Wal, RL (reprint author), Penn State Univ, John & Willie Leone Family Dept Energy & Mineral, University Pk, PA 16802 USA. EM ruv12@psu.edu NR 39 TC 3 Z9 3 U1 2 U2 26 PU SOC APPLIED SPECTROSCOPY PI FREDERICK PA 5320 SPECTRUM DRIVE SUITE C, FREDERICK, MD 21703 USA SN 0003-7028 EI 1943-3530 J9 APPL SPECTROSC JI Appl. Spectrosc. PD JUN PY 2014 VL 68 IS 6 BP 649 EP 656 DI 10.1366/13-07160 PG 8 WC Instruments & Instrumentation; Spectroscopy SC Instruments & Instrumentation; Spectroscopy GA AH6JH UT WOS:000336236700005 PM 25014720 ER PT J AU Connelley, MS Greene, TP AF Connelley, Michael S. Greene, Thomas P. TI NEAR-IR SPECTROSCOPIC MONITORING OF CLASS I PROTOSTARS: VARIABILITY OF ACCRETION AND WIND INDICATORS SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared: stars; stars: formation; stars: protostars ID YOUNG STELLAR OBJECTS; T-TAURI STARS; MOLECULAR-HYDROGEN EMISSION; MAIN-SEQUENCE STARS; INFRARED FILTER SET; MIDINFRARED VARIABILITY; PHOTOMETRIC VARIABILITY; HEI LAMBDA-10830; P-OPHIUCHI; ORION AB We present the results of a program that monitored the near-IR spectroscopic variability of a sample of 19 embedded protostars. Spectra were taken on time intervals from 2 days to 3 yr, over a wavelength range from 0.85 mu m to 2.45 mu m, for 4-9 epochs of observations per target. We found that the spectra of all targets are variable and that every emission feature observed is also variable (although not for all targets). With one exception, there were no drastic changes in the continua of the spectra, nor did any line completely disappear, nor did any line appear that was not previously apparent. This analysis focuses on understanding the connection between accretion (traced by H Br gamma and CO) and the wind (traced by He I, [Fe II], and sometimes H-2). For both accretion and wind tracers, the median variability was constant versus the time interval between observations; however, the maximum variability that we observed increased with the time interval between observations. Extinction is observed to vary within the minimum sampling time of 2 days, suggesting extinguishing material within a few stellar radii at high disk latitudes. The variability of [Fe II] and H-2 were correlated for most (but not all) of the 7 young stellar objects showing both features, and the amplitude of the variability depends on the veiling. Although the occurrence of CO and Br gamma emission are connected, their variability is uncorrelated, suggesting that these emissions originate in separate regions near the protostar (e.g., disk and wind). The variability of Br gamma and wind tracers were found to be positively correlated, negatively correlated, or uncorrelated, depending on the target. The variability of Br gamma, [Fe II], and H-2 always lies on a plane, although the orientation of the plane in three dimensions depends on the target. While we do not understand all interactions behind the variability that we observed, we have shown that spectroscopic variability is a powerful tool toward understanding the star formation process. C1 [Connelley, Michael S.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [Greene, Thomas P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Connelley, MS (reprint author), Univ Hawaii, Inst Astron, 640 N Aohoku Pl, Hilo, HI 96720 USA. FU National Aeronautics and Space Administration; National Science Foundation FX We are grateful for the professional assistance from Bill Golish, Dave Griep, Paul Sears, and Eric Volquardsen at the IRTF. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and NASA's Astrophysics Data System. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of NASA's Astrophysics Data System. This research was supported by an appointment to the NASA Postdoctoral Program at the Ames Research Center, administered by the Oak Ridge Associated Universities through a contract with NASA. NR 44 TC 8 Z9 8 U1 0 U2 0 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 JUN PY 2014 VL 147 IS 6 AR 125 DI 10.1088/0004-6256/147/6/125 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6TC UT WOS:000336262600001 ER PT J AU Coughlin, JL Thompson, SE Bryson, ST Burke, CJ Caldwell, DA Christiansen, JL Haas, MR Howell, SB Jenkins, JM Kolodziejczak, JJ Mullally, FR Rowe, JF AF Coughlin, Jeffrey L. Thompson, Susan E. Bryson, Stephen T. Burke, Christopher J. Caldwell, Douglas A. Christiansen, Jessie L. Haas, Michael R. Howell, Steve B. Jenkins, Jon M. Kolodziejczak, Jeffery J. Mullally, Fergal R. Rowe, Jason F. TI CONTAMINATION IN THE KEPLER FIELD. IDENTIFICATION OF 685 KOIs AS FALSE POSITIVES VIA EPHEMERIS MATCHING BASED ON Q1-Q12 DATA (vol 147, pg 119, 2014) SO ASTRONOMICAL JOURNAL LA English DT Correction C1 [Coughlin, Jeffrey L.; Thompson, Susan E.; Burke, Christopher J.; Caldwell, Douglas A.; Jenkins, Jon M.; Mullally, Fergal R.; Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA. [Coughlin, Jeffrey L.; Thompson, Susan E.; Bryson, Stephen T.; Burke, Christopher J.; Caldwell, Douglas A.; Haas, Michael R.; Howell, Steve B.; Jenkins, Jon M.; Mullally, Fergal R.; Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Christiansen, Jessie L.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Kolodziejczak, Jeffery J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Coughlin, JL (reprint author), SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA. EM jeffrey.l.coughlin@nasa.gov RI Caldwell, Douglas/L-7911-2014 OI Caldwell, Douglas/0000-0003-1963-9616 NR 1 TC 1 Z9 1 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 JUN PY 2014 VL 147 IS 6 AR 163 DI 10.1088/0004-6256/147/6/163 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6TC UT WOS:000336262600039 ER PT J AU Liu, WM Padgett, DL Terebey, S Angione, J Rebull, LM McCollum, B Fajardo-Acosta, S Leisawitz, D AF Liu, Wilson M. Padgett, Deborah L. Terebey, Susan Angione, John Rebull, Luisa M. McCollum, Bruce Fajardo-Acosta, Sergio Leisawitz, David TI WIDE-FIELD INFRARED SURVEY EXPLORER OBSERVATIONS OF YOUNG STELLAR OBJECTS IN THE LYNDS 1509 DARK CLOUD IN AURIGA SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared: stars; stars: formation; stars: pre-main sequence ID MOLECULAR CLOUD; MU-M; CATALOG; MIPS; SKY AB The Wide-Field Infrared Survey Explorer (WISE) has uncovered a striking cluster of young stellar object (YSO) candidates associated with the L1509 dark cloud in Auriga. The WISE observations, at 3.4 mu m, 4.6 mu m, 12 mu m, and 22 mu m, show a number of objects with colors consistent with YSOs, and their spectral energy distributions suggest the presence of circumstellar dust emission, including numerous Class I, flat spectrum, and Class II objects. In general, the YSOs in L1509 are much more tightly clustered than YSOs in other dark clouds in the Taurus-Auriga star forming region, with Class I and flat spectrum objects confined to the densest aggregates, and Class II objects more sparsely distributed. We estimate a most probable distance of 485-700 pc, and possibly as far as the previously estimated distance of 2 kpc. C1 [Liu, Wilson M.; McCollum, Bruce; Fajardo-Acosta, Sergio] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Padgett, Deborah L.; Leisawitz, David] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Terebey, Susan; Angione, John] Calif State Univ Los Angeles, Dept Phys & Astron, Los Angeles, CA 90032 USA. [Rebull, Luisa M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Liu, WM (reprint author), WIYN Observ, 950 North Cherry Ave, Tucson, AZ 85719 USA. EM wliu@ipac.caltech.edu OI Rebull, Luisa/0000-0001-6381-515X FU National Aeronautics and Space Administration; National Science Foundation; WISE; WISE Science Data Center FX This publication makes use of data products from the Widefield Infrared Survey Explorer, a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. W.M.L. acknowledges support from WISE and the WISE Science Data Center. This research made use of the SIMBAD database. NR 28 TC 1 Z9 1 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 JUN PY 2014 VL 147 IS 6 AR 133 DI 10.1088/0004-6256/147/6/133 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6TC UT WOS:000336262600009 ER PT J AU Andrews, SM Chandler, CJ Isella, A Birnstiel, T Rosenfeld, KA Wilner, DJ Perez, LM Ricci, L Carpenter, JM Calvet, N Corder, SA Deller, AT Dullemond, CP Greaves, JS Harris, RJ Henning, T Kwon, W Lazio, J Linz, H Mundy, LG Sargent, AI Storm, S Testi, L AF Andrews, Sean M. Chandler, Claire J. Isella, Andrea Birnstiel, T. Rosenfeld, K. A. Wilner, D. J. Perez, L. M. Ricci, L. Carpenter, J. M. Calvet, N. Corder, S. A. Deller, A. T. Dullemond, C. P. Greaves, J. S. Harris, R. J. Henning, Th. Kwon, W. Lazio, J. Linz, H. Mundy, L. G. Sargent, A. I. Storm, S. Testi, L. TI RESOLVED MULTIFREQUENCY RADIO OBSERVATIONS OF GG Tau SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; protoplanetary disks; radio continuum: planetary systems; stars: individual (GG Tau) ID PROTOPLANETARY ACCRETION DISKS; YOUNG STELLAR OBJECTS; STAR-FORMING REGION; DUST GRAIN-SIZE; CIRCUMSTELLAR DISKS; CIRCUMBINARY DISK; TRANSITION DISK; TEMPERATURE-GRADIENT; MILLIMETER EMISSION; OPTICAL-CONSTANTS AB We present subarcsecond resolution observations of continuum emission associated with the GG Tau quadruple star system at wavelengths of 1.3, 2.8, 7.3, and 50 mm. These data confirm that the GG Tau A binary is encircled by a circumbinary ring at a radius of 235 AU with a FWHM width of similar to 60 AU. We find no clear evidence for a radial gradient in the spectral shape of the ring, suggesting that the particle size distribution is spatially homogeneous on angular scales greater than or similar to 0 ''.1. A central point source, likely associated with the primary component (GG Tau Aa), exhibits a composite spectrum from dust and free-free emission. Faint emission at 7.3 mm is observed toward the low-mass star GG Tau Ba, although its origin remains uncertain. Using these measurements of the resolved, multifrequency emission structure of the GG Tau A system, models of the far-infrared to radio spectrum are developed to place constraints on the grain size distribution and dust mass in the circumbinary ring. The non-negligible curvature present in the ring spectrum implies a maximum particle size of 1-10 mm, although we are unable to place strong constraints on the distribution shape. The corresponding dust mass is 30-300 M-circle plus, at a temperature of 20-30 K. We discuss how this significant concentration of relatively large particles in a narrow ring at a large radius might be produced in a local region of higher gas pressures (i.e., a particle "trap") located near the inner edge of the circumbinary disk. C1 [Andrews, Sean M.; Birnstiel, T.; Rosenfeld, K. A.; Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chandler, Claire J.; Perez, L. M.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Isella, Andrea; Ricci, L.; Carpenter, J. M.; Sargent, A. I.] CALTECH, Pasadena, CA 91125 USA. [Calvet, N.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Corder, S. A.] Joint ALMA Observ, Santiago, Chile. [Deller, A. T.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Dullemond, C. P.] Heidelberg Univ, Ctr Astron, Heidelberg, Germany. [Greaves, J. S.] Univ St Andrews, St Andrews KY16 9SS, Fife, Scotland. [Harris, R. J.] Univ Illinois, Dept Astronony, Urbana, IL 61810 USA. [Henning, Th.; Linz, H.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kwon, W.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Lazio, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA. [Mundy, L. G.; Storm, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Testi, L.] European So Observ, Garching, Germany. [Testi, L.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. RP Andrews, SM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sandrews@cfa.harvard.edu OI Dullemond, Cornelis/0000-0002-7078-5910; Deller, Adam/0000-0001-9434-3837 FU NASA [NNX12AJ04G]; NSF [AST-1109334]; National Science Foundation; CARMA partner universities FX We thank Mark Reid for valuable discussions about data modeling and an anonymous referee for helpful suggestions. S.M.A. and T.B. acknowledge support from NASA Origins of Solar Systems grant NNX12AJ04G. A.I., L.M.P., and J.M.C. acknowledge support from NSF award AST-1109334. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. The VLA is run by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 97 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 JUN 1 PY 2014 VL 787 IS 2 AR 148 DI 10.1088/0004-637X/787/2/148 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700053 ER PT J AU Cannon, BE Smith, CW Isenberg, PA Vasquez, BJ Joyce, CJ Murphy, N Nuno, RG AF Cannon, Bradford E. Smith, Charles W. Isenberg, Philip A. Vasquez, Bernard J. Joyce, Colin J. Murphy, Neil Nuno, Raquel G. TI ULYSSES OBSERVATIONS OF MAGNETIC WAVES DUE TO NEWBORN INTERSTELLAR PICKUP IONS. II. APPLICATION OF TURBULENCE CONCEPTS TO LIMITING WAVE ENERGY AND OBSERVABILITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE instabilities; magnetic fields; solar wind; Sun: heliosphere; turbulence; waves ID ROTATING RAREFACTION REGIONS; DISTANT SOLAR-WIND; MHD TURBULENCE; OUTER HELIOSPHERE; DISSIPATION RANGE; BOW SHOCK; 1 AU; FIELD; EXCITATION; PROTONS AB The low-frequency magnetic waves that arise from the isotropization of newborn interstellar pickup ions (PUIs) are reasonably well described by linear and quasi-linear kinetic theory in so far as those theories predict the wave frequency and polarization in the spacecraft frame. Those theories fail to describe the scarce observability of the waves. Quasilinear theory predicts that the wave power should accumulate over long periods of time as the relatively weak kinetic instability slowly adds power to the observed spectrum. At the same time it has been argued that the same wave energy must serve as a secondary source of thermal ion heating in the outer heliosphere once the initial turbulence is depleted. To the extent that turbulent transport of the wave energy acts against the spectrally confined accumulation of wave energy, turbulence should be a limiting factor in observability. We argue that turbulence does limit the observability of the waves and we use turbulence theory to predict the observed wave energy. We compare this prediction against a database of 502 wave observations attributed to newborn interstellar PUIs observed by the Ulysses spacecraft. C1 [Cannon, Bradford E.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Smith, Charles W.; Isenberg, Philip A.; Vasquez, Bernard J.; Joyce, Colin J.] Univ New Hampshire, Inst Study Earth Oceans & Space, Dept Phys, Durham, NH 03824 USA. [Smith, Charles W.; Isenberg, Philip A.; Vasquez, Bernard J.; Joyce, Colin J.] Univ New Hampshire, Inst Study Earth Oceans & Space, Ctr Space Sci, Durham, NH 03824 USA. [Murphy, Neil] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nuno, Raquel G.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. RP Cannon, BE (reprint author), Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. EM bc13h@my.fsu.edu; Charles.Smith@unh.edu; Phil.Isenberg@unh.edu; Bernie.Vasquez@unh.edu; cjl46@wildcats.unh.edu; Neil.Murphy@jpl.nasa.gov; raquel.nuno@asu.edu FU NASA Guest Investigator grant [NNX07AH75G]; NSF grant [ATM0635863]; Caltech subcontract [44A1085631]; NASA [NNX13AF97G, NNX11AJ37G]; NSF [AGS0962506]; NASA Space Grant program FX This work was supported in part by NASA Guest Investigator grant NNX07AH75G and NSF grant ATM0635863. C.W.S. is supported by Caltech subcontract 44A1085631 to theUniversity of New Hampshire in support of the ACE/MAG instrument. Part of the ACE mandate is to better understand the role of pickup ions in the heliosphere. Portions of this research were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. P.A.I. and B. J.V. are supported by NASA grants NNX13AF97G and NNX11AJ37G as well as NSF grant AGS0962506. B.E.C. was an undergraduate physics major working within the Space Science Center at the time this work was performed and worked as an undergraduate intern at JPL during the summer of 2012, supported by the NASA Space Grant program. C.J.J. is a graduate student in the Physics program at UNH who earlier initiated this line of investigation. NR 66 TC 7 Z9 7 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 JUN 1 PY 2014 VL 787 IS 2 AR 133 DI 10.1088/0004-637X/787/2/133 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700038 ER PT J AU Casagrande, L Aguirre, VS Stello, D Huber, D Serenelli, AM Cassisi, S Dotter, A Milone, AP Hodgkin, S Marino, AF Lund, MN Pietrinferni, A Asplund, M Feltzing, S Flynn, C Grundahl, F Nissen, PE Schonrich, R Schlesinger, KJ Wang, W AF Casagrande, L. Aguirre, V. Silva Stello, D. Huber, D. Serenelli, A. M. Cassisi, S. Dotter, A. Milone, A. P. Hodgkin, S. Marino, A. F. Lund, M. N. Pietrinferni, A. Asplund, M. Feltzing, S. Flynn, C. Grundahl, F. Nissen, P. E. Schoenrich, R. Schlesinger, K. J. Wang, W. TI STROMGREN SURVEY FOR ASTEROSEISMOLOGY AND GALACTIC ARCHAEOLOGY: LET THE SAGA BEGIN SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: stellar content; stars: abundances; stars: distances; stars: fundamental parameters; stars: oscillations; surveys; techniques: photometric ID RED-GIANT STARS; SOLAR-LIKE OSCILLATIONS; MAIN-SEQUENCE STARS; CLUSTER NGC 6819; WIYN OPEN CLUSTER; EFFECTIVE TEMPERATURE SCALE; HEAVY-ELEMENT DISPERSION; GENEVA-COPENHAGEN SURVEY; KEPLER INPUT CATALOG; UVBY-BETA PHOTOMETRY AB Asteroseismology has the capability of precisely determining stellar properties that would otherwise be inaccessible, such as radii, masses, and thus ages of stars. When coupling this information with classical determinations of stellar parameters, such as metallicities, effective temperatures, and angular diameters, powerful new diagnostics for Galactic studies can be obtained. The ongoing Stromgren survey for Asteroseismology and Galactic Archaeology has the goal of transforming the Kepler field into a new benchmark for Galactic studies, similar to the solar neighborhood. Here we present the first results from a stripe centered at a Galactic longitude of 74 degrees and covering latitude from about 8 degrees to 20 degrees, which includes almost 1000 K giants with seismic information and the benchmark open cluster NGC 6819. We describe the coupling of classical and seismic parameters, the accuracy as well as the caveats of the derived effective temperatures, metallicities, distances, surface gravities, masses, and radii. Confidence in the achieved precision is corroborated by the detection of the first and secondary clumps in a population of field stars with a ratio of 2 to 1 and by the negligible scatter in the seismic distances among NGC 6819 member stars. An assessment of the reliability of stellar parameters in the Kepler Input Catalog is also performed, and the impact of our results for population studies in the Milky Way is discussed, along with the importance of an all-sky Stromgren survey. C1 [Casagrande, L.; Dotter, A.; Milone, A. P.; Marino, A. F.; Asplund, M.; Schlesinger, K. J.] Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Aguirre, V. Silva; Lund, M. N.; Grundahl, F.; Nissen, P. E.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Stello, D.] Univ Sydney, Sydney Inst Astron SIfA, Sch Phys, Sydney, NSW 2006, Australia. [Huber, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huber, D.] SETI Inst, Mountain View, CA 94043 USA. [Serenelli, A. M.] Inst Space Sci IEEC CSIC, Fac Ciencies, E-08193 Barcelona, Spain. [Cassisi, S.; Pietrinferni, A.] INAF Osservatorio Astronomico Collurania, I-64100 Teramo, Italy. [Hodgkin, S.] Inst Astron, Cambridge CB3 0HA, England. [Feltzing, S.] Lund Observ, Dept Astron & Theoret Phys, Lund, Sweden. [Flynn, C.] Swinburne Univ Technol, Ctr Astrophys & Supercomputing, Hawthorn, Vic 3122, Australia. [Schoenrich, R.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Schoenrich, R.] Univ Oxford, Rudolf Peierls Ctr Theoret Phys, Oxford OX1 3NP, England. [Wang, W.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. RP Casagrande, L (reprint author), Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. EM luca.casagrande@anu.edu.au OI Pietrinferni, Adriano/0000-0003-3795-9031; Cassisi, Santi/0000-0001-5870-3735; Serenelli, Aldo/0000-0001-6359-2769; Lund, Mikkel Norup/0000-0001-9214-5642 FU National Aeronautics and Space Administration; National Science Foundation; Stellar Astrophysics Centre; Danish National Research Foundation [DNRF106]; ASTERISK project (ASTERoseismic Investigations); SONG; Kepler - European Research Council [267864]; NASA; MICINN grant [AYA2011-24704]; Australian Research Council Laureate Fellowship [FL110100012] FX We thank the referee for a prompt and constructive report. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This paper makes use of data from the AAVSO Photometric All Sky Survey, whose funding has been provided by the Robert Martin Ayers Sciences Fund. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (grant agreement No. DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler), funded by the European Research Council (grant agreement No. 267864). D.H. is supported by an appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. A.M.S. is partially supported by MICINN grant AYA2011-24704. This work has been supported by an Australian Research Council Laureate Fellowship to M.A. (grant FL110100012). NR 159 TC 38 Z9 38 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 JUN 1 PY 2014 VL 787 IS 2 AR 110 DI 10.1088/0004-637X/787/2/110 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700015 ER PT J AU Cohen, MH Meier, DL Arshakian, TG Homan, DC Hovatta, T Kovalev, YY Lister, ML Pushkarev, AB Richards, JL Savolainen, T AF Cohen, M. H. Meier, D. L. Arshakian, T. G. Homan, D. C. Hovatta, T. Kovalev, Y. Y. Lister, M. L. Pushkarev, A. B. Richards, J. L. Savolainen, T. TI STUDIES OF THE JET IN BL LACERTAE. I. RECOLLIMATION SHOCK AND MOVING EMISSION FEATURES SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: individual (BL Lacertae); galaxies: active; galaxies: jets; magnetohydrodynamics (MHD); waves ID ACTIVE GALACTIC NUCLEI; HELICAL MAGNETIC-FIELD; LINKING ACCRETION FLOW; COMPACT RADIO-SOURCES; BASE-LINE ARRAY; BLACK-HOLE MASS; RELATIVISTIC JETS; NUMERICAL SIMULATIONS; FARADAY-ROTATION; SCALE JET AB Parsec-scale VLBA images of BL Lac at 15 GHz show that the jet contains a permanent quasi-stationary emission feature 0.26 mas (0.34 pc projected) from the core, along with numerous moving features. In projection, the tracks of the moving features cluster around an axis at a position angle of -166.degrees 6 that connects the core with the standing feature. The moving features appear to emanate from the standing feature in a manner strikingly similar to the results of numerical two-dimensional relativistic magneto-hydrodynamic(RMHD) simulations in which moving shocks are generated at a recollimation shock (RCS). Because of this, and the close analogy to the jet feature HST-1 in M87, we identify the standing feature in BL Lac as an RCS. We assume that the magnetic field dominates the dynamics in the jet, and that the field is predominantly toroidal. From this we suggest that the moving features are compressions established by slow and fast mode magneto- acoustic MHD waves. We illustrate the situation with a simple model in which the slowest moving feature is a slow-mode wave, and the fastest feature is a fast-mode wave. In the model, the beam has Lorentz factor Gamma(gal)(beam) approximate to 3.5 in the frame of the host galaxy and the fast mode wave has Lorentz factor Gamma(beam)(Fwave) approximate to 1.6 in the frame of the beam. This gives a maximum apparent speed for the moving features, beta(app) = v(app)/c = 10. In this model the Lorentz factor of the pattern in the galaxy frame is approximately three times larger than that of the beam itself. C1 [Cohen, M. H.; Hovatta, T.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Meier, D. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Arshakian, T. G.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Arshakian, T. G.] Byurakan Astrophys Observ, Byurakan 378433, Armenia. [Arshakian, T. G.] Isaac Newton Inst Chile, Armenian Branch, Santiago, Chile. [Homan, D. C.] Denison Univ, Dept Phys, Granville, OH 43023 USA. [Hovatta, T.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Kovalev, Y. Y.] Ctr Astro Space, Lebedev Phys Inst, Moscow 117997, Russia. [Kovalev, Y. Y.; Pushkarev, A. B.; Savolainen, T.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Lister, M. L.; Richards, J. L.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA. [Pushkarev, A. B.] Pulkovo Observ, St Petersburg 196140, Russia. [Pushkarev, A. B.] Crimean Astrophys Observ, UA-98409 Nauchnyi, Crimea, Ukraine. RP Cohen, MH (reprint author), CALTECH, Dept Astron, Pasadena, CA 91125 USA. EM mhc@astro.caltech.edu RI Kovalev, Yuri/J-5671-2013; Pushkarev, Alexander/M-9997-2015; OI Kovalev, Yuri/0000-0001-9303-3263; Savolainen, Tuomas/0000-0001-6214-1085 FU Jenny and Antti Wihuri foundation; Academy of Finland [267324]; Russian Foundation for Basic Research [13-02-12103]; Research Program OFN-17 of the Division of Physics; Russian Academy of Sciences; Dynasty Foundation; "Non-stationary processes in the Universe" Program of the Presidium of the Russian Academy of Sciences; DFG [Os 177/2-1]; MOJAVE program under NASA-Fermi grant [11-Fermi11-0019] FX We thank the anonymous referee whose comments substantially improved the paper. We are grateful to Ken Kellermann and the rest of the MOJAVE team for their comments and for their years of work in producing the data base that makes this work possible. T.H. was supported in part by a grant from the Jenny and Antti Wihuri foundation and by the Academy of Finland project number 267324. Y.Y.K. is partly supported by the Russian Foundation for Basic Research (project 13-02-12103), Research Program OFN-17 of the Division of Physics, Russian Academy of Sciences, and the Dynasty Foundation. A.B.P. was supported by the "Non-stationary processes in the Universe" Program of the Presidium of the Russian Academy of Sciences. T.G.A. acknowledges support by DFG project number Os 177/2-1. The VLBA is a facility of the National Radio Astronomy Observatory, a facility of the National Science Foundation that is operated under cooperative agreement with Associated Universities, Inc. The MOJAVE program is supported under NASA-Fermi grant 11-Fermi11-0019. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of NASA's Astrophysics Data System. NR 67 TC 17 Z9 17 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 JUN 1 PY 2014 VL 787 IS 2 AR 151 DI 10.1088/0004-637X/787/2/151 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700056 ER PT J AU Crockett, NR Bergin, EA Neill, JL Favre, C Schilke, P Lis, DC Bell, TA Blake, G Cernicharo, J Emprechtinger, M Esplugues, GB Gupta, H Kleshcheva, M Lord, S Marcelino, N McGuire, BA Pearson, J Phillips, TG Plume, R van der Tak, F Tercero, B Yu, SS AF Crockett, Nathan R. Bergin, Edwin A. Neill, Justin L. Favre, Cecile Schilke, Peter Lis, Dariusz C. Bell, Tom A. Blake, Geoffrey Cernicharo, Jose Emprechtinger, Martin Esplugues, Gisela B. Gupta, Harshal Kleshcheva, Maria Lord, Steven Marcelino, Nuria McGuire, Brett A. Pearson, John Phillips, Thomas G. Plume, Rene van der Tak, Floris Tercero, Belen Yu, Shanshan TI HERSCHEL OBSERVATIONS OF EXTRAORDINARY SOURCES: ANALYSIS OF THE HIFI 1.2 THz WIDE SPECTRAL SURVEY TOWARD ORION KL. I. METHODS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: abundances; ISM: individual objects (Orion KL); ISM: molecules ID MOLECULAR LINE SURVEY; KLEINMANN-LOW NEBULA; STAR-FORMING REGION; LIMITED MILLIMETER SURVEY; RADIO-SOURCE-I; SUBMILLIMETER ARRAY; SOURCES HEXOS; APERTURE SYNTHESIS; HOT CORE; INTERSTELLAR-MOLECULES AB We present a comprehensive analysis of a broadband spectral line survey of the Orion Kleinmann-Low nebula (Orion KL), one of the most chemically rich regions in the Galaxy, using the HIFI instrument on board the Herschel Space Observatory. This survey spans a frequency range from 480 to 1907 GHz at a resolution of 1.1 MHz. These observations thus encompass the largest spectral coverage ever obtained toward this high-mass star-forming region in the submillimeter with high spectral resolution and include frequencies > 1 THz, where the Earth's atmosphere prevents observations from the ground. In all, we detect emission from 39 molecules (79 isotopologues). Combining this data set with ground-based millimeter spectroscopy obtained with the IRAM 30 m telescope, we model the molecular emission from the millimeter to the far-IR using the XCLASS program, which assumes local thermodynamic equilibrium (LTE). Several molecules are also modeled with the MADEX non-LTE code. Because of the wide frequency coverage, our models are constrained by transitions over an unprecedented range in excitation energy. A reduced chi(2) analysis indicates that models for most species reproduce the observed emission well. In particular, most complex organics are well fit by LTE implying gas densities are high (> 10(6) cm(-3)) and excitation temperatures and column densities are well constrained. Molecular abundances are computed using H-2 column densities also derived from the HIFI survey. The distribution of rotation temperatures, T-rot, for molecules detected toward the hot core is significantly wider than the compact ridge, plateau, and extended ridge T-rot distributions, indicating the hot core has the most complex thermal structure. C1 [Crockett, Nathan R.; Bergin, Edwin A.; Neill, Justin L.; Favre, Cecile] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Schilke, Peter] Univ Cologne, Inst Phys, D-50937 Cologne, Germany. [Crockett, Nathan R.; Emprechtinger, Martin; Phillips, Thomas G.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Bell, Tom A.; Cernicharo, Jose; Esplugues, Gisela B.; Tercero, Belen] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, E-28850 Madrid, Spain. [Blake, Geoffrey; Kleshcheva, Maria] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Blake, Geoffrey; McGuire, Brett A.] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. [Gupta, Harshal; Pearson, John; Yu, Shanshan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lord, Steven] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Marcelino, Nuria] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Plume, Rene] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N IN4, Canada. [van der Tak, Floris] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [van der Tak, Floris] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. RP Crockett, NR (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. RI Yu, Shanshan/D-8733-2016 FU NASA FX We thank the anonymous referee for giving comments that greatly improved the paper. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada, and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France, and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA); Sweden: Chalmers University of Technology-MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University-Stockholm Observatory; Switzerland: ETH Zurich, FHNW; and USA: Caltech, JPL, NHSC. 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. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 116 TC 30 Z9 30 U1 1 U2 11 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 JUN 1 PY 2014 VL 787 IS 2 AR 112 DI 10.1088/0004-637X/787/2/112 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700017 ER PT J AU Huppenkothen, D D'Angelo, C Watts, AL Heil, L van der Klis, M van der Horst, AJ Kouveliotou, C Baring, MG Gogus, E Granot, J Kaneko, Y Lin, L von Kienlin, A Younes, G AF Huppenkothen D'Angelo, C. Watts, A. L. Heil, L. van der Klis, M. van der Horst, A. J. Kouveliotou, C. Baring, M. G. Gogus, E. Granot, J. Kaneko, Y. Lin, L. von Kienlin, A. Younes, G. TI QUASI-PERIODIC OSCILLATIONS IN SHORT RECURRING BURSTS OF THE SOFT GAMMA REPEATER J1550-5418 SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; methods: statistical; pulsars: individual (SGR J1550-5418); stars: magnetic field; stars: neutron; X-rays: bursts ID MAGNETIZED NEUTRON-STARS; PULSAR 1E 1547.0-5408; X-RAY OSCILLATIONS; SGR 1806-20; GIANT-FLARE; MAGNETOELASTIC OSCILLATIONS; STATISTICAL PROPERTIES; RADIATIVE MECHANISM; 2004 HYPERFLARE; CRUST AB The discovery of quasi-periodic oscillations (QPOs) in magnetar giant flares has opened up prospects for neutron star asteroseismology. The scarcity of giant flares makes a search for QPOs in the shorter, far more numerous bursts from soft gamma repeaters (SGRs) desirable. In Huppenkothen et al., we developed a Bayesian method for searching for QPOs in short magnetar bursts, taking into account the effects of the complicated burst structure, and have shown its feasibility on a small sample of bursts. Here we apply the same method to a much larger sample from a burst storm of 286 bursts from SGR J1550-5418. We report a candidate signal at 260 Hz in a search of the individual bursts, which is fairly broad. We also find two QPOs at similar to 93 Hz, and one at 127 Hz, when averaging periodograms from a number of bursts in individual triggers, at frequencies close to QPOs previously observed in magnetar giant flares. Finally, for the first time, we explore the overall burst variability in the sample and report a weak anti-correlation between the power-law index of the broadband model characterizing aperiodic burst variability and the burst duration: shorter bursts have steeper power-law indices than longer bursts. This indicates that longer bursts vary over a broader range of timescales and are not simply longer versions of the short bursts. C1 [Huppenkothen; D'Angelo, C.; Watts, A. L.; Heil, L.; van der Klis, M.; van der Horst, A. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Kouveliotou, C.] NASA, Marshall Space Flight Ctr, Astrophys Off, Huntsville, AL 35812 USA. [Kouveliotou, C.; Younes, G.] NSSTC, Huntsville, AL 35805 USA. [Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. [Gogus, E.] Sabanci Univ, TR-34956 Istanbul, Turkey. [Granot, J.] Open Univ Israel, Dept Nat Sci, IL-43537 Raanana, Israel. [Lin, L.] APC, Francois Arago Ctr, F-75205 Paris, France. [von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Younes, G.] Univ Space Res Assoc, Huntsville, AL 35806 USA. RP Huppenkothen, D (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Postbus 94249, NL-1090 GE Amsterdam, Netherlands. EM D.Huppenkothen@uva.nl FU Netherlands Organization for Scientific Research (NWO) Vidi Fellowship; NASA [NNH07ZDA001-GLAST]; European Research Council [247295] FX The authors thank Phil Uttley and Yuri Levin for useful discussions and the referee for helpful suggestions. D.H., C.D., and A.L.W. acknowledge support from a Netherlands Organization for Scientific Research (NWO) Vidi Fellowship (PI: A. Watts). C.K. was partially supported by NASA grant NNH07ZDA001-GLAST. This publication is part of the GBM/Magnetar Key Project (NASA grant NNH07ZDA001-GLAST; PI: C. Kouveliotou). A.J.v.d.H. acknowledges support from the European Research Council via Advanced Investigator Grant No. 247295 (PI: R.A.M.J. Wijers). NR 67 TC 17 Z9 17 U1 3 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2014 VL 787 IS 2 AR 128 DI 10.1088/0004-637X/787/2/128 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700033 ER PT J AU Ko, YK Muglach, K Wang, YM Young, PR Lepri, ST AF Ko, Yuan-Kuen Muglach, Karin Wang, Yi-Ming Young, Peter R. Lepri, Susan T. TI TEMPORAL EVOLUTION OF SOLAR WIND ION COMPOSITION AND THEIR SOURCE CORONAL HOLES DURING THE DECLINING PHASE OF CYCLE 23. I. LOW- LATITUDE EXTENSION OF POLAR CORONAL HOLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar wind; Sun: corona; Sun: magnetic fields ID HELIOSPHERIC MAGNETIC-FIELDS; ACTIVE-REGION OUTFLOWS; MASS EJECTIONS; CHARGE STATES; ELECTRON-TEMPERATURE; PARTICLE EVENTS; ATOMIC DATABASE; IN-SITU; 1 AU; INTERPLANETARY AB We analyzed 27 solar wind (SW) intervals during the declining phase of cycle 23, whose source coronal holes (CHs) can be unambiguously identified and are associated with one of the polar CHs. We found that the SW ions have a temporal trend of decreasing ionization state, and such a trend is different between the slow and fast SW. The photospheric magnetic field, both inside and at the outside boundary of the CH, also exhibits a trend of decrease with time. However, EUV line emissions from different layers of the atmosphere exhibit different temporal trends. The coronal emission inside the CH generally increases toward the CH boundary as the underlying field increases in strength and becomes less unipolar. In contrast, this relationship is not seen in the coronal emission averaged over the entire CH. For C and O SW ions that freeze-in at lower altitude, stronger correlation between their ionization states and field strength (both signed and unsigned) appears in the slow SW, while for Fe ions that freeze-in at higher altitude, stronger correlation appears in the fast SW. Such correlations are seen both inside the CH and at its boundary region. On the other hand, the coronal electron temperature correlates well with the SW ion composition only in the boundary region. Our analyses, although not able to determine the likely footpoint locations of the SW of different speeds, raise many outstanding questions for how the SW is heated and accelerated in response to the long-term evolution of the solar magnetic field. C1 [Ko, Yuan-Kuen; Wang, Yi-Ming] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Muglach, Karin] Artep Inc, Ellicott City, MD 21042 USA. [Muglach, Karin] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Young, Peter R.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Lepri, Susan T.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP Ko, YK (reprint author), Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. EM yuan-kuen.ko@nrl.navy.mil RI Lepri, Susan/I-8611-2012; OI Young, Peter/0000-0001-9034-2925 FU National Science Foundation; NASA [HGI NNH10AN82I] FX We thank the ACE SWICS, SWEPAM, and MAG instrument teams and the ACE Science Center for providing the ACE data. We would like to thank J. Laming and M. Popecki for helpful discussions and the anonymous referee for helpful comments. SOHO is a project of international cooperation between ESA and NASA. The He I image is courtesy of the Mauna Loa Solar Observatory, operated by the High Altitude Observatory, as part of the National Center for Atmospheric Research (NCAR). NCAR is supported by the National Science Foundation. CHIANTI is a collaborative project involving researchers at NRL (USA), RAL (UK), and the Universities of Cambridge (UK), George Mason (USA), and Florence (Italy). The CDS synoptic maps were initially processed by Steven Chapman of University of Central Lancashire, UK. This work was supported by NASA grant HGI NNH10AN82I. NR 73 TC 10 Z9 10 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2014 VL 787 IS 2 AR 121 DI 10.1088/0004-637X/787/2/121 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700026 ER PT J AU Masson, S McCauley, P Golub, L Reeves, KK DeLuca, EE AF Masson, Sophie McCauley, Patrick Golub, Leon Reeves, Katharine K. DeLuca, Edward E. TI DYNAMICS OF THE TRANSITION CORONA SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: magnetic fields; Sun: UV radiation ID 3-DIMENSIONAL MAGNETIC RECONNECTION; QUASI-SEPARATRIX LAYERS; X-RAY; ACTIVE-REGION; SOLAR CORONA; NULL-POINT; FLARE EMISSIONS; MODEL; TOPOLOGY; FIELD AB Magnetic reconnection between the open and closed magnetic fields in the corona is believed to play a crucial role in the corona/heliosphere coupling. At large scale, the exchange of open/closed connectivity is expected to occur in pseudo-streamer (PS) structures. However, there is neither clear observational evidence of how such coupling occurs in PSs, nor evidence for how the magnetic reconnection evolves. Using a newly developed technique, we enhance the off-limb magnetic fine structures observed with the Atmospheric Imaging Assembly and identify a PS-like feature located close to the northern coronal hole. We first identify that the magnetic topology associated with the observation is a PS, null-point (NP) related topology bounded by the open field. By comparing the magnetic field configuration with the EUV emission regions, we determined that most of the magnetic flux associated with plasma emission are small loops below the PS basic NP and open field bounding the PS topology. In order to interpret the evolution of the PS, we referred to a three-dimensional MHD interchange reconnection modeling the exchange of connectivity between small closed loops and the open field. The observed PS fine structures follow the dynamics of the magnetic field before and after reconnecting at the NP obtained by the interchange model. Moreover, the pattern of the EUV plasma emission is the same as the shape of the expected plasma emission location derived from the simulation. These morphological and dynamical similarities between the PS observations and the results from the simulation strongly suggest that the evolution of the PS, and in particular the opening/closing of the field, occurs via interchange/slipping reconnection at the basic NP of the PS. Besides identifying the mechanism at work in the large-scale coupling between the open and closed fields, our results highlight that interchange reconnection in PSs is a gradual physical process that differs from the impulsive reconnection of the solar-jet model. C1 [Masson, Sophie] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA. [Masson, Sophie] Catholic Univ Amer, Washington, DC 20064 USA. [McCauley, Patrick; Golub, Leon; Reeves, Katharine K.; DeLuca, Edward E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Masson, S (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM sophie.masson@nasa.gov RI Reeves, Katharine/P-9163-2014; McCauley, Patrick/P-7747-2015; DeLuca, Edward/L-7534-2013 OI Reeves, Katharine/0000-0002-6903-6832; Golub, Leon/0000-0001-9638-3082; McCauley, Patrick/0000-0002-1450-7350; DeLuca, Edward/0000-0001-7416-2895 FU Lockheed-Martin [SP02H1701R]; NASA TRT Program; NASA SRT Program; NASA Postdoctoral Program FX The authors thank the referees for the pertinent comments that helped to improve the manuscript, as well as J. Klimchuck and G. Aulanier for helpful discussions. This work partially supported under contract SP02H1701R from Lockheed-Martin to SAO. The work of Sophie Masson was supported by the NASA TR&T and SR&T Programs. S.M. gratefully acknowledges support from the NASA Postdoctoral Program, administrated by Oak Ridge Associated University through a contract with NASA, during her stay at NASA Goddard Space Flight Center. NR 51 TC 8 Z9 8 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 JUN 1 PY 2014 VL 787 IS 2 AR 145 DI 10.1088/0004-637X/787/2/145 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700050 ER PT J AU Mostl, C Amla, K Hall, JR Liewer, PC De Jong, EM Colaninno, RC Veronig, AM Rollett, T Temmer, M Peinhart, V Davies, JA Lugaz, N Liu, YD Farrugia, CJ Luhmann, JG Vrsnak, B Harrison, RA Galvin, AB AF Moestl, C. Amla, K. Hall, J. R. Liewer, P. C. De Jong, E. M. Colaninno, R. C. Veronig, A. M. Rollett, T. Temmer, M. Peinhart, V. Davies, J. A. Lugaz, N. Liu, Y. D. Farrugia, C. J. Luhmann, J. G. Vrsnak, B. Harrison, R. A. Galvin, A. B. TI CONNECTING SPEEDS, DIRECTIONS AND ARRIVAL TIMES OF 22 CORONAL MASS EJECTIONS FROM THE SUN TO 1 AU SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar; terrestrial relations; Sun: coronal mass ejections (CMEs); Sun: heliosphere ID IN-SITU OBSERVATIONS; CME-CME INTERACTION; SOLAR-WIND; INNER HELIOSPHERE; MAGNETIC CLOUDS; WHITE-LIGHT; STEREO OBSERVATIONS; KINEMATICS; SPACECRAFT; EARTH AB Forecasting the in situ properties of coronal mass ejections (CMEs) from remote images is expected to strongly enhance predictions of space weather and is of general interest for studying the interaction of CMEs with planetary environments. We study the feasibility of using a single heliospheric imager (HI) instrument, imaging the solar wind density from the Sun to 1 AU, for connecting remote images to in situ observations of CMEs. We compare the predictions of speed and arrival time for 22 CMEs (in 2008-2012) to the corresponding interplanetary coronal mass ejection (ICME) parameters at in situ observatories (STEREO PLASTIC/IMPACT, Wind SWE/MFI). The list consists of front-and backsided, slow and fast CMEs (up to 2700 km s(-1)). We track the CMEs to 34.9 +/- 7.1 deg elongation from the Sun with J maps constructed using the SATPLOT tool, resulting in prediction lead times of - 26.4 +/- 15.3 hr. The geometrical models we use assume different CME front shapes (fixed-Phi, harmonic mean, self-similar expansion) and constant CME speed and direction. We find no significant superiority in the predictive capability of any of the three methods. The absolute difference between predicted and observed ICME arrival times is 8.1 +/- 6.3 hr (rms value of 10.9 hr). Speeds are consistent to within 284 +/- 288 km s(-1) . Empirical corrections to the predictions enhance their performance for the arrival times to 6.1 +/- 5.0 hr (rms value of 7.9 hr), and for the speeds to 53 +/- 50 km s(-1). These results are important for Solar Orbiter and a space weather mission positioned away from the Sun-Earth line. C1 [Moestl, C.; Veronig, A. M.; Rollett, T.; Temmer, M.; Peinhart, V.] Graz Univ, Inst Phys, Kanzelhohe Observ IGAM, A-8010 Graz, Austria. [Moestl, C.; Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Moestl, C.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. [Amla, K.; Hall, J. R.; Liewer, P. C.; De Jong, E. M.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Colaninno, R. C.] Naval Res Lab, Div Space Sci, Washington, DC USA. [Davies, J. A.; Harrison, R. A.] RAL Space, Didcot, Oxon, England. [Lugaz, N.; Farrugia, C. J.; Galvin, A. B.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Lugaz, N.; Farrugia, C. J.; Galvin, A. B.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Liu, Y. D.] Chinese Acad Sci, Natl Space Sci Ctr, State Key Lab Space Weather, Beijing, Peoples R China. [Vrsnak, B.] Univ Zagreb, Fac Geodesy, Hvar Observ, HR-10000 Zagreb, Croatia. RP Mostl, C (reprint author), Graz Univ, Inst Phys, Kanzelhohe Observ IGAM, A-8010 Graz, Austria. EM christian.moestl@uni-graz.at RI Lugaz, Noe/C-1284-2008; Veronig, Astrid/B-8422-2009; OI Lugaz, Noe/0000-0002-1890-6156; Temmer, Manuela/0000-0003-4867-7558; Liu, Ying/0000-0002-3483-5909; Moestl, Christian/0000-0001-6868-4152; Amerstorfer, Tanja/0000-0001-9024-6706; Colaninno, Robin/0000-0002-3253-4205 FU Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme; Austrian Science Fund (FWF) [P26174-N27, V195-N16]; European Union [263252 [COMESEP], 284461 [eHEROES], 606692 [HELCATS]]; STEREO grant [NAS5-03131]; NASA [NNX13AP39G]; NASA STEREO grant; [AGS-1239704] FX This research was supported by a Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme. C. M. and T. R. thank the Austrian Science Fund (FWF): [P26174-N27]. M. T. was also supported by the Austrian Science Fund (FWF): V195-N16. The presented work has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreements No. 263252 [COMESEP], No. 284461 [eHEROES] and No. 606692 [HELCATS]. T. R. gratefully acknowledges the JungforscherInnenfonds of the Council of the University Graz. Work at the University of California, Berkeley, was supported from STEREO grant NAS5-03131. The work of K. A., J. R. H., P. C. L., and E. M. D. was conducted at the Jet Propulsion Laboratory, California Institute of Technology under a contract from NASA. N. L. was supported by AGS-1239704. It is also supported by NASA grant NNX13AP39G and NASA STEREO grant to U. N. H. We acknowledge the use of Wind data provided by the magnetometer and the solar wind experiment teams at NASA/GSFC, and we thank the center for geomagnetism in Kyoto for providing the Dst indices. We also thank the "International study of earth affecting transients" (ISEST) team lead by Jie Zhang. NR 85 TC 49 Z9 49 U1 1 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2014 VL 787 IS 2 AR 119 DI 10.1088/0004-637X/787/2/119 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700024 ER PT J AU Robinson, TD Ennico, K Meadows, VS Sparks, W Bussey, DJ Schwieterman, EW Breiner, J AF Robinson, Tyler D. Ennico, Kimberly Meadows, Victoria S. Sparks, William Bussey, D. Ben J. Schwieterman, Edward W. Breiner, Jonathan TI DETECTION OF OCEAN GLINT AND OZONE ABSORPTION USING LCROSS EARTH OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; Earth; Moon; planets and satellites: atmospheres; planets and satellites: terrestrial planets; radiative transfer ID EXTRASOLAR TERRESTRIAL PLANETS; PHOTOMETRIC VARIABILITY; VEGETATION SIGNATURE; THERMAL EMISSION; KEPLER-MISSION; CIRRUS CLOUDS; LIGHT CURVES; WIDE-FIELD; SPECTRA; EXOPLANETS AB The Lunar CRater Observation and Sensing Satellite (LCROSS) observed the distant Earth on three occasions in 2009. These data span a range of phase angles, including a rare crescent phase view. For each epoch, the satellite acquired near-infrared and mid-infrared full-disk images, and partial-disk spectra at 0.26-0.65 mu m (lambda/Delta lambda similar to 500) and 1.17-2.48 mu m (lambda/Delta lambda similar to 50). Spectra show strong absorption features due to water vapor and ozone, which is a biosignature gas. We perform a significant recalibration of the UV-visible spectra and provide the first comparison of high-resolution visible Earth spectra to the NASA Astrobiology Institute's Virtual Planetary Laboratory three-dimensional spectral Earth model. We find good agreement with the observations, reproducing the absolute brightness and dynamic range at all wavelengths for all observation epochs, thus validating the model to within the similar to 10% data calibration uncertainty. Data-model comparisons reveal a strong ocean glint signature in the crescent phase data set, which is well matched by our model predictions throughout the observed wavelength range. This provides the first observational test of a technique that could be used to determine exoplanet habitability from disk-integrated observations at visible and near-infrared wavelengths, where the glint signal is strongest. We examine the detection of the ozone 255 nm Hartley and 400-700 nm Chappuis bands. While the Hartley band is the strongest ozone feature in Earth's spectrum, false positives for its detection could exist. Finally, we discuss the implications of these findings for future exoplanet characterization missions. C1 [Robinson, Tyler D.; Ennico, Kimberly; Meadows, Victoria S.; Sparks, William; Bussey, D. Ben J.; Schwieterman, Edward W.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Robinson, Tyler D.; Meadows, Victoria S.; Sparks, William; Schwieterman, Edward W.] Univ Washington, NASA Astrobiol Inst, Virtual Planetary Lab, Seattle, WA 98195 USA. [Meadows, Victoria S.; Schwieterman, Edward W.; Breiner, Jonathan] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Sparks, William] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Bussey, D. Ben J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Robinson, TD (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA. EM tyler.d.robinson@nasa.gov RI Ennico, Kimberly/L-9606-2014; OI Robinson, Tyler/0000-0002-3196-414X; Schwieterman, Edward/0000-0002-2949-2163 FU National Aeronautics and Space Administration through the NASA Astrobiology Institute [NNH05ZDA001C]; NASA Lunar Science Institute (NLSI) [NNH08ZDA008C]; NASA Postdoctoral Program at the Ames Research Center; NASA [NAS5-26555] FX This work was performed as part of the NASA Astrobiology Institute's Virtual Planetary Laboratory, supported by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under solicitation No. NNH05ZDA001C. This research was also supported by the NASA Lunar Science Institute (NLSI) under solicitation No. NNH08ZDA008C, "Scientific and Exploration Potential of the Lunar Poles" (PI: B. Bussey). T.R. gratefully acknowledges support from an appointment to the NASA Postdoctoral Program at the Ames Research Center, administered by Oak Ridge Associated Universities. STScI is operated by the Association for Universities of Research in Astronomy, Inc., under NASA contract NAS5-26555. Some of the results in this paper have been derived using the HEALPix (Gorski et al. 2005) package. NR 72 TC 16 Z9 16 U1 3 U2 11 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 JUN 1 PY 2014 VL 787 IS 2 AR 171 DI 10.1088/0004-637X/787/2/171 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700076 ER PT J AU Stevenson, R Bauer, JM Kramer, EA Grav, T Mainzer, AK Masiero, JR AF Stevenson, R. Bauer, J. M. Kramer, E. A. Grav, T. Mainzer, A. K. Masiero, J. R. TI LINGERING GRAINS OF TRUTH AROUND COMET 17P/HOLMES SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets: general; comets: individual (17P/Holmes) ID 2007 OUTBURST; THERMAL-MODEL; SIZE DISTRIBUTION; HALE-BOPP; NUCLEUS; DUST; ALBEDO; PHOTOMETRY; ASTEROIDS; MOTION AB Comet 17P/Holmes underwent a massive outburst in 2007 October, brightening by a factor of almost a million in under 48 hr. We used infrared images taken by the Wide-Field Infrared Survey Explorer mission to characterize the comet as it appeared at a heliocentric distance of 5.1 AU almost 3 yr after the outburst. The comet appeared to be active with a coma and dust trail along the orbital plane. We constrained the diameter, albedo, and beaming parameter of the nucleus to 4.135 +/- 0.610 km, 0.03 +/- 0.01, and 1.03 +/- 0.21, respectively. The properties of the nucleus are consistent with those of other Jupiter family comets. The best-fit temperature of the coma was 134 +/- 11 K, slightly higher than the blackbody temperature at that heliocentric distance. Using Finson-Probstein modeling, we found that the morphology of the trail was consistent with ejection during the 2007 outburst and was made up of dust grains between 250 mu m and a few cm in radius. The trail mass was similar to 1.2-5.3 x 10(10) kg. C1 [Stevenson, R.; Bauer, J. M.; Mainzer, A. K.; Masiero, J. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bauer, J. M.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Kramer, E. A.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. [Grav, T.] Planetary Sci Inst, Tucson, AZ 85719 USA. RP Stevenson, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 183-427, Pasadena, CA 91109 USA. EM Rachel.A.Stevenson@jpl.nasa.gov OI Masiero, Joseph/0000-0003-2638-720X FU National Aeronautics and Space Administration; NASA Postdoctoral Fellowship Program; JPL Graduate Fellowship Program; NASA Earth and Space Sciences Fellowship program; NASA through the Near Earth Object Observations Program FX This publication makes use of data products from the Wide-field Infrared Survey Explorer and NEOWISE, 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. R. S. acknowledges support from the NASA Postdoctoral Fellowship Program. E. K. was supported by the JPL Graduate Fellowship Program and the NASA Earth and Space Sciences Fellowship program. This research was funded in part by a grant from NASA through the Near Earth Object Observations Program for the NEOWISE project, and was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 57 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 JUN 1 PY 2014 VL 787 IS 2 AR 116 DI 10.1088/0004-637X/787/2/116 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700021 ER PT J AU Tanaka, YT Stawarz, L Finke, J Cheung, CC Dermer, CD Kataoka, J Bamba, A Dubus, G De Naurois, M Wagner, SJ Fukazawa, Y Thompson, DJ AF Tanaka, Y. T. Stawarz, L. Finke, J. Cheung, C. C. Dermer, C. D. Kataoka, J. Bamba, A. Dubus, G. De Naurois, M. Wagner, S. J. Fukazawa, Y. Thompson, D. J. TI EXTREME BLAZARS STUDIED WITH FERMI-LAT AND SUZAKU: 1ES 0347-121 AND BLAZAR CANDIDATE HESS J1943+213 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: individual (HESS J1943+213, 1ES 0347-121); galaxies: active; galaxies: jets; gamma rays: galaxies; radiation mechanisms: non-thermal; X-rays: galaxies ID GAMMA-RAY EMISSION; BL LACERTAE OBJECT; INTERGALACTIC MAGNETIC-FIELD; LARGE-AREA TELESCOPE; EXTRAGALACTIC BACKGROUND LIGHT; SPECTRAL ENERGY-DISTRIBUTIONS; ACTIVE GALACTIC NUCLEI; MULTIWAVELENGTH OBSERVATIONS; TEV BLAZARS; INTEGRAL SOURCES AB We report on our study of high-energy properties of two peculiar TeV emitters: the "extreme blazar" 1ES 0347-121 and the "extreme blazar candidate" HESS J1943+213 located near the Galactic plane. Both objects are characterized by quiescent synchrotron emission with flat spectra extending up to the hard X-ray range, and both were reported to be missing GeV counterparts in the Fermi Large Area Telescope (LAT) two-year Source Catalog. We analyze a 4.5 yr accumulation of the Fermi-LAT data, resulting in the detection of 1ES 0347-121 in the GeV band, as well as in improved upper limits for HESS J1943+213. We also present the analysis results of newly acquired Suzaku data for HESS J1943+213. The X-ray spectrum is well represented by a single power law extending up to 25 keV with photon index 2.00 +/- 0.02 and a moderate absorption in excess of the Galactic value, which is in agreement with previous X-ray observations. No short-term X-ray variability was found over the 80 ks duration of the Suzaku exposure. Under the blazar hypothesis, we modeled the spectral energy distributions of 1ES 0347-121 and HESS J1943+213, and we derived constraints on the intergalactic magnetic field strength and source energetics. We conclude that although the classification of HESS J1943+213 has not yet been determined, the blazar hypothesis remains the most plausible option since, in particular, the broadband spectra of the two analyzed sources along with the source model parameters closely resemble each other, and the newly available Wide-field Infrared Survey Explorer and UKIRT Infrared Deep Sky Survey data for HESS J1943+213 are consistent with the presence of an elliptical host at the distance of approximately similar to 600 Mpc. C1 [Tanaka, Y. T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima 7398526, Japan. [Stawarz, L.] Inst Space & Astronaut Sci, JAXA, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Finke, J.; Cheung, C. C.; Dermer, C. D.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Bamba, A.] Aoyama Gakuin Univ, Dept Math & Phys, Sagamihara, Kanagawa 2525258, Japan. [Dubus, G.] UJF Grenoble 1 CNRS INSU, Inst Planetol & Astrophys Grenoble IPAG UMR 527, F-38041 Grenoble, France. [De Naurois, M.] Ecole Polytech, CNRS, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Wagner, S. J.] Heidelberg Univ, D-69117 Heidelberg, Germany. [Fukazawa, Y.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Tanaka, YT (reprint author), Hiroshima Univ, Hiroshima Astrophys Sci Ctr, 1-3-1 Kagamiyama, Higashihiroshima 7398526, Japan. EM ytanaka@hep01.hepl.hiroshima-u.ac.jp RI XRAY, SUZAKU/A-1808-2009; OI Dubus, Guillaume/0000-0002-5130-2514 FU Kakenhi [24840031]; Polish NSC grant [DEC-2012/04/A/ST9/00083]; NASA DPR [S-15633-Y] FX Y.T.T is supported by Kakenhi 24840031. L.S. was supported by Polish NSC grant DEC-2012/04/A/ST9/00083. Work by C.C.C. at NRL is supported in part by NASA DPR S-15633-Y. NR 66 TC 10 Z9 10 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 JUN 1 PY 2014 VL 787 IS 2 AR 155 DI 10.1088/0004-637X/787/2/155 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6ND UT WOS:000336246700060 ER PT J AU Scott, JM Hackney, K Downs, M Guined, J Ploutz-Snyder, R Fiedler, J Cunningham, D Ploutz-Snyder, L AF Scott, Jessica M. Hackney, Kyle Downs, Meghan Guined, Jamie Ploutz-Snyder, Robert Fiedler, James Cunningham, David Ploutz-Snyder, Lori TI The Metabolic Cost of an Integrated Exercise Program Performed During 14 Days of Bed Rest SO AVIATION SPACE AND ENVIRONMENTAL MEDICINE LA English DT Article DE disuse; energy expenditure; spaceflight; post-exercise oxygen consumption ID POSTEXERCISE OXYGEN-CONSUMPTION; INTERNATIONAL-SPACE-STATION; ENERGY-EXPENDITURE; MUSCLE; DURATION; FLIGHT; INACTIVITY; INTENSITY; SHUTTLE; BALANCE AB Background: Exercise countermeasures designed to mitigate muscle atrophy during long-duration spaceflight may not be as effective if crewmembers are in negative energy balance (energy output > energy input). This study determined the energy cost of supine exercise (resistance, interval, aerobic) during the spaceflight analogue of bed rest. Methods: Nine subjects (eight men and one woman; 34.5 +/- 8.2 yr) completed 14 d of bed rest and concomitant exercise countermeasures. Body mass and basal metabolic rate (BMR) were assessed before and during bed rest. Exercise energy expenditure was measured during and immediately after [excess post-exercise oxygen consumption (EPOC)] each of five different exercise protocols (30-s, 2-min, and 4-min intervals, continuous aerobic, and a variety of resistance exercises) during bed rest. Results: On days when resistance and continuous aerobic exercise were performed daily, energy expenditure was significantly greater (2879 +/- 280 kcal) than 2-min (2390 +/- 237 kcal), 30-s (2501 +/- 264 kcal), or 4-min (2546 +/- 264 kcal) exercise. There were no significant differences in BMR (pre-bed rest: 1649 +/- 216 kcal; week 1: 1632 +/- 174 kcal; week 2: 1657 +/- 176 kcal) or body mass (pre-bed rest: 75.2 +/- 10.1 kg; post-bed rest: 75.2 +/- 9.6 kg). Discussion: These findings highlight the importance of energy balance for long-duration crewmembers completing a high-intensity exercise program with multiple exercise sessions daily. C1 [Scott, Jessica M.; Ploutz-Snyder, Robert; Fiedler, James; Ploutz-Snyder, Lori] Univ Space Res Assoc, Houston, TX USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Scott, JM (reprint author), NASA, Lyndon B Johnson Space Ctr, Univ Space Res Assoc, 2101 NASA Pkwy,B261,SK3, Houston, TX 77058 USA. EM jessica.m.scott@nasa.gov FU National Aeronautics and Space Administration's Human Research Program; Canadian Natural Sciences and Engineering Post Doctoral Fellowship Program FX This study was funded by a grant from the National Aeronautics and Space Administration's Human Research Program. Additional support came from the Canadian Natural Sciences and Engineering Post Doctoral Fellowship Program. NR 29 TC 0 Z9 1 U1 0 U2 7 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 JUN PY 2014 VL 85 IS 6 BP 612 EP 617 DI 10.3357/ASEM.3772.2014 PG 6 WC Public, Environmental & Occupational Health; Medicine, General & Internal; Sport Sciences SC Public, Environmental & Occupational Health; General & Internal Medicine; Sport Sciences GA AH9QZ UT WOS:000336478200003 PM 24919381 ER PT J AU Baheru, T Chowdhury, AG Bitsuamlak, G Masters, FJ Tokay, A AF Baheru, Thomas Chowdhury, Arindam Gan Bitsuamlak, Girma Masters, Forrest J. Tokay, Ali TI Simulation of wind-driven rain associated with tropical storms and hurricanes using the 12-fan Wall of Wind SO BUILDING AND ENVIRONMENT LA English DT Article DE Low-rise building; Raindrop size distribution; Tropical cyclone rainfall; Wind-driven rain simulation; Wall of Wind ID DROP-SIZE DISTRIBUTIONS; BUILDING FACADES; CYCLONES; MODEL AB Wind-driven rain (WDR) is among the important environmental variables that affect the performance and durability of building enclosure systems. Although the need to investigate multi-level effects of WDR on building structures has increased through time, the available methods of investigation have been generally limited to field study and application of computational fluid dynamics. This paper investigates the parameters of tropical storm and hurricane-level WDR and presents a methodology of experimental simulation of WDR that may complement the two other investigation methods. Tropical cyclone WDR data acquired through National Aeronautics and Space Administrations' Tropical Rainfall Measuring Mission ground validation program were used to study the characteristics of tropical storm and hurricane-level WDR and derive the values of target parameters, which were later used in the experimental simulation process. Procedure for determination of target WDR rate, simulation of raindrop size distribution and its integral parameters, and selection of type and number of nozzles are discussed in detail. Similarity requirements and important scaling considerations of WDR simulation were addressed. The procedure was used to simulate WDR using the 12-fan Wall of Wind facility at Florida International University. The experimental simulation results demonstrated satisfactory representation of target rainfall intensity and raindrop size distribution in the test setup. The WDR simulation methodology presented herein may be used for simulation of WDR in testing facilities to evaluate water intrusion in buildings during tropical cyclones, develop solutions to promote functional longevity of building envelope, and enhance current simplified test protocols given in international standards. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Baheru, Thomas; Chowdhury, Arindam Gan] Florida Int Univ, Dept Civil & Environm Engn, Miami, FL 33199 USA. [Bitsuamlak, Girma] Univ Western Ontario, Dept Civil & Environm Engn, London, ON, Canada. [Masters, Forrest J.] Univ Florida, Dept Civil & Coastal Eng, Gainesville, FL USA. [Tokay, Ali] Univ Maryland, Joint Ctr Earth Syst Technol, Baltimore, MD 21201 USA. [Tokay, Ali] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Chowdhury, AG (reprint author), Florida Int Univ, Dept Civil & Environm Engn, Miami, FL 33199 USA. EM chowdhur@fiu.edu RI Masters, Forrest/D-1287-2011 OI Masters, Forrest/0000-0001-8203-9846 FU National Science Foundation (NSF) [CMMI-1234004]; National Science Foundation (NSF MRI) [CMMI-0923365]; Florida Sea Grant College Program (FSGCP) [R/C-D-19] FX We acknowledge the National Science Foundation (NSF Award No.: CMMI-1234004 and NSF MRI Award No.: CMMI-0923365) for supporting the simulation of the wind driven rain. We also acknowledge the Florida Sea Grant College Program (FSGCP, Grant No.: R/C-D-19) for supporting the Wall of Wind research related to water intrusion. Wall of Wind facility construction has been supported by the Florida Center of Excellence in Hurricane Damage Mitigation and Product Development. The findings presented in this paper, however, are those of the authors alone and do not necessarily represent the views of sponsoring agencies. We thank Dr. Tokay Ali, NASA Goddard Space Flight Center, Greenbelt, Maryland for providing RSD data collected during hurricane. Dr. Forrest Masters of University of Florida provided the PIP instrument used to measure simulated wind-driven rain. The authors are grateful to the American Architectural Manufacturers Association (AAMA) for purchasing the sensor. NR 40 TC 2 Z9 2 U1 2 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0360-1323 EI 1873-684X J9 BUILD ENVIRON JI Build. Environ. PD JUN PY 2014 VL 76 BP 18 EP 29 DI 10.1016/j.buildenv.2014.03.002 PG 12 WC Construction & Building Technology; Engineering, Environmental; Engineering, Civil SC Construction & Building Technology; Engineering GA AH8BQ UT WOS:000336359500003 ER PT J AU Walker, RT Parizek, BR Alley, RB Brunt, KM Anandakrishnan, S AF Walker, Ryan T. Parizek, Byron R. Alley, Richard B. Brunt, Kelly M. Anandakrishnan, Sridhar TI Ice-shelf flexure and tidal forcing of Bindschadler Ice Stream, West Antarctica SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE ice shelf; ice stream; ocean tides; viscoelastic ID GROUNDING ZONE; LASER ALTIMETRY; FLOW; DYNAMICS; INSAR; MODEL; TIDES; MODIS AB Viscoelastic models of ice-shelf flexure and ice-stream velocity perturbations are combined into a single efficient flowline model to study tidal forcing of grounded ice. The magnitude and timing of ice-stream response to tidally driven changes in hydrostatic pressure and/or basal drag are found to depend significantly on bed rheology, with only a perfectly plastic bed allowing instantaneous velocity response at the grounding line. The model can reasonably reproduce GPS observations near the grounding zone of Bindschadler Ice Stream (formerly Ice Stream D) on semidiurnal time scales; however, other forcings such as tidally driven ice-shelf slope transverse to the flowline and flexurally driven till deformation must also be considered if diurnal motion is to be matched. (C) 2014 Elsevier B.V. All rights reserved. C1 [Walker, Ryan T.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Parizek, Byron R.] Penn State DuBois, Du Bois, PA 15801 USA. [Alley, Richard B.; Anandakrishnan, Sridhar] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Brunt, Kelly M.] Goddard Earth Sci Technol & Res GESTAR, Houston, TX USA. [Walker, Ryan T.; Brunt, Kelly M.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA. RP Walker, RT (reprint author), NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Mail Code 615,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. EM ryan.t.walker@nasa.gov FU NSF [0424589, 1338832, 0944286]; NASA [NNX10AI04G, NNX12AD03A, NNX12AP50G]; NASA Science Innovation Fund FX This research was supported by NSF under grants 0424589 (R.B.A., B.R.P.), 1338832 (R.B.A., B.R.P.), and 0944286 (R.B.A.), and by NASA under grants NNX10AI04G (R.B.A., B.R.P., R.T.W.), NNX12AD03A (R.T.W.), NNX12AP50G (R.T.W.), and the NASA Science Innovation Fund (K.M.B.). NR 39 TC 4 Z9 4 U1 2 U2 18 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 JUN 1 PY 2014 VL 395 BP 184 EP 193 DI 10.1016/j.epsl.2014.03.049 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AH4PK UT WOS:000336110300018 ER PT J AU Bryan, DR Bosley, KL Hicks, AC Haltuch, MA Wakefield, WW AF Bryan, David R. Bosley, Keith L. Hicks, Allan C. Haltuch, Melissa A. Wakefield, W. Waldo TI Quantitative video analysis of flatfish herding behavior and impact on effective area swept of a survey trawl SO FISHERIES RESEARCH LA English DT Article DE Area swept; Flatfish; Herding behavior; Trawl surveys; Video-analysis ID CAPTURE EFFICIENCY; BRIDLE EFFICIENCY; GROUNDFISH; LENGTH; GEAR AB Uncertainty in fish behavior can introduce bias into density calculations from fishery-independent bottom trawl surveys that provide relative abundance estimates and population trends for stock assessments. In situ video was used to quantify flatfish behavioral responses to a bottom trawl sweep to improve the understanding of survey and assessment results. The behavior of 632 flatfishes was recorded during four tows. More than 90% of fish were observed in a perpendicular orientation away from the sweeps indicating a herding response. There was no significant effect of fish length on fish orientation or whether it reacted or remained stationary during the observation. Only 1.3% of fish were observed escaping the sweeps. A generalized linear model was used to estimate that at a distance of 73.8 cm (+/- 3.4 SE) 50% of observed fish reacted to the sweep. The mean distance that stationary fish were first observed reacting to the sweep was 36.6 cm (+/- 2.0 SE). Quantitative analysis indicates that flatfish herding occurs along trawl sweeps and the effective area swept is greater than the wing spread. Thus, the use of wing spread to calculate relative abundance estimates explains bias in stock assessment estimates of survey catchability that are greater than expected. (C) 2014 Elsevier B.V. All rights reserved. C1 [Bryan, David R.; Hicks, Allan C.; Haltuch, Melissa A.] NOAA, Fishery Resource Anal & Monitoring Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Seattle, WA 98112 USA. [Bosley, Keith L.; Wakefield, W. Waldo] Natl Ocean & Atmospher Adm, Fishery Resource Anal & Monitoring Div, NW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA. RP Bryan, DR (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, 4600 Rickenbacker Causeway, Miami, FL 33149 USA. EM dbryan@rsmas.miami.edu NR 29 TC 5 Z9 5 U1 0 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-7836 EI 1872-6763 J9 FISH RES JI Fish Res. PD JUN PY 2014 VL 154 BP 120 EP 126 DI 10.1016/j.fishres.2014.02.007 PG 7 WC Fisheries SC Fisheries GA AH4RZ UT WOS:000336117000012 ER PT J AU Lang, TF Saeed, IH Streeper, T Carballido-Gamio, J Harnish, RJ Frassetto, LA Lee, SMC Sibonga, JD Keyak, JH Spiering, BA Grodsinsky, CM Bloomberg, JJ Cavanagh, PR AF Lang, Thomas F. Saeed, Isra H. Streeper, Timothy Carballido-Gamio, Julio Harnish, Roy J. Frassetto, Lynda A. Lee, Stuart M. C. Sibonga, Jean D. Keyak, Joyce H. Spiering, Barry A. Grodsinsky, Carlos M. Bloomberg, Jacob J. Cavanagh, Peter R. TI Spatial Heterogeneity in the Response of the Proximal Femur to Two Lower-Body Resistance Exercise Regimens SO JOURNAL OF BONE AND MINERAL RESEARCH LA English DT Article DE RESISTANCE EXERCISE; BONE DENSITY; MUSCLE ATTENUATION; BONE STRENGTH; QUANTITATIVE COMPUTED TOMOGRAPHY; FINITE ELEMENT MODELING ID LONG-DURATION SPACEFLIGHT; HIP FRACTURE; BONE MASS; COMPUTED-TOMOGRAPHY; FEMORAL STRENGTH; OLDER-ADULTS; WOMEN; OSTEOPOROSES; ASSOCIATION; RISK AB Understanding the skeletal effects of resistance exercise involves delineating the spatially heterogeneous response of bone to load distributions from different muscle contractions. Bone mineral density (BMD) analyses may obscure these patterns by averaging data from tissues with variable mechanoresponse. To assess the proximal femoral response to resistance exercise, we acquired pretraining and posttraining quantitative computed tomography (QCT) images in 22 subjects (25-55 years, 9 males, 13 females) performing two resistance exercises for 16 weeks. One group (SQDL, n=7) performed 4 sets each of squats and deadlifts, a second group (ABADD, n=8) performed 4 sets each of standing hip abductions and adductions, and a third group (COMBO, n=7) performed two sets each of squat/deadlift and abduction/adduction exercise. Subjects exercised three times weekly, and the load was adjusted each session to maximum effort. We used voxel-based morphometry (VBM) to visualize BMD distributions. Hip strength computations used finite element modeling (FEM) with stance and fall loading conditions. We used QCT analysis for cortical and trabecular BMD, and cortical tissue volume. For muscle size and density, we analyzed the cross-sectional area (CSA) and mean Hounsfield unit (HU) in the hip extensor, flexor, abductor, and adductor muscle groups. Whereas SQDL increased vertebral BMD, femoral neck cortical BMD and volume, and stance hip strength, ABADD increased trochanteric cortical volume. The COMBO group showed no changes in any parameter. VBM showed different effects of ABADD and SQDL exercise, with the former causing focal changes of trochanteric cortical bone, and the latter showing diffuse changes in the femoral neck and head. ABADD exercise increased adductor CSA and HU, whereas SQDL exercise increased the hip extensor CSA and HU. In conclusion, we observed different proximal femoral bone and muscle tissue responses to SQDL and ABADD exercise. This study supports VBM and volumetric QCT (vQCT) to quantify the spatially heterogeneous effects of types of muscle contractions on bone. (c) 2014 American Society for Bone and Mineral Research. C1 [Lang, Thomas F.; Saeed, Isra H.; Streeper, Timothy; Carballido-Gamio, Julio; Harnish, Roy J.; Frassetto, Lynda A.] Univ Calif San Francisco, San Francisco, CA 94143 USA. [Lee, Stuart M. C.; Spiering, Barry A.] Wyle Sci Technol & Engn Grp, Houston, TX USA. [Sibonga, Jean D.; Bloomberg, Jacob J.] NASA, Johnson Spaceflight Ctr, Houston, TX USA. [Keyak, Joyce H.] Univ Calif Irvine, Dept Radiol Sci, Irvine, CA 92717 USA. [Keyak, Joyce H.] Univ Calif Irvine, Dept Biomed Engn, Irvine, CA USA. [Keyak, Joyce H.] Univ Calif Irvine, Dept Mech & Aerosp Engn, Irvine, CA 92717 USA. [Grodsinsky, Carlos M.] Zin Technol, Cleveland, OH USA. [Cavanagh, Peter R.] Univ Washington, Dept Orthopaed Surg & Sports Med, Seattle, WA 98195 USA. RP Lang, TF (reprint author), Univ Calif San Francisco, 185 Berry St,Suite 350, San Francisco, CA 94143 USA. EM Thomas.Lang@ucsf.edu OI Lang, Thomas/0000-0002-3720-8038 FU National Space Biomedical Research Grant [BL-01301]; National Institute on Aging [R01-AG-28832, R01-AG-29571] FX This work was supported by the National Space Biomedical Research Grant BL-01301 and the National Institute on Aging Grants R01-AG-28832 and R01-AG-29571. NR 27 TC 7 Z9 7 U1 2 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0884-0431 EI 1523-4681 J9 J BONE MINER RES JI J. Bone Miner. Res. PD JUN PY 2014 VL 29 IS 6 BP 1337 EP 1345 DI 10.1002/jbmr.2155 PG 9 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA AH3DJ UT WOS:000336001500004 PM 24293094 ER PT J AU Sanchez, HD Bongiovanni, A Lara-Lopez, MA Oteo, I Cepa, J Garcia, AMP Sanchez-Portal, M Ederoclite, A Lutz, D Cresci, G Delvecchio, I Berta, S Magnelli, B Popesso, P Pozzi, F Riguccini, L AF Dominguez Sanchez, H. Bongiovanni, A. Lara-Lopez, M. A. Oteo, I. Cepa, J. Perez Garcia, A. M. Sanchez-Portal, M. Ederoclite, A. Lutz, D. Cresci, G. Delvecchio, I. Berta, S. Magnelli, B. Popesso, P. Pozzi, F. Riguccini, L. TI Herschel far-IR counterparts of SDSS galaxies: analysis of commonly used star formation rate estimates SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: fundamental parameters; galaxies: star formation; infrared: galaxies ID SPECTRAL ENERGY-DISTRIBUTIONS; FORMATION RATE INDICATORS; EVOLUTION SURVEY COSMOS; DIGITAL SKY SURVEY; SIMILAR-TO 3; FORMING GALAXIES; DUST ATTENUATION; HIGH-REDSHIFT; H-ALPHA; SPECTROSCOPIC SAMPLE AB We study a hundred of galaxies from the spectroscopic Sloan Digital Sky Survey (SDSS) with individual detections in the far-infrared Herschel Photodetector Array Camera and Spectrometer bands (100 or 160 mu m) and in the GALEX far-ultraviolet band up to z similar to 0.4 in the COSMOS and Lockman Hole fields. The galaxies are divided into four spectral and four morphological types. For the star-forming and unclassifiable galaxies, we calculate dust extinctions from the ultraviolet (UV) slope, the H alpha/H beta ratio and the L-IR/L-UV ratio. There is a tight correlation between the dust extinction and both L-IR and metallicity. We calculate SFRtotal and compare it with other star formation rate (SFR) estimates (H alpha, UV, SDSS) finding very good agreement between them with smaller dispersions than typical SFR uncertainties. We study the effect of mass and metallicity, finding that it is only significant at high masses for SFRH alpha. For the AGN and composite galaxies, we find a tight correlation between SFR and LIR (sigma similar to 0.29), while the dispersion in the SFR-L-UV relation is larger (sigma similar to 0.57). The galaxies follow the prescriptions of the Fundamental Plane in the M-Z-SFR space. C1 [Dominguez Sanchez, H.; Bongiovanni, A.; Oteo, I.; Cepa, J.; Perez Garcia, A. M.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain. [Dominguez Sanchez, H.] CSIC INTA, Ctr Astrobiol, Dept Astrofis, E-28850 Madrid, Spain. [Dominguez Sanchez, H.; Bongiovanni, A.; Oteo, I.; Cepa, J.; Perez Garcia, A. M.] Univ La Laguna, Dept Astrofis, E-38205 San Cristobal la Laguna, Spain. [Lara-Lopez, M. A.] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Sanchez-Portal, M.] INSA ESAC, Herschel Sci Ctr, E-28692 Madrid, Spain. [Ederoclite, A.] Ctr Estudios Fis Cosmos Aragon, E-44001 Teruel, Spain. [Lutz, D.; Berta, S.; Magnelli, B.; Popesso, P.] MPE, D-85741 Garching, Germany. [Cresci, G.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Delvecchio, I.; Pozzi, F.] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy. [Riguccini, L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Riguccini, L.] BAER Inst, Sonoma, CA 95476 USA. RP Sanchez, HD (reprint author), Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain. EM helena@iac.es OI Cresci, Giovanni/0000-0002-5281-1417; Delvecchio, Ivan/0000-0001-8706-2252 FU Spanish Ministry of Economy and Competitiveness (MINECO) [AYA2011-29517-C03-01]; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX The authors would like to thank the referee for the useful comments that helped to improve the clarity of this paper. This work was supported by the Spanish Ministry of Economy and Competitiveness (MINECO) under grant AYA2011-29517-C03-01. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This work uses Sloan Digital Sky Survey (SDSS) data. Funding for the SDSS and SDSS-II was 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 Monbukagakusho, the Max Planck Society and the Higher Education Funding Council for England. The SDSS was managed by the Astrophysical Research Consortium for the Participating Institutions. GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. The authors gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. HD would like to thank J. Vega for technical support. NR 110 TC 9 Z9 9 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2014 VL 441 IS 1 BP 2 EP 23 DI 10.1093/mnras/stu503 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6OC UT WOS:000336249300001 ER PT J AU Stacy, A Pawlik, AH Bromm, V Loeb, A AF Stacy, Athena Pawlik, Andreas H. Bromm, Volker Loeb, Abraham TI The mutual interaction between Population III stars and self-annihilating dark matter SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: formation; galaxies: formation; cosmology: theory; early Universe ID 1ST STARS; EARLY UNIVERSE; PRIMORDIAL PROTOSTARS; PROTOSTELLAR FEEDBACK; MOLECULAR-HYDROGEN; GALACTIC HALOS; BLACK-HOLES; LAMBDA-CDM; FRAGMENTATION; EVOLUTION AB We use cosmological simulations of high-redshift minihaloes to investigate the effect of dark matter annihilation (DMA) on the collapse of primordial gas. We numerically investigate the evolution of the gas as it assembles in a Population III stellar disc. We find that when DMA effects are neglected, the disc undergoes multiple fragmentation events beginning at similar to 500 yr after the appearance of the first protostar. On the other hand, DMA heating and ionization of the gas speeds the initial collapse of gas to protostellar densities and also affects the stability of the developing disc against fragmentation, depending on the DM distribution. We compare the evolution when we model the DM density with an analytical DM profile which remains centrally peaked, and when we simulate the DM profile using N-body particles (the 'live' DM halo). When utilizing the analytical DM profile, DMA suppresses disc fragmentation for similar to 3500 yr after the first protostar forms, in agreement with earlier work. However, when using a 'live' DM halo, the central DM density peak is gradually flattened due to the mutual interaction between the DM and the rotating gaseous disc, reducing the effects of DMA on the gas, and enabling secondary protostars of mass similar to 1M(circle dot) to be formed within similar to 900 yr. These simulations demonstrate that DMA is ineffective in suppressing gas collapse and subsequent fragmentation, rendering the formation of long-lived dark stars unlikely. However, DMA effects may still be significant in the early collapse and disc formation phase of primordial gas evolution. C1 [Stacy, Athena] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Stacy, Athena] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pawlik, Andreas H.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Bromm, Volker] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Bromm, Volker] Univ Texas Austin, Texas Cosmol Ctr, Austin, TX 78712 USA. [Loeb, Abraham] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. RP Stacy, A (reprint author), Univ Calif Berkeley, Berkeley, CA 94720 USA. EM athena.stacy@berkeley.edu FU European Union [301096-proFeSsoR]; NSF [AST-1009928]; NASA ATFP grant [NNX09AJ33G] FX AS is grateful to John Mather for helpful comments and discussion. The authors thank Simon Glover for helpful comments. 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 and the Texas Advanced Computing Center (TACC). AHP receives funding from the European Union's Seventh Framework Programme (FP7/2007-2013) under grant agreement number 301096-proFeSsoR. VB acknowledges support from NSF grant AST-1009928 and NASA ATFP grant NNX09AJ33G. NR 74 TC 5 Z9 5 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2014 VL 441 IS 1 BP 822 EP 836 DI 10.1093/mnras/stu621 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6OC UT WOS:000336249300065 ER PT J AU McKernan, B Ford, KES Kocsis, B Lyra, W Winter, LM AF McKernan, B. Ford, K. E. S. Kocsis, B. Lyra, W. Winter, L. M. TI Intermediate- mass black holes in AGN discs - II. Model predictions and observational constraints SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion accretion discs; planets and satellites: formation; planet-disc interactions; protoplanetary discs; galaxies: active; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; COMPACT BINARY INSPIRALS; WAVE STANDARD SIRENS; X-RAY-EMISSION; GAS PILE-UP; PROTOPLANETARY DISKS; GLOBULAR-CLUSTERS; ACCRETION DISK; GRAVITATIONAL-RADIATION; NUMERICAL SIMULATIONS AB If intermediate-mass black holes (IMBHs) grow efficiently in gas discs around supermassive black holes, their host active galactic nucleus (AGN) discs should exhibit myriad observational signatures. Gap-opening IMBHs in AGN discs can exhibit spectral features and variability analogous to gapped protoplanetary discs. Agap-opening IMBH in the innermost disc imprints ripples and oscillations on the broad Fe K alpha line which may be detectable with future X-ray missions. A non-gap-opening IMBH will accrete and produce a soft X-ray excess relative to continuum emission. An IMBH on a retrograde orbit in an AGN disc will not open a gap and will generate soft X-rays from a bow-shock 'headwind'. Accreting IMBH in a large cavity can generate ULX-like X-ray luminosities and LINER-like optical line ratios from local ionized gas. We propose that many LINERs house a weakly accreting MBH binary in a large central disc cavity and will be luminous sources of gravitational waves (GW). IMBHs in galactic nuclei may also be detected via intermittent observational signatures including: UV/X-ray flares due to tidal disruption events, asymmetric X-ray intensity distributions as revealed by AGN transits, quasi-periodic oscillations and underluminous Type Ia supernovae. GW emitted during IMBH inspiral and collisions may be detected with eLISA and LIGO, particularly from LINERs. We summarize observational signatures and compare to current data where possible or suggest future observations. C1 [McKernan, B.; Ford, K. E. S.] CUNY, Dept Sci, Borough Manhattan Community Coll, New York, NY 10007 USA. [McKernan, B.; Ford, K. E. S.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [McKernan, B.; Ford, K. E. S.] CUNY, Grad Ctr, New York, NY 10016 USA. [McKernan, B.; Ford, K. E. S.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Kocsis, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kocsis, B.] Inst Adv Study, Princeton, NJ 08540 USA. [Lyra, W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lyra, W.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Winter, L. M.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80303 USA. RP McKernan, B (reprint author), CUNY, Dept Sci, Borough Manhattan Community Coll, New York, NY 10007 USA. EM bmckernan@amnh.org RI Kocsis, Bence/C-3061-2013 OI Kocsis, Bence/0000-0002-4865-7517 FU NSF PAARE [AST-1153335]; W.M. Keck Foundation Fund of the Institute for Advanced Study; NASA [NNX11AF29G]; National Science Foundation [AST10-09802]; NASA through the Sagan Fellowship Program; [NASA-APRA08-0117] FX We thank the referee for a report that helped us condense and focus this paper. We acknowledge very useful discussions with Tahir Yaqoob, Stephan Rosswog, Zoltan Haiman, Ari Laor, Hagai Perets, Kayhan Gultekin and Mordecai Mac Low. BM and KESF acknowledge support from NASA-APRA08-0117 and NSF PAARE AST-1153335. BK was supported in part by the W.M. Keck Foundation Fund of the Institute for Advanced Study and NASA grant NNX11AF29G. WL acknowledges support by the National Science Foundation under grant no. AST10-09802. 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. NR 99 TC 6 Z9 6 U1 0 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2014 VL 441 IS 1 BP 900 EP 909 DI 10.1093/mnras/stu553 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6OC UT WOS:000336249300070 ER PT J AU Ramiaramanantsoa, T Moffat, AFJ Chene, AN Richardson, ND Henrichs, HF Desforges, S Antoci, V Rowe, JF Matthews, JM Kuschnig, R Weiss, WW Sasselov, D Rucinski, SM Guenther, DB AF Ramiaramanantsoa, Tahina Moffat, Anthony F. J. Chene, Andre-Nicolas Richardson, Noel D. Henrichs, Huib F. Desforges, Sebastien Antoci, Victoria Rowe, Jason F. Matthews, Jaymie M. Kuschnig, Rainer Weiss, Werner W. Sasselov, Dimitar Rucinski, Slavek M. Guenther, David B. TI MOST detects corotating bright spots on the mid-O-type giant xi Persei SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; stars: massive; stars: rotation; starspots ID IUE MEGA CAMPAIGN; EARLY-TYPE STARS; SHORT-TERM VARIABILITY; BETA-CEPHEI STARS; WIND VARIABILITY; MASSIVE STARS; INTERACTION REGIONS; STELLAR WINDS; MAIN-SEQUENCE; PHOTOMETRY AB We have used the MOST (Microvariability and Oscillations of STars) microsatellite to obtain four weeks of contiguous high-precision broad-band visual photometry of the O7.5III(n)((f)) star xi Persei in 2011 November. This star is well known from previous work to show prominent DACs (discrete absorption components) on time-scales of about 2 d from UV spectroscopy and non-radial pulsation with one (l = 3) p-mode oscillation with a period of 3.5 h from optical spectroscopy. Our MOST-orbit (101.4min) binned photometry fails to reveal any periodic light variations above the 0.1 mmag 3 sigma noise level for periods of a few hours, while several prominent Fourier peaks emerge at the 1 mmag level in the two-day period range. These longer period variations are unlikely due to pulsations, including gravity modes. From our simulations based upon a simple spot model, we deduce that we are seeing the photometric modulation of several corotating bright spots on the stellar surface. In our model, the starting times (random) and lifetimes (up to several rotations) vary from one spot to another yet all spots rotate at the same period of 4.18 d, the best-estimated rotation period of the star. This is the first convincing reported case of corotating bright spots on an O star, with important implications for drivers of the DACs (resulting from corotating interaction regions) with possible bright-spot generation via a breakout at the surface of a global magnetic field generated by a subsurface convection zone. C1 [Ramiaramanantsoa, Tahina; Moffat, Anthony F. J.; Richardson, Noel D.; Desforges, Sebastien] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Chene, Andre-Nicolas] Northern Operat Ctr, Gemini Observ, Hilo, HI 96720 USA. [Chene, Andre-Nicolas] Univ Valparaiso, Dept Fis & Astron, Playa Ancha, Chile. [Chene, Andre-Nicolas] Univ Concepcion, Dept Astron, Concepcion, Chile. [Henrichs, Huib F.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Antoci, Victoria] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Matthews, Jaymie M.; Kuschnig, Rainer] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rucinski, Slavek M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Guenther, David B.] St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada. RP Ramiaramanantsoa, T (reprint author), Univ Montreal, Dept Phys, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada. EM tahina@astro.umontreal.ca FU NSERC (Canada); FQRNT (Quebec); Chilean Centro de Astrofisica FONDAP [15010003]; Chilean Centro de Excelencia en Astrofisica y Tecnologias Afines (CATA); Comite Mixto ESO-Gobierno de Chile; GEMINI-CONICYT [32110005]; Danish National Research Foundation; ASTERISK project; European Research Council [267864]; Austrian Space Agency; Austrian Science Fund; CRAQ (Centre de Recherche en Astrophysique du Quebec) FX We gratefully acknowledge useful conversations with Paul Charbonneau, Nicole St-Louis, Stan Owocki and, Alex Fullerton in relation to this project. DBG, JMM, AFJM, and SMR are supported by NSERC (Canada), with additional support to AFJM from FQRNT (Quebec). ANC gratefully acknowledges support from the Chilean Centro de Astrofisica FONDAP no. 15010003 and the Chilean Centro de Excelencia en Astrofisica y Tecnologias Afines (CATA). ANC also received support from the Comite Mixto ESO-Gobierno de Chile and GEMINI-CONICYT no. 32110005. VA acknowledges the Stellar Astrophysics Centre (SAC) funded by the Danish National Research Foundation. VA also received support from the ASTERISK project (ASTERoseismic Investigations with SONG and Kelper) funded by the European Research Council (Grant agreement no.: 267864). RK and WWW are supported by the Austrian Space Agency and the Austrian Science Fund. NDR acknowledges his CRAQ (Centre de Recherche en Astrophysique du Quebec) fellowship. NR 68 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 JUN PY 2014 VL 441 IS 1 BP 910 EP 917 DI 10.1093/mnras/stu619 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6OC UT WOS:000336249300071 ER PT J AU Swinyard, BM Polehampton, ET Hopwood, R Valtchanov, I Lu, N Fulton, T Benielli, D Imhof, P Marchili, N Baluteau, JP Bendo, GJ Ferlet, M Griffin, MJ Lim, TL Makiwa, G Naylor, DA Orton, GS Papageorgiou, A Pearson, CP Schulz, B Sidher, SD Spencer, LD van der Wiel, MHD Wu, R AF Swinyard, B. M. Polehampton, E. T. Hopwood, R. Valtchanov, I. Lu, N. Fulton, T. Benielli, D. Imhof, P. Marchili, N. Baluteau, J. -P. Bendo, G. J. Ferlet, M. Griffin, M. J. Lim, T. L. Makiwa, G. Naylor, D. A. Orton, G. S. Papageorgiou, A. Pearson, C. P. Schulz, B. Sidher, S. D. Spencer, L. D. van der Wiel, M. H. D. Wu, R. TI Calibration of the Herschel SPIRE Fourier Transform Spectrometer SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE instrumentation: spectrographs; space vehicles: instruments; techniques: spectroscopic ID BRIGHTNESS TEMPERATURE SPECTRA; CIRCUMSTELLAR ENVELOPES; NEAR-MILLIMETER; THERMAL INERTIA; INSTRUMENT; URANUS; MARS; SPECTROSCOPY; PERFORMANCE; WAVELENGTHS AB The Herschel Spectral and Photometric REceiver (SPIRE) instrument consists of an imaging photometric camera and an imaging Fourier Transform Spectrometer (FTS), both operating over a frequency range of similar to 450-1550 GHz. In this paper, we briefly review the FTS design, operation, and data reduction, and describe in detail the approach taken to relative calibration (removal of instrument signatures) and absolute calibration against standard astronomical sources. The calibration scheme assumes a spatially extended source and uses the Herschel telescope as primary calibrator. Conversion from extended to point-source calibration is carried out using observations of the planet Uranus. The model of the telescope emission is shown to be accurate to within 6 per cent and repeatable to better than 0.06 per cent and, by comparison with models of Mars and Neptune, the Uranus model is shown to be accurate to within 3 per cent. Multiple observations of a number of point-like sources show that the repeatability of the calibration is better than 1 per cent, if the effects of the satellite absolute pointing error (APE) are corrected. The satellite APE leads to a decrement in the derived flux, which can be up to similar to 10 per cent (1 sigma) at the high-frequency end of the SPIRE range in the first part of the mission, and similar to 4 per cent after Herschel operational day 1011. The lower frequency range of the SPIRE band is unaffected by this pointing error due to the larger beam size. Overall, for well-pointed, point-like sources, the absolute flux calibration is better than 6 per cent, and for extended sources where mapping is required it is better than 7 per cent. C1 [Swinyard, B. M.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Swinyard, B. M.; Polehampton, E. T.; Ferlet, M.; Lim, T. L.; Pearson, C. P.; Sidher, S. D.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England. [Polehampton, E. T.; Fulton, T.; Imhof, P.; Makiwa, G.; Naylor, D. A.; van der Wiel, M. H. D.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1J 1B1, Canada. [Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England. [Valtchanov, I.] ESA, European Space Astron Ctr, Herschel Sci Ctr, E-28691 Villanueva De La Canada, Spain. [Lu, N.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Fulton, T.; Imhof, P.; Schulz, B.] Blue Sky Spect, Lethbridge, AB T1J 0N9, Canada. [Benielli, D.; Baluteau, J. -P.] Univ Aix Marseille, LAM, F-13388 Marseille 13, France. [Benielli, D.; Baluteau, J. -P.] CNRS, UMR7326, F-13388 Marseille 13, France. [Marchili, N.] Univ Padua, Dipartimento Fis & Astron, I-35131 Padua, Italy. [Bendo, G. J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, UK ALMA Reg Ctr Node, Manchester M13 9PL, Lancs, England. [Griffin, M. J.; Papageorgiou, A.; Spencer, L. D.] Cardiff Univ, Sch Phys & Astron, The Parade CF24 3AA, Wales. [Orton, G. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Pearson, C. P.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Wu, R.] CEA Saclay, Serv Astrophys, Lab AIM, CEA DSM,CNRS,Irfu, F-91191 Gif Sur Yvette, France. RP Swinyard, BM (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM bruce.swinyard@stfc.ac.uk RI van der Wiel, Matthijs/M-4531-2014 OI van der Wiel, Matthijs/0000-0002-4325-3011 FU CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA); ASI fellowship [I/005/11/0] FX SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA).; NM is funded by an ASI fellowship under contract number I/005/11/0. NR 48 TC 23 Z9 23 U1 0 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2014 VL 440 IS 4 BP 3658 EP 3674 DI 10.1093/mnras/stu409 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AH6AT UT WOS:000336213800058 ER EF